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Thread: HUBBLE UPDATES

  1. #1
    StarLab Guest
    HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science


    DAILY REPORT # 3833


    PERIOD COVERED: DOY 96


    OBSERVATIONS SCHEDULED


    ACS/HRC 10431


    A Search for Faint Companions of Altair


    We propose to use the innovative new technique of spectral
    deconvolution {Sparks & Ford 2002} to search for very faint
    companions, possibly extrasolar planets shining by reflected light,
    around Altair, the nearest bright, single star to the Sun. The
    technique offers a Poisson-limited detection capability that brings
    Jovian-class planets into the realm of feasibility for a select few
    stars. We turn the wavelength dependence of the coronagraphic PSF to
    advantage and use it to eliminate stray light from the host star. As
    part of the detection process, we obtain a spectrum over the
    wavelength range, 750 nm to 1 micron, with 9% resolution. The search
    will be orders of magnitude more sensitive than all previous efforts
    and should take us to within about an order of magnitude of the Jovian
    luminosity flux limit.


    ACS/HRC/WFC 10389


    ACS CCDs daily monitor - Cycle 13 - Part 2


    This program consists of a set of basic tests to monitor, the read
    noise, the development of hot pixels and test for any source of noise
    in ACS CCD detectors. The files, biases and dark will be used to
    create reference files for science calibration. This programme will be
    for the entire lifetime of ACS.


    ACS/HRC/WFC/WFPC2 10384


    Focus Monitor


    The focus of HST is measured from WFPC2/PC and ACS/HRC images of
    stars. Multiple exposures are taken in parallel over an orbit to
    determine the influence of breathing on the derived mean focus.
    Observations are taken of clusters with suitable orientations to
    ensure stars appear in all fields.


    ACS/WFC/NIC/NIC3/WFPC 10246 2 The HST survey of the Orion Nebula
    Cluster


    We propose a Treasury Program of 104 HST orbits to perform the
    definitive study of the Orion Nebula Cluster, the Rosetta stone of
    star formation. We will cover with unprecedented sensitivity {23-25
    mag}, dynamic range {~12 mag}, spatial resolution {50mas}, and
    simultaneous spectral coverage {5 bands} a ~450 square arcmin field
    centered on the Trapezium stars. This represents a tremendous gain
    over the shallow WFC1 study made in 1991 with the aberrated HST on an
    area ~15 times smaller. We maximize the HST observing efficiency using
    ACS/WFC and WFPC2 in parallel with two opposite roll angles, to cover
    the same total field. We will assemble the richest, most accurate and
    unbiased HR diagram for pre-main-sequence objects ever made. Combined
    with the optical spectroscopy already available for ~1000 sources and
    new deep near-IR imaging and spectroscopy {that we propose as Joint
    HST-NOAO observations}, we will be able to attack and possibly solve
    the most compelling questions on stellar evolution: the calibration of
    pre-main-sequence evolutionary tracks, mass segration and the
    variation of the initial mass function in different environments, the
    evolution of mass accretion rates vs. age and environment, disk
    dissipation in environments dominated by hard vs. soft-UV radiation,
    stellar multiplicity vs. disk fraction. In addition, we expect to
    discover and classify an unknown, but substantial, population of
    pre-Main Sequence binaries, low mass stars and brown dwarfs down to
    ~10 MJup. This is also the best possible way to discover dark
    silhouette disks in the outskirts of the Orion Nebula and study their
    evolutionary status through multicolor imaging. This program is timely
    and extremely well leveraged to other programs targeting Orion: the
    ACS H-alpha survey of the Orion Nebula, the recently completed 850ks
    ultradeep Chandra survey, the large GTO programs to be performed with
    SIRTF, plus the availability of 2MASS and various deep JHK surveys of
    the core recently done with 8m class telescopes.


    NIC1/NIC2/NIC3 8792


    NICMOS Post-SAA calibration - CR Persistence Part 3


    A new procedure proposed to alleviate the CR-persistence problem of
    NICMOS. Dark frames will be obtained immediately upon exiting the SAA
    contour 23, and every time a NICMOS exposure is scheduled within 50
    minutes of coming out of the SAA. The darks will be obtained in
    parallel in all three NICMOS Cameras. The POST-SAA darks will be
    non-standard reference files available to users with a USEAFTER
    date/time mark. The keyword 'USEAFTER=date/time' will also be added to
    the header of each POST-SAA DARK frame. The keyword must be populated
    with the time, in addition to the date, because HST crosses the SAA ~8
    times per day so each POST-SAA DARK will need to have the appropriate
    time specified, for users to identify the ones they need. Both the raw
    and processed images will be archived as POST-SAA DARKSs. Generally we
    expect that all NICMOS science/calibration observations started within
    50 minutes of leaving an SAA will need such maps to remove the CR
    persistence from the science images. Each observation will need its
    own CRMAP, as different SAA passages leave different imprints on the
    NICMOS detectors.


    NIC3/WFPC2 10277


    Ages and Metallicities of the Intergalactic Globular Cluster
    Population in Abell 1185


    We will obtain deep NICMOS observations of a recently discovered
    population of intergalactic globular clusters in the nearby galaxy
    cluster Abell 1185. These H band observations in conjunction with deep
    V and I images that we obtained with ACS in Cycle 11 will allow us to
    measure the ages and metallicities of these objects from their optical
    and near-infrared colors, which will provide important insights to
    their origin. We will also obtain parallel observations with both ACS
    and WFPC2. ACS parallel observations will be used to obtain deep
    images to search for intergalactic globular clusters in a different
    region of Abell 1185. WFPC2 parallel observations will be used to
    obtain images of interacting galaxy pair Arp 105, to search for
    globular clusters currently being ejected into intergalactic space as
    a result of this encounter.


    FLIGHT OPERATIONS SUMMARY:


    Significant Spacecraft Anomalies: (The following are preliminary
    reports of potential non-nominal performance that will be
    investigated.) None


    COMPLETED OPS REQs:
    17411-1 Off-line +BB and +B SPA Trim Relays @ 096/1313z


    OPS NOTES EXECUTED: None


    SCHEDULED SUCCESSFUL FAILURE TIMES
    FGS Gsacq 07 07
    FGS Reacq 07 07
    FHST Update 10 10
    LOSS of LOCK


    SIGNIFICANT EVENTS: None

  2. #2
    Join Date
    Jun 2005
    Posts
    595
    Now yer talkin'! It seems that there might be valuable research to be done by an appropriately situated telescope. S

  3. #3
    StarLab Guest
    These Daily HST reports do come out every day ...so I'll try to post as many as I can in this string, both for reference and for comments.

  4. #4
    StarLab Guest
    HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science


    DAILY REPORT # 3834


    PERIOD COVERED: DOY 97


    OBSERVATIONS SCHEDULED


    ACS/HRC 10130


    Systemic Proper Motions of the Magellanic Clouds from Astrometry with
    ACS: II. Second Epoch Images


    We request second epoch observations with ACS of Magellanic Cloud
    fields centered on the 40 quasars in the LMC and SMC for which we have
    first epoch Cycle 11 data. The new data will determine the systemic
    proper motion of the Clouds. An extensive astrometric analysis of the
    first epoch data shows that follow-up observations with a two year
    baseline will allow us to measure the proper motion of the clouds to
    within 0.022 mas/year in each of the two orthogonal directions
    {assuming that we can image 25 quasars, i.e., with a realistic
    Snapshot Program completion rate}. The best weighted combination of
    all previous measurements has a seven times larger error than what we
    expect. We will determine the proper motion of the clouds with 2%
    accuracy. When combined with HI data for the Magellanic Stream this
    will constrain both the mass distribution in the Galactic Halo and
    theoretical models for the origin of the Magellanic Stream. Previous
    measurements are too crude for such constraints. Our data will provide
    by far the most accurate proper motion measurement for any Milky Way
    satellite.


    ACS/WFC 10187


    Direct imaging of the progenitors of massive, core-collapse supernovae


    Modern supernovae searches in the nearby Universe are discovering
    large numbers of SNe which have massive star progenitors {Types II, Ib
    and Ic}. The extensive HST image archives of galaxies within ~20Mpc
    enables their individual bright stellar content to be resolved. As
    massive, evolved stars are the most luminous single objects in a
    galaxy, the progenitors of core-collapse SNe should be directly
    detectable on pre- explosion images. In our ongoing HST programme we
    have detected the first red supergiant progenitor of a normal type II
    supernova, shown that SN 1993J came from a binary system, and set
    direct mass-limits on three other type II supernovae progenitors.
    These discoveries are providing strong constraints on theoretical
    models of pre- supernova stellar evolution that predict which stars
    produce which type of supernovae. We request time to continue this
    successful project, and require ACS observations of future SNe which
    are discovered in galaxies closer than 20Mpc which have pre-explosion
    HST archive images available. These observations will allow the SNe to
    be precisely positioned on the pre-explosion frames with the required
    astrometric accuracy of around 0.05", and provide 3-colour photometry
    of the surrounding stellar populations for reddening estimations. The
    goal of this project is to directly identify the progenitor stars of
    core-collapse supernovae. We will compare the results to our own
    stellar evolutionary tracks in order to determine masses or
    restrictive mass-limits for the progenitors.


    ACS/WFC/NIC/NIC3/WFPC 10246 2 The HST survey of the Orion Nebula
    Cluster


    We propose a Treasury Program of 104 HST orbits to perform the
    definitive study of the Orion Nebula Cluster, the Rosetta stone of
    star formation. We will cover with unprecedented sensitivity {23-25
    mag}, dynamic range {~12 mag}, spatial resolution {50mas}, and
    simultaneous spectral coverage {5 bands} a ~450 square arcmin field
    centered on the Trapezium stars. This represents a tremendous gain
    over the shallow WFC1 study made in 1991 with the aberrated HST on an
    area ~15 times smaller. We maximize the HST observing efficiency using
    ACS/WFC and WFPC2 in parallel with two opposite roll angles, to cover
    the same total field. We will assemble the richest, most accurate and
    unbiased HR diagram for pre-main-sequence objects ever made. Combined
    with the optical spectroscopy already available for ~1000 sources and
    new deep near-IR imaging and spectroscopy {that we propose as Joint
    HST-NOAO observations}, we will be able to attack and possibly solve
    the most compelling questions on stellar evolution: the calibration of
    pre-main-sequence evolutionary tracks, mass segration and the
    variation of the initial mass function in different environments, the
    evolution of mass accretion rates vs. age and environment, disk
    dissipation in environments dominated by hard vs. soft-UV radiation,
    stellar multiplicity vs. disk fraction. In addition, we expect to
    discover and classify an unknown, but substantial, population of
    pre-Main Sequence binaries, low mass stars and brown dwarfs down to
    ~10 MJup. This is also the best possible way to discover dark
    silhouette disks in the outskirts of the Orion Nebula and study their
    evolutionary status through multicolor imaging. This program is timely
    and extremely well leveraged to other programs targeting Orion: the
    ACS H-alpha survey of the Orion Nebula, the recently completed 850ks
    ultradeep Chandra survey, the large GTO programs to be performed with
    SIRTF, plus the availability of 2MASS and various deep JHK surveys of
    the core recently done with 8m class telescopes.


    ACS/WFC/WFPC2 10402


    The Formation and Evolution of Spirals: An ACS and WFPC2 Imaging
    Survey of Nearby Galaxies


    Over 50% of galaxies in the local universe are spirals. Yet the star
    formation histories and evolution of this crucial population remain
    poorly understood. We propose to combine archival data with new
    ACS/WFC and WFPC2 observations of 11 galaxies, to tackle a
    comprehensive investigation of nearby spirals covering the entire
    spiral sequence. The new observations will fill a serious deficiency
    in HST's legacy, and maximize the scientific return of existing HST
    data. The filter combination of UBVI, and Halpha is ideal for studying
    stellar populations, dust properties, and the ISM. Our immediate
    scientific objectives are: {i} to use the resolved cluster
    populations, both young massive clusters and ancient globular clusters
    as a chronometer, to understand how spirals assembled as a function of
    time; {ii} study the rapid disruption properties of young clusters;
    and {iii} understand dust distributions in spirals from pc to kpc
    scales. Each of these goals provides an important step towards
    charting the evolution of galaxies, and an essential baseline for
    interpreting the galaxy populations being surveyed in both the early
    and present universe. The resolution of our survey, which exploits the
    excellent imaging capabilities of HST's two optical cameras, will
    enable us to understand the record of star cluster, and galaxy
    formation in a level of detail which is not possible for more distant
    systems. Finally, the proposed observations will provide a key to
    interpret an extensive, multiwavelength archive of space- and ground-
    based data at lower spatial resolution {SPITZER, CHANDRA, GALEX,
    NICMOS P alpha and H band imaging} for local spirals.


    ACS/WFC/WFPC2 10424


    The White Dwarf Cooling Age and Dynamical History of the Metal-Poor
    Globular Cluster NGC 6397


    We propose to determine the white dwarf cooling age in the nearest
    metal-poor {[Fe/H]=- 2} globular cluster, NGC 6397. This globular
    cluster provides the best opportunity to test the white dwarf cooling
    age in such a metal-poor system and at the same time provide a
    comparison with the more metal-rich cluster {M4} which we recently
    successfully observed with HST. Any {or even no} age difference
    between these clusters will be important in understanding the
    age-metallicity relation for these systems which reflects the star
    formation history in the early Galaxy. The absolute age is an
    important cosmological constraint. We expect to be able to detect age
    DIFFERENCES between these clusters at the 0.5 Gyr level and absolute
    ages should be accurate to 1.0 Gyr. In addition, and in contrast with
    M4, NGC 6397 is highly dynamically evolved, has a collapsed core, and
    the distribution of its white dwarfs throughout the cluster have
    almost certainly been modified by dynamical processes. We are using
    N-body simulations specifically developed for this cluster to
    understand these modifications and to include their effects in our
    measurement of the white dwarf luminosity function and cooling age.
    Among the dynamical questions we expect to answer with this proposal
    are: 1} what was the primordial binary frequency in NGC 6397? 2} can
    we explain the high central concentration with a population of massive
    white dwarfs and/or neutron stars? 3} do we see sufficient central
    binaries to reverse the core collapse of the cluster?


    NIC1/NIC2/NIC3 8792


    NICMOS Post-SAA calibration - CR Persistence Part 3


    A new procedure proposed to alleviate the CR-persistence problem of
    NICMOS. Dark frames will be obtained immediately upon exiting the SAA
    contour 23, and every time a NICMOS exposure is scheduled within 50
    minutes of coming out of the SAA. The darks will be obtained in
    parallel in all three NICMOS Cameras. The POST-SAA darks will be
    non-standard reference files available to users with a USEAFTER
    date/time mark. The keyword 'USEAFTER=date/time' will also be added to
    the header of each POST-SAA DARK frame. The keyword must be populated
    with the time, in addition to the date, because HST crosses the SAA ~8
    times per day so each POST-SAA DARK will need to have the appropriate
    time specified, for users to identify the ones they need. Both the raw
    and processed images will be archived as POST-SAA DARKSs. Generally we
    expect that all NICMOS science/calibration observations started within
    50 minutes of leaving an SAA will need such maps to remove the CR
    persistence from the science images. Each observation will need its
    own CRMAP, as different SAA passages leave different imprints on the
    NICMOS detectors.


    NIC2 10176


    Coronagraphic Survey for Giant Planets Around Nearby Young Stars


    A systematic imaging search for extra-solar Jovian planets is now
    possible thanks to recent progress in identifying "young stars near
    Earth". For most of the proposed young {<~ 30 Myrs} and nearby {<~ 60
    pc} targets, we can detect a few Jupiter-mass planets as close as a
    few tens of AUs from the primary stars. This represents the first time
    that potential analogs of our solar system - that is planetary systems
    with giant planets having semi-major axes comparable to those of the
    four giant planets of the Solar System - come within the grasp of
    existing instrumentation. Our proposed targets have not been observed
    for planets with the Hubble Space Telescope previously. Considering
    the very successful earlier NICMOS observations of low mass brown
    dwarfs and planetary disks among members of the TW Hydrae Association,
    a fair fraction of our targets should also turn out to posses low mass
    brown dwarfs, giant planets, or dusty planetary disks because our
    targets are similar to {or even better than} the TW Hydrae stars in
    terms of youth and proximity to Earth. Should HST time be awarded and
    planetary mass candidates be found, proper motion follow-up of
    candidate planets will be done with ground-based AOs.


    WFPC2 10170


    Atmospheric Variability on Uranus and Neptune


    We propose Snapshot observations of Uranus and Neptune to monitor
    changes in their atmospheres on time scales of weeks, months, and
    years. Uranus is rapidly approaching equinox in 2007, with another 4
    degrees of latitude becoming visible every year. Recent HST
    observations during this epoch {including 6818: Hammel, Lockwood, and
    Rages; 7885: Hammel, Karkoschka, and Marley; 8680: Hammel, Rages,
    Lockwood, and Marley; and 8634: Rages, Hammel, Lockwood, Marley, and
    McKay} have revealed strongly wavelength-dependent latitudinal
    structure and the presence of numerous visible-wavelength cloud
    features in the northern hemisphere. Long-term ground-based
    observations {Lockwood and Thompson 1999} show seasonal brightness
    changes whose origins are not well understood. Recent near-IR images
    of Neptune obtained using adaptive optics on the Keck Telescope
    together with images from our Cycle 9 Snapshot program {8634} show a
    general increase in activity at south temperate latitudes as well as
    the possible development of another Great Dark Spot. Further Snapshot
    observations of these two dynamic planets will elucidate the nature of
    long-term changes in their zonal atmospheric bands and clarify the
    processes of formation, evolution, and dissipation of discrete albedo
    features.


    FLIGHT OPERATIONS SUMMARY:


    Significant Spacecraft Anomalies: (The following are preliminary
    reports of potential non-nominal performance that will be
    investigated.) None


    COMPLETED OPS REQs: None


    OPS NOTES EXECUTED:
    1326-0 Restore Trickle Charge Elapse Timer Limit @ 097/1400Z


    SCHEDULED SUCCESSFUL FAILURE TIMES
    FGS Gsacq 12 12
    FGS Reacq 04 04
    FHST Update 16 16
    LOSS of LOCK


    SIGNIFICANT EVENTS: None

  5. #5
    StarLab Guest
    HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science


    DAILY REPORT # 3835


    PERIOD COVERED: DOYs 98-100


    OBSERVATIONS SCHEDULED


    NIC1/NIC2/NIC3 8792


    NICMOS Post-SAA calibration - CR Persistence Part 3


    A new procedure proposed to alleviate the CR-persistence problem of
    NICMOS. Dark frames will be obtained immediately upon exiting the SAA
    contour 23, and every time a NICMOS exposure is scheduled within 50
    minutes of coming out of the SAA. The darks will be obtained in
    parallel in all three NICMOS Cameras. The POST-SAA darks will be
    non-standard reference files available to users with a USEAFTER
    date/time mark. The keyword &#39;USEAFTER=date/time&#39; will also be added to
    the header of each POST-SAA DARK frame. The keyword must be populated
    with the time, in addition to the date, because HST crosses the SAA ~8
    times per day so each POST-SAA DARK will need to have the appropriate
    time specified, for users to identify the ones they need. Both the raw
    and processed images will be archived as POST-SAA DARKSs. Generally we
    expect that all NICMOS science/calibration observations started within
    50 minutes of leaving an SAA will need such maps to remove the CR
    persistence from the science images. Each observation will need its
    own CRMAP, as different SAA passages leave different imprints on the
    NICMOS detectors.


    ACS/WFC/WFPC2 10424


    The White Dwarf Cooling Age and Dynamical History of the Metal-Poor
    Globular Cluster NGC 6397


    We propose to determine the white dwarf cooling age in the nearest
    metal-poor {[Fe/H]=- 2} globular cluster, NGC 6397. This globular
    cluster provides the best opportunity to test the white dwarf cooling
    age in such a metal-poor system and at the same time provide a
    comparison with the more metal-rich cluster {M4} which we recently
    successfully observed with HST. Any {or even no} age difference
    between these clusters will be important in understanding the
    age-metallicity relation for these systems which reflects the star
    formation history in the early Galaxy. The absolute age is an
    important cosmological constraint. We expect to be able to detect age
    DIFFERENCES between these clusters at the 0.5 Gyr level and absolute
    ages should be accurate to 1.0 Gyr. In addition, and in contrast with
    M4, NGC 6397 is highly dynamically evolved, has a collapsed core, and
    the distribution of its white dwarfs throughout the cluster have
    almost certainly been modified by dynamical processes. We are using
    N-body simulations specifically developed for this cluster to
    understand these modifications and to include their effects in our
    measurement of the white dwarf luminosity function and cooling age.
    Among the dynamical questions we expect to answer with this proposal
    are: 1} what was the primordial binary frequency in NGC 6397? 2} can
    we explain the high central concentration with a population of massive
    white dwarfs and/or neutron stars? 3} do we see sufficient central
    binaries to reverse the core collapse of the cluster?


    ACS/HRC/WFC 10389


    ACS CCDs daily monitor - Cycle 13 - Part 2


    This program consists of a set of basic tests to monitor, the read
    noise, the development of hot pixels and test for any source of noise
    in ACS CCD detectors. The files, biases and dark will be used to
    create reference files for science calibration. This programme will be
    for the entire lifetime of ACS.


    ACS/WFC/NIC/NIC3/W 10246 FPC2 The HST survey of the Orion Nebula
    Cluster


    We propose a Treasury Program of 104 HST orbits to perform the
    definitive study of the Orion Nebula Cluster, the Rosetta stone of
    star formation. We will cover with unprecedented sensitivity {23-25
    mag}, dynamic range {~12 mag}, spatial resolution {50mas}, and
    simultaneous spectral coverage {5 bands} a ~450 square arcmin field
    centered on the Trapezium stars. This represents a tremendous gain
    over the shallow WFC1 study made in 1991 with the aberrated HST on an
    area ~15 times smaller. We maximize the HST observing efficiency using
    ACS/WFC and WFPC2 in parallel with two opposite roll angles, to cover
    the same total field. We will assemble the richest, most accurate and
    unbiased HR diagram for pre-main-sequence objects ever made. Combined
    with the optical spectroscopy already available for ~1000 sources and
    new deep near-IR imaging and spectroscopy {that we propose as Joint
    HST-NOAO observations}, we will be able to attack and possibly solve
    the most compelling questions on stellar evolution: the calibration of
    pre-main-sequence evolutionary tracks, mass segration and the
    variation of the initial mass function in different environments, the
    evolution of mass accretion rates vs. age and environment, disk
    dissipation in environments dominated by hard vs. soft-UV radiation,
    stellar multiplicity vs. disk fraction. In addition, we expect to
    discover and classify an unknown, but substantial, population of
    pre-Main Sequence binaries, low mass stars and brown dwarfs down to
    ~10 MJup. This is also the best possible way to discover dark
    silhouette disks in the outskirts of the Orion Nebula and study their
    evolutionary status through multicolor imaging. This program is timely
    and extremely well leveraged to other programs targeting Orion: the
    ACS H-alpha survey of the Orion Nebula, the recently completed 850ks
    ultradeep Chandra survey, the large GTO programs to be performed with
    SIRTF, plus the availability of 2MASS and various deep JHK surveys of
    the core recently done with 8m class telescopes.


    ACS/WFC 10210


    Groups of Dwarf Galaxies: Pools of Mostly Dark Matter?


    Within 5 Mpc, there are 6 groups with well-known luminous galaxies but
    there also appears to be a comparable number of groups containing only
    dwarfs. If these dwarf entities are truly bound then M/L values are an
    order of magnitude higher than values found for groups with luminous
    spiral galaxies. There are theoretical reasons to anticipate that low
    mass halos may frequently be mostly dark. The dynamical influence of
    low mass halos is negligible in familiar groups with luminous members.
    By contrast, a study of the dynamics of `groups of dwarfs&#39; may provide
    direct evidence of the existence of dark matter potential wells with
    few baryons. The goal of the present study is to gather detailed
    information on the 3-D distribution of dwarf galaxies suspected to lie
    within 7 groups of dwarfs within 5 Mpc. Distances with 7% relative
    accuracy can be measured with the Tip of the Giant Branch method with
    ACS and integrations within 1 orbit per target.


    NIC2 10173


    Infrared Snapshots of 3CR Radio Galaxies


    Radio galaxies are an important class of extragalactic objects: they
    are one of the most energetic astrophysical phenomena and they provide
    an exceptional probe of the evolving Universe, lying typically in high
    density regions but well-represented across a wide redshift range. In
    earlier Cycles we carried out extensive HST observations of the 3CR
    sources in order to acquire a complete and quantitative inventory of
    the structure, contents and evolution of these important objects.
    Amongst the results, we discovered new optical jets, dust lanes,
    face-on disks with optical jets, and revealed point-like nuclei whose
    properties support FR-I/BL Lac unified schemes. Here, we propose to
    obtain NICMOS infrared images of 3CR sources with z<0.3 as a major
    enhancement to an already superb dataset. We aim to deshroud dusty
    galaxies, study the underlying host galaxy free from the distorting
    effects of dust, locate hidden regions of star formation and establish
    the physical characteristics of the dust itself. We will measure
    frequency and spectral energy distributions of point-like nuclei,
    expected to be stronger and more prevalent in the IR, seek spectral
    turnovers in known synchrotron jets and find new jets. We will
    strongly test unified AGN schemes and merge these data with existing
    X-ray to radio observations. The resulting database will be an
    incredibly valuable resource to the astronomical community for years
    to come.


    WFPC2 10170


    Atmospheric Variability on Uranus and Neptune


    We propose Snapshot observations of Uranus and Neptune to monitor
    changes in their atmospheres on time scales of weeks, months, and
    years. Uranus is rapidly approaching equinox in 2007, with another 4
    degrees of latitude becoming visible every year. Recent HST
    observations during this epoch {including 6818: Hammel, Lockwood, and
    Rages; 7885: Hammel, Karkoschka, and Marley; 8680: Hammel, Rages,
    Lockwood, and Marley; and 8634: Rages, Hammel, Lockwood, Marley, and
    McKay} have revealed strongly wavelength-dependent latitudinal
    structure and the presence of numerous visible-wavelength cloud
    features in the northern hemisphere. Long-term ground-based
    observations {Lockwood and Thompson 1999} show seasonal brightness
    changes whose origins are not well understood. Recent near-IR images
    of Neptune obtained using adaptive optics on the Keck Telescope
    together with images from our Cycle 9 Snapshot program {8634} show a
    general increase in activity at south temperate latitudes as well as
    the possible development of another Great Dark Spot. Further Snapshot
    observations of these two dynamic planets will elucidate the nature of
    long-term changes in their zonal atmospheric bands and clarify the
    processes of formation, evolution, and dissipation of discrete albedo
    features.


    FGS 10106


    An Astrometric Calibration of the Cepheid Period-Luminosity Relation


    We propose to measure the parallaxes of 10 Galactic Cepheid variables.
    When these parallaxes {with 1-sigma precisions of 10% or better} are
    added to our recent HST FGS parallax determination of delta Cep
    {Benedict et al 2002}, we anticipate determining the Period-Luminosity
    relation zero point with a 0.03 mag precision. In addition to
    permitting the test of assumptions that enter into other Cepheid
    distance determination techniques, this calibration will reintroduce
    Galactic Cepheids as a fundamental step in the extragalactic distance
    scale ladder. A Period-Luminosity relation derived from solar
    metallicity Cepheids can be applied directly to extragalactic solar
    metallicity Cepheids, removing the need to bridge with the Large
    Magellanic Cloud and its associated metallicity complications.


    FLIGHT OPERATIONS SUMMARY:


    Significant Spacecraft Anomalies: (The following are preliminary
    reports of potential non-nominal performance that will be
    investigated.)


    HSTAR #9764: GSACQ(3,1,1) failed, search radius limit exceeded @
    098/09:47:24z GSacq(3,1,1) at 098/09:42:46 failed to gyro control due
    to Search Radius Limit Exceeded on FGS 3 at 09:47:24 and a second time
    at 09:50:27. Roll delay update at 08:45:49 had attitude errors of
    5.176 on V1, 1.795 V2, 7.622 V3. Map at 09:51:00 had attitude errors
    of 4.528, 10.110, -9.884. Observations Affected: ACS 23 to 28, NICMOS
    73 to 75, WFPC 205 to 209. The Subsequent REacq(3,1,1) at 098/10:38:17
    failed to RGA control. Under investigation.


    HSTAR #9767: GSaq(1,3,1) failed, search radius limit exceeded @
    098/23:58:31z GSacq(1,3,1) at 098/23:53:36z failed to gyro control due
    to search radius limit exceed on FGS 1 at 23:58:31z. The REacq at
    01:02:01z was successful. Observations Affected: WFPC 224 - 225, NIC
    78. Under investigation.


    HSTAR #9768: REACQ(1,3,1) requires 2 attempts to acquire Fine Lock
    (FL) @ 100/ 01:04:04z. REACQ(1,3,1) at 100/01:01:38z required two
    attempts to enter FL, with Scan Step Limit exceeded at 01:04:04z.
    Second attempt to acquire was successful. Primary GSACQ had no
    problems. Under investigation.


    HSTAR #9769: NICMOS suspended, debug exception @ 100/23:3:56z. NICMOS
    status buffer message 104, Parameter 2, Time 37290, was received at
    acquisition of signal at 23:07:45. Parameter 2 indicates a DEBUG
    EXCEPTION occurred. Under investigation.


    HSTAR #9770: GSACQ(1,3,3) Fine Lock Backup @ 101/06:30:00z.
    GSACQ(1,3,3) occurred at 05:51:24z while vehicle was LOS. At AOS at
    06:30z, vehicle was in Fine Lock on FGS 3 only, QF1STOPF and QSTOP
    flags were set. Additional information will be available after
    Engineering Dump is merged. Observations affected: WFPC 9 to 13, ACS
    15 to 19, NICMOS 6. Under investigation. Under investigation.


    COMPLETED OPS REQs:
    17416-2 Eclipse Management, GMT Day 098 @ 098/2355z
    17417-1 NICMOS Memory Dump after Suspend @ 100/08:42:21z


    OPS NOTES EXECUTED:
    0916-0 Tabulation of Slew Attitude Error (Miss-distance) @ 101/0035z
    1327-0 Exec 272 while NICMOS is Suspended @ 101/0316z


    SCHEDULED SUCCESSFUL FAILURE TIMES
    FGS
    Gsacq 28 26
    098/09:47:24z, 098/23:58:31z
    FGS
    Reacq 17 16 098/10:38:17z
    FHST Update 34 34
    LOSS of LOCK


    SIGNIFICANT EVENTS:


    Eclipse Summary of SE Eclipse Flash Report (Fri, 08 Apr 2005) There
    were five eclipse events occurring between GMT 98/18:05 to 98/22:39.
    OPS Request 17416 was successfully executed in preparation for these
    events by temporarily disabling the Rate of Charge and SA Cold
    Protection safemode tests. The CSS timer was also modified to prevent
    software logic from potentially detecting a false CSS failure due to
    the eclipse. With trickle charge verified and a forward link available
    following the fifth eclipse, resetting of the safemode tests and CSS
    timer to their nominal state was completed at 23:55. Preliminary
    results from limited real-time data appear to indicate that trickle
    charge was still reached during all but the last eclipse. Near EON at
    22:31, the fifth eclipse started as well as a 127.14 deg vehicle
    maneuver which caused trickle charge not to be reached before start of
    night as anticipated. Trickle charge was reached in the following
    orbit day at about 23:50 and EPS is nominal.


    NICMOS suspended at 100/23:03:46 due to an Intel Debug Exception (ESB
    104, P=2). HSTAR 9769 was generated by the FOT. NICMOS memory was
    successfully dumped via Ops Request 17417 at 101/08:42z and the files
    transferred to the Payload FSW team for analysis. NICMOS recovery is
    scheduled to begin at 101/12:50z via Ops Request 17418.

  6. #6
    Join Date
    Jan 2004
    Posts
    1,085
    You beat me to it&#33;&#33;&#33;&#33;

    I was going to post today&#39;s report on the board but I thought it was probably too long but I see you have begun a new string with the DAILY reports&#33;



    BTW, Happy Birthday&#33;

  7. #7
    StarLab Guest
    BTW, Happy Birthday&#33;
    Aww, thanx Madspace&#33;

    BTW, I&#39;ve patented this string muahaha&#33;

  8. #8
    StarLab Guest
    And, I am true to my word:


    HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science


    DAILY REPORT # 3836


    PERIOD COVERED: DOY 101


    OBSERVATIONS SCHEDULED


    ACS/HRC/WFC 10389


    ACS CCDs daily monitor - Cycle 13 - Part 2


    This program consists of a set of basic tests to monitor, the read
    noise, the development of hot pixels and test for any source of noise
    in ACS CCD detectors. The files, biases and dark will be used to
    create reference files for science calibration. This programme will be
    for the entire lifetime of ACS.


    ACS/WFC/NIC/NIC3/WFPC 10246 2 The HST survey of the Orion Nebula
    Cluster


    We propose a Treasury Program of 104 HST orbits to perform the
    definitive study of the Orion Nebula Cluster, the Rosetta stone of
    star formation. We will cover with unprecedented sensitivity {23-25
    mag}, dynamic range {~12 mag}, spatial resolution {50mas}, and
    simultaneous spectral coverage {5 bands} a ~450 square arcmin field
    centered on the Trapezium stars. This represents a tremendous gain
    over the shallow WFC1 study made in 1991 with the aberrated HST on an
    area ~15 times smaller. We maximize the HST observing efficiency using
    ACS/WFC and WFPC2 in parallel with two opposite roll angles, to cover
    the same total field. We will assemble the richest, most accurate and
    unbiased HR diagram for pre-main-sequence objects ever made. Combined
    with the optical spectroscopy already available for ~1000 sources and
    new deep near-IR imaging and spectroscopy {that we propose as Joint
    HST-NOAO observations}, we will be able to attack and possibly solve
    the most compelling questions on stellar evolution: the calibration of
    pre-main-sequence evolutionary tracks, mass segration and the
    variation of the initial mass function in different environments, the
    evolution of mass accretion rates vs. age and environment, disk
    dissipation in environments dominated by hard vs. soft-UV radiation,
    stellar multiplicity vs. disk fraction. In addition, we expect to
    discover and classify an unknown, but substantial, population of
    pre-Main Sequence binaries, low mass stars and brown dwarfs down to
    ~10 MJup. This is also the best possible way to discover dark
    silhouette disks in the outskirts of the Orion Nebula and study their
    evolutionary status through multicolor imaging. This program is timely
    and extremely well leveraged to other programs targeting Orion: the
    ACS H-alpha survey of the Orion Nebula, the recently completed 850ks
    ultradeep Chandra survey, the large GTO programs to be performed with
    SIRTF, plus the availability of 2MASS and various deep JHK surveys of
    the core recently done with 8m class telescopes.


