Hubble Space Telescope Daily Report #3136 – 12 Jun 2002

HUBBLE SPACE TELESCOPE

DAILY REPORT # 3136

PERIOD COVERED: DOY 163: 0000Z (UTC) 06/11/02 – 0000Z (UTC) 06/12/02

OBSERVATIONS SCHEDULED AND ACCOMPLISHED:

STIS/CCD 8588

Gamma-Ray Bursts and their Host Environments.

The Space Telescope Imaging Spectrograph (CCD) was used to investigate the
physics of gamma-ray bursts {GRBs} and the nature of their host galaxies. The
approach is three-pronged: 1} rapid HST ultraviolet spectroscopy and Chandra
imaging obtained within two days of an outburst will allow probing the physics
of the relativistic fireball and the nature of the ISM surrounding the GRB; 2}
long-term optical monitoring of the optical transient {OT} will permit testing
the hypothesis that GRBs are frequently highly collimated and to determine
whether supernovae underlie GRBs; 3} Chandra and HST observations of “dark”
GRBs
will allow probing one of the greater mysteries surrounding GRBs, the nature of
the bursts without optical counterparts.

STIS 8643

Ultraviolet Properties of the Metal Rich M87 Globular Cluster System

We propose to use STIS imaging to obtain far-ultraviolet photometry of the
metal
rich globular cluster system of the elliptical galaxy M87. This system
represents a key link between the well understood populations of the clusters
and the hot stars in elliptical galaxies, where our physical insight is
presently limited. Our goal is to establish the relationship between cluster
metal abundance and the production of UV-bright populations of stars on the
“extreme horizontal branch” at T{eff} > 16000K. These stars are the source of
the surprising “ultraviolet-upturn” phenomenon in elliptical galaxies. Our
observations will fill a major gap in the present coverage of cluster metal
abundances. This would be an important step in understanding the dependence of
the upturn on its parent stellar population. A basic motivation is the
expectation that the UV-upturn could be the most sensitive probe of the
ages and
abundances of elliptical galaxy populations. We plan to observe 3 fields in
M87,
which will provide a sample of ~ 30–50 UV-detected objects in the brightest 3
magnitudes of its cluster luminosity function. The program is technically
challenging but appears feasible. Relatively long integrations are needed,
under
conditions of minimum dayglow emission from Earth’s atmosphere.

NICMOS 8790

NICMOS Post-SAA calibration – CR Persistence Part 1.

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.

STIS/CCD 8902

Dark Monitor-Part 2.

The Space Telescope Imaging Spectrograph (CCD) was used to monitor the darks.

STIS/CCD 8904

Bias Monitor-Part 2.

The Space Telescope Imaging Spectrograph (CCD) was used to monitor the bias in
the 1×1, 1×2, 2×1, and 2×2 bin settings at gain=1, and 1×1 at gain = 4 in order
to build up high-S/N superbiases and track the evolution of hot columns.

STIS/CCD 8906

Hot Pixel Annealing.

The Space Telescope Imaging Spectrograph (CCD) was used to measure the
effectiveness of the CCD hot pixel annealing process by measuring the dark
current behavior before and after annealing and by searching for any window
contamination effects. In addition, CTE performance is examined by looking for
traps in a low signal level flat.

WFPC2 8934

WFPC2 Decontaminations and Associated Observations Pt. 3/3

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 8938

WFPC2 CYCLE 9 SUPPLEMENTAL DARKS pt3/3.

This dark calibration program obtains 3 dark frames every day to provide data
for monitoring and characterizing the evolution of hot pixels.

ACS/WFC/HRC 8947

Weekly Test.

The Advanced Camera for Surveys (WFC and HRC) was used to perform basic
tests to
monitor, the read noise, the development of hot pixels and test for any source
of noise in ACS CCD detectors. This program will be executed at least once
a day
for the entire lifetime of ACS.

STIS/CCD 9066

Closing in on the Hydrogen Reionization Edge of the Universe.