    ACS/WFC 10189


    PANS-Probing Acceleration Now with Supernovae


    Type Ia supernovae {SNe Ia} provide the most direct evidence for an
    accelerating Universe, a result widely attributed to dark energy.
    Using HST in Cycle 11 we extended the Hubble diagram with 6 of the 7
    highest-redshift SNe Ia known, all at z>1.25, providing conclusive
    evidence of an earlier epoch of cosmic deceleration. The full sample
    of 16 new SNe Ia match the cosmic concordance model and are
    inconsistent with a simple model of evolution or dust as alternatives
    to dark energy. Understanding dark energy may be the biggest current
    challenge to cosmology and particle physics. To understand the nature
    of dark energy, we seek to measure its two most fundamental
    properties: its evolution {i.e., dw/dz}, and its recent equation of
    state {i.e., w{z=0}}. SNe Ia at z>1, beyond the reach of the ground
    but squarely within the reach of HST with ACS, are crucial to break
    the degeneracy in the measurements of these two basic aspects of dark
    energy. The SNe Ia we have discovered and measured with HST in Cycle
    11, now double the precision of our knowledge of both properties. Here
    we propose to quadruple the sample of SNe Ia at z>1 in the next two
    cycles, complementing on-going surveys from the ground at z<1, and
    again doubling the precision of dark energy constraints. Should the
    current best fit model prove to be the correct one, the precision
    expected from the current proposal will suffice to rule out a
    cosmological constant at the 99% confidence level. Whatever the
    result, these objects will provide the basis with which to extend our
    empirical knowledge of this newly discovered and dominant component of
    the Universe, and will remain one of the most significant legacies of
    HST. In addition, our survey and follow-up data will greatly enhance
    the value of the archival data within the target Treasury fields for
    galaxy studies.


    ACS/WFC/WFPC2 10402


    The Formation and Evolution of Spirals: An ACS and WFPC2 Imaging
    Survey of Nearby Galaxies


    Over 50% of galaxies in the local universe are spirals. Yet the star
    formation histories and evolution of this crucial population remain
    poorly understood. We propose to combine archival data with new
    ACS/WFC and WFPC2 observations of 11 galaxies, to tackle a
    comprehensive investigation of nearby spirals covering the entire
    spiral sequence. The new observations will fill a serious deficiency
    in HST&#39;s legacy, and maximize the scientific return of existing HST
    data. The filter combination of UBVI, and Halpha is ideal for studying
    stellar populations, dust properties, and the ISM. Our immediate
    scientific objectives are: {i} to use the resolved cluster
    populations, both young massive clusters and ancient globular clusters
    as a chronometer, to understand how spirals assembled as a function of
    time; {ii} study the rapid disruption properties of young clusters;
    and {iii} understand dust distributions in spirals from pc to kpc
    scales. Each of these goals provides an important step towards
    charting the evolution of galaxies, and an essential baseline for
    interpreting the galaxy populations being surveyed in both the early
    and present universe. The resolution of our survey, which exploits the
    excellent imaging capabilities of HST&#39;s two optical cameras, will
    enable us to understand the record of star cluster, and galaxy
    formation in a level of detail which is not possible for more distant
    systems. Finally, the proposed observations will provide a key to
    interpret an extensive, multiwavelength archive of space- and ground-
    based data at lower spatial resolution {SPITZER, CHANDRA, GALEX,
    NICMOS P alpha and H band imaging} for local spirals.


    FGS 10106


    An Astrometric Calibration of the Cepheid Period-Luminosity Relation


    We propose to measure the parallaxes of 10 Galactic Cepheid variables.
    When these parallaxes {with 1-sigma precisions of 10% or better} are
    added to our recent HST FGS parallax determination of delta Cep
    {Benedict et al 2002}, we anticipate determining the Period-Luminosity
    relation zero point with a 0.03 mag precision. In addition to
    permitting the test of assumptions that enter into other Cepheid
    distance determination techniques, this calibration will reintroduce
    Galactic Cepheids as a fundamental step in the extragalactic distance
    scale ladder. A Period-Luminosity relation derived from solar
    metallicity Cepheids can be applied directly to extragalactic solar
    metallicity Cepheids, removing the need to bridge with the Large
    Magellanic Cloud and its associated metallicity complications.


    FGS 10113


    Trigonometric Calibration of the Period- Luminosity Relations for
    Fundamental and First- Overtone Galactic Cepheids


    Cepheids are the primary distance indicators for the extragalactic
    distance scale and the Hubble constant. The Hubble Constant Key
    Project set the zero-point for their Cepheid distance scale by
    adopting a distance to the LMC, averaged over a variety of techniques.
    However, different methods give an LMC distance modulus ranging from
    18.1 to 18.8, and the uncertainty in the Cepheid zero-point is now the
    largest contributor to the error budget for H_0. Moreover, the low
    metallicity of the LMC raises additional concerns, since the PL
    relation probably depends on metallicity. The zero-point can be
    determined from Hipparcos parallaxes of Galactic Cepheids out to
    several hundred parsecs, but with a typical parallax error of 0.5-1
    mas, the Hipparcos error bars are uncomfortably large for this
    demanding application. By contrast, HST&#39;s FGS1R interferometer can
    achieve astrometric accuracy of 0.2 mas. We propose to use FGS1R to
    determine trigonometric parallaxes for a sample of 9 nearby Cepheids,
    including both fundamental {F} and first-overtone {FO} pulsators. We
    show that the improvement in the PL relations for F and FO Cepheids
    will be dramatic. We will determine the PL slopes from our nearby
    solar- metallicity sample alone, without recourse to nearby galaxies
    and the issue of [Fe/H] dependence. The zero-point will be determined
    robustly to about 0.05 mag, based on accurate, purely geometrical
    measurements.


    NIC1/NIC2/NIC3 8792


    NICMOS Post-SAA calibration - CR Persistence Part 3


    A new procedure proposed to alleviate the CR-persistence problem of
    NICMOS. Dark frames will be obtained immediately upon exiting the SAA
    contour 23, and every time a NICMOS exposure is scheduled within 50
    minutes of coming out of the SAA. The darks will be obtained in
    parallel in all three NICMOS Cameras. The POST-SAA darks will be
    non-standard reference files available to users with a USEAFTER
    date/time mark. The keyword &#39;USEAFTER=date/time&#39; will also be added to
    the header of each POST-SAA DARK frame. The keyword must be populated
    with the time, in addition to the date, because HST crosses the SAA ~8
    times per day so each POST-SAA DARK will need to have the appropriate
    time specified, for users to identify the ones they need. Both the raw
    and processed images will be archived as POST-SAA DARKSs. Generally we
    expect that all NICMOS science/calibration observations started within
    50 minutes of leaving an SAA will need such maps to remove the CR
    persistence from the science images. Each observation will need its
    own CRMAP, as different SAA passages leave different imprints on the
    NICMOS detectors.


    FLIGHT OPERATIONS SUMMARY:


    Significant Spacecraft Anomalies: (The following are preliminary
    reports of potential non-nominal performance that will be
    investigated.)


    HSTAR #9771: GSACQ(1,3,3) Fine Lock Backup @ 102/06:07:52z
    GSACQ(1,3,3) occurred at 05:50:37z while vehicle was LOS. At AOS at
    06:07:52z, vehicle was in Fine Lock on FGS 3 only, QF1STOPF and QSTOP
    flags were set. Further information after engineering recorder dump.
    This acquisition uses the same guide star ID&#39;s as yesterday&#39;s HSTAR
    9770. Observations affected: WFPC 54 to 58, ACS 63 to 67, NICMOS 30.
    Under investigation.


    COMPLETED OPS REQs:
    17418-0 NICMOS Suspend Recovery @ 101/1303z


    OPS NOTES EXECUTED:
    1328-1 Adjust Battery 6 Temperature High Yellow Limit @ 101/1605z


    SCHEDULED SUCCESSFUL FAILURE TIMES
    FGS Gsacq 12 12
    FGS Reacq 04 04
    FHST Update 17 17
    LOSS of LOCK


    SIGNIFICANT EVENTS:


    NICMOS has been successfully recovered back to Operate via Ops Request
    17418. The buffer box and mechanism temperatures were well within
    their turn-on ranges and NICMOS science resumed. The first
    post-recovery proposal began at 101/17:05. The Payload FSW analysis of
    the memory dump shows this event to be in family with previous Intel
    Debug Exceptions. This event occurred while NICMOS was operating all
    three detectors in parallel.

  9. #9
    StarLab Guest
    HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science


    DAILY REPORT # 3837


    PERIOD COVERED: DOY 102


    OBSERVATIONS SCHEDULED


    ACS/HRC 10272


    A Snapshot Survey of the Sites of Recent, Nearby Supernovae


    During the past few years, robotic {or nearly robotic} searches for
    supernovae {SNe}, most notably our Lick Observatory Supernova Search
    {LOSS}, have found hundreds of SNe, many of them in quite nearby
    galaxies {cz < 4000 km/s}. Most of the objects were discovered before
    maximum brightness, and have follow-up photometry and spectroscopy;
    they include some of the best-studied SNe to date. We propose to
    conduct a snapshot imaging survey of the sites of some of these nearby
    objects, to obtain late-time photometry that {through the shape of the
    light and color curves} will help reveal the origin of their lingering
    energy. The images will also provide high- resolution information on
    the local environment of SNe that are far superior to what we can
    procure from the ground. For example, we will obtain color-color and
    color-magnitude diagrams of stars in these SN sites, to determine
    their progenitor masses and constraints on the reddening. Recovery of
    the SNe in the new HST images will also allow us to actually pinpoint
    their progenitor stars in cases where pre-explosion images exist in
    the HST archive. Use of ACS rather than WFPC2 will make our snapshot
    survey even more valuable than our Cycle 9 survey. This Proposal is
    complementary to our Cycle 13 archival proposal, in which we outline a
    plan for using existing HST images to glean information about SN
    environments.


    ACS/WFC/NIC/NIC3/WFPC 10246 2 The HST survey of the Orion Nebula
    Cluster


    We propose a Treasury Program of 104 HST orbits to perform the
    definitive study of the Orion Nebula Cluster, the Rosetta stone of
    star formation. We will cover with unprecedented sensitivity {23-25
    mag}, dynamic range {~12 mag}, spatial resolution {50mas}, and
    simultaneous spectral coverage {5 bands} a ~450 square arcmin field
    centered on the Trapezium stars. This represents a tremendous gain
    over the shallow WFC1 study made in 1991 with the aberrated HST on an
    area ~15 times smaller. We maximize the HST observing efficiency using
    ACS/WFC and WFPC2 in parallel with two opposite roll angles, to cover
    the same total field. We will assemble the richest, most accurate and
    unbiased HR diagram for pre-main-sequence objects ever made. Combined
    with the optical spectroscopy already available for ~1000 sources and
    new deep near-IR imaging and spectroscopy {that we propose as Joint
    HST-NOAO observations}, we will be able to attack and possibly solve
    the most compelling questions on stellar evolution: the calibration of
    pre-main-sequence evolutionary tracks, mass segration and the
    variation of the initial mass function in different environments, the
    evolution of mass accretion rates vs. age and environment, disk
    dissipation in environments dominated by hard vs. soft-UV radiation,
    stellar multiplicity vs. disk fraction. In addition, we expect to
    discover and classify an unknown, but substantial, population of
    pre-Main Sequence binaries, low mass stars and brown dwarfs down to
    ~10 MJup. This is also the best possible way to discover dark
    silhouette disks in the outskirts of the Orion Nebula and study their
    evolutionary status through multicolor imaging. This program is timely
    and extremely well leveraged to other programs targeting Orion: the
    ACS H-alpha survey of the Orion Nebula, the recently completed 850ks
    ultradeep Chandra survey, the large GTO programs to be performed with
    SIRTF, plus the availability of 2MASS and various deep JHK surveys of
    the core recently done with 8m class telescopes.


    ACS/WFC/NIC3 10339


    PANS


    Type Ia supernovae {SNe Ia} provide the only direct evidence for an
    accelerating universe, an extraordinary result that needs the most
    rigorous test. The case for cosmic acceleration rests on the
    observation that SNe Ia at z = 0.5 are about 0.25 mag fainter than
    they would be in a universe without acceleration. A powerful and
    straightforward way to assess the reliability of the SN Ia measurement
    and the conceptual framework of its interpretation is to look for
    cosmic deceleration at z > 1. This would be a clear signature of a
    mixed dark-matter and dark-energy universe. Systematic errors in the
    SNe Ia result attributed to grey dust or cosmic evolution of the SN Ia
    peak luminosity would not show this change of sign. We have obtained a
    toehold on this putative ``epoch of deceleration&#39;&#39; with SN 1997ff at z
    = 1.7, and 3 more at z > 1 from our Cycle 11 program, all found and
    followed by HST. However, this is too important a test to rest on just
    a few objects, anyone of which could be subject to a lensed
    line-of-sight or misidentification. Here we propose to extend our
    measurement with observations of twelve SNe Ia in the range 1.0 < z <
    1.5 or 6 such SNe Ia and 1 ultradistant SN Ia at z = 2, that will be
    discovered as a byproduct from proposed Treasury and DD programs.
    These objects will provide a much firmer foundation for a conclusion
    that touches on important questions of fundamental physics.


    FGS 10113


    Trigonometric Calibration of the Period- Luminosity Relations for
    Fundamental and First- Overtone Galactic Cepheids


    Cepheids are the primary distance indicators for the extragalactic
    distance scale and the Hubble constant. The Hubble Constant Key
    Project set the zero-point for their Cepheid distance scale by
    adopting a distance to the LMC, averaged over a variety of techniques.
    However, different methods give an LMC distance modulus ranging from
    18.1 to 18.8, and the uncertainty in the Cepheid zero-point is now the
    largest contributor to the error budget for H_0. Moreover, the low
    metallicity of the LMC raises additional concerns, since the PL
    relation probably depends on metallicity. The zero-point can be
    determined from Hipparcos parallaxes of Galactic Cepheids out to
    several hundred parsecs, but with a typical parallax error of 0.5-1
    mas, the Hipparcos error bars are uncomfortably large for this
    demanding application. By contrast, HST&#39;s FGS1R interferometer can
    achieve astrometric accuracy of 0.2 mas. We propose to use FGS1R to
    determine trigonometric parallaxes for a sample of 9 nearby Cepheids,
    including both fundamental {F} and first-overtone {FO} pulsators. We
    show that the improvement in the PL relations for F and FO Cepheids
    will be dramatic. We will determine the PL slopes from our nearby
    solar- metallicity sample alone, without recourse to nearby galaxies
    and the issue of [Fe/H] dependence. The zero-point will be determined
    robustly to about 0.05 mag, based on accurate, purely geometrical
    measurements.


    NIC1/NIC2/NIC3 8792


    NICMOS Post-SAA calibration - CR Persistence Part 3


    A new procedure proposed to alleviate the CR-persistence problem of
    NICMOS. Dark frames will be obtained immediately upon exiting the SAA
    contour 23, and every time a NICMOS exposure is scheduled within 50
    minutes of coming out of the SAA. The darks will be obtained in
    parallel in all three NICMOS Cameras. The POST-SAA darks will be
    non-standard reference files available to users with a USEAFTER
    date/time mark. The keyword &#39;USEAFTER=date/time&#39; will also be added to
    the header of each POST-SAA DARK frame. The keyword must be populated
    with the time, in addition to the date, because HST crosses the SAA ~8
    times per day so each POST-SAA DARK will need to have the appropriate
    time specified, for users to identify the ones they need. Both the raw
    and processed images will be archived as POST-SAA DARKSs. Generally we
    expect that all NICMOS science/calibration observations started within
    50 minutes of leaving an SAA will need such maps to remove the CR
    persistence from the science images. Each observation will need its
    own CRMAP, as different SAA passages leave different imprints on the
    NICMOS detectors.


    WFPC2 10360


    WFPC2 CYCLE 13 INTERNAL MONITOR


    This calibration proposal is the Cycle 13 routine internal monitor for
    WFPC2, to be run weekly to monitor the health of the cameras. A
    variety of internal exposures are obtained in order to provide a
    monitor of the integrity of the CCD camera electronics in both bays
    {gain 7 and gain 15}, a test for quantum efficiency in the CCDs, and a
    monitor for possible buildup of contaminants on the CCD windows.


    FLIGHT OPERATIONS SUMMARY:


    Significant Spacecraft Anomalies: (The following are preliminary
    reports of potential non-nominal performance that will be
    investigated.)


    HSTAR #9772: GSACQ(1,2,2) Fine Lock Backup @ 103/06:07:38z
    GSACQ(1,2,2) occurred at 05:50:49z while vehicle was LOS. At AOS at
    06:07:38z, vehicle was in Fine Lock on FGS 2 only, QF1STOPF, QF1SSLEX,
    QSTEPEXC and QSTOP flags were set. Further information after
    engineering recorder dump. Observations affected: WFPC 86 to 90, ACS
    128 to 132, NICMOS 53. Under investigation.


    COMPLETED OPS REQs: None


    OPS NOTES EXECUTED: None


    SCHEDULED SUCCESSFUL FAILURE TIMES
    FGS Gsacq 12 12
    FGS Reacq 02 02
    FHST Update 17 17
    LOSS of LOCK


    SIGNIFICANT EVENTS: None

  10. #10
    StarLab Guest
    HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science


    DAILY REPORT # 3838


    PERIOD COVERED: DOY 103


    OBSERVATIONS SCHEDULED


    ACS/HRC/WFC 10389


    ACS CCDs daily monitor - Cycle 13 - Part 2


    This program consists of a set of basic tests to monitor, the read
    noise, the development of hot pixels and test for any source of noise
    in ACS CCD detectors. The files, biases and dark will be used to
    create reference files for science calibration. This programme will be
    for the entire lifetime of ACS.


    ACS/WFC/NIC/NIC3/WFPC 10246 2 The HST survey of the Orion Nebula
    Cluster


    We propose a Treasury Program of 104 HST orbits to perform the
    definitive study of the Orion Nebula Cluster, the Rosetta stone of
    star formation. We will cover with unprecedented sensitivity {23-25
    mag}, dynamic range {~12 mag}, spatial resolution {50mas}, and
    simultaneous spectral coverage {5 bands} a ~450 square arcmin field
    centered on the Trapezium stars. This represents a tremendous gain
    over the shallow WFC1 study made in 1991 with the aberrated HST on an
    area ~15 times smaller. We maximize the HST observing efficiency using
    ACS/WFC and WFPC2 in parallel with two opposite roll angles, to cover
    the same total field. We will assemble the richest, most accurate and
    unbiased HR diagram for pre-main-sequence objects ever made. Combined
    with the optical spectroscopy already available for ~1000 sources and
    new deep near-IR imaging and spectroscopy {that we propose as Joint
    HST-NOAO observations}, we will be able to attack and possibly solve
    the most compelling questions on stellar evolution: the calibration of
    pre-main-sequence evolutionary tracks, mass segration and the
    variation of the initial mass function in different environments, the
    evolution of mass accretion rates vs. age and environment, disk
    dissipation in environments dominated by hard vs. soft-UV radiation,
    stellar multiplicity vs. disk fraction. In addition, we expect to
    discover and classify an unknown, but substantial, population of
    pre-Main Sequence binaries, low mass stars and brown dwarfs down to
    ~10 MJup. This is also the best possible way to discover dark
    silhouette disks in the outskirts of the Orion Nebula and study their
    evolutionary status through multicolor imaging. This program is timely
    and extremely well leveraged to other programs targeting Orion: the
    ACS H-alpha survey of the Orion Nebula, the recently completed 850ks
    ultradeep Chandra survey, the large GTO programs to be performed with
    SIRTF, plus the availability of 2MASS and various deep JHK surveys of
    the core recently done with 8m class telescopes.


    ACS/WFC/NIC3 10339


    PANS


    Type Ia supernovae {SNe Ia} provide the only direct evidence for an
    accelerating universe, an extraordinary result that needs the most
    rigorous test. The case for cosmic acceleration rests on the
    observation that SNe Ia at z = 0.5 are about 0.25 mag fainter than
    they would be in a universe without acceleration. A powerful and
    straightforward way to assess the reliability of the SN Ia measurement
    and the conceptual framework of its interpretation is to look for
    cosmic deceleration at z > 1. This would be a clear signature of a
    mixed dark-matter and dark-energy universe. Systematic errors in the
    SNe Ia result attributed to grey dust or cosmic evolution of the SN Ia
    peak luminosity would not show this change of sign. We have obtained a
    toehold on this putative ``epoch of deceleration&#39;&#39; with SN 1997ff at z
    = 1.7, and 3 more at z > 1 from our Cycle 11 program, all found and
    followed by HST. However, this is too important a test to rest on just
    a few objects, anyone of which could be subject to a lensed
    line-of-sight or misidentification. Here we propose to extend our
    measurement with observations of twelve SNe Ia in the range 1.0 < z <
    1.5 or 6 such SNe Ia and 1 ultradistant SN Ia at z = 2, that will be
    discovered as a byproduct from proposed Treasury and DD programs.
    These objects will provide a much firmer foundation for a conclusion
    that touches on important questions of fundamental physics.


    ACS/WFC/WFPC2 10136


    Post-AGB Stars in the Halo of M81


    Post-asymptotic-giant-branch {PAGB} stars of spectral types A-F are
    the brightest members of Population II. We have shown, using
    ground-based observations, that PAGB stars have tremendous potential
    as highly efficient standard candles and as tracers of halo
    populations and late stellar evolution. Our analysis of PAGB stars in
    archival HST images of M32, based on the equivalent of one orbit of
    HST time, precisely reproduces the accepted distance. We propose to
    obtain ACS/WFC and WFPC2 images of fields in the halo of M81, as
    another test of the PAGB method. We show that 4 orbits of HST data
    will produce a distance of comparable accuracy to the much more
    laborious Cepheid technique. If successful on M81, we will propose in
    the next cycle to measure the distance to Virgo using our method, a
    distance ladder that has only two rungs {trigonometric parallaxes of
    subdwarfs to calibrate PAGB stars in globular clusters, and then PAGB
    stars in Virgo}.


    NIC1/NIC2/NIC3 8792


    NICMOS Post-SAA calibration - CR Persistence Part 3


    A new procedure proposed to alleviate the CR-persistence problem of
    NICMOS. Dark frames will be obtained immediately upon exiting the SAA
    contour 23, and every time a NICMOS exposure is scheduled within 50
    minutes of coming out of the SAA. The darks will be obtained in
    parallel in all three NICMOS Cameras. The POST-SAA darks will be
    non-standard reference files available to users with a USEAFTER
    date/time mark. The keyword &#39;USEAFTER=date/time&#39; will also be added to
    the header of each POST-SAA DARK frame. The keyword must be populated
    with the time, in addition to the date, because HST crosses the SAA ~8
    times per day so each POST-SAA DARK will need to have the appropriate
    time specified, for users to identify the ones they need. Both the raw
    and processed images will be archived as POST-SAA DARKSs. Generally we
    expect that all NICMOS science/calibration observations started within
    50 minutes of leaving an SAA will need such maps to remove the CR
    persistence from the science images. Each observation will need its
    own CRMAP, as different SAA passages leave different imprints on the
    NICMOS detectors.


    WFPC2 10112


    HST Observations of Astrophysically Important Visual Binaries


    This is a continuation of a project begun in Cycle 7 and continued up
    through Cycle 11. The program consists of annual or biannual WFPC2 or
    FGS observations of three visual binary stars that will ultimately
    yield fundamental astrophysical results, once their orbits and masses
    are determined. Our targets are the following: {1} Procyon {P = 41
    yr}, for which our first WFPC2 images yielded an extremely accurate
    angular separation of the bright F star and its much fainter
    white-dwarf companion. Combined with ground-based astrometry of the
    bright star, our observation significantly revised downward the
    derived masses, and brought Procyon A into excellent agreement with
    theoretical evolutionary tracks for the first time. With the continued
    monitoring proposed here, we will obtain masses to an accuracy of
    better than 1%, providing a testbed for theories of both Sun- like
    stars and white dwarfs. {2} G 107-70, a close double white dwarf {P =
    19 yr} that promises to add two accurate masses to the tiny handful of
    white-dwarf masses that are directly known from dynamical
    measurements. {3} Mu Cas {P = 21 yr}, a famous metal- deficient G
    dwarf for which accurate masses will lead to the stars&#39; helium
    contents, with cosmological implications.


    FLIGHT OPERATIONS SUMMARY:


    Significant Spacecraft Anomalies: (The following are preliminary
    reports of potential non-nominal performance that will be
    investigated.) None


    COMPLETED OPS REQs: None


    OPS NOTES EXECUTED: None


    SCHEDULED SUCCESSFUL FAILURE TIMES
    FGS Gsacq 10 10
    FGS Reacq 6 6
    FHST Update 11 11
    LOSS of LOCK


    SIGNIFICANT EVENTS: None

  11. #11
    Join Date
    Jan 2004
    Posts
    1,085
    Hope you had a good day&#33;

    You needn&#39;t worry I had no intention of copying this string&#33; :P

  12. #12
    StarLab Guest
    They&#39;re still coming, hopefully soon this string will be pinned. B)

    HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science


    DAILY REPORT # 3839


    PERIOD COVERED: DOY 104


    OBSERVATIONS SCHEDULED


    ACS/HRC 10377


    ACS Earth Flats


    High signal sky flats will be obtained by observing the bright Earth
    with the HRC and WFC. These observations will be used to verify the
    accuracy of the flats currently used by the pipeline and will provide
    a comparison with flats derived via other techniques: L- flats from
    stellar observations, sky flats from stacked GO observations, and
    internal flats using the calibration lamps. Weekly coronagraphic
    monitoring is required to assess the changing position of the spots.


    ACS/WFC 10152


    A Snapshot Survey of a Complete Sample of X-ray Luminous Galaxy
    Clusters from Redshift 0.3 to 0.7


    We propose a public, uniform imaging survey of a well-studied,
    complete, and homogeneous sample of X-ray clusters. The sample of 73
    clusters spans the redshift range between 0.3-0.7. The samples spans
    almost 2 orders of magnitude of X-ray luminosity, where half of the
    sample has X-ray luminosities greater than 10^44 erg/s {0.5- 2.0 keV}.
    These snapshots will be used to obtain a fair census of the the
    morphology of cluster galaxies in the cores of clusters, to detect
    radial and tangential arc candidates, to detect optical jet
    candidates, and to provide an approximate estimate of the shear signal
    of the clusters themselves, and potentially an assessment of the
    contribution of large scale structure to lensing shear.


    ACS/WFC/NIC/NIC3/WFPC 10246 2 The HST survey of the Orion Nebula
    Cluster


    We propose a Treasury Program of 104 HST orbits to perform the
    definitive study of the Orion Nebula Cluster, the Rosetta stone of
    star formation. We will cover with unprecedented sensitivity {23-25
    mag}, dynamic range {~12 mag}, spatial resolution {50mas}, and
    simultaneous spectral coverage {5 bands} a ~450 square arcmin field
    centered on the Trapezium stars. This represents a tremendous gain
    over the shallow WFC1 study made in 1991 with the aberrated HST on an
    area ~15 times smaller. We maximize the HST observing efficiency using
    ACS/WFC and WFPC2 in parallel with two opposite roll angles, to cover
    the same total field. We will assemble the richest, most accurate and
    unbiased HR diagram for pre-main-sequence objects ever made. Combined
    with the optical spectroscopy already available for ~1000 sources and
    new deep near-IR imaging and spectroscopy {that we propose as Joint
    HST-NOAO observations}, we will be able to attack and possibly solve
    the most compelling questions on stellar evolution: the calibration of
    pre-main-sequence evolutionary tracks, mass segration and the
    variation of the initial mass function in different environments, the
    evolution of mass accretion rates vs. age and environment, disk
    dissipation in environments dominated by hard vs. soft-UV radiation,
    stellar multiplicity vs. disk fraction. In addition, we expect to
    discover and classify an unknown, but substantial, population of
    pre-Main Sequence binaries, low mass stars and brown dwarfs down to
    ~10 MJup. This is also the best possible way to discover dark
    silhouette disks in the outskirts of the Orion Nebula and study their
    evolutionary status through multicolor imaging. This program is timely
    and extremely well leveraged to other programs targeting Orion: the
    ACS H-alpha survey of the Orion Nebula, the recently completed 850ks
    ultradeep Chandra survey, the large GTO programs to be performed with
    SIRTF, plus the availability of 2MASS and various deep JHK surveys of
    the core recently done with 8m class telescopes.


    ACS/WFC/NIC3 10339


    PANS


    Type Ia supernovae {SNe Ia} provide the only direct evidence for an
    accelerating universe, an extraordinary result that needs the most
    rigorous test. The case for cosmic acceleration rests on the
    observation that SNe Ia at z = 0.5 are about 0.25 mag fainter than
    they would be in a universe without acceleration. A powerful and
    straightforward way to assess the reliability of the SN Ia measurement
    and the conceptual framework of its interpretation is to look for
    cosmic deceleration at z > 1. This would be a clear signature of a
    mixed dark-matter and dark-energy universe. Systematic errors in the
    SNe Ia result attributed to grey dust or cosmic evolution of the SN Ia
    peak luminosity would not show this change of sign. We have obtained a
    toehold on this putative ``epoch of deceleration&#39;&#39; with SN 1997ff at z
    = 1.7, and 3 more at z > 1 from our Cycle 11 program, all found and
    followed by HST. However, this is too important a test to rest on just
    a few objects, anyone of which could be subject to a lensed
    line-of-sight or misidentification. Here we propose to extend our
    measurement with observations of twelve SNe Ia in the range 1.0 < z <
    1.5 or 6 such SNe Ia and 1 ultradistant SN Ia at z = 2, that will be
    discovered as a byproduct from proposed Treasury and DD programs.
    These objects will provide a much firmer foundation for a conclusion
    that touches on important questions of fundamental physics.


    ACS/WFC/WFPC2 10402


    The Formation and Evolution of Spirals: An ACS and WFPC2 Imaging
    Survey of Nearby Galaxies


    Over 50% of galaxies in the local universe are spirals. Yet the star
    formation histories and evolution of this crucial population remain
    poorly understood. We propose to combine archival data with new
    ACS/WFC and WFPC2 observations of 11 galaxies, to tackle a
    comprehensive investigation of nearby spirals covering the entire
    spiral sequence. The new observations will fill a serious deficiency
    in HST&#39;s legacy, and maximize the scientific return of existing HST
    data. The filter combination of UBVI, and Halpha is ideal for studying
    stellar populations, dust properties, and the ISM. Our immediate
    scientific objectives are: {i} to use the resolved cluster
    populations, both young massive clusters and ancient globular clusters
    as a chronometer, to understand how spirals assembled as a function of
    time; {ii} study the rapid disruption properties of young clusters;
    and {iii} understand dust distributions in spirals from pc to kpc
    scales. Each of these goals provides an important step towards
    charting the evolution of galaxies, and an essential baseline for
    interpreting the galaxy populations being surveyed in both the early
    and present universe. The resolution of our survey, which exploits the
    excellent imaging capabilities of HST&#39;s two optical cameras, will
    enable us to understand the record of star cluster, and galaxy
    formation in a level of detail which is not possible for more distant
    systems. Finally, the proposed observations will provide a key to
    interpret an extensive, multiwavelength archive of space- and ground-
    based data at lower spatial resolution {SPITZER, CHANDRA, GALEX,
    NICMOS P alpha and H band imaging} for local spirals.


    NIC1/NIC2 10410


    Anisotropy and obscuration in the near-nuclear regions of powerful
    radio galaxies


    Despite the success of the orientation-based unified schemes for
    powerful radio sources, we are still far from understanding the
    distribution of obscuring material in the near-nuclear regions of such
    sources, and how this distribution evolves with radio power. Following
    on from our highly successful Cycle 7 pilot observations of Cygnus A,
    we propose a near-IR polarimetric survey of a complete sample of
    powerful radio galaxies in order map the near-nuclear illumination
    cones, and investigate the distribution of obscuring material on a 0.1
    to 1kpc scale. In particular, the observations will allow us to test
    the "receding torus model&#39;&#39; which predicts that the opening angles of
    the illumination cones are smaller in low redshift/low power radio
    galaxies than in their high redshift/high power counterparts.We will
    also investigate whether AGN- and jet-driven outflows have a
    substantial effect on distribution of obscuring material by "hollowing
    out&#39;&#39; the quasar illumination cones in the more powerful sources.
    Finally, by using our polarization maps to search for signs of
    intrinsic anisotropy in the near-IR continuum within the cones, we
    will investigate the geometry of the near-IR continuum emitting
    regions close to the quasar nuclei. These observations are not only
    crucial for our understanding of radio source unification, but also
    provide key information about the effects of AGN-induced outflows on
    the ISM of the host galaxies.


    NIC1/NIC2/NIC3 8792


    NICMOS Post-SAA calibration - CR Persistence Part 3


    A new procedure proposed to alleviate the CR-persistence problem of
    NICMOS. Dark frames will be obtained immediately upon exiting the SAA
    contour 23, and every time a NICMOS exposure is scheduled within 50
    minutes of coming out of the SAA. The darks will be obtained in
    parallel in all three NICMOS Cameras. The POST-SAA darks will be
    non-standard reference files available to users with a USEAFTER
    date/time mark. The keyword &#39;USEAFTER=date/time&#39; will also be added to
    the header of each POST-SAA DARK frame. The keyword must be populated
    with the time, in addition to the date, because HST crosses the SAA ~8
    times per day so each POST-SAA DARK will need to have the appropriate
    time specified, for users to identify the ones they need. Both the raw
    and processed images will be archived as POST-SAA DARKSs. Generally we
    expect that all NICMOS science/calibration observations started within
    50 minutes of leaving an SAA will need such maps to remove the CR
    persistence from the science images. Each observation will need its
    own CRMAP, as different SAA passages leave different imprints on the
    NICMOS detectors.


    FLIGHT OPERATIONS SUMMARY:


    Significant Spacecraft Anomalies: (The following are preliminary
    reports of potential non-nominal performance that will be
    investigated.) None


    COMPLETED OPS REQs: None


    OPS NOTES EXECUTED: None


    SCHEDULED SUCCESSFUL FAILURE TIMES
    FGS Gsacq 9 9
    FGS Reacq 5 5
    FHST Update 15 15
    LOSS of LOCK


    SIGNIFICANT EVENTS: None

  13. #13
    StarLab Guest
    Apparently there are no weekend updates...so here&#39;s the next one:

    HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science


    DAILY REPORT # 3840


    PERIOD COVERED: DOYs 105-107


    OBSERVATIONS SCHEDULED


    NIC1/NIC2/NIC3 8793


    NICMOS Post-SAA calibration - CR Persistence Part 4


    A new procedure proposed to alleviate the CR-persistence problem of
    NICMOS. Dark frames will be obtained immediately upon exiting the SAA
    contour 23, and every time a NICMOS exposure is scheduled within 50
    minutes of coming out of the SAA. The darks will be obtained in
    parallel in all three NICMOS Cameras. The POST-SAA darks will be
    non-standard reference files available to users with a USEAFTER
    date/time mark. The keyword &#39;USEAFTER=date/time&#39; will also be added to
    the header of each POST-SAA DARK frame. The keyword must be populated
    with the time, in addition to the date, because HST crosses the SAA ~8
    times per day so each POST-SAA DARK will need to have the appropriate
    time specified, for users to identify the ones they need. Both the raw
    and processed images will be archived as POST-SAA DARKSs. Generally we
    expect that all NICMOS science/calibration observations started within
    50 minutes of leaving an SAA will need such maps to remove the CR
    persistence from the science images. Each observation will need its
    own CRMAP, as different SAA passages leave different imprints on the
    NICMOS detectors.


    NIC1/NIC2/NIC3 8792


    NICMOS Post-SAA calibration - CR Persistence Part 3


    A new procedure proposed to alleviate the CR-persistence problem of
    NICMOS. Dark frames will be obtained immediately upon exiting the SAA
    contour 23, and every time a NICMOS exposure is scheduled within 50
    minutes of coming out of the SAA. The darks will be obtained in
    parallel in all three NICMOS Cameras. The POST-SAA darks will be
    non-standard reference files available to users with a USEAFTER
    date/time mark. The keyword &#39;USEAFTER=date/time&#39; will also be added to
    the header of each POST-SAA DARK frame. The keyword must be populated
    with the time, in addition to the date, because HST crosses the SAA ~8
    times per day so each POST-SAA DARK will need to have the appropriate
    time specified, for users to identify the ones they need. Both the raw
    and processed images will be archived as POST-SAA DARKSs. Generally we
    expect that all NICMOS science/calibration observations started within
    50 minutes of leaving an SAA will need such maps to remove the CR
    persistence from the science images. Each observation will need its
    own CRMAP, as different SAA passages leave different imprints on the
    NICMOS detectors.


    ACS/HRC/WFC 10436


    Black Hole Growth and the Black Hole Mass -- Bulge Relations for AGNs


    Recent work has shown that the mass of a black hole is tightly
    correlated with the bulge mass of its host galaxy. This relation needs
    to be understood in the context of black hole growth in its active
    phase. Highly accreting AGNs, like narrow line Seyfert 1 galaxies
    {NLS1s}, are found to lie below the black hole mass -- bulge velocity
    dispersion correlation of normal galaxies and broad line AGNs. This
    result was obtained using FWHM{[OIII]} as a surrogate for the bulge
    velocity dispersion. To test this result we propose to obtain high
    resolution images of 10 NLS1s that do not lie on the black hole
    mass--sigma relation and measure accurate bulge parameters {luminosity
    and effective radius}. We will obtain an alternate handle on the bulge
    velocity dispersion through the fundamental plane relations and also
    find the locus of these NLS1s on the black hole mass--bulge luminosity
    plane. Testing this result is crucial to understanding the role of
    accretion on black hole growth, the observed correlations of the black
    hole mass with the bulge, and the formation and evolution of galaxies.


    ACS/WFC/NIC2/WFPC 10413 2 Resolving the Red Giant Population in Early
    Type Galaxies


    This project addresses the fundamental issue of the age and abundance
    of the stellar populations in early type galaxies. We propose deep
    imaging observations with ACS/WFC in F606W, F814W, and NICMOS/NIC2 in
    F110W, F160W to create optical/IR color-magnitude diagrams of the
    upper red giant branch in the nearest example of a bona fide
    elliptical galaxy, NGC3379, and simultaneously in the disk and halo of
    its companion, the S0 galaxy NGC3384. These observations will build
    upon the results from our NICMOS study of NGC3379, which produced the
    first deep IR color-magnitude data for a normal, luminous elliptical
    galaxy. This is the most direct way to establish the metallicity,
    metallicity spread, and presence of intermediate age populations in
    these representative Hubble types, exploring their star formation
    histories and evolution. The data will enable comparison with M32, the
    M31 halo, NGC5128, and other nearby galaxies similarly observed with
    HST.


    ACS/HRC/WFC 10389


    ACS CCDs daily monitor - Cycle 13 - Part 2


    This program consists of a set of basic tests to monitor, the read
    noise, the development of hot pixels and test for any source of noise
    in ACS CCD detectors. The files, biases and dark will be used to
    create reference files for science calibration. This programme will be
    for the entire lifetime of ACS.


    NIC1/NIC2/NIC3 10380


    Cycle 13 NICMOS dark current, shading profile, and read noise
    monitoring program


    The purpose of this proposal is to monitor the dark current, read
    noise, and shading profile for all three NICMOS detectors throughout
    the duration of Cycle 13. This proposal is an essentially unchanged
    continuation of PID 9993 which cover the duration of Cycle 12.


    WFPC2 10363


    WFPC2 CYCLE 13 Intflat and Visflat Sweeps and Filter Rotation Anomaly
    Monitor


    Using intflat observations, this WFPC2 proposal is designed to monitor
    the pixel-to-pixel flatfield response and provide a linearity check.
    The intflat sequences, to be done once during the year, are similar to
    those from the Cycle 12 program 10075. The images will provide a
    backup database as well as allow monitoring of the gain ratios. The
    sweep is a complete set of internal flats, cycling through both
    shutter blades and both gains. The linearity test consists of a series
    of intflats in F555W, in each gain and each shutter. As in Cycle 12,
    we plan to continue to take extra visflat, intflat, and earthflat
    exposures to test the repeatability of filter wheel motions.


    NIC3 10337


    The COSMOS 2-Degree ACS Survey NICMOS Parallels


    The COSMOS 2-Degree ACS Survey NICMOS Parallels. This program is a
    companion to program 10092.


    ACS/HRC 10255


    A Never Before Explored Phase Space: Resolving Close White Dwarf / Red
    Dwarf


    We propose an ACS Snapshot imaging survey to resolve a well-defined
    sample of highly probable white dwarf plus red dwarf close binaries.
    These candidates were selected from a search for white dwarfs with
    infrared excess from the 2MASS database. They represent unresolved
    systems {separations less than approximately 2" in the 2MASS images}
    and are distributed over the whole sky. Our HST+ACS observations will
    be sensitive to a separation range {1-20 AU} never before probed by
    any means. The proposed study will be the first empirical test of
    binary star parameters in the post-AGB phase, and cannot be
    accomplished from the ground. By resolving as few as 20 of our ~100
    targets with HST, we will be able to characterize the distribution of
    orbital semi- major axes and secondary star masses.


    ACS/WFC/NIC/NIC3/W 10246 FPC2 The HST survey of the Orion Nebula
    Cluster


    We propose a Treasury Program of 104 HST orbits to perform the
    definitive study of the Orion Nebula Cluster, the Rosetta stone of
    star formation. We will cover with unprecedented sensitivity {23-25
    mag}, dynamic range {~12 mag}, spatial resolution {50mas}, and
    simultaneous spectral coverage {5 bands} a ~450 square arcmin field
    centered on the Trapezium stars. This represents a tremendous gain
    over the shallow WFC1 study made in 1991 with the aberrated HST on an
    area ~15 times smaller. We maximize the HST observing efficiency using
    ACS/WFC and WFPC2 in parallel with two opposite roll angles, to cover
    the same total field. We will assemble the richest, most accurate and
    unbiased HR diagram for pre-main-sequence objects ever made. Combined
    with the optical spectroscopy already available for ~1000 sources and
    new deep near-IR imaging and spectroscopy {that we propose as Joint
    HST-NOAO observations}, we will be able to attack and possibly solve
    the most compelling questions on stellar evolution: the calibration of
    pre-main-sequence evolutionary tracks, mass segration and the
    variation of the initial mass function in different environments, the
    evolution of mass accretion rates vs. age and environment, disk
    dissipation in environments dominated by hard vs. soft-UV radiation,
    stellar multiplicity vs. disk fraction. In addition, we expect to
    discover and classify an unknown, but substantial, population of
    pre-Main Sequence binaries, low mass stars and brown dwarfs down to
    ~10 MJup. This is also the best possible way to discover dark
    silhouette disks in the outskirts of the Orion Nebula and study their
    evolutionary status through multicolor imaging. This program is timely
    and extremely well leveraged to other programs targeting Orion: the
    ACS H-alpha survey of the Orion Nebula, the recently completed 850ks
    ultradeep Chandra survey, the large GTO programs to be performed with
    SIRTF, plus the availability of 2MASS and various deep JHK surveys of
    the core recently done with 8m class telescopes.


    ACS/WFC 10217


    The ACS Fornax Cluster Survey


    The two rich clusters nearest to the Milky Way, and the only large
    collections of early- type galaxies within ~ 25 Mpc, are the Virgo and
    Fornax Clusters. We propose to exploit the exceptional imaging
    capabilities of the ACS/WFC to carry out the most comprehensive
    imaging survey to date of early-type galaxies in Fornax: the ACS
    Fornax Cluster Survey. Deep ACS/WFC images -- in the F475W {g&#39;} and
    F850LP {z&#39;} bands -- will be acquired for 44 E, S0, dE, dE, N and dS0
    cluster members. In Cycle 11, we initiated a similar program targeting
    early-type galaxies in the Virgo Cluster {the ACS Virgo Cluster
    Survey; GO-9401}. Our proposed survey of Fornax would yield an
    extraordinary dataset which would complement that already in hand for
    Virgo, and allow a definitive study of the role played by environment
    in the structure, formation and evolution of early-type galaxies and
    their globular cluster systems, nuclei, stellar populations, dust
    content, nuclear morphologies and merger histories. It would also be a
    community resource for years to come and, together with the ACS Virgo
    Cluster Survey, constitute one of the lasting legacies of HST.


    NIC1 10208


    NICMOS Differential Imaging Search for Planetary Mass Companions to
    Nearby Young Brown Dwarfs


    We propose to use the differential spectral imaging capability of
    HST/NICMOS {NIC1} to search for planetary mass companions. We target
    the twelve most nearby {within 30 pc}, isolated {no known close
    companion}, and young {< 1Gyr} brown dwarfs. All of them have spectral
    type L and show signs of Lithium absorption, which clearly proves
    their substellar nature and youth. Planetary mass companions with
    masses down to 6 Jupiter masses, and at separations larger than 3 A.U.
    are bright enough for a direct detection with HST/NICMOS using the
    spectral differential imaging technique in two narrow-band filters
    placed on and off molecular bands. The proposed project has the
    potential to lead to the first direct detection of a planetary mass
    object in orbit around a nearby brown dwarf.


    ACS/WFC/NIC2 10189


    PANS-Probing Acceleration Now with Supernovae


    Type Ia supernovae {SNe Ia} provide the most direct evidence for an
    accelerating Universe, a result widely attributed to dark energy.
    Using HST in Cycle 11 we extended the Hubble diagram with 6 of the 7
    highest-redshift SNe Ia known, all at z>1.25, providing conclusive
    evidence of an earlier epoch of cosmic deceleration. The full sample
    of 16 new SNe Ia match the cosmic concordance model and are
    inconsistent with a simple model of evolution or dust as alternatives
    to dark energy. Understanding dark energy may be the biggest current
    challenge to cosmology and particle physics. To understand the nature
    of dark energy, we seek to measure its two most fundamental
    properties: its evolution {i.e., dw/dz}, and its recent equation of
    state {i.e., w{z=0}}. SNe Ia at z>1, beyond the reach of the ground
    but squarely within the reach of HST with ACS, are crucial to break
    the degeneracy in the measurements of these two basic aspects of dark
    energy. The SNe Ia we have discovered and measured with HST in Cycle
    11, now double the precision of our knowledge of both properties. Here
    we propose to quadruple the sample of SNe Ia at z>1 in the next two
    cycles, complementing on-going surveys from the ground at z<1, and
    again doubling the precision of dark energy constraints. Should the
    current best fit model prove to be the correct one, the precision
    expected from the current proposal will suffice to rule out a
    cosmological constant at the 99% confidence level. Whatever the
    result, these objects will provide the basis with which to extend our
    empirical knowledge of this newly discovered and dominant component of
    the Universe, and will remain one of the most significant legacies of
    HST. In addition, our survey and follow-up data will greatly enhance
    the value of the archival data within the target Treasury fields for
    galaxy studies.


    NIC2 10177


    Solar Systems In Formation: A NICMOS Coronagraphic Survey of
    Protoplanetary and Debris Disks


    Until recently, despite decades of concerted effort applied to
    understanding the formation processes that gave birth to our solar
    system, the detailed morphology of circumstellar material that must
    eventually form planets has been virtually impossible to discern. The
    advent of high contrast, coronagraphic imaging as implemented with the
    instruments aboard HST has dramatically enhanced our understanding of
    natal planetary system formation. Even so, only a handful of evolved
    disks {~ 1 Myr and older} have been imaged and spatially resolved in
    light scattered from their constituent grains. To elucidate the
    physical processes and properties in potentially planet-forming
    circumstellar disks, and to understand the nature and evolution of
    their grains, a larger spatially resolved and photometrically reliable
    sample of such systems must be observed. Thus, we propose a highly
    sensitive circumstellar disk imaging survey of a well-defined and
    carefully selected sample of YSOs {1-10 Myr T Tau and HAeBe stars} and
    {> app 10 Myr} main sequence stars, to probe the posited epoch of
    planetary system formation, and to provide this critically needed
    imagery. Our resolved images will shed light on the spatial
    distributions of the dust in these thermally emissive disks. In
    combination with their long wavelength SEDs the physical properties of
    the grains will be discerned, or constrained by our photometrically
    accurate surface brightness sensitivity limits for faint disks which
    elude detection. Our sample builds on the success of the exploratory
    GTO 7233 program, using two-roll per orbit PSF-subtracted NICMOS
    coronagraphy to provide the highest detection sensitivity to the
    smallest disks around bright stars which can be imaged with HST. Our
    sample will discriminate between proposed evolutionary scenarios while
    providing a legacy of cataloged morphologies for interpreting mid- and
    far-IR SEDs that the recently launched Spitzer Space Telescope will
    deliver.


    NIC2 10176


    Coronagraphic Survey for Giant Planets Around Nearby Young Stars


    A systematic imaging search for extra-solar Jovian planets is now
    possible thanks to recent progress in identifying "young stars near
    Earth". For most of the proposed young {<~ 30 Myrs} and nearby {<~ 60
    pc} targets, we can detect a few Jupiter-mass planets as close as a
    few tens of AUs from the primary stars. This represents the first time
    that potential analogs of our solar system - that is planetary systems
    with giant planets having semi-major axes comparable to those of the
    four giant planets of the Solar System - come within the grasp of
    existing instrumentation. Our proposed targets have not been observed
    for planets with the Hubble Space Telescope previously. Considering
    the very successful earlier NICMOS observations of low mass brown
    dwarfs and planetary disks among members of the TW Hydrae Association,
    a fair fraction of our targets should also turn out to posses low mass
    brown dwarfs, giant planets, or dusty planetary disks because our
    targets are similar to {or even better than} the TW Hydrae stars in
    terms of youth and proximity to Earth. Should HST time be awarded and
    planetary mass candidates be found, proper motion follow-up of
    candidate planets will be done with ground-based AOs.


    ACS/WFC 10174


    Dark-matter halos and evolution of high-z early-type galaxies


    Gravitational lensing and stellar dynamics provide two complementary
    methods to determine the mass distribution and evolution of luminous
    and dark-matter in early-type {E/S0} galaxies. The combined study of
    stellar dynamics and gravitational lensing allows one to break
    degeneracies inherent to each method separately, providing a clean
    probe of the internal structure of massive galaxies. Since most lens
    galaxies are at redshifts z=0.1-1.0, they also provide the required
    look-back time to study their structural and stellar-population
    evolution. We recently analyzed 5 E/S0 lens galaxies between z=0.5 and
    1.0, combining exquisite Hubble Space Telescope imaging data with
    kinematic data from ground-based Keck spectroscopy, placing the first
    precise constraints on the dark- matter mass fraction and its inner
    slope beyond the local Universe. To expand the sample to ~30 systems
    -- required to study potential trends and evolution in the E/S0 mass
    profiles -- we propose to target the 49 E/S0 lens-galaxy candidates
    discovered by Bolton et al. {2004} from the Sloan Digital Sky Survey
    {SDSS}. With the average lens rate being 40% and some systems having a
    lensing probability close to unity, we expect to discover ~20 strong
    gravitational lenses from the sample. This will triple the current
    sample of 9 E/S0 systems, with data in hand. With the sample of 30
    systems, we will be able to determine the average slope of the
    dark-matter and total mass profile of E/S0 galaxies to 10% and 4%
    accuracy, respectively. If present, we can simultaneously detect 10%
    evolution in the total mass slope with 95% confidence. This will
    provide unprecedented constraints on E/S0 galaxies beyond the local
    Universe and allow a stringent test of their formation scenarios and
    the standard cosmological model.


    NIC1 10143


    Ultracool companions to the nearest L dwarfs


    We propose to conduct the most sensitive survey to date for low mass
    companions to nearby L dwarfs. We will use NICMOS to image targets
    drawn from a volume-complete sample of 70 L dwarfs within 20 parsecs.
    The combination of infrared imaging and proximity will allow us to
    search for T dwarf companions at separations as small as 1.6 AU. This
    is crucial, since no ultracool binaries are currently known with
    separations exceeding 15 AU. Only 10 dwarfs in this sample have
    previous HST observations primarily at optical wavelengths. With the
    increased sensitivity of our survey, we will provide the most
    stringent test to date of brown dwarf models which envisage formation
    as ejected stellar embryos. In addition, our observations will be
    capable of detecting binaries with mass ratios as low as 0.3, and will
    therefore also test the apparent preference for equal-mass ultracool
    binaries. Finally, our observations offer the best prospect to date of
    detecting companions significantly cooler than the coolest t dwarf
    currently known.


    FGS 10106


    An Astrometric Calibration of the Cepheid Period-Luminosity Relation


    We propose to measure the parallaxes of 10 Galactic Cepheid variables.
    When these parallaxes {with 1-sigma precisions of 10% or better} are
    added to our recent HST FGS parallax determination of delta Cep
    {Benedict et al 2002}, we anticipate determining the Period-Luminosity
    relation zero point with a 0.03 mag precision. In addition to
    permitting the test of assumptions that enter into other Cepheid
    distance determination techniques, this calibration will reintroduce
    Galactic Cepheids as a fundamental step in the extragalactic distance
    scale ladder. A Period-Luminosity relation derived from solar
    metallicity Cepheids can be applied directly to extragalactic solar
    metallicity Cepheids, removing the need to bridge with the Large
    Magellanic Cloud and its associated metallicity complications.


    ACS/WFC/WFPC2 10092


    The COSMOS 2-Degree ACS Survey


    We will undertake a 2 square degree imaging survey {Cosmic Evolution
    Survey -- COSMOS} with ACS in the I {F814W} band of the VIMOS
    equatorial field. This wide field survey is essential to understand
    the interplay between Large Scale Structure {LSS} evolution and the
    formation of galaxies, dark matter and AGNs and is the one region of
    parameter space completely unexplored at present by HST. The
    equatorial field was selected for its accessibility to all
    ground-based telescopes and low IR background and because it will
    eventually contain ~100, 000 galaxy spectra from the VLT-VIMOS
    instrument. The imaging will detect over 2 million objects with I> 27
    mag {AB, 10 sigma}, over 35, 000 Lyman Break Galaxies {LBGs} and
    extremely red galaxies out to z ~ 5. COSMOS is the only HST project
    specifically designed to probe the formation and evolution of
    structures ranging from galaxies up to Coma-size clusters in the epoch
    of peak galaxy, AGN, star and cluster formation {z ~0.5 to 3}. The
    size of the largest structures necessitate the 2 degree field. Our
    team is committed to the assembly of several public ancillary datasets
    including the optical spectra, deep XMM and VLA imaging, ground-based
    optical/IR imaging, UV imaging from GALEX and IR data from SIRTF.
    Combining the full-spectrum multiwavelength imaging and spectroscopic
    coverage with ACS sub-kpc resolution, COSMOS will be Hubble&#39;s ultimate
    legacy for understanding the evolution of both the visible and dark
    universe.


    FLIGHT OPERATIONS SUMMARY:


    Significant Spacecraft Anomalies: (The following are preliminary
    reports of potential non-nominal performance that will be
    investigated.)


    HSTAR 9774: GSACQ(3,2,2) failed, Search Radius Limit on FGS 3 @
    107/2151z. Guide Star Acquisition GSACQ(3,2,2) at 21:45:04z failed to
    gyro control due to Search Radius Limit exceeded on FGS 3 at 21:51:32
    and again at 21:55:41z. 486 ESB "A0C" received. Full Maneuver Updates
    prior to failure had normal size errors. REacq(3,2,2)sheduled for
    107/23:13:47 - 23:19:31 also failed due to SRLEX on FGS#3.
    Observations affected: ACS 89 to 91,1,2 and WFPC 1. Under
    investigation.


    HSTAR 9775: GSacq (3,1,1) resulted in FLBU 1,0,1 @ 108/0112z
    GSacq(3,1,1) scheduled at 108/01:04:51z resulted in fine lock backup
    (1,0,1), due to scan step limit exceeded on FGS 3 at 108/01:12:11z.
    Possible Observations affected: WFPC 1. Previous FM updates scheduled
    for 108/00:41:14z and 00:43:59z both passed with small error. The
    following map scheduled for 108/01:55z had attitude errors of -8.089,
    -6.777 and -6.901 arcsec. Under investigation.


    COMPLETED OPS REQs: None


    OPS NOTES EXECUTED: None


    SCHEDULED SUCCESSFUL FAILURE TIMES
    FGS
    Gsacq 31 30 107/2145z
    (HSTAR 9774)
    FGS
    Reacq 21 20 107/2313z
    (HSTAR 9774)
    FHST Update 36 36
    LOSS of LOCK


    SIGNIFICANT EVENTS:None

  14. #14
    Join Date
    Nov 2004
    Posts
    55
    I think Altair is a great target to search for potential planets; the star is metal-rich, which has been shown to have a positive correlation with the probability of planets. Not to mention that they could be the first planets ever directly detected around an A-star.

  15. #15
    StarLab Guest
    HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science


    DAILY REPORT # 3841


    PERIOD COVERED: DOY 108


    OBSERVATIONS SCHEDULED


    ACS 10140


    Identification of a magnetic anomaly at Jupiter from satellite
    footprints


    Repeated imaging of Jupiter&#39;s aurora has shown that the northern main
    oval has a distorted &#39;kidney bean&#39; shape in the general range of
    90-140? System III longitude, which appears unchanged since 1994.
    While it is more difficult to observe the conjugate regions in the
    southern aurora, no corresponding distortion appears in the south.
    Recent improved accuracy in locating the satellite footprint auroral
    emissions has provided new information about the geometry of Jupiter&#39;s
    magnetic field in this and other areas. The study of the magnetic
    field provides us with insight into the state of matter and the
    dynamics deep down Jupiter. There is currently no other way to do this
    from orbit. The persistent pattern of the main oval implies a
    disturbance of the local magnetic field, and the increased latitudinal
    separation of the locus of satellite footprints from each other and
    from the main oval implies a locally weaker field strength. It is
    possible that these phenomena result from a magnetic anomaly in
    Jupiter&#39;s intrinsic magnetic field, as was proposed by A. Dessler in
    the 1970&#39;s. There is presently only limited evidence from the scarcity
    of auroral footprints observed in this longitude range. We propose to
    obtain HST UV images with specific observing geometries of Jupiter to
    determine the locations of the auroral footprints of Io, Europa, and
    Ganymede in cycle 13 to accurately determine the magnetic field
    geometry in the suggested anomaly region, and to either confirm or
    refute the suggestion of a local magnetic anomaly.


    ACS/HRC 10391


    Wavelength and Flux Calibration of the ACS prisms


    The wavelength calibration of the SBC {PR110L and PR130L} and HRC
    {PR200L} prisms will be established by observing a planetary nebula in
    the LMC and QSOs at carefully selected redshifts. Flux calibrations
    will be derived for each prism by observing white dwarf standards.


    ACS/HRC/WFC 10370


    CCD Hot Pixel Annealing


    Hot pixel annealing will continue to be performed once every 4 weeks.
    The CCD TECs will be turned off and heaters will be activated to bring
    the detector temperatures to about +20C. This state will be held for
    approximately 12 hours, after which the heaters are turned off, the
    TECs turned on, and the CCDs returned to normal operating condition.
    To assess the effectiveness of the annealing, a bias and four dark
    images will be taken before and after the annealing procedure for both
    WFC and HRC. The HRC darks are taken in parallel with the WFC darks.
    The charge transfer efficiency {CTE} of the ACS CCD detectors declines
    as damage due to on-orbit radiation exposure accumulates. This
    degradation has been closely monitored at regular intervals, because
    it is likely to determine the useful lifetime of the CCDs. We will now
    combine the annealling activity with the charge transfer efficiency
    monitoring and also merge into the routine dark image collection. To
    this end, the CTE monitoring exposures have been moved into this
    proposal . All the data for this program is acquired using internal
    targets {lamps} only, so all of the exposures should be taken during
    Earth occultation time {but not during SAA passages}. This program
    emulates the ACS pre-flight ground calibration and post-launch SMOV
    testing {program 8948}, so that results from each epoch can be
    directly compared. Extended Pixel Edge Response {EPER} and First Pixel
    Response {FPR} data will be obtained over a range of signal levels for
    both the Wide Field Channel {WFC}, and the High Resolution Channel
    {HRC}.


    ACS/HRC/WFC 10389


    ACS CCDs daily monitor - Cycle 13 - Part 2


    This program consists of a set of basic tests to monitor, the read
    noise, the development of hot pixels and test for any source of noise
    in ACS CCD detectors. The files, biases and dark will be used to
    create reference files for science calibration. This programme will be
    for the entire lifetime of ACS.


    ACS/HRC/WFC 10399


    Accurate and Robust Calibration of the Extragalactic Distance Scale
    with the Maser Galaxy NGC4258 II


    The extragalactic distance scale {EDS} is defined by a comparison of
    Cepheid Period- Luminosity {PL} relations for nearby galaxies and the
    LMC, whose uncertain distance is thereby the SOLE anchor. Studies of
    masers orbiting the central black hole in NGC4258 have provided the
    most accurate extragalactic distance ever {7.2+/-0.5 Mpc}, and new
    radio data and analysis techniques will reduce the uncertainty to <
    3.5% {0.07 mag} by 2005. Since this distance is well determined and
    based on geometric arguments, NGC4258 can provide a much needed new
    anchor for the EDS. Ultimately, the combination of an independent
    measurement of H0 and measurements of CMB fluctuations {e.g., WMAP}
    can be used to directly constrain cosmological parameters including
    the equation of state of dark energy. In our Cycle 12 proposal, we
    defined a program spanning two cycles. The Cycle 12 portion was
    accepted. We have acquired WFC images and are constructing well
    sampled PL relations in 3 colors {BVI}. The purpose of the Cycle 13
    observations is to address systematic sources of error and is crucial
    for the success of the entire program. To disentangle the effects of
    reddening and metallicity, and to characterize the effects of
    blending, we require 50 orbits to obtain H-band photometry
    {NICMOS/NIC2} and high resolution images {ACS/HRC}.


    ACS/HRC/WFC 10436


    Black Hole Growth and the Black Hole Mass -- Bulge Relations for AGNs


    Recent work has shown that the mass of a black hole is tightly
    correlated with the bulge mass of its host galaxy. This relation needs
    to be understood in the context of black hole growth in its active
    phase. Highly accreting AGNs, like narrow line Seyfert 1 galaxies
    {NLS1s}, are found to lie below the black hole mass -- bulge velocity
    dispersion correlation of normal galaxies and broad line AGNs. This
    result was obtained using FWHM{[OIII]} as a surrogate for the bulge
    velocity dispersion. To test this result we propose to obtain high
    resolution images of 10 NLS1s that do not lie on the black hole
    mass--sigma relation and measure accurate bulge parameters {luminosity
    and effective radius}. We will obtain an alternate handle on the bulge
    velocity dispersion through the fundamental plane relations and also
    find the locus of these NLS1s on the black hole mass--bulge luminosity
    plane. Testing this result is crucial to understanding the role of
    accretion on black hole growth, the observed correlations of the black
    hole mass with the bulge, and the formation and evolution of galaxies.


    ACS/WFC 10369


    ACS internal CTE monitor


    The charge transfer efficiency {CTE} of the ACS CCD detectors will
    decline as damage due to on-orbit radiation exposure accumulates. This
    degradation will be closely monitored at regular intervals, because it
    is likely to determine the useful lifetime of the CCDs. All the data
    for this program is acquired using internal targets {lamps} only, so
    all of the exposures should be taken during Earth occultation time
    {but not during SAA passages}. This program emulates the ACS
    pre-flight ground calibration and post-launch SMOV testing {program
    8948}, so that results from each epoch can be directly compared.
    Extended Pixel Edge Response {EPER} and First Pixel Response {FPR}
    data will be obtained over a range of signal levels for both the Wide
    Field Channel {WFC}, and the High Resolution Channel {HRC}.


    ACS/WFC 10412


    The host galaxies of dust-reddened quasars


    We have used the 2MASS near-infrared and FIRST radio surveys, together
    with the Palomar Observatory Sky Survey plates to select a sample of
    dust-reddened, radio- intermediate quasars. We wish to use ACS to
    study the host galaxies of these quasars. The dust reddening of the
    quasars makes it possible to study the hosts at rest-frame optical-UV
    wavelengths much more easily than the hosts of normal quasars of
    similar bolometric luminosity. Our study will compare the hosts of our
    dust-reddened quasars to those of normal quasars from the HST archive
    to test the hypothesis that dust-reddened quasars are young objects,
    whose hosts still show morphological evidence of recent merger events
    which triggered the quasar.


    FGS 10104


    Calibrating the Mass-Luminosity Relation at the End of the Main
    Sequence


    We propose to use HST-FGS1R to calibrate the mass-luminosity relation
    {MLR} for stars less massive than 0.2 Msun, with special emphasis on
    objects near the stellar/brown dwarf border. Our goals are to
    determine M_V values to 0.05 magnitude, masses to 5 than double the
    number of objects with masses determined to be less than 0.20 Msun.
    This program uses the combination of HST-FGS3/FGS1R at optical
    wavelengths and ground-based infrared interferometry to examine
    nearby, subarcsecond binary systems. The high precision measurements
    with HST-FGS3/FGS1R {to 1 mas in the separations} for these faint
    targets {V = 10--15} simply cannot be equaled by any ground based
    technique. As a result of these measurements, we are deriving high
    quality luminosities and masses for the components in the observed
    systems, and characterizing their spectral energy distributions from
    0.5 to 2.2 Mum. Several of the objects included have M < 0.1 Msun,
    placing them at the very end of the stellar main sequence. Three of
    the targets are brown dwarf candidates, including the current low mass
    record holder, GJ 1245C, with a mass of 0.062 +/- 0.004 Msun. The
    payoff of this proposal is high because all 10 of the systems selected
    have already been resolved with HST- FGS3/FGS1R during Cycles 5--10
    and contain most of the reddest objects for which masses can be
    determined.


    NIC2 10418


    Morphologies and Color Gradients of Galaxies with the Oldest Stellar
    Populations at High Redshifts We have isolated a sample of 9 luminous
    {~2L*} galaxies with the very oldest stellar populations at their
    respective redshifts. The galaxies have been found in radio-source
    fields chosen to be at the key redshifts z~1.5 and z~2.5, which allow
    the cleanest separation of old stellar populations from highly
    reddened starbursts with colors derived from standard filter
    combinations. Ground-based observations in excellent seeing and with
    adaptive optics of 3 of these galaxies indicate that all 3 are
    dominated by well relaxed disks of old stars, suggesting that the
    first large stellar systems to form in the universe were disks in
    which star formation proceeded extremely rapidly and efficiently. In
    order to test this conjecture, we are requesting NICMOS2 exposures of
    our sample to obtain high S/N imaging in the F160W filter to determine
    detailed morphologies of the old stellar population, coupled with
    either NICMOS2 F110W or ACS F814W exposures {depending on redshift} to
    determine color gradients and/or other systematic color variations
    that might provide clues to formation processes.