The Space Telescope Imaging Spectrograph (CCD) was used in parallel constrain
the Hydrogen reionization edge in emission that marks the transition from a
neutral to a fully ionized IGM at a predicted redshifts.

NICMOS 9269

NICMOS Parallel Thermal Background

NICMOS Camera 3 pure parallel exposures in the F222M filter will be
obtained for
the entire duration of SMOV to establish the stability of the
HST+NCS+Instrument
thermal emission.

ACS 9289

Low Redshift Cluster Gravitational Lensing Survey

This proposal has two main scientific goals: to determine the dark matter
distribution of massive galaxy clusters, and to observe the high redshift
universe using these clusters as powerful cosmic telescopes. Deep, g, r, i, z
imaging of a sample of low-z {0.2-0.4} clusters will yield a large sample of
lensed background galaxies with reliable photometric redshifts. Using multiple
pointings with a central overlap region we will reach HDF-like depth in the
central, highly magnified cluster region and a shallower but wider coverage in
the outer cluster regions. By combining strong and weak lensing constraints
with
the photometric redshift information it will be possible to precisely measure
the cluster dark matter distribution with an unprecedented combination of high
spatial resolution and area coverage, avoiding many of the uncertainties which
plague ground-based studies and yielding definitive answers about the structure
of massive dark matter haloes. In addition, the cosmological parameters can be
constrained in a largely model independent way using the multiply lensed
objects
due to the dependence of the Einsteinng radius on the distance to the
source. We0ÐUÏ–can also expect to detect several highly magnified dropout galaxies behind the
clusters in the redshift ranges 4-5 5-6 and 7-8, corresponding to a drop in the
flux in the g, r, and i bands relative to longer wavelength. We will obtain the
best information to date on the giant arcs already known in these clusters,
making possible detailed, pixel-by-pixel studies of their star formation rate,
dust distribution and structural components, including spiral arms, out to a
redshift of around z~2.5 in several passbands.

WF/PC-2 9318

POMS Test Proposal: WFII Parallel Archive Proposal Continuation.

The WF/PC-2 was used to perform the generic target version of the WFPC2
Archival
Pure Parallel program. The program was used to take parallel images of random
areas of the sky, following the recommendations of the Parallels Working
Group.

ACS/CAL 9558

ACS weekly Test

This program consists of basic tests to monitor, the read noise, the
development
of hot pixels and test for any source of noise in ACS CCD detectors. This
programme will be executed once a day for the entire lifetime of ACS.

ACS/WFC 9575

Default {Archival} Pure Parallel Program.

The Advanced Camera for Surveys (WFC) was used to test ACS pure parallels in
POMS.

ACS/WFC 9584

ACS Default {Archival} Pure Parallel Program II.

The Advanced Camera for Surveys (WFC) was used to test ACS pure parallels.

STIS 9618

STIS MAMA Dispersion Solutions

Obtain wavecals just deep enough to constrain wavelength and spatial distortion
maps without overusing the calibration lamp. For the first time on orbit, data
will be obtained at all available central wavelengths. This information will
help constrain global models of STIS optical performance being developed at ECF
and STScI. During the observations, MSM monthly offsets will be set to zero to
complement observations over the past couple of cycles, which occurred at
extreme
monthly offsets. The echelle observations at zero offset will yield dispersion
solutions that are directly applicable to all echelle science data obtained
after monthly offsets are disabled.

FLIGHT OPERATIONS SUMMARY:

HSTARS: (For additional details on see
http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf)

8692 – ‘A’ string backbone data server hung @ 164/0530z

COMPLETED OPS REQs: None

OPS NOTES EXECUTED:

911-0 – Limit Management During WFPC2 Decontamination (M001) @ 163/1425z

                     SCHEDULED     SUCCESSFUL    FAILURE TIMES

FGS GSacq              7                    7

FGS REacq              9                    9

FHST Update            14                 14

LOSS of LOCK          None

Operations Notes:

‘C’ string configured for R/T Operations @ 164/0720z (see HSTAR 8692)

SIGNIFICANT EVENTS: None