    WFPC2 10359


    WFPC2 CYCLE 13 Standard Darks


    This dark calibration program obtains dark frames every week in order
    to provide data for the ongoing calibration of the CCD dark current
    rate, and to monitor and characterize the evolution of hot pixels.
    Over an extended period these data will also provide a monitor of
    radiation damage to the CCDs.


    WFPC2 10363


    WFPC2 CYCLE 13 Intflat and Visflat Sweeps and Filter Rotation Anomaly
    Monitor


    Using intflat observations, this WFPC2 proposal is designed to monitor
    the pixel-to-pixel flatfield response and provide a linearity check.
    The intflat sequences, to be done once during the year, are similar to
    those from the Cycle 12 program 10075. The images will provide a
    backup database as well as allow monitoring of the gain ratios. The
    sweep is a complete set of internal flats, cycling through both
    shutter blades and both gains. The linearity test consists of a series
    of intflats in F555W, in each gain and each shutter. As in Cycle 12,
    we plan to continue to take extra visflat, intflat, and earthflat
    exposures to test the repeatability of filter wheel motions.


    FLIGHT OPERATIONS SUMMARY:


    Significant Spacecraft Anomalies: (The following are preliminary
    reports of potential non-nominal performance that will be
    investigated.) None


    COMPLETED OPS REQs: None


    OPS NOTES EXECUTED: None


    SCHEDULED SUCCESSFUL FAILURE TIMES
    FGS Gsacq 12 12
    FGS Reacq 6 6
    FHST Update 20 20
    LOSS of LOCK


    SIGNIFICANT EVENTS: None

  16. #16
    StarLab Guest
    HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science


    DAILY REPORT # 3843


    PERIOD COVERED: DOY 110


    OBSERVATIONS SCHEDULED


    ACS/HRC 10391


    Wavelength and Flux Calibration of the ACS prisms


    The wavelength calibration of the SBC {PR110L and PR130L} and HRC
    {PR200L} prisms will be established by observing a planetary nebula in
    the LMC and QSOs at carefully selected redshifts. Flux calibrations
    will be derived for each prism by observing white dwarf standards.


    ACS/HRC 10435


    Merger-Induced Populations in Early-Type Galaxy Cores


    Hierarchical formation models predict that early-type galaxies are
    built up over an extended period from mergers of smaller systems, a
    process which should leave long- lived signatures in their light
    profiles and stellar population colors. Merger events should have
    continued up to relatively recent times {the last 1-5 Gyr}, and many
    ellipticals and S0 bulges should therefore show evidence of multiple,
    discrete, intermediate-age populations. Although there is substantial
    observational support for a dissipational merger origin for some
    early-type galaxies, most do not exhibit the expected anomalies in
    either their light profiles or color distributions. However, existing
    searches {mainly in the V and I bands} have not probed very deeply.
    Here we propose high resolution, broad-band, near-ultraviolet
    {2500-3400 A} imaging of the cores of bright early-type galaxies. This
    is the most sensitive probe available for the detection of
    spatially-segregated, multiple population components with ages in the
    range 1-5 Gyr. Our sample consists of dust- and AGN-free systems with
    both normal and mildly anomalous central light profiles. There is very
    little existing information on the near-UV structure of early-type
    galaxies, and our program would effectively explore new terrain.


    ACS/HRC/WFC 10389


    ACS CCDs daily monitor - Cycle 13 - Part 2


    This program consists of a set of basic tests to monitor, the read
    noise, the development of hot pixels and test for any source of noise
    in ACS CCD detectors. The files, biases and dark will be used to
    create reference files for science calibration. This programme will be
    for the entire lifetime of ACS.


    ACS/HRC/WFC 10436


    Black Hole Growth and the Black Hole Mass -- Bulge Relations for AGNs


    Recent work has shown that the mass of a black hole is tightly
    correlated with the bulge mass of its host galaxy. This relation needs
    to be understood in the context of black hole growth in its active
    phase. Highly accreting AGNs, like narrow line Seyfert 1 galaxies
    {NLS1s}, are found to lie below the black hole mass -- bulge velocity
    dispersion correlation of normal galaxies and broad line AGNs. This
    result was obtained using FWHM{[OIII]} as a surrogate for the bulge
    velocity dispersion. To test this result we propose to obtain high
    resolution images of 10 NLS1s that do not lie on the black hole
    mass--sigma relation and measure accurate bulge parameters {luminosity
    and effective radius}. We will obtain an alternate handle on the bulge
    velocity dispersion through the fundamental plane relations and also
    find the locus of these NLS1s on the black hole mass--bulge luminosity
    plane. Testing this result is crucial to understanding the role of
    accretion on black hole growth, the observed correlations of the black
    hole mass with the bulge, and the formation and evolution of galaxies.


    ACS/WFC 10174


    Dark-matter halos and evolution of high-z early-type galaxies


    Gravitational lensing and stellar dynamics provide two complementary
    methods to determine the mass distribution and evolution of luminous
    and dark-matter in early-type {E/S0} galaxies. The combined study of
    stellar dynamics and gravitational lensing allows one to break
    degeneracies inherent to each method separately, providing a clean
    probe of the internal structure of massive galaxies. Since most lens
    galaxies are at redshifts z=0.1-1.0, they also provide the required
    look-back time to study their structural and stellar-population
    evolution. We recently analyzed 5 E/S0 lens galaxies between z=0.5 and
    1.0, combining exquisite Hubble Space Telescope imaging data with
    kinematic data from ground-based Keck spectroscopy, placing the first
    precise constraints on the dark- matter mass fraction and its inner
    slope beyond the local Universe. To expand the sample to ~30 systems
    -- required to study potential trends and evolution in the E/S0 mass
    profiles -- we propose to target the 49 E/S0 lens-galaxy candidates
    discovered by Bolton et al. {2004} from the Sloan Digital Sky Survey
    {SDSS}. With the average lens rate being 40% and some systems having a
    lensing probability close to unity, we expect to discover ~20 strong
    gravitational lenses from the sample. This will triple the current
    sample of 9 E/S0 systems, with data in hand. With the sample of 30
    systems, we will be able to determine the average slope of the
    dark-matter and total mass profile of E/S0 galaxies to 10% and 4%
    accuracy, respectively. If present, we can simultaneously detect 10%
    evolution in the total mass slope with 95% confidence. This will
    provide unprecedented constraints on E/S0 galaxies beyond the local
    Universe and allow a stringent test of their formation scenarios and
    the standard cosmological model.


    ACS/WFC 10369


    ACS internal CTE monitor


    The charge transfer efficiency {CTE} of the ACS CCD detectors will
    decline as damage due to on-orbit radiation exposure accumulates. This
    degradation will be closely monitored at regular intervals, because it
    is likely to determine the useful lifetime of the CCDs. All the data
    for this program is acquired using internal targets {lamps} only, so
    all of the exposures should be taken during Earth occultation time
    {but not during SAA passages}. This program emulates the ACS
    pre-flight ground calibration and post-launch SMOV testing {program
    8948}, so that results from each epoch can be directly compared.
    Extended Pixel Edge Response {EPER} and First Pixel Response {FPR}
    data will be obtained over a range of signal levels for both the Wide
    Field Channel {WFC}, and the High Resolution Channel {HRC}.


    ACS/WFC 10374


    ACS photometric Stability


    This program consists of three parts. In the first part we will
    observe a subset of the ACS white dwarfs with HRC and ACS to verify
    repeatability to ~0.2%, because the filter shifts are based on
    photometric differences between stars of ~1%. These observations are
    also required to establish relative magnitudes of the primary WD
    standards at the 0.1% level. Targets should be GD153 and G191B2B,
    which seems to have the largest V mag error of ~0.008 mag. One orbit
    on the most important filters, including the grism and the prisms,
    should be expended with each camera for both stars for a total of 4
    orbits. In the second part will observe with HRC and WFC a solar
    analog star, P330E, to estimate any shifts in the short and the long
    wavelength cutoffs of selected filters. Complete filter bandpasses can
    be derived directly from the ratio of grism observations with and
    without the filter in place. The grism is on filter wheel 1, while
    four filters of interest F330W, F344N, F660N, and F814W are on wheel
    2. Each grism observation requires 3 settings: filter alone,
    filter+grism, and grism alone. In the third part we obtain high S/N
    photometric and spectroscopic observations of three red stars, VB-8
    {M7}, 2M0038+18 {L3.5} and 2M0559-14 {T5} with HRC and WFC to verify
    the photometry at the new standard position and to obtain accurate
    calibration {1% or better} of the grism spectra.


    ACS/WFC 10412


    The host galaxies of dust-reddened quasars


    We have used the 2MASS near-infrared and FIRST radio surveys, together
    with the Palomar Observatory Sky Survey plates to select a sample of
    dust-reddened, radio- intermediate quasars. We wish to use ACS to
    study the host galaxies of these quasars. The dust reddening of the
    quasars makes it possible to study the hosts at rest-frame optical-UV
    wavelengths much more easily than the hosts of normal quasars of
    similar bolometric luminosity. Our study will compare the hosts of our
    dust-reddened quasars to those of normal quasars from the HST archive
    to test the hypothesis that dust-reddened quasars are young objects,
    whose hosts still show morphological evidence of recent merger events
    which triggered the quasar.


    ACS/WFC/WFPC2 10402


    The Formation and Evolution of Spirals: An ACS and WFPC2 Imaging
    Survey of Nearby Galaxies


    Over 50% of galaxies in the local universe are spirals. Yet the star
    formation histories and evolution of this crucial population remain
    poorly understood. We propose to combine archival data with new
    ACS/WFC and WFPC2 observations of 11 galaxies, to tackle a
    comprehensive investigation of nearby spirals covering the entire
    spiral sequence. The new observations will fill a serious deficiency
    in HST&#39;s legacy, and maximize the scientific return of existing HST
    data. The filter combination of UBVI, and Halpha is ideal for studying
    stellar populations, dust properties, and the ISM. Our immediate
    scientific objectives are: {i} to use the resolved cluster
    populations, both young massive clusters and ancient globular clusters
    as a chronometer, to understand how spirals assembled as a function of
    time; {ii} study the rapid disruption properties of young clusters;
    and {iii} understand dust distributions in spirals from pc to kpc
    scales. Each of these goals provides an important step towards
    charting the evolution of galaxies, and an essential baseline for
    interpreting the galaxy populations being surveyed in both the early
    and present universe. The resolution of our survey, which exploits the
    excellent imaging capabilities of HST&#39;s two optical cameras, will
    enable us to understand the record of star cluster, and galaxy
    formation in a level of detail which is not possible for more distant
    systems. Finally, the proposed observations will provide a key to
    interpret an extensive, multiwavelength archive of space- and ground-
    based data at lower spatial resolution {SPITZER, CHANDRA, GALEX,
    NICMOS P alpha and H band imaging} for local spirals.


    FGS 10106


    An Astrometric Calibration of the Cepheid Period-Luminosity Relation


    We propose to measure the parallaxes of 10 Galactic Cepheid variables.
    When these parallaxes {with 1-sigma precisions of 10% or better} are
    added to our recent HST FGS parallax determination of delta Cep
    {Benedict et al 2002}, we anticipate determining the Period-Luminosity
    relation zero point with a 0.03 mag precision. In addition to
    permitting the test of assumptions that enter into other Cepheid
    distance determination techniques, this calibration will reintroduce
    Galactic Cepheids as a fundamental step in the extragalactic distance
    scale ladder. A Period-Luminosity relation derived from solar
    metallicity Cepheids can be applied directly to extragalactic solar
    metallicity Cepheids, removing the need to bridge with the Large
    Magellanic Cloud and its associated metallicity complications.


    FGS 10386


    Long Term Monitoring of FGS1r in Position Mode


    It is known from our experience with FGS3, and later with FGS1r, that
    an FGS on orbit experiences long term evolution, presumably due to
    disorption of water from the instrument&#39;s graphite epoxy composites.
    This manifests principally as a change in the plate scale and
    secondarily as a change in the geometric distortions. These effects
    are well modeled by adjustments to the rhoA and kA parameters which
    are used to transform the star selector servo angles into FGS {x, y}
    detector space coordinates. By observing the relative positions of
    selected stars in a standard cluster at a fixed telescope pointing and
    orientation, the evolution of rhoA and kA can be monitored and
    calibrated to preserve the astrometric performance of FGS1r.


    WFPC2 9964


    Dynamical Masses of White Dwarfs from Resolved Sirius-Like Binaries


    In Cycle 8 we initiated a WFPC2 snapshot survey for resolved,
    ``Sirius-like&#39;&#39; systems containing hot white-dwarf companions of
    cooler main-sequence stars. Out of 17 systems observed to date, 8 have
    been resolved with WFPC2 by using UV filters. Two of the resolved
    systems---56 Persei and Zeta Cygni---have predicted or known orbital
    periods short enough that dynamical masses can be determined for the
    white dwarfs within reasonable times. These would thus add to the
    extremely small number of white dwarfs presently having accurately and
    directly measured masses. We propose to image them annually in the UV
    with WFPC2. In addition, we will observe Zeta Cyg with FGS in order to
    measure the absolute motion of the optical component, needed for the
    mass solution. We also propose to observe Sirius itself with WFPC2
    over the next 3 Cycles. The resulting astrometric data will not only
    greatly improve the precision of the binary orbit and the dynamical
    mass measurements for both the main-sequence and white-dwarf
    components, but will also test definitively for the claimed presence
    of a third body in this famous system.


    FLIGHT OPERATIONS SUMMARY:


    Significant Spacecraft Anomalies: (The following are preliminary
    reports of potential non-nominal performance that will be
    investigated.)


    HSTAR 9783: Gsacq(2,3,3) results in Fine Lock Backup @ 111/0217z.
    At 111/02:16:50 GSacq(2,3,3) scheduled at 111/02:13:41 resulted in
    fine lock backup (2,0,2) due to scan step limit exceeded on FGS 3.
    Observations affected: NIC 30-31, ACS 114-117. Under investigation.


    COMPLETED OPS REQs:
    17421-0 Genslew for proposal 10263 - slot 13 @ 110/1657z
    17422-0 Genslew for proposal 10263 - slot 12 @ 110/1659z
    17422-0 Genslew for proposal 10330 - slot 01 @ 110/1700z
    17423-0 Genslew for proposal 10330 - slot 02 @ 110/1702z


    OPS NOTES EXECUTED: None


    SCHEDULED SUCCESSFUL FAILURE TIMES
    FGS Gsacq 08 08
    FGS Reacq 07 07
    FHST Update 16 16
    LOSS of LOCK


    SIGNIFICANT EVENTS: None

  17. #17
    StarLab Guest
    Well, it&#39;s certainly been a while, so here&#39;s the next one:


    HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science


    DAILY REPORT # 3844


    PERIOD COVERED: DOY 111


    OBSERVATIONS SCHEDULED


    ACS/HRC 10330


    Coronagraphic search for disks around nearby stars


    We will use the coronagraphic and imaging modes of the High Resolution
    camera to study of the role of circumstellar disks in planetary system
    formation over timescales of ~1-1000 Myr. Our targets comprise pre
    Main-Sequence {MS} and MS stars, selected by infrared excess, and
    targets selected from SIRTF surveys. Some targets, like Beta Pictoris
    have debris disks that have been detected at optical or near-IR
    wavelengths, while others have disks inferred from mid-IR or ISO
    observations. We will obtain multicolor images of each target&#39;s
    circumstellar environment for the purpose of {1} detecting and
    characterizing disk morphologies over all scales {including warps and
    regions of enhanced or depleted density}, and {2} seeking evidence of
    embedded planets. Direct and occulted images will be recorded for
    studying the disks within 2 arcseconds of these targets; the
    coronagraph will be used to image the outer regions of the disks.
    Together with existing infrared observations, we will provide
    constraints on the sizes, distribution, and composition of dust
    grains. Unconfirmed disks will first be imaged in F606W, and if they
    exist we may later observe them in F435W and F814W.


    ACS/HRC 10391


    Wavelength and Flux Calibration of the ACS prisms


    The wavelength calibration of the SBC {PR110L and PR130L} and HRC
    {PR200L} prisms will be established by observing a planetary nebula in
    the LMC and QSOs at carefully selected redshifts. Flux calibrations
    will be derived for each prism by observing white dwarf standards.


    ACS/HRC/WFC 10263


    SAINTS - Supernova 1987A INTensive Survey


    SAINTS is a program to observe SN 1987A, the brightest supernova in
    383 years, as it transforms into supernova remnant {SNR} 1987A, the
    youngest supernova remnant. HST is the unique and perfect match in
    scale and in field for spatially-resolved observations of SN 1987A.
    Rapid changes are taking place in a violent encounter between the
    fastest-moving debris and the circumstellar ring. This one-time-only
    event, leading to suddenly appearing hotspots and new emission that
    can reveal previously hidden gas, is powered by shocks that can be
    studied simultaneously with HST and with Chandra to great advantage.
    Both the optical and X-ray flux from the ring are rising rapidly so
    prompt observations are needed in Cycle 13. Our previous observations
    reveal a remarkable reverse shock moving upstream through the
    expanding debris. The reverse shock provides a powerful tool for
    dissecting the radial structure of the vanished star. The debris from
    the explosion itself, still excited by radioactivity, is now well
    resolved by ACS and seen to be aspherical, providing direct clues to
    the mechanism of the explosion. Many questions about SN 1987A remain
    unanswered. SAINTS is a comprehensive attempt to use HST to establish
    the facts of SN 1987A, help to answer interesting questions, and to
    observe the birth of SNR 1987A.


    ACS/WFC 10369


    ACS internal CTE monitor


    The charge transfer efficiency {CTE} of the ACS CCD detectors will
    decline as damage due to on-orbit radiation exposure accumulates. This
    degradation will be closely monitored at regular intervals, because it
    is likely to determine the useful lifetime of the CCDs. All the data
    for this program is acquired using internal targets {lamps} only, so
    all of the exposures should be taken during Earth occultation time
    {but not during SAA passages}. This program emulates the ACS
    pre-flight ground calibration and post-launch SMOV testing {program
    8948}, so that results from each epoch can be directly compared.
    Extended Pixel Edge Response {EPER} and First Pixel Response {FPR}
    data will be obtained over a range of signal levels for both the Wide
    Field Channel {WFC}, and the High Resolution Channel {HRC}.


    ACS/WFC/WFPC2 10129


    Resolving Globular Clusters in NGC 1399


    We intend to use the ACS/WFC to measure structural parameters {half
    light radius, King core radius and concentration parameter} of
    individual globular clusters {GCs} in NGC 1399. Very little is known
    about structural parameters of globular clusters as a function of
    radius outside the Local Group. The proposed observations, arranged in
    a 3x3 ACS mosaic, will allow us to perform the first detailed
    wide-field study of structural parameters of globular clusters in a
    giant elliptical galaxy. In particular we will: 1} study the
    size-galactocentric distance relation of globular clusters out to ~55
    kpc {~1.6 eff. radius of the GCS} and determine whether the observed
    differences in sizes between metal-rich and metal-poor globular
    cluster in early-type galaxies are primordial and thereby reflect
    fundamental differences in formation, or are due to projection
    effects; 2} match the GC position observed with HST/ACS with X-ray
    binaries identified over the full Chandra field, and use the above
    sizes to constrain physical models for X-ray binary formation in GCs.
    3} The wealth of ground-based data available for this system
    {photometry+spectroscopy}, will allow us to correlate the structural
    properties with other GC properties, such as their chemical
    composition, luminosity, etc.


    NIC1/NIC2 10410


    Anisotropy and obscuration in the near-nuclear regions of powerful
    radio galaxies


    Despite the success of the orientation-based unified schemes for
    powerful radio sources, we are still far from understanding the
    distribution of obscuring material in the near-nuclear regions of such
    sources, and how this distribution evolves with radio power. Following
    on from our highly successful Cycle 7 pilot observations of Cygnus A,
    we propose a near-IR polarimetric survey of a complete sample of
    powerful radio galaxies in order map the near-nuclear illumination
    cones, and investigate the distribution of obscuring material on a 0.1
    to 1kpc scale. In particular, the observations will allow us to test
    the "receding torus model&#39;&#39; which predicts that the opening angles of
    the illumination cones are smaller in low redshift/low power radio
    galaxies than in their high redshift/high power counterparts.We will
    also investigate whether AGN- and jet-driven outflows have a
    substantial effect on distribution of obscuring material by "hollowing
    out&#39;&#39; the quasar illumination cones in the more powerful sources.
    Finally, by using our polarization maps to search for signs of
    intrinsic anisotropy in the near-IR continuum within the cones, we
    will investigate the geometry of the near-IR continuum emitting
    regions close to the quasar nuclei. These observations are not only
    crucial for our understanding of radio source unification, but also
    provide key information about the effects of AGN-induced outflows on
    the ISM of the host galaxies.


    NIC1/NIC2/NIC3 8793


    NICMOS Post-SAA calibration - CR Persistence Part 4


    A new procedure proposed to alleviate the CR-persistence problem of
    NICMOS. Dark frames will be obtained immediately upon exiting the SAA
    contour 23, and every time a NICMOS exposure is scheduled within 50
    minutes of coming out of the SAA. The darks will be obtained in
    parallel in all three NICMOS Cameras. The POST-SAA darks will be
    non-standard reference files available to users with a USEAFTER
    date/time mark. The keyword &#39;USEAFTER=date/time&#39; will also be added to
    the header of each POST-SAA DARK frame. The keyword must be populated
    with the time, in addition to the date, because HST crosses the SAA ~8
    times per day so each POST-SAA DARK will need to have the appropriate
    time specified, for users to identify the ones they need. Both the raw
    and processed images will be archived as POST-SAA DARKSs. Generally we
    expect that all NICMOS science/calibration observations started within
    50 minutes of leaving an SAA will need such maps to remove the CR
    persistence from the science images. Each observation will need its
    own CRMAP, as different SAA passages leave different imprints on the
    NICMOS detectors.


    WFPC2 10363


    WFPC2 CYCLE 13 Intflat and Visflat Sweeps and Filter Rotation Anomaly
    Monitor


    Using intflat observations, this WFPC2 proposal is designed to monitor
    the pixel-to-pixel flatfield response and provide a linearity check.
    The intflat sequences, to be done once during the year, are similar to
    those from the Cycle 12 program 10075. The images will provide a
    backup database as well as allow monitoring of the gain ratios. The
    sweep is a complete set of internal flats, cycling through both
    shutter blades and both gains. The linearity test consists of a series
    of intflats in F555W, in each gain and each shutter. As in Cycle 12,
    we plan to continue to take extra visflat, intflat, and earthflat
    exposures to test the repeatability of filter wheel motions.


    FLIGHT OPERATIONS SUMMARY:


    Significant Spacecraft Anomalies: (The following are preliminary
    reports of potential non-nominal performance that will be
    investigated.)


    HSTAR 9784: ACS TA Failed due to Guide Star Acg failure @ 111/1724z.
    ACS TA (target acquisition) scheduled at 111/17:23:16 (HD-100623)
    failed due to REACQ failure (HSTAR#9785).Observations affected: ACS
    139-142; Proposal 10330, titled Coronagraphic search for disks around
    nearby stars. Under investigation.


    HSTAR 9785: REACQ(2,1,2) fails to RGA control, scan step limit
    exceeded on FGS 2. REACQ(2,1,2) at 111/17:17:32 ended in gyro control
    due to 4 occurrences of scan step limit exceeded on FGS 2 beginning at
    17:19:41. Initial GSACQ(2,1,2) at 15:42:17 was successful with no scan
    step limits exceeded. ACS target acquisition failed due to this REACQ
    failure (HSTAR 9784). Under investigation.


    Observations affected: ACS 139 to 142.


    COMPLETED OPS REQs: None


    OPS NOTES EXECUTED:
    1331-0 Change JERRCNT Limit @111/2130z


    SCHEDULED SUCCESSFUL FAILURE TIMES
    FGS Gsacq 07 07
    FGS
    Reacq 12 11
    111/1720z(HSTAR#9785)
    FHST Update 08 08
    LOSS of LOCK


    SIGNIFICANT EVENTS: None

  18. #18
    StarLab Guest
    Okay, so they use a lot of technical terms - it is still an easy skim-through, though...

  19. #19
    Join Date
    May 2005
    Posts
    155
    Hey StarLab, I found something you might be interested in. See below link, it&#39;s an article about the Hubbles 15th birthday(toady&#33, they&#39;ve got some new photos of two of the telescope&#39;s most popular targets: the M51 Whirlpool Galaxy and the Eagle Nebula.

    Happy 15th birthday Hubble.

  20. #20
    StarLab Guest
    Cool stuff, Tyrie&#33; And now, here we have....

    HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science


    DAILY REPORT # 3845


    PERIOD COVERED: DOYs 112-114


    OBSERVATIONS SCHEDULED


    ACS/HRC/WFPC2 9827


    UV extinction by dust in unexplored LMC environments


    The ensemble of results from studies of the UV extinction in the Milky
    Way, Magellanic Clouds {MC}, M31 and M33, indicates a complex
    dependence of the dust properties with environment, where starburst
    activity and metallicity are relevant factors. Work in the LMC to
    date, based on IUE data, has several drawbacks: a} only supergiants
    could be used, b} they all have moderate extinction, c} the IUE S/N is
    limited, d} the large IUE slit may include light from other sources,
    such as scattered light from dust or faint companion stars, e} studies
    are confined to few {extreme} environments. We propose to obtain UV
    extinction curves more accurate than previous ones, sampling four
    environments in the LMC with different levels of star formation
    activity, including the general field, hitherto unexplored. The
    results will characterize the properties of dust in different
    conditions, at the LMC metallicity, which is useful to interpret
    integrated properties of distant galaxies, as well as GALEX upcoming
    UV surveys. A complementary study is planned with FUSE in the far-UV
    range. The combined results will provide insight on the properties of
    small grains.


    ACS/WFC 9811


    Establishing the Metallicity Distribution in Normal Giant Ellipticals


    NGC 3377 and 3379, the Leo Group ellipticals at d=11 Mpc, are the
    nearest E galaxies commonly regarded to be structurally" normal", and
    as such, they are keystone objects for understanding the evolution and
    early star formation history of large ellipticals. The ACS/WFC camera
    now gives us the ability to obtain the metallicity distribution
    function {MDF} of their stellar population by direct resolution and
    photometry of their halo stars. To do this, we will follow the same
    highly successful techniques we have previously used for NGC 5128 with
    WFPC2 {V, I} imaging: the {V-I} colors of the brightest red-giant
    stars are highly sensitive to metallicity, and their locations in the
    color-magnitude diagram can be used for direct construction of the
    MDF. This will be a major step forward to understanding the formation
    history of these cosmologically dominant galaxies.


    NIC1/NIC2/NIC3 8793


    NICMOS Post-SAA calibration - CR Persistence Part 4


    A new procedure proposed to alleviate the CR-persistence problem of
    NICMOS. Dark frames will be obtained immediately upon exiting the SAA
    contour 23, and every time a NICMOS exposure is scheduled within 50
    minutes of coming out of the SAA. The darks will be obtained in
    parallel in all three NICMOS Cameras. The POST-SAA darks will be
    non-standard reference files available to users with a USEAFTER
    date/time mark. The keyword &#39;USEAFTER=date/time&#39; will also be added to
    the header of each POST-SAA DARK frame. The keyword must be populated
    with the time, in addition to the date, because HST crosses the SAA ~8
    times per day so each POST-SAA DARK will need to have the appropriate
    time specified, for users to identify the ones they need. Both the raw
    and processed images will be archived as POST-SAA DARKSs. Generally we
    expect that all NICMOS science/calibration observations started within
    50 minutes of leaving an SAA will need such maps to remove the CR
    persistence from the science images. Each observation will need its
    own CRMAP, as different SAA passages leave different imprints on the
    NICMOS detectors.


    NIC1/NIC2/NIC3 10454


    Extreme count rates linearity test for NICMOS


    This NICMOS calibration proposal tests the linearity of the detectors
    at count rates falling at the low and high extremes of what is
    feasible. This program is a response to the discovery that grism
    observations obtained with NIC3 show a systematic offset from spectra
    taken with STIS and ACS in the 0.8-1.0 micron overlap region. The
    observations are consistent with a NIC3 sensitivity that depends on
    incident flux, i.e. count rate. By observing one bright star
    {BD+17D4708, the Sloan Digital Sky Survey absolute standard} and two
    faint stars {SNAP-2, a solar analog star; WD1657+343, a white dwarf}
    in a number of filters we will check whether this is an intrinsic
    feature of the all NICMOS detectors, something intrinsic to NIC3, or a
    result of a not understood effect of the grism observations. We will
    furthermore be able to test whether the effect has a wavelength
    dependence. The data will be reduced in exactly the same fashion as
    has been done before for the photometric calibration program, so a
    direct comparison with previous data can be made. In addition, we will
    obtain extra spectroscopic data on WD1657+343, the faintest and best
    modeled white dwarf of the stars on which the original discovery of
    the non-linearity was made. This will reduce the errors in this
    spectrum from 5% to 2% and will allow a better estimate of the effect.
    In order to ease scheduling, there are no time constraints specified
    in the proposal. However, because of the potentially important
    implications of this effect, it is very important that these orbits be
    scheduled as soon as possible. They could be critical for the proper
    calibration of NICMOS The targets have visibility 1} BD+17D4708: 16
    Apr - 17 Jan 2} SNAP-2: 3 Feb-1 Mar 3} WD1657+343: 3 Feb-26 Feb


    ACS/HRC/WFC 10438


    The Late Formation of Satellite Galaxies


    Tiny isolated HII regions have been discovered up to 30 kpc from the
    closest galaxy in the NOAO Survey for Ionization in Neutral Gas
    Galaxies {SINGG}. These halo HII regions can be ionized by only a few
    OB stars and seem to be most commonly found in interacting systems.
    They may represent the beginning of the formation of satellite
    galaxies at low redshift and/or are the source of the numerous
    intracluster planetary nebula. The halo HII regions are a unique mode
    of star formation in a low density and low metallicity environment and
    high resolution HST images are required to identify their underlying
    stellar populations. Determining the stellar populations of these HII
    regions will establish whether in-situ star formation is a significant
    contributor to the stellar content and enrichment of galactic halos
    and intergalactic space. In particular, ACS/HRC observations are
    required for their resolution, UV sensitivity, and wide wavelength
    coverage, allowing young and intermediate age populations to be
    identified. Parallel ACS/WFC observations will explore the possibility
    of a further stellar population in the interactive debris. The results
    of this project have implications on the formation of satellite
    galaxies, the origin of Galactic halo B stars, IGM ionization and
    enrichment, and star formation principles.


    ACS/HRC/WFC 10436


    Black Hole Growth and the Black Hole Mass -- Bulge Relations for AGNs


    Recent work has shown that the mass of a black hole is tightly
    correlated with the bulge mass of its host galaxy. This relation needs
    to be understood in the context of black hole growth in its active
    phase. Highly accreting AGNs, like narrow line Seyfert 1 galaxies
    {NLS1s}, are found to lie below the black hole mass -- bulge velocity
    dispersion correlation of normal galaxies and broad line AGNs. This
    result was obtained using FWHM{[OIII]} as a surrogate for the bulge
    velocity dispersion. To test this result we propose to obtain high
    resolution images of 10 NLS1s that do not lie on the black hole
    mass--sigma relation and measure accurate bulge parameters {luminosity
    and effective radius}. We will obtain an alternate handle on the bulge
    velocity dispersion through the fundamental plane relations and also
    find the locus of these NLS1s on the black hole mass--bulge luminosity
    plane. Testing this result is crucial to understanding the role of
    accretion on black hole growth, the observed correlations of the black
    hole mass with the bulge, and the formation and evolution of galaxies.


    ACS/HRC 10434


    Particle accelerators in space: resolving them for the first time


    The detection of optical counterparts of hot spots in radio galaxies
    has been a challenge in astrophysics since the 1960s. Being located at
    several 100 kpc away from the AGN, they represent the most striking
    sites of interaction between the AGN ejecta and the ambient
    inter-galactic medium. Particle acceleration is thought to drive their
    emission and therefore, due to their remote locations, hot spots are
    the best laboratories to study the physics of that mechanism in
    detail. Using carefully directed selection criteria and the VLT we
    have discovered hot spots in the optical at an unprecedented detection
    rate, all of them disclosing very intriguing structure. This structure
    pinpoints the regions where electrons are accelerated to highly
    relativistic energies -- the particle accelerators. With HST we aim at
    resolving these accelerators for the very first time. This will enable
    us to establish the nature and origin of these relativistic particles
    in the hot spots of radio galaxies. The results of these studies not
    only represent a key for understanding the evolution of radio sources
    but also provide important input to plasma acceleration problems in
    general.


    ACS/WFC 10412


    The host galaxies of dust-reddened quasars


    We have used the 2MASS near-infrared and FIRST radio surveys, together
    with the Palomar Observatory Sky Survey plates to select a sample of
    dust-reddened, radio- intermediate quasars. We wish to use ACS to
    study the host galaxies of these quasars. The dust reddening of the
    quasars makes it possible to study the hosts at rest-frame optical-UV
    wavelengths much more easily than the hosts of normal quasars of
    similar bolometric luminosity. Our study will compare the hosts of our
    dust-reddened quasars to those of normal quasars from the HST archive
    to test the hypothesis that dust-reddened quasars are young objects,
    whose hosts still show morphological evidence of recent merger events
    which triggered the quasar.


    ACS/HRC 10391


    Wavelength and Flux Calibration of the ACS prisms


    The wavelength calibration of the SBC {PR110L and PR130L} and HRC
    {PR200L} prisms will be established by observing a planetary nebula in
    the LMC and QSOs at carefully selected redshifts. Flux calibrations
    will be derived for each prism by observing white dwarf standards.


    ACS/HRC/WFC 10389


    ACS CCDs daily monitor - Cycle 13 - Part 2


    This program consists of a set of basic tests to monitor, the read
    noise, the development of hot pixels and test for any source of noise
    in ACS CCD detectors. The files, biases and dark will be used to
    create reference files for science calibration. This programme will be
    for the entire lifetime of ACS.


    ACS/HRC 10377


    ACS Earth Flats


    High signal sky flats will be obtained by observing the bright Earth
    with the HRC and WFC. These observations will be used to verify the
    accuracy of the flats currently used by the pipeline and will provide
    a comparison with flats derived via other techniques: L- flats from
    stellar observations, sky flats from stacked GO observations, and
    internal flats using the calibration lamps. Weekly coronagraphic
    monitoring is required to assess the changing position of the spots.


    ACS/WFC 10369


    ACS internal CTE monitor


    The charge transfer efficiency {CTE} of the ACS CCD detectors will
    decline as damage due to on-orbit radiation exposure accumulates. This
    degradation will be closely monitored at regular intervals, because it
    is likely to determine the useful lifetime of the CCDs. All the data
    for this program is acquired using internal targets {lamps} only, so
    all of the exposures should be taken during Earth occultation time
    {but not during SAA passages}. This program emulates the ACS
    pre-flight ground calibration and post-launch SMOV testing {program
    8948}, so that results from each epoch can be directly compared.
    Extended Pixel Edge Response {EPER} and First Pixel Response {FPR}
    data will be obtained over a range of signal levels for both the Wide
    Field Channel {WFC}, and the High Resolution Channel {HRC}.


    ACS/HRC 10330


    Coronagraphic search for disks around nearby stars


    We will use the coronagraphic and imaging modes of the High Resolution
    camera to study of the role of circumstellar disks in planetary system
    formation over timescales of ~1-1000 Myr. Our targets comprise pre
    Main-Sequence {MS} and MS stars, selected by infrared excess, and
    targets selected from SIRTF surveys. Some targets, like Beta Pictoris
    have debris disks that have been detected at optical or near-IR
    wavelengths, while others have disks inferred from mid-IR or ISO
    observations. We will obtain multicolor images of each target&#39;s
    circumstellar environment for the purpose of {1} detecting and
    characterizing disk morphologies over all scales {including warps and
    regions of enhanced or depleted density}, and {2} seeking evidence of
    embedded planets. Direct and occulted images will be recorded for
    studying the disks within 2 arcseconds of these targets; the
    coronagraph will be used to image the outer regions of the disks.
    Together with existing infrared observations, we will provide
    constraints on the sizes, distribution, and composition of dust
    grains. Unconfirmed disks will first be imaged in F606W, and if they
    exist we may later observe them in F435W and F814W.


    ACS/HRC/WFC 10263


    SAINTS - Supernova 1987A Intensive Survey


    SAINTS is a program to observe SN 1987A, the brightest supernova in
    383 years, as it transforms into supernova remnant {SNR} 1987A, the
    youngest supernova remnant. HST is the unique and perfect match in
    scale and in field for spatially-resolved observations of SN 1987A.
    Rapid changes are taking place in a violent encounter between the
    fastest-moving debris and the circumstellar ring. This one-time-only
    event, leading to suddenly appearing hotspots and new emission that
    can reveal previously hidden gas, is powered by shocks that can be
    studied simultaneously with HST and with Chandra to great advantage.
    Both the optical and X-ray flux from the ring are rising rapidly so
    prompt observations are needed in Cycle 13. Our previous observations
    reveal a remarkable reverse shock moving upstream through the
    expanding debris. The reverse shock provides a powerful tool for
    dissecting the radial structure of the vanished star. The debris from
    the explosion itself, still excited by radioactivity, is now well
    resolved by ACS and seen to be aspherical, providing direct clues to
    the mechanism of the explosion. Many questions about SN 1987A remain
    unanswered. SAINTS is a comprehensive attempt to use HST to establish
    the facts of SN 1987A, help to answer interesting questions, and to
    observe the birth of SNR 1987A.


    ACS/HRC 10259


    Planetary nebulae in the SMC: a study of stellar evolution and
    populations in an extremely low-metallicity environment


    The final phase of the evolution of low- and intermediate-mass stars,
    the planetary nebula {PN} ejection, is thought to largely contribute
    to the carbon and nitrogen enrichment in galaxies, in particular in
    old stellar populations. Stellar generations forming from a carbon-
    and nitrogen-enriched medium are a necessary condition for planetary
    and life formation. It is essential to understand how stars go through
    the process of shedding their chemically-enriched shells, and to test
    the predictions of stellar evolution theory on the relationship
    between stellar mass and elemental enrichment. Magellanic Cloud PNs
    are ideal probes for this study. Their abundances can be directly
    related to the mass of the central stars and to that of the stellar
    progenitor, without the great {distance and reddening} uncertainties
    that affect Galactic PNs. The UV lines are essential for calculating
    the abundances of the element related to stellar evolution {C, N, O}
    and to progenitor populations {e.g., Ne}. We propose to acquire UV
    spectroscopy of the SMC PNs whose morphology and central star
    properties has been previously determined by us with HST. We will
    derive the {C, N, O} abundance-to-mass relation, and determine the
    extent to which the mass of the progenitors of asymmetric PNs exceed
    that of symmetric PNs. We will also test the PN luminosity function,
    and probe cosmic recycling, in a very low-metallicity environment.


    ACS/HRC 10198


    Probing the Dynamics of the Galactic Bar through the Kinematics of
    Microlensed Stars


    The observed optical depths to microlensing of stars in the Galactic
    bulge are difficult to reconcile with our present understanding of
    Galactic dynamics. The main source of uncertainty in those comparisons
    is now shifting from microlensing measurements to the dynamical models
    of the Galactic bar. We propose to constrain the Galactic bar models
    with proper motion observations of Bulge stars that underwent
    microlensing by determining both the kinematic identity of the
    microlensed sources and the importance of streaming motions. The
    lensed stars are typically farther than randomly selected stars.
    Therefore, our proper motion determinations for 36 targeted MACHO
    events will provide valuable constraints on the dynamics of bulge
    stars as a function of distance. The first epoch data for our proposed
    events is already available in the HST archive so the project can be
    completed within a single HST cycle. The exceptional spatial
    resolution of HST is essential for completion of the project.
    Constraints on the total mass in the bulge will ultimately lead to the
    determination of the amount of dark matter in inner Galaxy.


    ACS/WFC 10174


    Dark-matter halos and evolution of high-z early-type galaxies


    Gravitational lensing and stellar dynamics provide two complementary
    methods to determine the mass distribution and evolution of luminous
    and dark-matter in early-type {E/S0} galaxies. The combined study of
    stellar dynamics and gravitational lensing allows one to break
    degeneracies inherent to each method separately, providing a clean
    probe of the internal structure of massive galaxies. Since most lens
    galaxies are at redshifts z=0.1-1.0, they also provide the required
    look-back time to study their structural and stellar-population
    evolution. We recently analyzed 5 E/S0 lens galaxies between z=0.5 and
    1.0, combining exquisite Hubble Space Telescope imaging data with
    kinematic data from ground-based Keck spectroscopy, placing the first
    precise constraints on the dark- matter mass fraction and its inner
    slope beyond the local Universe. To expand the sample to ~30 systems
    -- required to study potential trends and evolution in the E/S0 mass
    profiles -- we propose to target the 49 E/S0 lens-galaxy candidates
    discovered by Bolton et al. {2004} from the Sloan Digital Sky Survey
    {SDSS}. With the average lens rate being 40% and some systems having a
    lensing probability close to unity, we expect to discover ~20 strong
    gravitational lenses from the sample. This will triple the current
    sample of 9 E/S0 systems, with data in hand. With the sample of 30
    systems, we will be able to determine the average slope of the
    dark-matter and total mass profile of E/S0 galaxies to 10% and 4%
    accuracy, respectively. If present, we can simultaneously detect 10%
    evolution in the total mass slope with 95% confidence. This will
    provide unprecedented constraints on E/S0 galaxies beyond the local
    Universe and allow a stringent test of their formation scenarios and
    the standard cosmological model.


    ACS/WFC/WFPC2 10129


    Resolving Globular Clusters in NGC 1399


    We intend to use the ACS/WFC to measure structural parameters {half
    light radius, King core radius and concentration parameter} of
    individual globular clusters {GCs} in NGC 1399. Very little is known
    about structural parameters of globular clusters as a function of
    radius outside the Local Group. The proposed observations, arranged in
    a 3x3 ACS mosaic, will allow us to perform the first detailed
    wide-field study of structural parameters of globular clusters in a
    giant elliptical galaxy. In particular we will: 1} study the
    size-galactocentric distance relation of globular clusters out to ~55
    kpc {~1.6 eff. radius of the GCS} and determine whether the observed
    differences in sizes between metal-rich and metal-poor globular
    cluster in early-type galaxies are primordial and thereby reflect
    fundamental differences in formation, or are due to projection
    effects; 2} match the GC position observed with HST/ACS with X-ray
    binaries identified over the full Chandra field, and use the above
    sizes to constrain physical models for X-ray binary formation in GCs.
    3} The wealth of ground-based data available for this system
    {photometry+spectroscopy}, will allow us to correlate the structural
    properties with other GC properties, such as their chemical
    composition, luminosity, etc.


    ACS/WFC/WFPC2 10092


    The COSMOS 2-Degree ACS Survey


    We will undertake a 2 square degree imaging survey {Cosmic Evolution
    Survey -- COSMOS} with ACS in the I {F814W} band of the VIMOS
    equatorial field. This wide field survey is essential to understand
    the interplay between Large Scale Structure {LSS} evolution and the
    formation of galaxies, dark matter and AGNs and is the one region of
    parameter space completely unexplored at present by HST. The
    equatorial field was selected for its accessibility to all
    ground-based telescopes and low IR background and because it will
    eventually contain ~100, 000 galaxy spectra from the VLT-VIMOS
    instrument. The imaging will detect over 2 million objects with I> 27
    mag {AB, 10 sigma}, over 35, 000 Lyman Break Galaxies {LBGs} and
    extremely red galaxies out to z ~ 5. COSMOS is the only HST project
    specifically designed to probe the formation and evolution of
    structures ranging from galaxies up to Coma-size clusters in the epoch
    of peak galaxy, AGN, star and cluster formation {z ~0.5 to 3}. The
    size of the largest structures necessitate the 2 degree field. Our
    team is committed to the assembly of several public ancillary datasets
    including the optical spectra, deep XMM and VLA imaging, ground-based
    optical/IR imaging, UV imaging from GALEX and IR data from SIRTF.
    Combining the full-spectrum multiwavelength imaging and spectroscopic
    coverage with ACS sub-kpc resolution, COSMOS will be Hubble&#39;s ultimate
    legacy for understanding the evolution of both the visible and dark
    universe.


    FLIGHT OPERATIONS SUMMARY:


    Significant Spacecraft Anomalies: (The following are preliminary
    reports of potential non-nominal performance that will be
    investigated.)


    HSTAR 9787: GS Acq (1,2,1) Failure to RGA Control 5/113/11:19:28z.
    GSAcq (1,2,1) scheduled at 113/11:15:40 failed to enter Fine Lock,
    with Search Radius Limit Exceeded at 113/11:19:28. All subsequent
    attempts failed. Possible Observations affected: ACS 203-206, NIC
    39-43 REAcq&#39;s scheduled at 113/12:51:30, 113/14:27:27, 113/16:03:23
    all failed to RGA control due to Search Radius Limit Exceeded. Under
    investigation.


    COMPLETED OPS REQs:
    17425-0 Genslew for Proposal 10263 Slot#3 @112/1705z
    17426-0 R/T Map @113/1311z
    17427-0 R/T Map @113/1612z


    OPS NOTES EXECUTED:
    1331-0 Change JERRCNT Limit @111/2130z


    SCHEDULED SUCCESSFUL FAILURE TIMES
    FGS
    Gsacq 24 23 @113/1119z
    (HSTAR#9787)
    FGS
    Reacq 22 19
    @113/1251z,1427z,1603z (HSTAR#9787)
    FHST Update 40 40
    LOSS of LOCK


    SIGNIFICANT EVENTS:


    The Hubble Space Telescope Team today celebrates the 15th anniversary
    of the launch of the Hubble Space Telescope (April 24, 1990).

  21. #21
    StarLab Guest
    This string had better be pinned. C&#39;mon, mods, you out there?

    HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science


    DAILY REPORT # 3846


    PERIOD COVERED: DOY 115


    OBSERVATIONS SCHEDULED


    ACS 10140


    Identification of a magnetic anomaly at Jupiter from satellite
    footprints


    Repeated imaging of Jupiter&#39;s aurora has shown that the northern main
    oval has a distorted &#39;kidney bean&#39; shape in the general range of
    90-140? System III longitude, which appears unchanged since 1994.
    While it is more difficult to observe the conjugate regions in the
    southern aurora, no corresponding distortion appears in the south.
    Recent improved accuracy in locating the satellite footprint auroral
    emissions has provided new information about the geometry of Jupiter&#39;s
    magnetic field in this and other areas. The study of the magnetic
    field provides us with insight into the state of matter and the
    dynamics deep down Jupiter. There is currently no other way to do this
    from orbit. The persistent pattern of the main oval implies a
    disturbance of the local magnetic field, and the increased latitudinal
    separation of the locus of satellite footprints from each other and
    from the main oval implies a locally weaker field strength. It is
    possible that these phenomena result from a magnetic anomaly in
    Jupiter&#39;s intrinsic magnetic field, as was proposed by A. Dessler in
    the 1970&#39;s. There is presently only limited evidence from the scarcity
    of auroral footprints observed in this longitude range. We propose to
    obtain HST UV images with specific observing geometries of Jupiter to
    determine the locations of the auroral footprints of Io, Europa, and
    Ganymede in cycle 13 to accurately determine the magnetic field
    geometry in the suggested anomaly region, and to either confirm or
    refute the suggestion of a local magnetic anomaly.


    ACS/HRC 10130


    Systemic Proper Motions of the Magellanic Clouds from Astrometry with
    ACS: II. Second Epoch Images


    We request second epoch observations with ACS of Magellanic Cloud
    fields centered on the 40 quasars in the LMC and SMC for which we have
    first epoch Cycle 11 data. The new data will determine the systemic
    proper motion of the Clouds. An extensive astrometric analysis of the
    first epoch data shows that follow-up observations with a two year
    baseline will allow us to measure the proper motion of the clouds to
    within 0.022 mas/year in each of the two orthogonal directions
    {assuming that we can image 25 quasars, i.e., with a realistic
    Snapshot Program completion rate}. The best weighted combination of
    all previous measurements has a seven times larger error than what we
    expect. We will determine the proper motion of the clouds with 2%
    accuracy. When combined with HI data for the Magellanic Stream this
    will constrain both the mass distribution in the Galactic Halo and
    theoretical models for the origin of the Magellanic Stream. Previous
    measurements are too crude for such constraints. Our data will provide
    by far the most accurate proper motion measurement for any Milky Way
    satellite.


    ACS/HRC 10238


    The nature of quasar host galaxies: combining ACS imaging and VLT
    Integral Field Spectroscopy.


    We propose to perform ACS/F606W imaging of a complete sample of 29
    quasar host galaxies {0.08<z<0.34}. The spatial resolving power of the
    ACS HRC, in combination with the acquisition of empirical PSFs and
    advanced deconvolution techniques, will allow to study in detail
    structures on scales of a few tens of parsecs, and to access the inner
    regions of the host galaxies, even in the presence of bright nuclei.
    We demonstrate that combining deep spectroscopy with high resolution
    imaging in stable PSF conditions definitely constitutes the solution
    to characterize the complex physical properties of quasar host
    galaxies, from their outer regions to the inner 0.1 kpc, where most of
    the information on the interplay between quasars and their hosts is
    hidden. We propose to combine new ACS images with existing Integral
    Field VLT Spectra. We will map the stellar and gas velocity fields in
    2D, constrain the mass models, derive the radial host M/L ratios, map
    and characterize the stellar populations and the ionization state of
    the gas.


    ACS/HRC 10377


    ACS Earth Flats


    High signal sky flats will be obtained by observing the bright Earth
    with the HRC and WFC. These observations will be used to verify the
    accuracy of the flats currently used by the pipeline and will provide
    a comparison with flats derived via other techniques: L- flats from
    stellar observations, sky flats from stacked GO observations, and
    internal flats using the calibration lamps. Weekly coronagraphic
    monitoring is required to assess the changing position of the spots.


    ACS/HRC 10396


    Star Clusters, Stellar Populations, and the Evolution of the Small
    Magellanic Cloud


    As the closest star forming dwarf galaxy, the SMC is the preferred
    location for detailed studies of this extremely common class of
    objects. We therefore propose to use the capabilities of ACS, which
    provide an improvement by an order of magnitude over what is possible
    with ground-based optical imaging surveys that are limited by
    confusion and depth, to measure key stellar population parameters in
    the SMC from VI color- magnitude diagrams. Our program focuses on
    regions where crowding makes HST essential and includes 7 star
    clusters and 7 field star locations. We will measure accurate ages of
    the clusters, test stellar evolution models, gain fiducial stellar
    sequences to use in fitting the field stars, check the form of the
    IMF, and substantially extend the study of RR Lyrae variables in the
    key NGC121 SMC globular cluster. The field pointings will allow us to
    reconstruct the star formation history, look for enhanced star
    formation that is expected when the SMC interacts with the LMC and/or
    Milky Way, and compare its main sequence luminosity {and mass}
    functions with those of the Milky Way, LMC, and UMi dwarf spheroidal.
    This proposal is part of a coordinated HST and ground-based study of
    the stellar history and star formation processes in the SMC.


    ACS/HRC 10426


    High resolution follow-up observations of the microlensing event OGLE
    2003-BLG- 235/MOA 2003-BLG-53


    We propose high resolution imaging observations using HST/ACS to
    confirm that the lens in the microlensing event OGLE 2003-BLG-235/MOA
    2003-BLG-53 is a planetary system. Modelling of ground based
    photometry of this event yields an extreme mass fraction of 0.004 {ApJ
    606, L155}. We aim to use high resolution imaging to isolate the flux
    of the lens star from the contributions of neighboring "blended" stars
    within 1-2 arcsecs. This will allow us to identify the nature of the
    lens star and hence determine the mass of the stellar and planetary
    components. The lens is most likely a main sequence star, but other
    possibilities cannot be ruled out. High resolution imaging
    observations are crucial in identifying the nature of the lens.


    ACS/HRC/WFC 10389


    ACS CCDs daily monitor - Cycle 13 - Part 2


    This program consists of a set of basic tests to monitor, the read
    noise, the development of hot pixels and test for any source of noise
    in ACS CCD detectors. The files, biases and dark will be used to
    create reference files for science calibration. This programme will be
    for the entire lifetime of ACS.


    ACS/WFC 10174


    Dark-matter halos and evolution of high-z early-type galaxies


    Gravitational lensing and stellar dynamics provide two complementary
    methods to determine the mass distribution and evolution of luminous
    and dark-matter in early-type {E/S0} galaxies. The combined study of
    stellar dynamics and gravitational lensing allows one to break
    degeneracies inherent to each method separately, providing a clean
    probe of the internal structure of massive galaxies. Since most lens
    galaxies are at redshifts z=0.1-1.0, they also provide the required
    look-back time to study their structural and stellar-population
    evolution. We recently analyzed 5 E/S0 lens galaxies between z=0.5 and
    1.0, combining exquisite Hubble Space Telescope imaging data with
    kinematic data from ground-based Keck spectroscopy, placing the first
    precise constraints on the dark- matter mass fraction and its inner
    slope beyond the local Universe. To expand the sample to ~30 systems
    -- required to study potential trends and evolution in the E/S0 mass
    profiles -- we propose to target the 49 E/S0 lens-galaxy candidates
    discovered by Bolton et al. {2004} from the Sloan Digital Sky Survey
    {SDSS}. With the average lens rate being 40% and some systems having a
    lensing probability close to unity, we expect to discover ~20 strong
    gravitational lenses from the sample. This will triple the current
    sample of 9 E/S0 systems, with data in hand. With the sample of 30
    systems, we will be able to determine the average slope of the
    dark-matter and total mass profile of E/S0 galaxies to 10% and 4%
    accuracy, respectively. If present, we can simultaneously detect 10%
    evolution in the total mass slope with 95% confidence. This will
    provide unprecedented constraints on E/S0 galaxies beyond the local
    Universe and allow a stringent test of their formation scenarios and
    the standard cosmological model.


    ACS/WFC 10369


    ACS internal CTE monitor


    The charge transfer efficiency {CTE} of the ACS CCD detectors will
    decline as damage due to on-orbit radiation exposure accumulates. This
    degradation will be closely monitored at regular intervals, because it
    is likely to determine the useful lifetime of the CCDs. All the data
    for this program is acquired using internal targets {lamps} only, so
    all of the exposures should be taken during Earth occultation time
    {but not during SAA passages}. This program emulates the ACS
    pre-flight ground calibration and post-launch SMOV testing {program
    8948}, so that results from each epoch can be directly compared.
    Extended Pixel Edge Response {EPER} and First Pixel Response {FPR}
    data will be obtained over a range of signal levels for both the Wide
    Field Channel {WFC}, and the High Resolution Channel {HRC}.


    ACS/WFC/NIC2 10189


    PANS-Probing Acceleration Now with Supernovae


    Type Ia supernovae {SNe Ia} provide the most direct evidence for an
    accelerating Universe, a result widely attributed to dark energy.
    Using HST in Cycle 11 we extended the Hubble diagram with 6 of the 7
    highest-redshift SNe Ia known, all at z>1.25, providing conclusive
    evidence of an earlier epoch of cosmic deceleration. The full sample
    of 16 new SNe Ia match the cosmic concordance model and are
    inconsistent with a simple model of evolution or dust as alternatives
    to dark energy. Understanding dark energy may be the biggest current
    challenge to cosmology and particle physics. To understand the nature
    of dark energy, we seek to measure its two most fundamental
    properties: its evolution {i.e., dw/dz}, and its recent equation of
    state {i.e., w{z=0}}. SNe Ia at z>1, beyond the reach of the ground
    but squarely within the reach of HST with ACS, are crucial to break
    the degeneracy in the measurements of these two basic aspects of dark
    energy. The SNe Ia we have discovered and measured with HST in Cycle
    11, now double the precision of our knowledge of both properties. Here
    we propose to quadruple the sample of SNe Ia at z>1 in the next two
    cycles, complementing on-going surveys from the ground at z<1, and
    again doubling the precision of dark energy constraints. Should the
    current best fit model prove to be the correct one, the precision
    expected from the current proposal will suffice to rule out a
    cosmological constant at the 99% confidence level. Whatever the
    result, these objects will provide the basis with which to extend our
    empirical knowledge of this newly discovered and dominant component of
    the Universe, and will remain one of the most significant legacies of
    HST. In addition, our survey and follow-up data will greatly enhance
    the value of the archival data within the target Treasury fields for
    galaxy studies.


    NIC1/NIC2/NIC3 8793


    NICMOS Post-SAA calibration - CR Persistence Part 4


    A new procedure proposed to alleviate the CR-persistence problem of
    NICMOS. Dark frames will be obtained immediately upon exiting the SAA
    contour 23, and every time a NICMOS exposure is scheduled within 50
    minutes of coming out of the SAA. The darks will be obtained in
    parallel in all three NICMOS Cameras. The POST-SAA darks will be
    non-standard reference files available to users with a USEAFTER
    date/time mark. The keyword &#39;USEAFTER=date/time&#39; will also be added to
    the header of each POST-SAA DARK frame. The keyword must be populated
    with the time, in addition to the date, because HST crosses the SAA ~8
    times per day so each POST-SAA DARK will need to have the appropriate
    time specified, for users to identify the ones they need. Both the raw
    and processed images will be archived as POST-SAA DARKSs. Generally we
    expect that all NICMOS science/calibration observations started within
    50 minutes of leaving an SAA will need such maps to remove the CR
    persistence from the science images. Each observation will need its
    own CRMAP, as different SAA passages leave different imprints on the
    NICMOS detectors.


    WFPC2 10359


    WFPC2 CYCLE 13 Standard Darks


    This dark calibration program obtains dark frames every week in order
    to provide data for the ongoing calibration of the CCD dark current
    rate, and to monitor and characterize the evolution of hot pixels.
    Over an extended period these data will also provide a monitor of
    radiation damage to the CCDs.


    WFPC2 10363


    WFPC2 CYCLE 13 Intflat and Visflat Sweeps and Filter Rotation Anomaly
    Monitor


    Using intflat observations, this WFPC2 proposal is designed to monitor
    the pixel-to-pixel flatfield response and provide a linearity check.
    The intflat sequences, to be done once during the year, are similar to
    those from the Cycle 12 program 10075. The images will provide a
    backup database as well as allow monitoring of the gain ratios. The
    sweep is a complete set of internal flats, cycling through both
    shutter blades and both gains. The linearity test consists of a series
    of intflats in F555W, in each gain and each shutter. As in Cycle 12,
    we plan to continue to take extra visflat, intflat, and earthflat
    exposures to test the repeatability of filter wheel motions.


    FLIGHT OPERATIONS SUMMARY:


    Significant Spacecraft Anomalies: (The following are preliminary
    reports of potential non-nominal performance that will be
    investigated.) None


    COMPLETED OPS REQs:
    17428-1 Genslew for Proposal 10263 Slot#4 @115/1906z
    17429-0 Genslew for Proposal 10263 Slot#5 @115/1908z


    OPS NOTES EXECUTED: None


    SCHEDULED SUCCESSFUL FAILURE TIMES
    FGS Gsacq 09 09
    FGS Reacq 09 09
    FHST Update 14 14
    LOSS of LOCK


    SIGNIFICANT EVENTS: None

  22. #22
    StarLab Guest
    HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science


    DAILY REPORT # 3847


    PERIOD COVERED: DOY 116


    OBSERVATIONS SCHEDULED


    ACS/HRC 10185


    When does Bipolarity Impose itself on the Extreme Mass Outflows from
    AGB Stars? An ACS SNAPshot Survey


    Essentially all well-characterized preplanetary nebulae {PPNe} --
    objects in transition between the AGB and planetary nebula
    evolutionary phases - are bipolar, whereas the mass-loss envelopes of
    AGB stars are strikingly spherical. In order to understand the
    processes leading to bipolar mass-ejection, we need to know at what
    stage of stellar evolution does bipolarity in the mass-loss first
    manifest itself? Our previous SNAPshot surveys of a PPNe sample {with
    ACS & NICMOS} show that roughly half our targets observed are
    resolved, with well-defined bipolar or multipolar morphologies.
    Spectroscopic surveys of our sample confirm that these objects have
    not yet evolved into planetary nebulae. Thus, the transformation from
    spherical to aspherical geometries has already fully developed by the
    time these dying stars have become preplanetary nebulae. From this new
    and surprising result, we hypothesize that the transformation to
    bipolarity begins during the very late AGB phase, and happens very
    quickly, just before, or as the stars are evolving off the AGB. We
    propose to test this hypothesis quantitatively, through a SNAPshot
    imaging survey of very evolved AGB stars which we believe are nascent
    preplanetary nebulae; with our target list being drawn from published
    lists of AGB stars with detected heavy mass-loss {from millimeter-wave
    observations}. This survey is crucial for determining how and when the
    bipolar geometry asserts itself. Supporting kinematic observations
    using long-slit optical spectroscopy {with the Keck}, millimeter and
    radio interferometric observations {with OVRO, VLA & VLBA} are being
    undertaken. The results from this survey {together with our previous
    work} will allow us to draw general conclusions about the onset of
    bipolar mass-ejection during late stellar evolution, and will provide
    crucial input for theories of post-AGB stellar evolution. Our survey
    will produce an archival legacy of long-standing value for future
    studies of dying stars.


    ACS/HRC 10255


    A Never Before Explored Phase Space: Resolving Close White Dwarf / Red
    Dwarf Binaries


    We propose an ACS Snapshot imaging survey to resolve a well-defined
    sample of highly probable white dwarf plus red dwarf close binaries.
    These candidates were selected from a search for white dwarfs with
    infrared excess from the 2MASS database. They represent unresolved
    systems {separations less than approximately 2" in the 2MASS images}
    and are distributed over the whole sky. Our HST+ACS observations will
    be sensitive to a separation range {1-20 AU} never before probed by
    any means. The proposed study will be the first empirical test of
    binary star parameters in the post-AGB phase, and cannot be
    accomplished from the ground. By resolving as few as 20 of our ~100
    targets with HST, we will be able to characterize the distribution of
    orbital semi- major axes and secondary star masses.


    ACS/HRC/WFC 10263


    SAINTS - Supernova 1987A INTensive Survey


    SAINTS is a program to observe SN 1987A, the brightest supernova in
    383 years, as it transforms into supernova remnant {SNR} 1987A, the
    youngest supernova remnant. HST is the unique and perfect match in
    scale and in field for spatially-resolved observations of SN 1987A.
    Rapid changes are taking place in a violent encounter between the
    fastest-moving debris and the circumstellar ring. This one-time-only
    event, leading to suddenly appearing hotspots and new emission that
    can reveal previously hidden gas, is powered by shocks that can be
    studied simultaneously with HST and with Chandra to great advantage.
    Both the optical and X-ray flux from the ring are rising rapidly so
    prompt observations are needed in Cycle 13. Our previous observations
    reveal a remarkable reverse shock moving upstream through the
    expanding debris. The reverse shock provides a powerful tool for
    dissecting the radial structure of the vanished star. The debris from
    the explosion itself, still excited by radioactivity, is now well
    resolved by ACS and seen to be aspherical, providing direct clues to
    the mechanism of the explosion. Many questions about SN 1987A remain
    unanswered. SAINTS is a comprehensive attempt to use HST to establish
    the facts of SN 1987A, help to answer interesting questions, and to
    observe the birth of SNR 1987A.


    ACS/WFC 10257


    Astrometric and Photometric Study of NGC 6397 for Internal Motions,
    Dark Binaries, and X-Ray Sources


    We propose to observe the central regions of the globular cluster NGC
    6397 with ACS/WFC once per month for the 10 months of its visibility
    in Cycle 13. The project has three main goals: {1} Measure internal
    motions for roughly 3000 stars within 150 arcseconds of the cluster
    center, using archival WFPC2 as a first epoch. The motion of the
    typical star will be measured to 10-20%. We will detect any central
    black hole {BH} with a mass greater than 1000 solar masses, and will
    also measure core-collapse signatures such as anisotropy. {2} Conduct
    the first-ever search for heavy binaries by looking for the
    astrometric "wobble" of the luminous secondary. We should find all
    heavy binaries in the field with separations between 1 and 5 AU and
    periods between 3 months and 5 years. {3} Search for optical
    counterparts to X-ray sources found by Chandra.


    ACS/WFC 10369


    ACS internal CTE monitor


    The charge transfer efficiency {CTE} of the ACS CCD detectors will
    decline as damage due to on-orbit radiation exposure accumulates. This
    degradation will be closely monitored at regular intervals, because it
    is likely to determine the useful lifetime of the CCDs. All the data
    for this program is acquired using internal targets {lamps} only, so
    all of the exposures should be taken during Earth occultation time
    {but not during SAA passages}. This program emulates the ACS
    pre-flight ground calibration and post-launch SMOV testing {program
    8948}, so that results from each epoch can be directly compared.
    Extended Pixel Edge Response {EPER} and First Pixel Response {FPR}
    data will be obtained over a range of signal levels for both the Wide
    Field Channel {WFC}, and the High Resolution Channel {HRC}.


    ACS/WFC/NIC/NIC3/WFPC 10246 2 The HST survey of the Orion Nebula
    Cluster


    We propose a Treasury Program of 104 HST orbits to perform the
    definitive study of the Orion Nebula Cluster, the Rosetta stone of
    star formation. We will cover with unprecedented sensitivity {23-25
    mag}, dynamic range {~12 mag}, spatial resolution {50mas}, and
    simultaneous spectral coverage {5 bands} a ~450 square arcmin field
    centered on the Trapezium stars. This represents a tremendous gain
    over the shallow WFC1 study made in 1991 with the aberrated HST on an
    area ~15 times smaller. We maximize the HST observing efficiency using
    ACS/WFC and WFPC2 in parallel with two opposite roll angles, to cover
    the same total field. We will assemble the richest, most accurate and
    unbiased HR diagram for pre-main-sequence objects ever made. Combined
    with the optical spectroscopy already available for ~1000 sources and
    new deep near-IR imaging and spectroscopy {that we propose as Joint
    HST-NOAO observations}, we will be able to attack and possibly solve
    the most compelling questions on stellar evolution: the calibration of
    pre-main-sequence evolutionary tracks, mass segration and the
    variation of the initial mass function in different environments, the
    evolution of mass accretion rates vs. age and environment, disk
    dissipation in environments dominated by hard vs. soft-UV radiation,
    stellar multiplicity vs. disk fraction. In addition, we expect to
    discover and classify an unknown, but substantial, population of
    pre-Main Sequence binaries, low mass stars and brown dwarfs down to
    ~10 MJup. This is also the best possible way to discover dark
    silhouette disks in the outskirts of the Orion Nebula and study their
    evolutionary status through multicolor imaging. This program is timely
    and extremely well leveraged to other programs targeting Orion: the
    ACS H-alpha survey of the Orion Nebula, the recently completed 850ks
    ultradeep Chandra survey, the large GTO programs to be performed with
    SIRTF, plus the availability of 2MASS and various deep JHK surveys of
    the core recently done with 8m class telescopes.


    ACS/WFC/NIC2 10189


    PANS-Probing Acceleration Now with Supernovae


    Type Ia supernovae {SNe Ia} provide the most direct evidence for an
    accelerating Universe, a result widely attributed to dark energy.
    Using HST in Cycle 11 we extended the Hubble diagram with 6 of the 7
    highest-redshift SNe Ia known, all at z>1.25, providing conclusive
    evidence of an earlier epoch of cosmic deceleration. The full sample
    of 16 new SNe Ia match the cosmic concordance model and are
    inconsistent with a simple model of evolution or dust as alternatives
    to dark energy. Understanding dark energy may be the biggest current
    challenge to cosmology and particle physics. To understand the nature
    of dark energy, we seek to measure its two most fundamental
    properties: its evolution {i.e., dw/dz}, and its recent equation of
    state {i.e., w{z=0}}. SNe Ia at z>1, beyond the reach of the ground
    but squarely within the reach of HST with ACS, are crucial to break
    the degeneracy in the measurements of these two basic aspects of dark
    energy. The SNe Ia we have discovered and measured with HST in Cycle
    11, now double the precision of our knowledge of both properties. Here
    we propose to quadruple the sample of SNe Ia at z>1 in the next two
    cycles, complementing on-going surveys from the ground at z<1, and
    again doubling the precision of dark energy constraints. Should the
    current best fit model prove to be the correct one, the precision
    expected from the current proposal will suffice to rule out a
    cosmological constant at the 99% confidence level. Whatever the
    result, these objects will provide the basis with which to extend our
    empirical knowledge of this newly discovered and dominant component of
    the Universe, and will remain one of the most significant legacies of
    HST. In addition, our survey and follow-up data will greatly enhance
    the value of the archival data within the target Treasury fields for
    galaxy studies.


    ACS/WFC/WFPC2 10092


    The COSMOS 2-Degree ACS Survey


    We will undertake a 2 square degree imaging survey {Cosmic Evolution
    Survey -- COSMOS} with ACS in the I {F814W} band of the VIMOS
    equatorial field. This wide field survey is essential to understand
    the interplay between Large Scale Structure {LSS} evolution and the
    formation of galaxies, dark matter and AGNs and is the one region of
    parameter space completely unexplored at present by HST. The
    equatorial field was selected for its accessibility to all
    ground-based telescopes and low IR background and because it will
    eventually contain ~100, 000 galaxy spectra from the VLT-VIMOS
    instrument. The imaging will detect over 2 million objects with I> 27
    mag {AB, 10 sigma}, over 35, 000 Lyman Break Galaxies {LBGs} and
    extremely red galaxies out to z ~ 5. COSMOS is the only HST project
    specifically designed to probe the formation and evolution of
    structures ranging from galaxies up to Coma-size clusters in the epoch
    of peak galaxy, AGN, star and cluster formation {z ~0.5 to 3}. The
    size of the largest structures necessitate the 2 degree field. Our
    team is committed to the assembly of several public ancillary datasets
    including the optical spectra, deep XMM and VLA imaging, ground-based
    optical/IR imaging, UV imaging from GALEX and IR data from SIRTF.
    Combining the full-spectrum multiwavelength imaging and spectroscopic
    coverage with ACS sub-kpc resolution, COSMOS will be Hubble&#39;s ultimate
    legacy for understanding the evolution of both the visible and dark
    universe.


    NIC1/NIC2/NIC3 8793


    NICMOS Post-SAA calibration - CR Persistence Part 4


    A new procedure proposed to alleviate the CR-persistence problem of
    NICMOS. Dark frames will be obtained immediately upon exiting the SAA
    contour 23, and every time a NICMOS exposure is scheduled within 50
    minutes of coming out of the SAA. The darks will be obtained in
    parallel in all three NICMOS Cameras. The POST-SAA darks will be
    non-standard reference files available to users with a USEAFTER
    date/time mark. The keyword &#39;USEAFTER=date/time&#39; will also be added to
    the header of each POST-SAA DARK frame. The keyword must be populated
    with the time, in addition to the date, because HST crosses the SAA ~8
    times per day so each POST-SAA DARK will need to have the appropriate
    time specified, for users to identify the ones they need. Both the raw
    and processed images will be archived as POST-SAA DARKSs. Generally we
    expect that all NICMOS science/calibration observations started within
    50 minutes of leaving an SAA will need such maps to remove the CR
    persistence from the science images. Each observation will need its
    own CRMAP, as different SAA passages leave different imprints on the
    NICMOS detectors.


    NIC2 10176


    Coronagraphic Survey for Giant Planets Around Nearby Young Stars


    A systematic imaging search for extra-solar Jovian planets is now
    possible thanks to recent progress in identifying "young stars near
    Earth". For most of the proposed young {<~ 30 Myrs} and nearby {<~ 60
    pc} targets, we can detect a few Jupiter-mass planets as close as a
    few tens of AUs from the primary stars. This represents the first time
    that potential analogs of our solar system - that is planetary systems
    with giant planets having semi-major axes comparable to those of the
    four giant planets of the Solar System - come within the grasp of
    existing instrumentation. Our proposed targets have not been observed
    for planets with the Hubble Space Telescope previously. Considering
    the very successful earlier NICMOS observations of low mass brown
    dwarfs and planetary disks among members of the TW Hydrae Association,
    a fair fraction of our targets should also turn out to posses low mass
    brown dwarfs, giant planets, or dusty planetary disks because our
    targets are similar to {or even better than} the TW Hydrae stars in
    terms of youth and proximity to Earth. Should HST time be awarded and
    planetary mass candidates be found, proper motion follow-up of
    candidate planets will be done with ground-based AOs.


    NIC3 10337


    The COSMOS 2-Degree ACS Survey NICMOS Parallels


    The COSMOS 2-Degree ACS Survey NICMOS Parallels. This program is a
    companion to program 10092.


    WFPC2 10360


    WFPC2 CYCLE 13 INTERNAL MONITOR


    This calibration proposal is the Cycle 13 routine internal monitor for
    WFPC2, to be run weekly to monitor the health of the cameras. A
    variety of internal exposures are obtained in order to provide a
    monitor of the integrity of the CCD camera electronics in both bays
    {gain 7 and gain 15}, a test for quantum efficiency in the CCDs, and a
    monitor for possible buildup of contaminants on the CCD windows.


    WFPC2 10363


    WFPC2 CYCLE 13 Intflat and Visflat Sweeps and Filter Rotation Anomaly
    Monitor


    Using intflat observations, this WFPC2 proposal is designed to monitor
    the pixel-to-pixel flatfield response and provide a linearity check.
    The intflat sequences, to be done once during the year, are similar to
    those from the Cycle 12 program 10075. The images will provide a
    backup database as well as allow monitoring of the gain ratios. The
    sweep is a complete set of internal flats, cycling through both
    shutter blades and both gains. The linearity test consists of a series
    of intflats in F555W, in each gain and each shutter. As in Cycle 12,
    we plan to continue to take extra visflat, intflat, and earthflat
    exposures to test the repeatability of filter wheel motions.


    FLIGHT OPERATIONS SUMMARY:


    Significant Spacecraft Anomalies: (The following are preliminary
    reports of potential non-nominal performance that will be
    investigated.) None


    COMPLETED OPS REQs: None


    OPS NOTES EXECUTED: None


    SCHEDULED SUCCESSFUL FAILURE TIMES
    FGS Gsacq 07 07
    FGS Reacq 10 10
    FHST Update 09 09
    LOSS of LOCK


    SIGNIFICANT EVENTS: None

  23. #23
    StarLab Guest
    HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science


    DAILY REPORT # 3848


    PERIOD COVERED: DOY 117


    OBSERVATIONS SCHEDULED


    ACS/HRC 10199


    The Most Massive Galaxies in the Universe: Double Trouble?


    We are proposing an HST snapshot survey of 70 objects with velocity
    dispersion larger than 350 km/s, selected from the Sloan Digital Sky
    Survey. Potentially this sample contains the most massive galaxies in
    the Universe. Some of these objects may be superpositions; HST imaging
    is the key to determining if they are single and massive or if they
    are two objects in projection. The objects which HST imaging shows to
    be single objects are interesting because they potentially harbor the
    most massive black holes, and because their existence places strong
    constraints on galaxy formation models. When combined with ground
    based data already in hand, the objects which HST imaging shows are
    superpositions provide valuable information about interaction rates of
    early- type galaxies as well as their dust content. They also
    constrain the allowed parameter space for models of binary
    gravitational lenses {such models are currently invoked to explain
    discrepancies in the distribution of lensed image flux ratios and
    separations}.


    ACS/HRC 10255


    A Never Before Explored Phase Space: Resolving Close White Dwarf / Red
    Dwarf Binaries


    We propose an ACS Snapshot imaging survey to resolve a well-defined
    sample of highly probable white dwarf plus red dwarf close binaries.
    These candidates were selected from a search for white dwarfs with
    infrared excess from the 2MASS database. They represent unresolved
    systems {separations less than approximately 2" in the 2MASS images}
    and are distributed over the whole sky. Our HST+ACS observations will
    be sensitive to a separation range {1-20 AU} never before probed by
    any means. The proposed study will be the first empirical test of
    binary star parameters in the post-AGB phase, and cannot be
    accomplished from the ground. By resolving as few as 20 of our ~100
    targets with HST, we will be able to characterize the distribution of
    orbital semi- major axes and secondary star masses.


    ACS/HRC/WFC 10263


    SAINTS - Supernova 1987A INTensive Survey


    SAINTS is a program to observe SN 1987A, the brightest supernova in
    383 years, as it transforms into supernova remnant {SNR} 1987A, the
    youngest supernova remnant. HST is the unique and perfect match in
    scale and in field for spatially-resolved observations of SN 1987A.
    Rapid changes are taking place in a violent encounter between the
    fastest-moving debris and the circumstellar ring. This one-time-only
    event, leading to suddenly appearing hotspots and new emission that
    can reveal previously hidden gas, is powered by shocks that can be
    studied simultaneously with HST and with Chandra to great advantage.
    Both the optical and X-ray flux from the ring are rising rapidly so
    prompt observations are needed in Cycle 13. Our previous observations
    reveal a remarkable reverse shock moving upstream through the
    expanding debris. The reverse shock provides a powerful tool for
    dissecting the radial structure of the vanished star. The debris from
    the explosion itself, still excited by radioactivity, is now well
    resolved by ACS and seen to be aspherical, providing direct clues to
    the mechanism of the explosion. Many questions about SN 1987A remain
    unanswered. SAINTS is a comprehensive attempt to use HST to establish
    the facts of SN 1987A, help to answer interesting questions, and to
    observe the birth of SNR 1987A.


    ACS/HRC/WFC 10389


    ACS CCDs daily monitor - Cycle 13 - Part 2


    This program consists of a set of basic tests to monitor, the read
    noise, the development of hot pixels and test for any source of noise
    in ACS CCD detectors. The files, biases and dark will be used to
    create reference files for science calibration. This programme will be
    for the entire lifetime of ACS.


    ACS/WFC/WFPC2 10092


    The COSMOS 2-Degree ACS Survey


    We will undertake a 2 square degree imaging survey {Cosmic Evolution
    Survey -- COSMOS} with ACS in the I {F814W} band of the VIMOS
    equatorial field. This wide field survey is essential to understand
    the interplay between Large Scale Structure {LSS} evolution and the
    formation of galaxies, dark matter and AGNs and is the one region of
    parameter space completely unexplored at present by HST. The
    equatorial field was selected for its accessibility to all
    ground-based telescopes and low IR background and because it will
    eventually contain ~100, 000 galaxy spectra from the VLT-VIMOS
    instrument. The imaging will detect over 2 million objects with I> 27
    mag {AB, 10 sigma}, over 35, 000 Lyman Break Galaxies {LBGs} and
    extremely red galaxies out to z ~ 5. COSMOS is the only HST project
    specifically designed to probe the formation and evolution of
    structures ranging from galaxies up to Coma-size clusters in the epoch
    of peak galaxy, AGN, star and cluster formation {z ~0.5 to 3}. The
    size of the largest structures necessitate the 2 degree field. Our
    team is committed to the assembly of several public ancillary datasets
    including the optical spectra, deep XMM and VLA imaging, ground-based
    optical/IR imaging, UV imaging from GALEX and IR data from SIRTF.
    Combining the full-spectrum multiwavelength imaging and spectroscopic
    coverage with ACS sub-kpc resolution, COSMOS will be Hubble&#39;s ultimate
    legacy for understanding the evolution of both the visible and dark
    universe.


    NIC1/NIC2/NIC3 8793


    NICMOS Post-SAA calibration - CR Persistence Part 4


    A new procedure proposed to alleviate the CR-persistence problem of
    NICMOS. Dark frames will be obtained immediately upon exiting the SAA
    contour 23, and every time a NICMOS exposure is scheduled within 50
    minutes of coming out of the SAA. The darks will be obtained in
    parallel in all three NICMOS Cameras. The POST-SAA darks will be
    non-standard reference files available to users with a USEAFTER
    date/time mark. The keyword &#39;USEAFTER=date/time&#39; will also be added to
    the header of each POST-SAA DARK frame. The keyword must be populated
    with the time, in addition to the date, because HST crosses the SAA ~8
    times per day so each POST-SAA DARK will need to have the appropriate
    time specified, for users to identify the ones they need. Both the raw
    and processed images will be archived as POST-SAA DARKSs. Generally we
    expect that all NICMOS science/calibration observations started within
    50 minutes of leaving an SAA will need such maps to remove the CR
    persistence from the science images. Each observation will need its
    own CRMAP, as different SAA passages leave different imprints on the
    NICMOS detectors.


    NIC3 10337


    The COSMOS 2-Degree ACS Survey NICMOS Parallels


    The COSMOS 2-Degree ACS Survey NICMOS Parallels. This program is a
    companion to program 10092.


    FLIGHT OPERATIONS SUMMARY:


    Significant Spacecraft Anomalies: (The following are preliminary
    reports of potential non-nominal performance that will be
    investigated.)


    HSTAR 9790: GSAcq(2,3,2) returns to SSM control @ 113/22:42:13z. OTA
    SE review of PTAS processing reveals GSAcq(2,3,2) at 113/22:42:13
    required two attempts to successfully acquire. It reached Fine Lock on
    both FGS&#39;s at 22:46:44 and returned to SSM control at 22:47:42. It
    successfully achieved fine lock at 22:48:38.


    HSTAR 9791: ReAcq(2,3,3) requires multiple entries into CT to achieve
    DataValid @ 110/00:18:30z. OTA SE review of the PTAS processing found
    that the ReAcq(2,3,3) at 110/00:18:30 required 2 CT entries on FGS2
    before achieving CT-DV. The ReAcq was successful and no science impact
    should have been seen.


    COMPLETED OPS REQs:
    17430-0 Genslew for Proposal 10263 Slot # 6 @ 117/14:51z


    OPS NOTES EXECUTED: None


    SCHEDULED SUCCESSFUL FAILURE TIMES
    FGS Gsacq 12 12
    FGS
    Reacq 05 05


    FHST Update 16 16
    LOSS of LOCK


    SIGNIFICANT EVENTS: None

  24. #24
    StarLab Guest
    HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science


    DAILY REPORT # 3849


    PERIOD COVERED: DOY 118


    OBSERVATIONS SCHEDULED


    ACS/HRC 10130


    Systemic Proper Motions of the Magellanic Clouds from Astrometry with
    ACS: II. Second Epoch Images


    We request second epoch observations with ACS of Magellanic Cloud
    fields centered on the 40 quasars in the LMC and SMC for which we have
    first epoch Cycle 11 data. The new data will determine the systemic
    proper motion of the Clouds. An extensive astrometric analysis of the
    first epoch data shows that follow-up observations with a two year
    baseline will allow us to measure the proper motion of the clouds to
    within 0.022 mas/year in each of the two orthogonal directions
    {assuming that we can image 25 quasars, i.e., with a realistic
    Snapshot Program completion rate}. The best weighted combination of
    all previous measurements has a seven times larger error than what we
    expect. We will determine the proper motion of the clouds with 2%
    accuracy. When combined with HI data for the Magellanic Stream this
    will constrain both the mass distribution in the Galactic Halo and
    theoretical models for the origin of the Magellanic Stream. Previous
    measurements are too crude for such constraints. Our data will provide
    by far the most accurate proper motion measurement for any Milky Way
    satellite.


    ACS/HRC/WFC 10263


    SAINTS - Supernova 1987A INTensive Survey


    SAINTS is a program to observe SN 1987A, the brightest supernova in
    383 years, as it transforms into supernova remnant {SNR} 1987A, the
    youngest supernova remnant. HST is the unique and perfect match in
    scale and in field for spatially-resolved observations of SN 1987A.
    Rapid changes are taking place in a violent encounter between the
    fastest-moving debris and the circumstellar ring. This one-time-only
    event, leading to suddenly appearing hotspots and new emission that
    can reveal previously hidden gas, is powered by shocks that can be
    studied simultaneously with HST and with Chandra to great advantage.
    Both the optical and X-ray flux from the ring are rising rapidly so
    prompt observations are needed in Cycle 13. Our previous observations
    reveal a remarkable reverse shock moving upstream through the
    expanding debris. The reverse shock provides a powerful tool for
    dissecting the radial structure of the vanished star. The debris from
    the explosion itself, still excited by radioactivity, is now well
    resolved by ACS and seen to be aspherical, providing direct clues to
    the mechanism of the explosion. Many questions about SN 1987A remain
    unanswered. SAINTS is a comprehensive attempt to use HST to establish
    the facts of SN 1987A, help to answer interesting questions, and to
    observe the birth of SNR 1987A.


    ACS/HRC/WFC 10399


    Accurate and Robust Calibration of the Extragalactic Distance Scale
    with the Maser Galaxy NGC4258 II


    The extragalactic distance scale {EDS} is defined by a comparison of
    Cepheid Period- Luminosity {PL} relations for nearby galaxies and the
    LMC, whose uncertain distance is thereby the SOLE anchor. Studies of
    masers orbiting the central black hole in NGC4258 have provided the
    most accurate extragalactic distance ever {7.2+/-0.5 Mpc}, and new
    radio data and analysis techniques will reduce the uncertainty to <
    3.5% {0.07 mag} by 2005. Since this distance is well determined and
    based on geometric arguments, NGC4258 can provide a much needed new
    anchor for the EDS. Ultimately, the combination of an independent
    measurement of H0 and measurements of CMB fluctuations {e.g., WMAP}
    can be used to directly constrain cosmological parameters including
    the equation of state of dark energy. In our Cycle 12 proposal, we
    defined a program spanning two cycles. The Cycle 12 portion was
    accepted. We have acquired WFC images and are constructing well
    sampled PL relations in 3 colors {BVI}. The purpose of the Cycle 13
    observations is to address systematic sources of error and is crucial
    for the success of the entire program. To disentangle the effects of
    reddening and metallicity, and to characterize the effects of
    blending, we require 50 orbits to obtain H-band photometry
    {NICMOS/NIC2} and high resolution images {ACS/HRC}.


    ACS/WFC/WFPC2 10092


    The COSMOS 2-Degree ACS Survey


    We will undertake a 2 square degree imaging survey {Cosmic Evolution
    Survey -- COSMOS} with ACS in the I {F814W} band of the VIMOS
    equatorial field. This wide field survey is essential to understand
    the interplay between Large Scale Structure {LSS} evolution and the
    formation of galaxies, dark matter and AGNs and is the one region of
    parameter space completely unexplored at present by HST. The
    equatorial field was selected for its accessibility to all
    ground-based telescopes and low IR background and because it will
    eventually contain ~100, 000 galaxy spectra from the VLT-VIMOS
    instrument. The imaging will detect over 2 million objects with I> 27
    mag {AB, 10 sigma}, over 35, 000 Lyman Break Galaxies {LBGs} and
    extremely red galaxies out to z ~ 5. COSMOS is the only HST project
    specifically designed to probe the formation and evolution of
    structures ranging from galaxies up to Coma-size clusters in the epoch
    of peak galaxy, AGN, star and cluster formation {z ~0.5 to 3}. The
    size of the largest structures necessitate the 2 degree field. Our
    team is committed to the assembly of several public ancillary datasets
    including the optical spectra, deep XMM and VLA imaging, ground-based
    optical/IR imaging, UV imaging from GALEX and IR data from SIRTF.
    Combining the full-spectrum multiwavelength imaging and spectroscopic
    coverage with ACS sub-kpc resolution, COSMOS will be Hubble&#39;s ultimate
    legacy for understanding the evolution of both the visible and dark
    universe.


    NIC1/NIC2/NIC3 8793


    NICMOS Post-SAA calibration - CR Persistence Part 4


    A new procedure proposed to alleviate the CR-persistence problem of
    NICMOS. Dark frames will be obtained immediately upon exiting the SAA
    contour 23, and every time a NICMOS exposure is scheduled within 50
    minutes of coming out of the SAA. The darks will be obtained in
    parallel in all three NICMOS Cameras. The POST-SAA darks will be
    non-standard reference files available to users with a USEAFTER
    date/time mark. The keyword &#39;USEAFTER=date/time&#39; will also be added to
    the header of each POST-SAA DARK frame. The keyword must be populated
    with the time, in addition to the date, because HST crosses the SAA ~8
    times per day so each POST-SAA DARK will need to have the appropriate
    time specified, for users to identify the ones they need. Both the raw
    and processed images will be archived as POST-SAA DARKSs. Generally we
    expect that all NICMOS science/calibration observations started within
    50 minutes of leaving an SAA will need such maps to remove the CR
    persistence from the science images. Each observation will need its
    own CRMAP, as different SAA passages leave different imprints on the
    NICMOS detectors.


    NIC2 10173


    Infrared Snapshots of 3CR Radio Galaxies


    Radio galaxies are an important class of extragalactic objects: they
    are one of the most energetic astrophysical phenomena and they provide
    an exceptional probe of the evolving Universe, lying typically in high
    density regions but well-represented across a wide redshift range. In
    earlier Cycles we carried out extensive HST observations of the 3CR
    sources in order to acquire a complete and quantitative inventory of
    the structure, contents and evolution of these important objects.
    Amongst the results, we discovered new optical jets, dust lanes,
    face-on disks with optical jets, and revealed point-like nuclei whose
    properties support FR-I/BL Lac unified schemes. Here, we propose to
    obtain NICMOS infrared images of 3CR sources with z<0.3 as a major
    enhancement to an already superb dataset. We aim to deshroud dusty
    galaxies, study the underlying host galaxy free from the distorting
    effects of dust, locate hidden regions of star formation and establish
    the physical characteristics of the dust itself. We will measure
    frequency and spectral energy distributions of point-like nuclei,
    expected to be stronger and more prevalent in the IR, seek spectral
    turnovers in known synchrotron jets and find new jets. We will
    strongly test unified AGN schemes and merge these data with existing
    X-ray to radio observations. The resulting database will be an
    incredibly valuable resource to the astronomical community for years
    to come.


    NIC3 10337


    The COSMOS 2-Degree ACS Survey NICMOS Parallels


    The COSMOS 2-Degree ACS Survey NICMOS Parallels. This program is a
    companion to program 10092.


    FLIGHT OPERATIONS SUMMARY:


    Significant Spacecraft Anomalies: (The following are preliminary
    reports of potential non-nominal performance that will be
    investigated.) None


    COMPLETED OPS REQs: None


    OPS NOTES EXECUTED: None


    SCHEDULED SUCCESSFUL FAILURE TIMES
    FGS Gsacq 13 13
    FGS
    Reacq 03 03


    FHST Update 20 20
    LOSS of LOCK


    SIGNIFICANT EVENTS: None

  25. #25
    StarLab Guest
    First one for this week enjoy&#33;

    HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science


    DAILY REPORT # 3850


    PERIOD COVERED: DOY 119-121


    OBSERVATIONS SCHEDULED


    NIC1/NIC2/NIC3 8793


    NICMOS Post-SAA calibration - CR Persistence Part 4


    A new procedure proposed to alleviate the CR-persistence problem of
    NICMOS. Dark frames will be obtained immediately upon exiting the SAA
    contour 23, and every time a NICMOS exposure is scheduled within 50
    minutes of coming out of the SAA. The darks will be obtained in
    parallel in all three NICMOS Cameras. The POST-SAA darks will be
    non-standard reference files available to users with a USEAFTER
    date/time mark. The keyword &#39;USEAFTER=date/time&#39; will also be added to
    the header of each POST-SAA DARK frame. The keyword must be populated
    with the time, in addition to the date, because HST crosses the SAA ~8
    times per day so each POST-SAA DARK will need to have the appropriate
    time specified, for users to identify the ones they need. Both the raw
    and processed images will be archived as POST-SAA DARKSs. Generally we
    expect that all NICMOS science/calibration observations started within
    50 minutes of leaving an SAA will need such maps to remove the CR
    persistence from the science images. Each observation will need its
    own CRMAP, as different SAA passages leave different imprints on the
    NICMOS detectors.


    ACS/HRC/WFC 10436


    Black Hole Growth and the Black Hole Mass -- Bulge Relations for AGNs


    Recent work has shown that the mass of a black hole is tightly
    correlated with the bulge mass of its host galaxy. This relation needs
    to be understood in the context of black hole growth in its active
    phase. Highly accreting AGNs, like narrow line Seyfert 1 galaxies
    {NLS1s}, are found to lie below the black hole mass -- bulge velocity
    dispersion correlation of normal galaxies and broad line AGNs. This
    result was obtained using FWHM{[OIII]} as a surrogate for the bulge
    velocity dispersion. To test this result we propose to obtain high
    resolution images of 10 NLS1s that do not lie on the black hole
    mass--sigma relation and measure accurate bulge parameters {luminosity
    and effective radius}. We will obtain an alternate handle on the bulge
    velocity dispersion through the fundamental plane relations and also
    find the locus of these NLS1s on the black hole mass--bulge luminosity
    plane. Testing this result is crucial to understanding the role of
    accretion on black hole growth, the observed correlations of the black
    hole mass with the bulge, and the formation and evolution of galaxies.


    ACS/WFC/WFPC2 10402


    The Formation and Evolution of Spirals: An ACS and WFPC2 Imaging
    Survey of Nearby Galaxies


    Over 50% of galaxies in the local universe are spirals. Yet the star
    formation histories and evolution of this crucial population remain
    poorly understood. We propose to combine archival data with new
    ACS/WFC and WFPC2 observations of 11 galaxies, to tackle a
    comprehensive investigation of nearby spirals covering the entire
    spiral sequence. The new observations will fill a serious deficiency
    in HST&#39;s legacy, and maximize the scientific return of existing HST
    data. The filter combination of UBVI, and Halpha is ideal for studying
    stellar populations, dust properties, and the ISM. Our immediate
    scientific objectives are: {i} to use the resolved cluster
    populations, both young massive clusters and ancient globular clusters
    as a chronometer, to understand how spirals assembled as a function of
    time; {ii} study the rapid disruption properties of young clusters;
    and {iii} understand dust distributions in spirals from pc to kpc
    scales. Each of these goals provides an important step towards
    charting the evolution of galaxies, and an essential baseline for
    interpreting the galaxy populations being surveyed in both the early
    and present universe. The resolution of our survey, which exploits the
    excellent imaging capabilities of HST&#39;s two optical cameras, will
    enable us to understand the record of star cluster, and galaxy
    formation in a level of detail which is not possible for more distant
    systems. Finally, the proposed observations will provide a key to
    interpret an extensive, multiwavelength archive of space- and ground-
    based data at lower spatial resolution {SPITZER, CHANDRA, GALEX,
    NICMOS P alpha and H band imaging} for local spirals.


    ACS/HRC/WFC 10399


    Accurate and Robust Calibration of the Extragalactic Distance Scale
    with the Maser Galaxy NGC4258 II


    The extragalactic distance scale {EDS} is defined by a comparison of
    Cepheid Period-Luminosity {PL} relations for nearby galaxies and the
    LMC, whose uncertain distance is thereby the SOLE anchor. Studies of
    masers orbiting the central black hole in NGC4258 have provided the
    most accurate extragalactic distance ever {7.2+/-0.5 Mpc}, and new
    radio data and analysis techniques will reduce the uncertainty to <
    3.5% {0.07 mag} by 2005. Since this distance is well determined and
    based on geometric arguments, NGC4258 can provide a much needed new
    anchor for the EDS. Ultimately, the combination of an independent
    measurement of H0 and measurements of CMB fluctuations {e.g., WMAP}
    can be used to directly constrain cosmological parameters including
    the equation of state of dark energy. In our Cycle 12 proposal, we
    defined a program spanning two cycles. The Cycle 12 portion was
    accepted. We have acquired WFC images and are constructing well
    sampled PL relations in 3 colors {BVI}. The purpose of the Cycle 13
    observations is to address systematic sources of error and is crucial
    for the success of the entire program. To disentangle the effects of
    reddening and metallicity, and to characterize the effects of
    blending, we require 50 orbits to obtain H-band photometry
    {NICMOS/NIC2} and high resolution images {ACS/HRC}.


    ACS/HRC/WFC 10389


    ACS CCDs daily monitor - Cycle 13 - Part 2


    This program consists of a set of basic tests to monitor, the read
    noise, the development of hot pixels and test for any source of noise
    in ACS CCD detectors. The files, biases and dark will be used to
    create reference files for science calibration. This programme will be
    for the entire lifetime of ACS.


    FGS 10387


    Monitoring FGS1r&#39;s Interferometric Response as a Function of Spectral
    Color


    This proposal obtains reference point source Transfer Functions
    {S-Curves} for FGS1r through the F583W filter and the F5ND attenuator
    at the center position of the FGS1r FOV for a variety of stars of
    different spectral types. These Transfer Functions are needed to
    support the analysis of GO science data for the study of close and
    wide binary star systems and for determining the angular size and
    shape of extended sources. This proposal observes stars that have been
    observed in previous cycles to monitor the long term evolution of the
    FGS1r S-curves. This proposal also {1} monitors the FGS1r Lateral
    Color response {using stars Latcol-A and Latcol-B}, {2} calibrates the
    "Pos/Trans" bias of a star&#39;s position as determined from Transfer mode
    and Position mode observations, and {3} calibrates the shift of a
    star&#39;s centroid when observed with F5ND relative to that when observed
    with F583W.


    ACS/HRC/WFC/WFPC2 10384


    Focus Monitor


    The focus of HST is measured from WFPC2/PC and ACS/HRC images of
    stars. Multiple exposures are taken in parallel over an orbit to
    determine the influence of breathing on the derived mean focus.
    Observations are taken of clusters with suitable orientations to
    ensure stars appear in all fields.


    ACS/WFC 10378


    ACS Polarimetry Calibration


    Observations are made of the Boomerang Nebula {highly polarized
    reflection nebula} to calibrate the ACS polarizers.


    ACS/WFC 10374


    ACS photometric Stability


    This program consists of three parts. In the first part we will
    observe a subset of the ACS white dwarfs with HRC and ACS to verify
    repeatability to ~0.2%, because the filter shifts are based on
    photometric differences between stars of ~1%. These observations are
    also required to establish relative magnitudes of the primary WD
    standards at the 0.1% level. Targets should be GD153 and G191B2B,
    which seems to have the largest V mag error of ~0.008 mag. One orbit
    on the most important filters, including the grism and the prisms,
    should be expended with each camera for both stars for a total of 4
    orbits. In the second part will observe with HRC and WFC a solar
    analog star, P330E, to estimate any shifts in the short and the long
    wavelength cutoffs of selected filters. Complete filter bandpasses can
    be derived directly from the ratio of grism observations with and
    without the filter in place. The grism is on filter wheel 1, while
    four filters of interest F330W, F344N, F660N, and F814W are on wheel
    2. Each grism observation requires 3 settings: filter alone,
    filter+grism, and grism alone. In the third part we obtain high S/N
    photometric and spectroscopic observations of three red stars, VB-8
    {M7}, 2M0038+18 {L3.5} and 2M0559-14 {T5} with HRC and WFC to verify
    the photometry at the new standard position and to obtain accurate
    calibration {1% or better} of the grism spectra.


    ACS/WFC 10361


    Earth Flats


    This proposal monitors flatfield stability. This proposal obtains
    sequences of Earth streak flats to construct high quality flat fields
    for the WFPC2 filter set. These flat fields will allow mapping of the
    OTA illumination pattern and will be used in conjunction with previous
    internal and external flats to generate new pipeline superflats. These
    Earth flats will complement the Earth flat data obtained during cycles
    4-12.


    NIC3 10337


    The COSMOS 2-Degree ACS Survey NICMOS Parallels


    The COSMOS 2-Degree ACS Survey NICMOS Parallels. This program is a
    companion to program 10092.


    ACS/HRC 10272


    A Snapshot Survey of the Sites of Recent, Nearby Supernovae


    During the past few years, robotic {or nearly robotic} searches for
    supernovae {SNe}, most notably our Lick Observatory Supernova Search
    {LOSS}, have found hundreds of SNe, many of them in quite nearby
    galaxies {cz < 4000 km/s}. Most of the objects were discovered before
    maximum brightness, and have follow-up photometry and spectroscopy;
    they include some of the best-studied SNe to date. We propose to
    conduct a snapshot imaging survey of the sites of some of these nearby
    objects, to obtain late-time photometry that {through the shape of the
    light and color curves} will help reveal the origin of their lingering
    energy. The images will also provide high-resolution information on
    the local environment of SNe that are far superior to what we can
    procure from the ground. For example, we will obtain color-color and
    color-magnitude diagrams of stars in these SN sites, to determine
    their progenitor masses and constraints on the reddening. Recovery of
    the SNe in the new HST images will also allow us to actually pinpoint
    their progenitor stars in cases where pre-explosion images exist in
    the HST archive. Use of ACS rather than WFPC2 will make our snapshot
    survey even more valuable than our Cycle 9 survey. This Proposal is
    complementary to our Cycle 13 archival proposal, in which we outline a
    plan for using existing HST images to glean information about SN
    environments.


    ACS/HRC 10255


    A Never Before Explored Phase Space: Resolving Close White Dwarf / Red
    Dwarf


    We propose an ACS Snapshot imaging survey to resolve a well-defined
    sample of highly probable white dwarf plus red dwarf close binaries.
    These candidates were selected from a search for white dwarfs with
    infrared excess from the 2MASS database. They represent unresolved
    systems {separations less than approximately 2" in the 2MASS images}
    and are distributed over the whole sky. Our HST+ACS observations will
    be sensitive to a separation range {1-20 AU} never before probed by
    any means. The proposed study will be the first empirical test of
    binary star parameters in the post-AGB phase, and cannot be
    accomplished from the ground. By resolving as few as 20 of our ~100
    targets with HST, we will be able to characterize the distribution of
    orbital semi-major axes and secondary star masses.


    ACS/HRC 10199


    The Most Massive Galaxies in the Universe: Double Trouble?


    We are proposing an HST snapshot survey of 70 objects with velocity
    dispersion larger than 350 km/s, selected from the Sloan Digital Sky
    Survey. Potentially this sample contains the most massive galaxies in
    the Universe. Some of these objects may be superpositions; HST imaging
    is the key to determining if they are single and massive or if they
    are two objects in projection. The objects which HST imaging shows to
    be single objects are interesting because they potentially harbor the
    most massive black holes, and because their existence places strong
    constraints on galaxy formation models. When combined with ground
    based data already in hand, the objects which HST imaging shows are
    superpositions provide valuable information about interaction rates of
    early-type galaxies as well as their dust content. They also constrain
    the allowed parameter space for models of binary gravitational lenses
    {such models are currently invoked to explain discrepancies in the
    distribution of lensed image flux ratios and separations}.


    ACS/WFC/NIC2 10189


    PANS-Probing Acceleration Now with Supernovae


    Type Ia supernovae {SNe Ia} provide the most direct evidence for an
    accelerating Universe, a result widely attributed to dark energy.
    Using HST in Cycle 11 we extended the Hubble diagram with 6 of the 7
    highest-redshift SNe Ia known, all at z>1.25, providing conclusive
    evidence of an earlier epoch of cosmic deceleration. The full sample
    of 16 new SNe Ia match the cosmic concordance model and are
    inconsistent with a simple model of evolution or dust as alternatives
    to dark energy. Understanding dark energy may be the biggest current
    challenge to cosmology and particle physics. To understand the nature
    of dark energy, we seek to measure its two most fundamental
    properties: its evolution {i.e., dw/dz}, and its recent equation of
    state {i.e., w{z=0}}. SNe Ia at z>1, beyond the reach of the ground
    but squarely within the reach of HST with ACS, are crucial to break
    the degeneracy in the measurements of these two basic aspects of dark
    energy. The SNe Ia we have discovered and measured with HST in Cycle
    11, now double the precision of our knowledge of both properties. Here
    we propose to quadruple the sample of SNe Ia at z>1 in the next two
    cycles, complementing on-going surveys from the ground at z<1, and
    again doubling the precision of dark energy constraints. Should the
    current best fit model prove to be the correct one, the precision
    expected from the current proposal will suffice to rule out a
    cosmological constant at the 99% confidence level. Whatever the
    result, these objects will provide the basis with which to extend our
    empirical knowledge of this newly discovered and dominant component of
    the Universe, and will remain one of the most significant legacies of
    HST. In addition, our survey and follow-up data will greatly enhance
    the value of the archival data within the target Treasury fields for
    galaxy studies.


    ACS/HRC 10185


    When does Bipolarity Impose itself on the Extreme Mass Outflows from
    AGB Stars? An ACS SNAPshot Survey


    Essentially all well-characterized preplanetary nebulae {PPNe} --
    objects in transition between the AGB and planetary nebula
    evolutionary phases - are bipolar, whereas the mass-loss envelopes of
    AGB stars are strikingly spherical. In order to understand the
    processes leading to bipolar mass-ejection, we need to know at what
    stage of stellar evolution does bipolarity in the mass-loss first
    manifest itself? Our previous SNAPshot surveys of a PPNe sample {with
    ACS & NICMOS} show that roughly half our targets observed are
    resolved, with well-defined bipolar or multipolar morphologies.
    Spectroscopic surveys of our sample confirm that these objects have
    not yet evolved into planetary nebulae. Thus, the transformation from
    spherical to aspherical geometries has already fully developed by the
    time these dying stars have become preplanetary nebulae. From this new
    and surprising result, we hypothesize that the transformation to
    bipolarity begins during the very late AGB phase, and happens very
    quickly, just before, or as the stars are evolving off the AGB. We
    propose to test this hypothesis quantitatively, through a SNAPshot
    imaging survey of very evolved AGB stars which we believe are nascent
    preplanetary nebulae; with our target list being drawn from published
    lists of AGB stars with detected heavy mass-loss {from millimeter-wave
    observations}. This survey is crucial for determining how and when the
    bipolar geometry asserts itself. Supporting kinematic observations
    using long-slit optical spectroscopy {with the Keck}, millimeter and
    radio interferometric observations {with OVRO, VLA & VLBA} are being
    undertaken. The results from this survey {together with our previous
    work} will allow us to draw general conclusions about the onset of
    bipolar mass-ejection during late stellar evolution, and will provide
    crucial input for theories of post-AGB stellar evolution. Our survey
    will produce an archival legacy of long-standing value for future
    studies of dying stars.


    NIC2 10177


    Solar Systems In Formation: A NICMOS Coronagraphic Survey of
    Protoplanetary and Debris Disks


    Until recently, despite decades of concerted effort applied to
    understanding the formation processes that gave birth to our solar
    system, the detailed morphology of circumstellar material that must
    eventually form planets has been virtually impossible to discern. The
    advent of high contrast, coronagraphic imaging as implemented with the
    instruments aboard HST has dramatically enhanced our understanding of
    natal planetary system formation. Even so, only a handful of evolved
    disks {~ 1 Myr and older} have been imaged and spatially resolved in
    light scattered from their constituent grains. To elucidate the
    physical processes and properties in potentially planet-forming
    circumstellar disks, and to understand the nature and evolution of
    their grains, a larger spatially resolved and photometrically reliable
    sample of such systems must be observed. Thus, we propose a highly
    sensitive circumstellar disk imaging survey of a well-defined and
    carefully selected sample of YSOs {1-10 Myr T Tau and HAeBe stars} and
    {> app 10 Myr} main sequence stars, to probe the posited epoch of
    planetary system formation, and to provide this critically needed
    imagery. Our resolved images will shed light on the spatial
    distributions of the dust in these thermally emissive disks. In
    combination with their long wavelength SEDs the physical properties of
    the grains will be discerned, or constrained by our photometrically
    accurate surface brightness sensitivity limits for faint disks which
    elude detection. Our sample builds on the success of the exploratory
    GTO 7233 program, using two-roll per orbit PSF- subtracted NICMOS
    coronagraphy to provide the highest detection sensitivity to the
    smallest disks around bright stars which can be imaged with HST. Our
    sample will discriminate between proposed evolutionary scenarios while
    providing a legacy of cataloged morphologies for interpreting mid- and
    far-IR SEDs that the recently launched Spitzer Space Telescope will
    deliver.


    ACS/WFC 10152


    A Snapshot Survey of a Complete Sample of X-ray Luminous Galaxy
    Clusters from Redshift 0.3 to 0.7


    We propose a public, uniform imaging survey of a well-studied,
    complete, and homogeneous sample of X-ray clusters. The sample of 73
    clusters spans the redshift range between 0.3-0.7. The samples spans
    almost 2 orders of magnitude of X-ray luminosity, where half of the
    sample has X-ray luminosities greater than 10^44 erg/s {0.5-2.0 keV}.
    These snapshots will be used to obtain a fair census of the the
    morphology of cluster galaxies in the cores of clusters, to detect
    radial and tangential arc candidates, to detect optical jet
    candidates, and to provide an approximate estimate of the shear signal
    of the clusters themselves, and potentially an assessment of the
    contribution of large scale structure to lensing shear.


    NIC1 10143


    Ultracool companions to the nearest L dwarfs


    We propose to conduct the most sensitive survey to date for low mass
    companions to nearby L dwarfs. We will use NICMOS to image targets
    drawn from a volume- complete sample of 70 L dwarfs within 20 parsecs.
    The combination of infrared imaging and proximity will allow us to
    search for T dwarf companions at separations as small as 1.6 AU. This
    is crucial, since no ultracool binaries are currently known with
    separations exceeding 15 AU. Only 10 dwarfs in this sample have
    previous HST observations primarily at optical wavelengths. With the
    increased sensitivity of our survey, we will provide the most
    stringent test to date of brown dwarf models which envisage formation
    as ejected stellar embryos. In addition, our observations will be
    capable of detecting binaries with mass ratios as low as 0.3, and will
    therefore also test the apparent preference for equal-mass ultracool
    binaries. Finally, our observations offer the best prospect to date of
    detecting companions significantly cooler than the coolest t dwarf
    currently known.


    ACS/WFC/WFPC2 10092


    The COSMOS 2-Degree ACS Survey


    We will undertake a 2 square degree imaging survey {Cosmic Evolution
    Survey -- COSMOS} with ACS in the I {F814W} band of the VIMOS
    equatorial field. This wide field survey is essential to understand
    the interplay between Large Scale Structure {LSS} evolution and the
    formation of galaxies, dark matter and AGNs and is the one region of
    parameter space completely unexplored at present by HST. The
    equatorial field was selected for its accessibility to all
    ground-based telescopes and low IR background and because it will
    eventually contain ~100, 000 galaxy spectra from the VLT-VIMOS
    instrument. The imaging will detect over 2 million objects with I> 27
    mag {AB, 10 sigma}, over 35, 000 Lyman Break Galaxies {LBGs} and
    extremely red galaxies out to z ~ 5. COSMOS is the only HST project
    specifically designed to probe the formation and evolution of
    structures ranging from galaxies up to Coma-size clusters in the epoch
    of peak galaxy, AGN, star and cluster formation {z ~0.5 to 3}. The
    size of the largest structures necessitate the 2 degree field. Our
    team is committed to the assembly of several public ancillary datasets
    including the optical spectra, deep XMM and VLA imaging, ground-based
    optical/IR imaging, UV imaging from GALEX and IR data from SIRTF.
    Combining the full-spectrum multiwavelength imaging and spectroscopic
    coverage with ACS sub-kpc resolution, COSMOS will be Hubble&#39;s ultimate
    legacy for understanding the evolution of both the visible and dark
    universe.


    FLIGHT OPERATIONS SUMMARY:


    Significant Spacecraft Anomalies: (The following are preliminary
    reports of potential non-nominal performance that will be
    investigated.)


    HSTARS:
    9792 - ACS 935 SEMAPHORE_TIMEOUT @ 122/0847z
    At 122/08:47:11, ACS 935 status
    buffer message P=35, T=21313 was received during ACS/WFC Obs. This is a
    routine status buffer message. This is Semaphore_Timeout. This results
    when the Take Data Flag goes down during CCD Post-Flash or a Filter
    wheel, Fold Mechanism, or Calibration door move.


    COMPLETED OPS REQUEST:
    17431-1 - NICMOS EEPROM and EDAC dump @122/00:49:49z


    COMPLETED OPS NOTES: (None)


    SCHEDULED SUCCESSFUL FAILURE TIMES
    FGS Gsacq 38 38
    FGS
    Reacq 14 14
    FHST Update 57 57
    LOSS of LOCK


    SIGNIFICANT EVENTS: None

  26. #26
    StarLab Guest
    Sorry, it&#39;s been a while, but here&#39;s the next one&#33; :

    HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science


    DAILY REPORT #3851


    PERIOD COVERED: DOY 122


    OBSERVATIONS SCHEDULED


    ACS/HRC 10198


    Probing the Dynamics of the Galactic Bar through the Kinematics of
    Microlensed Stars


    The observed optical depths to microlensing of stars in the Galactic
    bulge are difficult to reconcile with our present understanding of
    Galactic dynamics. The main source of uncertainty in those comparisons
    is now shifting from microlensing measurements to the dynamical models
    of the Galactic bar. We propose to constrain the Galactic bar models
    with proper motion observations of Bulge stars that underwent
    microlensing by determining both the kinematic identity of the
    microlensed sources and the importance of streaming motions. The
    lensed stars are typically farther than randomly selected stars.
    Therefore, our proper motion determinations for 36 targeted MACHO
    events will provide valuable constraints on the dynamics of bulge
    stars as a function of distance. The first epoch data for our proposed
    events is already available in the HST archive so the project can be
    completed within a single HST cycle. The exceptional spatial
    resolution of HST is essential for completion of the project.
    Constraints on the total mass in the bulge will ultimately lead to the
    determination of the amount of dark matter in inner Galaxy.


    ACS/HRC 10272


    A Snapshot Survey of the Sites of Recent, Nearby Supernovae


    During the past few years, robotic {or nearly robotic} searches for
    supernovae {SNe}, most notably our Lick Observatory Supernova Search
    {LOSS}, have found hundreds of SNe, many of them in quite nearby
    galaxies {cz < 4000 km/s}. Most of the objects were discovered before
    maximum brightness, and have follow-up photometry and spectroscopy;
    they include some of the best-studied SNe to date. We propose to
    conduct a snapshot imaging survey of the sites of some of these nearby
    objects, to obtain late-time photometry that {through the shape of the
    light and color curves} will help reveal the origin of their lingering
    energy. The images will also provide high-resolution information on
    the local environment of SNe that are far superior to what we can
    procure from the ground. For example, we will obtain color-color and
    color-magnitude diagrams of stars in these SN sites, to determine
    their progenitor masses and constraints on the reddening. Recovery of
    the SNe in the new HST images will also allow us to actually pinpoint
    their progenitor stars in cases where pre-explosion images exist in
    the HST archive. Use of ACS rather than WFPC2 will make our snapshot
    survey even more valuable than our Cycle 9 survey. This Proposal is
    complementary to our Cycle 13 archival proposal, in which we outline a
    plan for using existing HST images to glean information about SN
    environments.


    ACS/HRC/WFC 10389


    ACS CCDs daily monitor - Cycle 13 - Part 2


    This program consists of a set of basic tests to monitor, the read
    noise, the development of hot pixels and test for any source of noise
    in ACS CCD detectors. The files, biases and dark will be used to
    create reference files for science calibration. This programme will be
    for the entire lifetime of ACS.


    ACS/WFC 10361


    Earth Flats


    This proposal monitors flatfield stability. This proposal obtains
    sequences of Earth streak flats to construct high quality flat fields
    for the WFPC2 filter set. These flat fields will allow mapping of the
    OTA illumination pattern and will be used in conjunction with previous
    internal and external flats to generate new pipeline superflats. These
    Earth flats will complement the Earth flat data obtained during cycles
    4-12.


    ACS/WFC/HRS 10371


    ACS CCD Flash Calibration


    This activity provides a set of CCD FLASH exposure reference images
    for each current level/shutter-side/detector combination, for the pair
    of FLASH LEDs on the instrument side currently in use. It also tests
    the short-term repeatability at the shortest FLASH exposure times that
    are expected to be used {1.0 sec}.


    ACS/WFC/NIC2 10189


    PANS-Probing Acceleration Now with Supernovae


    Type Ia supernovae {SNe Ia} provide the most direct evidence for an
    accelerating Universe, a result widely attributed to dark energy.
    Using HST in Cycle 11 we extended the Hubble diagram with 6 of the 7
    highest-redshift SNe Ia known, all at z>1.25, providing conclusive
    evidence of an earlier epoch of cosmic deceleration. The full sample
    of 16 new SNe Ia match the cosmic concordance model and are
    inconsistent with a simple model of evolution or dust as alternatives
    to dark energy. Understanding dark energy may be the biggest current
    challenge to cosmology and particle physics. To understand the nature
    of dark energy, we seek to measure its two most fundamental
    properties: its evolution {i.e., dw/dz}, and its recent equation of
    state {i.e., w{z=0}}. SNe Ia at z>1, beyond the reach of the ground
    but squarely within the reach of HST with ACS, are crucial to break
    the degeneracy in the measurements of these two basic aspects of dark
    energy. The SNe Ia we have discovered and measured with HST in Cycle
    11, now double the precision of our knowledge of both properties. Here
    we propose to quadruple the sample of SNe Ia at z>1 in the next two
    cycles, complementing on-going surveys from the ground at z<1, and
    again doubling the precision of dark energy constraints. Should the
    current best fit model prove to be the correct one, the precision
    expected from the current proposal will suffice to rule out a
    cosmological constant at the 99% confidence level. Whatever the
    result, these objects will provide the basis with which to extend our
    empirical knowledge of this newly discovered and dominant component of
    the Universe, and will remain one of the most significant legacies of
    HST. In addition, our survey and follow-up data will greatly enhance
    the value of the archival data within the target Treasury fields for
    galaxy studies.


    ACS/WFC/WFPC2 10092


    The COSMOS 2-Degree ACS Survey


    We will undertake a 2 square degree imaging survey {Cosmic Evolution
    Survey -- COSMOS} with ACS in the I {F814W} band of the VIMOS
    equatorial field. This wide field survey is essential to understand
    the interplay between Large Scale Structure {LSS} evolution and the
    formation of galaxies, dark matter and AGNs and is the one region of
    parameter space completely unexplored at present by HST. The
    equatorial field was selected for its accessibility to all
    ground-based telescopes and low IR background and because it will
    eventually contain ~100, 000 galaxy spectra from the VLT-VIMOS
    instrument. The imaging will detect over 2 million objects with I> 27
    mag {AB, 10 sigma}, over 35, 000 Lyman Break Galaxies {LBGs} and
    extremely red galaxies out to z ~ 5. COSMOS is the only HST project
    specifically designed to probe the formation and evolution of
    structures ranging from galaxies up to Coma-size clusters in the epoch
    of peak galaxy, AGN, star and cluster formation {z ~0.5 to 3}. The
    size of the largest structures necessitate the 2 degree field. Our
    team is committed to the assembly of several public ancillary datasets
    including the optical spectra, deep XMM and VLA imaging, ground-based
    optical/IR imaging, UV imaging from GALEX and IR data from SIRTF.
    Combining the full-spectrum multiwavelength imaging and spectroscopic
    coverage with ACS sub-kpc resolution, COSMOS will be Hubble&#39;s ultimate
    legacy for understanding the evolution of both the visible and dark
    universe.


    FGS 10197


    The Astrophysical Parameters of Very Metal-Poor Halo Binaries


    Little is currently known concerning the mass-luminosity relation
    {MLR} of Population II stars. In Cycle 10, we began an initial study
    with FGS1 to resolve a sample of known spectroscopic binaries
    preselected as high-velocity and/or low metallicity objects. This has
    resulted in significant new information about the astrophysical
    parameters of metal-poor stars, but was limited mainly to intermediate
    metallicities, not to true Population II stars. A new sample of
    metal-poor spectroscopic binaries identified by Latham and his
    collaborators {e.g. Latham et al 2002} contains three new very
    metal-poor objects resolvable with FGS. We propose to observe these
    binaries and obtain additional observations of two very important
    resolved targets from our initial sample. As with that program, we
    will couple the already-known spectroscopic orbits with astrometric
    information which only FGS can deliver at present. To ensure that the
    most will be gained from these data, we also request observations of
    three metal-poor single stars to be used as calibration objects. In
    combination with results from our previous program, these observations
    can be expected to resolve the question of the location of the
    Population II main sequence and give valuable insight into the
    accuracy of isochrone fitting for determination of globular clusters
    ages. Due to the combination of target magnitudes and expected
    separations, no object in this sample can be resolved without the
    unique capabilities of FGS.


    NIC1/NIC2/NIC3 8793


    NICMOS Post-SAA calibration - CR Persistence Part 4


    A new procedure proposed to alleviate the CR-persistence problem of
    NICMOS. Dark frames will be obtained immediately upon exiting the SAA
    contour 23, and every time a NICMOS exposure is scheduled within 50
    minutes of coming out of the SAA. The darks will be obtained in
    parallel in all three NICMOS Cameras. The POST-SAA darks will be
    non-standard reference files available to users with a USEAFTER
    date/time mark. The keyword &#39;USEAFTER=date/time&#39; will also be added to
    the header of each POST-SAA DARK frame. The keyword must be populated
    with the time, in addition to the date, because HST crosses the SAA ~8
    times per day so each POST-SAA DARK will need to have the appropriate
    time specified, for users to identify the ones they need. Both the raw
    and processed images will be archived as POST-SAA DARKSs. Generally we
    expect that all NICMOS science/calibration observations started within
    50 minutes of leaving an SAA will need such maps to remove the CR
    persistence from the science images. Each observation will need its
    own CRMAP, as different SAA passages leave different imprints on the
    NICMOS detectors.


    NIC2 10176


    Coronagraphic Survey for Giant Planets Around Nearby Young Stars


    A systematic imaging search for extra-solar Jovian planets is now
    possible thanks to recent progress in identifying "young stars near
    Earth". For most of the proposed young {<~ 30 Myrs} and nearby {<~ 60
    pc} targets, we can detect a few Jupiter-mass planets as close as a
    few tens of AUs from the primary stars. This represents the first time
    that potential analogs of our solar system - that is planetary systems
    with giant planets having semi-major axes comparable to those of the
    four giant planets of the Solar System - come within the grasp of
    existing instrumentation. Our proposed targets have not been observed
    for planets with the Hubble Space Telescope previously. Considering
    the very successful earlier NICMOS observations of low mass brown
    dwarfs and planetary disks among members of the TW Hydrae Association,
    a fair fraction of our targets should also turn out to posses low mass
    brown dwarfs, giant planets, or dusty planetary disks because our
    targets are similar to {or even better than} the TW Hydrae stars in
    terms of youth and proximity to Earth. Should HST time be awarded and
    planetary mass candidates be found, proper motion follow-up of
    candidate planets will be done with ground-based AOs.


    NIC2 10177


    Solar Systems In Formation: A NICMOS Coronagraphic Survey of
    Protoplanetary and Debris Disks Until recently, despite decades of
    concerted effort applied to understanding the formation processes that
    gave birth to our solar system, the detailed morphology of
    circumstellar material that must eventually form planets has been
    virtually impossible to discern. The advent of high contrast,
    coronagraphic imaging as implemented with the instruments aboard HST
    has dramatically enhanced our understanding of natal planetary system
    formation. Even so, only a handful of evolved disks {~ 1 Myr and
    older} have been imaged and spatially resolved in light scattered from
    their constituent grains. To elucidate the physical processes and
    properties in potentially planet-forming circumstellar disks, and to
    understand the nature and evolution of their grains, a larger
    spatially resolved and photometrically reliable sample of such systems
    must be observed. Thus, we propose a highly sensitive circumstellar
    disk imaging survey of a well-defined and carefully selected sample of
    YSOs {1-10 Myr T Tau and HAeBe stars} and {> app 10 Myr} main sequence
    stars, to probe the posited epoch of planetary system formation, and
    to provide this critically needed imagery. Our resolved images will
    shed light on the spatial distributions of the dust in these thermally
    emissive disks. In combination with their long wavelength SEDs the
    physical properties of the grains will be discerned, or constrained by
    our photometrically accurate surface brightness sensitivity limits for
    faint disks which elude detection. Our sample builds on the success of
    the exploratory GTO 7233 program, using two-roll per orbit PSF-
    subtracted NICMOS coronagraphy to provide the highest detection
    sensitivity to the smallest disks around bright stars which can be
    imaged with HST. Our sample will discriminate between proposed
    evolutionary scenarios while providing a legacy of cataloged
    morphologies for interpreting mid- and far-IR SEDs that the recently
    launched Spitzer Space Telescope will deliver.


    NIC3 10337


    The COSMOS 2-Degree ACS Survey NICMOS Parallels


    The COSMOS 2-Degree ACS Survey NICMOS Parallels. This program is a
    companion to program 10092.


    WFPC2 10132


    UV Confirmation of New Quasar Sightlines Suitable for the Study of
    Intergalactic Helium


    The reionization of intergalactic helium is thought to have occurred
    between redshifts of about 3 and 4. The study of HeII Lyman-alpha
    absorption towards a half- dozen quasars at 2.7<z<3.5 demonstrates the
    great potential of such probes of the IGM, but the current
    critically-small sample limits confidence in resulting cosmological
    inferences. The requisite unobscured quasar sightlines to
    high-redshift are extremely rare, especially due to severe absorption
    in random intervening Lyman-limit systems, but SDSS provides hundreds
    of bright, new quasars at such redshifts potentially suitable for HeII
    studies. Our cycle 13 SNAP program proposes to verify the UV
    detectability of 40 new, bright, z>2.9 SDSS quasars, but with special
    emphasis on extending helium studies to the highest redshift
    sightlines. Our proposed approach has already proven successful, and
    additional sightlines will enable follow-up spectal observations to
    measure the spectrum and evolution of the ionizing background
    radiation, the density of intergalactic baryons, and the epoch of
    reionization of the IGM.


    WFPC2 10356


    WFPC2 Cycle 13 Decontaminations and Associated Observations


    This proposal is for the monthly WFPC2 decons. Also included are
    instrument monitors tied to decons: photometric stability check, focus
    monitor, pre- and post- decon internals {bias, intflats, kspots, &
    darks}, UV throughput check, VISFLAT sweep, and internal UV flat
    check.


    WFPC2 10362


    WFPC2 Cycle 13 UV Earth Flats


    Monitor flat field stability. This proposal obtains sequences of earth
    streak flats to improve the quality of pipeline flat fields for the
    WFPC2 UV filter set. These Earth flats will complement the UV earth
    flat data obtained during cycles 8-12.


    FLIGHT OPERATIONS SUMMARY:


    Significant Spacecraft Anomalies: (The following are preliminary
    reports of potential non-nominal performance that will be
    investigated.)


    HSTARS:


    9793 - GSacq(1,2,2) Results in Fine Lock Backup GSacq(2,0,2) @
    122/15:37:54z GSACQ(1,2,2) scheduled for 122/15:37:54 - 15:45:05
    resulted in Fine Lock on FGS 2 only due to scan step limit exceeded on
    FGS 1. The previous Updated scheduled at 15:06, 15:09 both passed with
    small attitude error. The following map scheduled for 16:03:11 showed
    attitude errors of: -3.161, -6.965 and -5.453 arcsec.


    COMPLETED OPS REQUEST: (None)


    COMPLETED OPS NOTES:
    1333-0 - Change JERRCNT Limit @ 122/15:21z


    SCHEDULED SUCCESSFUL FAILURE TIMES
    FGS Gsacq 13 13
    FGS
    Reacq 05 05
    FHST Update 21 21
    LOSS of LOCK


    SIGNIFICANT EVENTS: (None)

  27. #27
    StarLab Guest
    HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science


    DAILY REPORT #3852


    PERIOD COVERED: DOY 123


    OBSERVATIONS SCHEDULED


    ACS/HRC 10259


    Planetary nebulae in the SMC: a study of stellar evolution and
    populations in an extremely low-metallicity environment


    The final phase of the evolution of low- and intermediate-mass stars,
    the planetary nebula {PN} ejection, is thought to largely contribute
    to the carbon and nitrogen enrichment in galaxies, in particular in
    old stellar populations. Stellar generations forming from a carbon-
    and nitrogen-enriched medium are a necessary condition for planetary
    and life formation. It is essential to understand how stars go through
    the process of shedding their chemically-enriched shells, and to test
    the predictions of stellar evolution theory on the relationship
    between stellar mass and elemental enrichment. Magellanic Cloud PNs
    are ideal probes for this study. Their abundances can be directly
    related to the mass of the central stars and to that of the stellar
    progenitor, without the great {distance and reddening} uncertainties
    that affect Galactic PNs. The UV lines are essential for calculating
    the abundances of the element related to stellar evolution {C, N, O}
    and to progenitor populations {e.g., Ne}. We propose to acquire UV
    spectroscopy of the SMC PNs whose morphology and central star
    properties has been previously determined by us with HST. We will
    derive the {C, N, O} abundance-to-mass relation, and determine the
    extent to which the mass of the progenitors of asymmetric PNs exceed
    that of symmetric PNs. We will also test the PN luminosity function,
    and probe cosmic recycling, in a very low-metallicity environment.


    ACS/WFC/NIC2 10189


    PANS-Probing Acceleration Now with Supernovae


    Type Ia supernovae {SNe Ia} provide the most direct evidence for an
    accelerating Universe, a result widely attributed to dark energy.
    Using HST in Cycle 11 we extended the Hubble diagram with 6 of the 7
    highest-redshift SNe Ia known, all at z>1.25, providing conclusive
    evidence of an earlier epoch of cosmic deceleration. The full sample
    of 16 new SNe Ia match the cosmic concordance model and are
    inconsistent with a simple model of evolution or dust as alternatives
    to dark energy. Understanding dark energy may be the biggest current
    challenge to cosmology and particle physics. To understand the nature
    of dark energy, we seek to measure its two most fundamental
    properties: its evolution {i.e., dw/dz}, and its recent equation of
    state {i.e., w{z=0}}. SNe Ia at z>1, beyond the reach of the ground
    but squarely within the reach of HST with ACS, are crucial to break
    the degeneracy in the measurements of these two basic aspects of dark
    energy. The SNe Ia we have discovered and measured with HST in Cycle
    11, now double the precision of our knowledge of both properties. Here
    we propose to quadruple the sample of SNe Ia at z>1 in the next two
    cycles, complementing on-going surveys from the ground at z<1, and
    again doubling the precision of dark energy constraints. Should the
    current best fit model prove to be the correct one, the precision
    expected from the current proposal will suffice to rule out a
    cosmological constant at the 99% confidence level. Whatever the
    result, these objects will provide the basis with which to extend our
    empirical knowledge of this newly discovered and dominant component of
    the Universe, and will remain one of the most significant legacies of
    HST. In addition, our survey and follow-up data will greatly enhance
    the value of the archival data within the target Treasury fields for
    galaxy studies.


    ACS/WFC/WFPC2 10092


    The COSMOS 2-Degree ACS Survey


    We will undertake a 2 square degree imaging survey {Cosmic Evolution
    Survey -- COSMOS} with ACS in the I {F814W} band of the VIMOS
    equatorial field. This wide field survey is essential to understand
    the interplay between Large Scale Structure {LSS} evolution and the
    formation of galaxies, dark matter and AGNs and is the one region of
    parameter space completely unexplored at present by HST. The
    equatorial field was selected for its accessibility to all
    ground-based telescopes and low IR background and because it will
    eventually contain ~100, 000 galaxy spectra from the VLT-VIMOS
    instrument. The imaging will detect over 2 million objects with I> 27
    mag {AB, 10 sigma}, over 35, 000 Lyman Break Galaxies {LBGs} and
    extremely red galaxies out to z ~ 5. COSMOS is the only HST project
    specifically designed to probe the formation and evolution of
    structures ranging from galaxies up to Coma-size clusters in the epoch
    of peak galaxy, AGN, star and cluster formation {z ~0.5 to 3}. The
    size of the largest structures necessitate the 2 degree field. Our
    team is committed to the assembly of several public ancillary datasets
    including the optical spectra, deep XMM and VLA imaging, ground-based
    optical/IR imaging, UV imaging from GALEX and IR data from SIRTF.
    Combining the full-spectrum multiwavelength imaging and spectroscopic
    coverage with ACS sub-kpc resolution, COSMOS will be Hubble&#39;s ultimate
    legacy for understanding the evolution of both the visible and dark
    universe.


    FGS 10432


    Precise Distances to Nearby Planetary Nebulae


    We propose to carry out astrometry with the FGS to obtain accurate and
    precise distances to four nearby planetary nebulae. In 1992, Cahn et
    al. noted that ``The distances to Galactic planetary nebulae remain a
    serious, if not THE most serious, problem in the field, despite
    decades of study.&#39;&#39; Twelve years later, the same statement still
    applies. Because the distances to planetary nebulae are so uncertain,
    our understanding of their masses, luminosities, scale height, birth
    rate, and evolutionary state is severely limited. To help remedy this
    problem, HST astrometry can guarantee parallaxes with half the error
    of any other available approach. These data, when combined with
    parallax measurements from the USNO, will improve distance
    measurements by more than a factor of two, producing more accurate
    distances with uncertainties that are of the order of ~6%. Lastly,
    most planetary nebula distance scales in the literature are
    statistical. They require several anchor points of known distance in
    order to calibrate their zero point. Our program will provide "gold
    standard" anchor points by the end of 2006, a decade before any
    anticipated results from future space astrometry missions.


    NIC1/NIC2/NIC3 8793


    NICMOS Post-SAA calibration - CR Persistence Part 4


    A new procedure proposed to alleviate the CR-persistence problem of
    NICMOS. Dark frames will be obtained immediately upon exiting the SAA
    contour 23, and every time a NICMOS exposure is scheduled within 50
    minutes of coming out of the SAA. The darks will be obtained in
    parallel in all three NICMOS Cameras. The POST-SAA darks will be
    non-standard reference files available to users with a USEAFTER
    date/time mark. The keyword &#39;USEAFTER=date/time&#39; will also be added to
    the header of each POST-SAA DARK frame. The keyword must be populated
    with the time, in addition to the date, because HST crosses the SAA ~8
    times per day so each POST-SAA DARK will need to have the appropriate
    time specified, for users to identify the ones they need. Both the raw
    and processed images will be archived as POST-SAA DARKSs. Generally we
    expect that all NICMOS science/calibration observations started within
    50 minutes of leaving an SAA will need such maps to remove the CR
    persistence from the science images. Each observation will need its
    own CRMAP, as different SAA passages leave different imprints on the
    NICMOS detectors.


    NIC2 10173


    Infrared Snapshots of 3CR Radio Galaxies


    Radio galaxies are an important class of extragalactic objects: they
    are one of the most energetic astrophysical phenomena and they provide
    an exceptional probe of the evolving Universe, lying typically in high
    density regions but well-represented across a wide redshift range. In
    earlier Cycles we carried out extensive HST observations of the 3CR
    sources in order to acquire a complete and quantitative inventory of
    the structure, contents and evolution of these important objects.
    Amongst the results, we discovered new optical jets, dust lanes,
    face-on disks with optical jets, and revealed point-like nuclei whose
    properties support FR-I/BL Lac unified schemes. Here, we propose to
    obtain NICMOS infrared images of 3CR sources with z<0.3 as a major
    enhancement to an already superb dataset. We aim to deshroud dusty
    galaxies, study the underlying host galaxy free from the distorting
    effects of dust, locate hidden regions of star formation and establish
    the physical characteristics of the dust itself. We will measure
    frequency and spectral energy distributions of point-like nuclei,
    expected to be stronger and more prevalent in the IR, seek spectral
    turnovers in known synchrotron jets and find new jets. We will
    strongly test unified AGN schemes and merge these data with existing
    X-ray to radio observations. The resulting database will be an
    incredibly valuable resource to the astronomical community for years
    to come.


    NIC3 10337


    The COSMOS 2-Degree ACS Survey NICMOS Parallels


    The COSMOS 2-Degree ACS Survey NICMOS Parallels. This program is a
    companion to program 10092.


    WFPC2 10356


    WFPC2 Cycle 13 Decontaminations and Associated Observations


    This proposal is for the monthly WFPC2 decons. Also included are
    instrument monitors tied to decons: photometric stability check, focus
    monitor, pre- and post- decon internals {bias, intflats, kspots, &
    darks}, UV throughput check, VISFLAT sweep, and internal UV flat
    check.


    FLIGHT OPERATIONS SUMMARY:


    Significant Spacecraft Anomalies: (The following are preliminary
    reports of potential non-nominal performance that will be
    investigated.)


    HSTARS:


    9794 - Unable to log on the A/string HSTNET desktop 124/01:40z FOT was
    unable to log on the A/string HSTNET desktop on NT1,6,7. Response Team
    had GDOC to run the External GUI Server partial recycle procedure. The
    problem was cleared. FOT was able to bring up the CCS pages.


    COMPLETED OPS REQUEST: (None)


    COMPLETED OPS NOTES:
    1334-0 - Turn Limits ON for certain OTA @ 123/09:16z


    SCHEDULED SUCCESSFUL FAILURE TIMES
    FGS Gsacq 06 06
    FGS
    Reacq 11 11
    FHST Update 10 10
    LOSS of LOCK


    SIGNIFICANT EVENTS: (None)

  28. #28
    StarLab Guest
    Next one:


    HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science


    DAILY REPORT # 3853


    PERIOD COVERED: DOY 124


    OBSERVATIONS SCHEDULED


    ACS/HRC/WFC 10389


    ACS CCDs daily monitor - Cycle 13 - Part 2


    This program consists of a set of basic tests to monitor, the read
    noise, the development of hot pixels and test for any source of noise
    in ACS CCD detectors. The files, biases and dark will be used to
    create reference files for science calibration. This programme will be
    for the entire lifetime of ACS.


    ACS/WFC/WFPC2 10092


    The COSMOS 2-Degree ACS Survey


    We will undertake a 2 square degree imaging survey {Cosmic Evolution
    Survey -- COSMOS} with ACS in the I {F814W} band of the VIMOS
    equatorial field. This wide field survey is essential to understand
    the interplay between Large Scale Structure {LSS} evolution and the
    formation of galaxies, dark matter and AGNs and is the one region of
    parameter space completely unexplored at present by HST. The
    equatorial field was selected for its accessibility to all
    ground-based telescopes and low IR background and because it will
    eventually contain ~100, 000 galaxy spectra from the VLT-VIMOS
    instrument. The imaging will detect over 2 million objects with I> 27
    mag {AB, 10 sigma}, over 35, 000 Lyman Break Galaxies {LBGs} and
    extremely red galaxies out to z ~ 5. COSMOS is the only HST project
    specifically designed to probe the formation and evolution of
    structures ranging from galaxies up to Coma-size clusters in the epoch
    of peak galaxy, AGN, star and cluster formation {z ~0.5 to 3}. The
    size of the largest structures necessitate the 2 degree field. Our
    team is committed to the assembly of several public ancillary datasets
    including the optical spectra, deep XMM and VLA imaging, ground-based
    optical/IR imaging, UV imaging from GALEX and IR data from SIRTF.
    Combining the full-spectrum multiwavelength imaging and spectroscopic
    coverage with ACS sub-kpc resolution, COSMOS will be Hubble&#39;s ultimate
    legacy for understanding the evolution of both the visible and dark
    universe.


    NIC1/NIC2/NIC3 8793


    NICMOS Post-SAA calibration - CR Persistence Part 4


    A new procedure proposed to alleviate the CR-persistence problem of
    NICMOS. Dark frames will be obtained immediately upon exiting the SAA
    contour 23, and every time a NICMOS exposure is scheduled within 50
    minutes of coming out of the SAA. The darks will be obtained in
    parallel in all three NICMOS Cameras. The POST-SAA darks will be
    non-standard reference files available to users with a USEAFTER
    date/time mark. The keyword &#39;USEAFTER=date/time&#39; will also be added to
    the header of each POST-SAA DARK frame. The keyword must be populated
    with the time, in addition to the date, because HST crosses the SAA ~8
    times per day so each POST-SAA DARK will need to have the appropriate
    time specified, for users to identify the ones they need. Both the raw
    and processed images will be archived as POST-SAA DARKSs. Generally we
    expect that all NICMOS science/calibration observations started within
    50 minutes of leaving an SAA will need such maps to remove the CR
    persistence from the science images. Each observation will need its
    own CRMAP, as different SAA passages leave different imprints on the
    NICMOS detectors.


    NIC2 10176


    Coronagraphic Survey for Giant Planets Around Nearby Young Stars


    A systematic imaging search for extra-solar Jovian planets is now
    possible thanks to recent progress in identifying "young stars near
    Earth". For most of the proposed young {<~ 30 Myrs} and nearby {<~ 60
    pc} targets, we can detect a few Jupiter-mass planets as close as a
    few tens of AUs from the primary stars. This represents the first time
    that potential analogs of our solar system - that is planetary systems
    with giant planets having semi-major axes comparable to those of the
    four giant planets of the Solar System - come within the grasp of
    existing instrumentation. Our proposed targets have not been observed
    for planets with the Hubble Space Telescope previously. Considering
    the very successful earlier NICMOS observations of low mass brown
    dwarfs and planetary disks among members of the TW Hydrae Association,
    a fair fraction of our targets should also turn out to posses low mass
    brown dwarfs, giant planets, or dusty planetary disks because our
    targets are similar to {or even better than} the TW Hydrae stars in
    terms of youth and proximity to Earth. Should HST time be awarded and
    planetary mass candidates be found, proper motion follow-up of
    candidate planets will be done with ground-based AOs.


    NIC3 10337


    The COSMOS 2-Degree ACS Survey NICMOS Parallels


    The COSMOS 2-Degree ACS Survey NICMOS Parallels. This program is a
    companion to program 10092.


    NIC3/WFPC2 10277


    Ages and Metallicities of the Intergalactic Globular Cluster
    Population in Abell 1185


    We will obtain deep NICMOS observations of a recently discovered
    population of intergalactic globular clusters in the nearby galaxy
    cluster Abell 1185. These H band observations in conjunction with deep
    V and I images that we obtained with ACS in Cycle 11 will allow us to
    measure the ages and metallicities of these objects from their optical
    and near-infrared colors, which will provide important insights to
    their origin. We will also obtain parallel observations with both ACS
    and WFPC2. ACS parallel observations will be used to obtain deep
    images to search for intergalactic globular clusters in a different
    region of Abell 1185. WFPC2 parallel observations will be used to
    obtain images of interacting galaxy pair Arp 105, to search for
    globular clusters currently being ejected into intergalactic space as
    a result of this encounter.


    WFPC2 10132


    UV Confirmation of New Quasar Sightlines Suitable for the Study of
    Intergalactic Helium The reionization of intergalactic helium is
    thought to have occurred between redshifts of about 3 and 4. The study
    of HeII Lyman-alpha absorption towards a half- dozen quasars at
    2.7<z<3.5 demonstrates the great potential of such probes of the IGM,
    but the current critically-small sample limits confidence in resulting
    cosmological inferences. The requisite unobscured quasar sightlines to
    high-redshift are extremely rare, especially due to severe absorption
    in random intervening Lyman-limit systems, but SDSS provides hundreds
    of bright, new quasars at such redshifts potentially suitable for HeII
    studies. Our cycle 13 SNAP program proposes to verify the UV
    detectability of 40 new, bright, z>2.9 SDSS quasars, but with special
    emphasis on extending helium studies to the highest redshift
    sightlines. Our proposed approach has already proven successful, and
    additional sightlines will enable follow-up spectal observations to
    measure the spectrum and evolution of the ionizing background
    radiation, the density of intergalactic baryons, and the epoch of
    reionization of the IGM.


    FLIGHT OPERATIONS SUMMARY:


    Significant Spacecraft Anomalies: (The following are preliminary
    reports of potential non-nominal performance that will be
    investigated.)


    HSTARS:


    9795 - ReAcq(1,0,1) requires multiple CT entries @ 116/19:07:03z OTA
    SE review of the PTAS processing found that the ReAcq(1,0,1) at
    116/19:07:03 required 3 CT entries on FGS1 before achieving CT-DV. The
    ReAcq was successful and no science impact should have been seen.


    9796 - Guide Star ReAquisition Fails Due to Scan Step Limit Exceeded @
    124/19:00:25z Guide Star ReAquisition, Reacq1,2,2, using FGS 1 and 2,
    at 124/19:00:25, failed to RGA control, Due to Scan Step Limite
    Exceeded on FGS 1.


    9797 - ReAcq(1,0,1) requires multiple CT entries @ 117/03:27:24z OTA
    SE review of the PTAS processing found that the ReAcq(1,0,1) at
    117/03:27:24 required 8 CT entries on FGS1 before achieving CT-DV. The
    ReAcq was successful and no science impact should have been seen.


    9798 - U2,3RD Roll Delay Update Failed on FHST 2 @ 125/07:10:25z FHST
    Roll Delay Update U2,3RD scheduled at 125/07:09:32 failed with error
    box results indicating "2 failed" for mnemonics QEBSTFG0, QEBSTFG1,
    QEBSTFG2. 486 status buffer message 901 was received at 07:10:25.
    GSACQ(1,2,2) at 07:24:03 was successful.


    COMPLETED OPS REQUEST: (None)


    COMPLETED OPS NOTES:
    915-3 - HSTAR Requirements for FHST Map/Update Failures @ 125/07:10:25z
    900-1 - Command Problem @ 125/08:40:02z


    SCHEDULED SUCCESSFUL FAILURE TIMES
    FGS Gsacq 12 12
    FGS Reacq 06 05 124/19:00:25z
    FHST Update 13 12 125/07:10:25z
    LOSS of LOCK


    SIGNIFICANT EVENTS: (None)

  29. #29
    StarLab Guest
    Wow...looks like they don&#39;t have much to say today... :blink:

    HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science


    DAILY REPORT # 3854


    PERIOD COVERED: DOY 125


    OBSERVATIONS SCHEDULED


    ACS/HRC 10377


    ACS Earth Flats


    High signal sky flats will be obtained by observing the bright Earth
    with the HRC and WFC. These observations will be used to verify the
    accuracy of the flats currently used by the pipeline and will provide
    a comparison with flats derived via other techniques: L-flats from
    stellar observations, sky flats from stacked GO observations, and
    internal flats using the calibration lamps. Weekly coronagraphic
    monitoring is required to assess the changing position of the spots.


    ACS/WFC 10152


    A Snapshot Survey of a Complete Sample of X-ray Luminous Galaxy
    Clusters from Redshift 0.3 to 0.7


    We propose a public, uniform imaging survey of a well-studied,
    complete, and homogeneous sample of X-ray clusters. The sample of 73
    clusters spans the redshift range between 0.3-0.7. The samples spans
    almost 2 orders of magnitude of X-ray luminosity, where half of the
    sample has X-ray luminosities greater than 10^44 erg/s {0.5-2.0 keV}.
    These snapshots will be used to obtain a fair census of the the
    morphology of cluster galaxies in the cores of clusters, to detect
    radial and tangential arc candidates, to detect optical jet
    candidates, and to provide an approximate estimate of the shear signal
    of the clusters themselves, and potentially an assessment of the
    contribution of large scale structure to lensing shear.


    ACS/WFC/WFPC2 10092


    The COSMOS 2-Degree ACS Survey


    We will undertake a 2 square degree imaging survey {Cosmic Evolution
    Survey -- COSMOS} with ACS in the I {F814W} band of the VIMOS
    equatorial field. This wide field survey is essential to understand
    the interplay between Large Scale Structure {LSS} evolution and the
    formation of galaxies, dark matter and AGNs and is the one region of
    parameter space completely unexplored at present by HST. The
    equatorial field was selected for its accessibility to all
    ground-based telescopes and low IR background and because it will
    eventually contain ~100, 000 galaxy spectra from the VLT-VIMOS
    instrument. The imaging will detect over 2 million objects with I> 27
    mag {AB, 10 sigma}, over 35, 000 Lyman Break Galaxies {LBGs} and
    extremely red galaxies out to z ~ 5. COSMOS is the only HST project
    specifically designed to probe the formation and evolution of
    structures ranging from galaxies up to Coma-size clusters in the epoch
    of peak galaxy, AGN, star and cluster formation {z ~0.5 to 3}. The
    size of the largest structures necessitate the 2 degree field. Our
    team is committed to the assembly of several public ancillary datasets
    including the optical spectra, deep XMM and VLA imaging, ground-based
    optical/IR imaging, UV imaging from GALEX and IR data from SIRTF.
    Combining the full-spectrum multiwavelength imaging and spectroscopic
    coverage with ACS sub-kpc resolution, COSMOS will be Hubble&#39;s ultimate
    legacy for understanding the evolution of both the visible and dark
    universe.


    FGS 10432


    Precise Distances to Nearby Planetary Nebulae


    We propose to carry out astrometry with the FGS to obtain accurate and
    precise distances to four nearby planetary nebulae. In 1992, Cahn et
    al. noted that ``The distances to Galactic planetary nebulae remain a
    serious, if not THE most serious, problem in the field, despite
    decades of study.&#39;&#39; Twelve years later, the same statement still
    applies. Because the distances to planetary nebulae are so uncertain,
    our understanding of their masses, luminosities, scale height, birth
    rate, and evolutionary state is severely limited. To help remedy this
    problem, HST astrometry can guarantee parallaxes with half the error
    of any other available approach. These data, when combined with
    parallax measurements from the USNO, will improve distance
    measurements by more than a factor of two, producing more accurate
    distances with uncertainties that are of the order of ~6%. Lastly,
    most planetary nebula distance scales in the literature are
    statistical. They require several anchor points of known distance in
    order to calibrate their zero point. Our program will provide "gold
    standard" anchor points by the end of 2006, a decade before any
    anticipated results from future space astrometry missions.


    NIC1/NIC2/NIC3 10381


    Photometric Stability


    This NICMOS calibration proposal carries out photometric monitoring
    observations during Cycle 13. The format of the program is identical
    to that of the Cycle 12 program 9995


    NIC1/NIC2/NIC3 8793


    NICMOS Post-SAA calibration - CR Persistence Part 4


    A new procedure proposed to alleviate the CR-persistence problem of
    NICMOS. Dark frames will be obtained immediately upon exiting the SAA
    contour 23, and every time a NICMOS exposure is scheduled within 50
    minutes of coming out of the SAA. The darks will be obtained in
    parallel in all three NICMOS Cameras. The POST-SAA darks will be
    non-standard reference files available to users with a USEAFTER
    date/time mark. The keyword &#39;USEAFTER=date/time&#39; will also be added to
    the header of each POST-SAA DARK frame. The keyword must be populated
    with the time, in addition to the date, because HST crosses the SAA ~8
    times per day so each POST-SAA DARK will need to have the appropriate
    time specified, for users to identify the ones they need. Both the raw
    and processed images will be archived as POST-SAA DARKSs. Generally we
    expect that all NICMOS science/calibration observations started within
    50 minutes of leaving an SAA will need such maps to remove the CR
    persistence from the science images. Each observation will need its
    own CRMAP, as different SAA passages leave different imprints on the
    NICMOS detectors.


    NIC3 10337


    The COSMOS 2-Degree ACS Survey NICMOS Parallels


    The COSMOS 2-Degree ACS Survey NICMOS Parallels. This program is a
    companion to program 10092.


    FLIGHT OPERATIONS SUMMARY:


    Significant Spacecraft Anomalies: (The following are preliminary
    reports of potential non-nominal performance that will be
    investigated.)


    HSTARS:


    9800 - GSAcq (1,3,1) Results in Fine Lock Backup GSAcq (1,0,1) @
    125/14:01:07z GSAcq (1,3,1) scheduled for 125/13:53:51 - 14:01:07
    resulted in Fine Lock on FGS 1 only due to scan step limit exceeded on
    FGS 3. The previous updates scheduled at 13:36 and 13:39 both passed
    with small attitude error. The following map scheduled for 14:30:xx
    showed attitude errors of: -1.026, -7.212 and -1.703 arcsec.


    COMPLETED OPS REQUEST: (None)


    COMPLETED OPS NOTES:
    0900-1 - Command Problem @ 125/20:16:44z
    0900-1 - Command Problem @ 125/20:22:23z
    1335-0 - EPS Limit Changes During High Sun Time @ 126/0600z


    SCHEDULED SUCCESSFUL FAILURE TIMES
    FGS Gsacq 13 13
    FGS Reacq 03 03
    FHST Update 17 17
    LOSS of LOCK


    SIGNIFICANT EVENTS: (None)

  30. #30
    StarLab Guest
    HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science


    DAILY REPORT # 3855


    PERIOD COVERED: DOY 126 - 128


    OBSERVATIONS SCHEDULED


    NIC1/NIC2/NIC3 8793


    NICMOS Post-SAA calibration - CR Persistence Part 4


    A new procedure proposed to alleviate the CR-persistence problem of
    NICMOS. Dark frames will be obtained immediately upon exiting the SAA
    contour 23, and every time a NICMOS exposure is scheduled within 50
    minutes of coming out of the SAA. The darks will be obtained in
    parallel in all three NICMOS Cameras. The POST-SAA darks will be
    non-standard reference files available to users with a USEAFTER
    date/time mark. The keyword &#39;USEAFTER=date/time&#39; will also be added to
    the header of each POST-SAA DARK frame. The keyword must be populated
    with the time, in addition to the date, because HST crosses the SAA ~8
    times per day so each POST-SAA DARK will need to have the appropriate
    time specified, for users to identify the ones they need. Both the raw
    and processed images will be archived as POST-SAA DARKSs. Generally we
    expect that all NICMOS science/calibration observations started within
    50 minutes of leaving an SAA will need such maps to remove the CR
    persistence from the science images. Each observation will need its
    own CRMAP, as different SAA passages leave different imprints on the
    NICMOS detectors.


    ACS/HRC/WFC 10436


    Black Hole Growth and the Black Hole Mass -- Bulge Relations for AGNs


    Recent work has shown that the mass of a black hole is tightly
    correlated with the bulge mass of its host galaxy. This relation needs
    to be understood in the context of black hole growth in its active
    phase. Highly accreting AGNs, like narrow line Seyfert 1 galaxies
    {NLS1s}, are found to lie below the black hole mass -- bulge velocity
    dispersion correlation of normal galaxies and broad line AGNs. This
    result was obtained using FWHM{[OIII]} as a surrogate for the bulge
    velocity dispersion. To test this result we propose to obtain high
    resolution images of 10 NLS1s that do not lie on the black hole
    mass--sigma relation and measure accurate bulge parameters {luminosity
    and effective radius}. We will obtain an alternate handle on the bulge
    velocity dispersion through the fundamental plane relations and also
    find the locus of these NLS1s on the black hole mass--bulge luminosity
    plane. Testing this result is crucial to understanding the role of
    accretion on black hole growth, the observed correlations of the black
    hole mass with the bulge, and the formation and evolution of galaxies.


    ACS/WFC 10429


    Streaming Towards Shapley: The Mass of the Richest Galaxy
    Concentration in the Local Universe


    The 600 km/s motion of the Local Group {LG} with respect to the cosmic
    microwave background {CMB} is now known to high accuracy. However, its
    precise origin remains poorly understood. The contribution to the
    motion from the pull of the rich Shapley supercluster at z = 0.048 is
    particularly controversial. This extreme mass concentration contains
    more than 20 Abell clusters within 35 Mpc of its very rich central
    cluster A3558, and is recognized as both the optically richest and the
    most X-ray luminous structure in the local {z < 0.1} universe. Yet,
    published values for the mass of Shapley continue to differ by an
    order of magnitude, and recent estimates of its pull on the LG range
    from negligible {20 km/s} to highly significant {300 km/s or more}.
    Here we propose to resolve this key issue by using ACS to measure
    high- precision surface brightness fluctuation {SBF} distances in
    order to make a direct measurement of the infall towards Shapley. We
    will target three Shapley foreground clusters where the infall is
    expected to be high {possibly 1000 km/s or more}, as well as the
    Shapley core, in order to test the assumption that it is at rest in
    the CMB. Prior to ACS, the Shapley region was unreachable for SBF, but
    ACS doubles the distance range of the SBF method with HST, enabling
    the distances to be measured to the required accuracy. The proposed
    measurements will place a firm limit on the largest mass fluctuation
    in the nearby universe and finally determine its contribution to the
    observed CMB dipole.


    ACS/HRC 10398


    Transcending Voyager: A Deeper Look at Neptune&#39;s Ring-Moon System


    We will use the High Resolution Channel {HRC} of ACS to study the
    inner rings, arcs and moons of Neptune with a sensitivity that exceeds
    that achieved by Voyager 2 during its 1989 flyby. Our study will
    reveal any moons down to V magnitude 25.5, to address a peculiar
    truncation in the size distribution of inner moons and to look for the
    "shepherds" and source bodies for Neptune&#39;s dusty rings. {For
    comparison, Neptune&#39;s smallest known moon is Naiad, at magnitude
    23.9}. Recent ground-based studies show that the mysterious arcs in
    the Adams Ring continue to shift and change, and may be fading away
    entirely. We will obtain the visual-band data uniquely necessary to
    determine whether the arcs are fading. Long-term monitoring of the
    arcs at high resolution and sensitivity will reveal their gradual
    changes more clearly and enable us to assess the role of Galatea,
    whose resonances are widely believed to confine the arcs.


    ACS/HRC/WFC 10389


    ACS CCDs daily monitor - Cycle 13 - Part 2


    This program consists of a set of basic tests to monitor, the read
    noise, the development of hot pixels and test for any source of noise
    in ACS CCD detectors. The files, biases and dark will be used to
    create reference files for science calibration. This programme will be
    for the entire lifetime of ACS.


    WFPC2 10356


    WFPC2 Cycle 13 Decontaminations and Associated Observations


    This proposal is for the monthly WFPC2 decons. Also included are
    instrument monitors tied to decons: photometric stability check, focus
    monitor, pre- and post- decon internals {bias, intflats, kspots, &
    darks}, UV throughput check, VISFLAT sweep, and internal UV flat
    check.


    NIC3 10337


    The COSMOS 2-Degree ACS Survey NICMOS Parallels


    The COSMOS 2-Degree ACS Survey NICMOS Parallels. This program is a
    companion to program 10092.


    ACS/HRC 10185


    When does Bipolarity Impose itself on the Extreme Mass Outflows from
    AGB Stars? An ACS SNAPshot Survey


    Essentially all well-characterized preplanetary nebulae {PPNe} --
    objects in transition between the AGB and planetary nebula
    evolutionary phases - are bipolar, whereas the mass-loss envelopes of
    AGB stars are strikingly spherical. In order to understand the
    processes leading to bipolar mass-ejection, we need to know at what
    stage of stellar evolution does bipolarity in the mass-loss first
    manifest itself? Our previous SNAPshot surveys of a PPNe sample {with
    ACS & NICMOS} show that roughly half our targets observed are
    resolved, with well-defined bipolar or multipolar morphologies.
    Spectroscopic surveys of our sample confirm that these objects have
    not yet evolved into planetary nebulae. Thus, the transformation from
    spherical to aspherical geometries has already fully developed by the
    time these dying stars have become preplanetary nebulae. From this new
    and surprising result, we hypothesize that the transformation to
    bipolarity begins during the very late AGB phase, and happens very
    quickly, just before, or as the stars are evolving off the AGB. We
    propose to test this hypothesis quantitatively, through a SNAPshot
    imaging survey of very evolved AGB stars which we believe are nascent
    preplanetary nebulae; with our target list being drawn from published
    lists of AGB stars with detected heavy mass-loss {from millimeter-wave
    observations}. This survey is crucial for determining how and when the
    bipolar geometry asserts itself. Supporting kinematic observations
    using long-slit optical spectroscopy {with the Keck}, millimeter and
    radio interferometric observations {with OVRO, VLA & VLBA} are being
    undertaken. The results from this survey {together with our previous
    work} will allow us to draw general conclusions about the onset of
    bipolar mass-ejection during late stellar evolution, and will provide
    crucial input for theories of post-AGB stellar evolution. Our survey
    will produce an archival legacy of long-standing value for future
    studies of dying stars.


    NIC2 10177


    Solar Systems In Formation: A NICMOS Coronagraphic Survey of
    Protoplanetary and Debris Disks


    Until recently, despite decades of concerted effort applied to
    understanding the formation processes that gave birth to our solar
    system, the detailed morphology of circumstellar material that must
    eventually form planets has been virtually impossible to discern. The
    advent of high contrast, coronagraphic imaging as implemented with the
    instruments aboard HST has dramatically enhanced our understanding of
    natal planetary system formation. Even so, only a handful of evolved
    disks {~ 1 Myr and older} have been imaged and spatially resolved in
    light scattered from their constituent grains. To elucidate the
    physical processes and properties in potentially planet-forming
    circumstellar disks, and to understand the nature and evolution of
    their grains, a larger spatially resolved and photometrically reliable
    sample of such systems must be observed. Thus, we propose a highly
    sensitive circumstellar disk imaging survey of a well-defined and
    carefully selected sample of YSOs {1-10 Myr T Tau and HAeBe stars} and
    {> app 10 Myr} main sequence stars, to probe the posited epoch of
    planetary system formation, and to provide this critically needed
    imagery. Our resolved images will shed light on the spatial
    distributions of the dust in these thermally emissive disks. In
    combination with their long wavelength SEDs the physical properties of
    the grains will be discerned, or constrained by our photometrically
    accurate surface brightness sensitivity limits for faint disks which
    elude detection. Our sample builds on the success of the exploratory
    GTO 7233 program, using two-roll per orbit PSF- subtracted NICMOS
    coronagraphy to provide the highest detection sensitivity to the
    smallest disks around bright stars which can be imaged with HST. Our
    sample will discriminate between proposed evolutionary scenarios while
    providing a legacy of cataloged morphologies for interpreting mid- and
    far-IR SEDs that the recently launched Spitzer Space Telescope will
    deliver.


    NIC2 10176


    Coronagraphic Survey for Giant Planets Around Nearby Young Stars


    A systematic imaging search for extra-solar Jovian planets is now
    possible thanks to recent progress in identifying "young stars near
    Earth". For most of the proposed young {<~ 30 Myrs} and nearby {<~ 60
    pc} targets, we can detect a few Jupiter-mass planets as close as a
    few tens of AUs from the primary stars. This represents the first time
    that potential analogs of our solar system - that is planetary systems
    with giant planets having semi-major axes comparable to those of the
    four giant planets of the Solar System - come within the grasp of
    existing instrumentation. Our proposed targets have not been observed
    for planets with the Hubble Space Telescope previously. Considering
    the very successful earlier NICMOS observations of low mass brown
    dwarfs and planetary disks among members of the TW Hydrae Association,
    a fair fraction of our targets should also turn out to posses low mass
    brown dwarfs, giant planets, or dusty planetary disks because our
    targets are similar to {or even better than} the TW Hydrae stars in
    terms of youth and proximity to Earth. Should HST time be awarded and
    planetary mass candidates be found, proper motion follow-up of
    candidate planets will be done with ground-based AOs.


    ACS/WFC 10174


    Dark-matter halos and evolution of high-z early-type galaxies


    Gravitational lensing and stellar dynamics provide two complementary
    methods to determine the mass distribution and evolution of luminous
    and dark-matter in early- type {E/S0} galaxies. The combined study of
    stellar dynamics and gravitational lensing allows one to break
    degeneracies inherent to each method separately, providing a clean
    probe of the internal structure of massive galaxies. Since most lens
    galaxies are at redshifts z=0.1-1.0, they also provide the required
    look-back time to study their structural and stellar-population
    evolution. We recently analyzed 5 E/S0 lens galaxies between z=0.5 and
    1.0, combining exquisite Hubble Space Telescope imaging data with
    kinematic data from ground-based Keck spectroscopy, placing the first
    precise constraints on the dark-matter mass fraction and its inner
    slope beyond the local Universe. To expand the sample to ~30 systems
    -- required to study potential trends and evolution in the E/S0 mass
    profiles -- we propose to target the 49 E/S0 lens-galaxy candidates
    discovered by Bolton et al. {2004} from the Sloan Digital Sky Survey
    {SDSS}. With the average lens rate being 40% and some systems having a
    lensing probability close to unity, we expect to discover ~20 strong
    gravitational lenses from the sample. This will triple the current
    sample of 9 E/S0 systems, with data in hand. With the sample of 30
    systems, we will be able to determine the average slope of the
    dark-matter and total mass profile of E/S0 galaxies to 10% and 4%
    accuracy, respectively. If present, we can simultaneously detect 10%
    evolution in the total mass slope with 95% confidence. This will
    provide unprecedented constraints on E/S0 galaxies beyond the local
    Universe and allow a stringent test of their formation scenarios and
    the standard cosmological model.


    ACS 10140


    Identification of a magnetic anomaly at Jupiter from satellite
    footprints


    Repeated imaging of Jupiter&#39;s aurora has shown that the northern main
    oval has a distorted &#39;kidney bean&#39; shape in the general range of
    90-140? System III longitude, which appears unchanged since 1994.
    While it is more difficult to observe the conjugate regions in the
    southern aurora, no corresponding distortion appears in the south.
    Recent improved accuracy in locating the satellite footprint auroral
    emissions has provided new information about the geometry of Jupiter&#39;s
    magnetic field in this and other areas. The study of the magnetic
    field provides us with insight into the state of matter and the
    dynamics deep down Jupiter. There is currently no other way to do this
    from orbit. The persistent pattern of the main oval implies a
    disturbance of the local magnetic field, and the increased latitudinal
    separation of the locus of satellite footprints from each other and
    from the main oval implies a locally weaker field strength. It is
    possible that these phenomena result from a magnetic anomaly in
    Jupiter&#39;s intrinsic magnetic field, as was proposed by A. Dessler in
    the 1970&#39;s. There is presently only limited evidence from the scarcity
    of auroral footprints observed in this longitude range. We propose to
    obtain HST UV images with specific observing geometries of Jupiter to
    determine the locations of the auroral footprints of Io, Europa, and
    Ganymede in cycle 13 to accurately determine the magnetic field
    geometry in the suggested anomaly region, and to either confirm or
    refute the suggestion of a local magnetic anomaly.


    ACS/WFC/WFPC2 10092


    The COSMOS 2-Degree ACS Survey


    We will undertake a 2 square degree imaging survey {Cosmic Evolution
    Survey -- COSMOS} with ACS in the I {F814W} band of the VIMOS
    equatorial field. This wide field survey is essential to understand
    the interplay between Large Scale Structure {LSS} evolution and the
    formation of galaxies, dark matter and AGNs and is the one region of
    parameter space completely unexplored at present by HST. The
    equatorial field was selected for its accessibility to all
    ground-based telescopes and low IR background and because it will
    eventually contain ~100, 000 galaxy spectra from the VLT-VIMOS
    instrument. The imaging will detect over 2 million objects with I> 27
    mag {AB, 10 sigma}, over 35, 000 Lyman Break Galaxies {LBGs} and
    extremely red galaxies out to z ~ 5. COSMOS is the only HST project
    specifically designed to probe the formation and evolution of
    structures ranging from galaxies up to Coma-size clusters in the epoch
    of peak galaxy, AGN, star and cluster formation {z ~0.5 to 3}. The
    size of the largest structures necessitate the 2 degree field. Our
    team is committed to the assembly of several public ancillary datasets
    including the optical spectra, deep XMM and VLA imaging, ground-based
    optical/IR imaging, UV imaging from GALEX and IR data from SIRTF.
    Combining the full-spectrum multiwavelength imaging and spectroscopic
    coverage with ACS sub-kpc resolution, COSMOS will be Hubble&#39;s ultimate
    legacy for understanding the evolution of both the visible and dark
    universe.


    FLIGHT OPERATIONS SUMMARY:


    Significant Spacecraft Anomalies: (The following are preliminary
    reports of potential non-nominal performance that will be
    investigated.)


    HSTARS:


    9801 - GSACQ(1,2,2) fine lock backup, search radius limit exceeded on
    FGS 2 @ 126/09:38:25z GSACQ(1,2,2) at 126/09:34:06 failed to fine lock
    backup on FGS 1 due to Search Radius Limit Exceeded on FGS 2 at
    09:38:25. Additional acquisition attempts also failed at 09:39:15 and
    09:40:43. FHST map at 09:43:00 showed attitude errors of 16.645,
    -7.867, -1.279.


    9803 - Event Failed To Configure at STGT @ 127/09:09:45z (Ref: CDS
    #39445) Due to an equipment failure at STGT. The MA ADPE hung at event
    start time and caused HST to lose 36 minutes and 29 second of R/T 32
    kb data non-recoverable. Anomaly start 127/09:09:45z Anomaly stop
    127/09:47:14z. CDS # 39445.


    COMPLETED OPS REQUEST: (None)


    COMPLETED OPS NOTES:
    0916-0 - Tabulation of Slew Attitude Error (Miss-distance) @ 129/0211z
    0915-3 - HSTAR Requirements for FHST Map/Update Failures @ 129/0214z
    0900-1 - COMMAND PROBLEM @ 128/18:35:39z
    0900-1 - COMMAND PROBLEM @ 129/08:29:58z


    SCHEDULED SUCCESSFUL FAILURE TIMES
    FGS Gsacq 31 31
    FGS Reacq 16 16
    FHST Update 44 43 129/02:14:38z
    LOSS of LOCK


    SIGNIFICANT EVENTS: (None)

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