Hubble Space Telescope Daily Report #3137 – 13 Jun 2002

HUBBLE SPACE TELESCOPE

DAILY REPORT # 3137

PERIOD COVERED: DOY 164: 0000Z (UTC) 06/12/02 – 0000Z (UTC) 06/13/02

OBSERVATIONS SCHEDULED (see HSTARS below for possible observation problems)

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.

WFPC2 8934

WFPC2 Decontaminations and Associated Observations Pt. 3/3

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.

WF/PC-2 9043

Cepheid Distances to Early-type Galaxies.

The WF/PC-2 was used to continue observations in the HST Key Project on the
Extragalactic Distance Scale and the HST project on the “Calibration of Nearby
Type Ia Supernovae” that have greatly improved our knowledge of the Hubble
Constant by providing a solid zero point for the Tully- Fisher {TF}
relation and
Type Ia Supernovae {SNIa}. However, severe inconsistencies remain for distance
estimators to early-type galaxies such as surface brightness fluctuations
{SBF},
the planetary nebula luminosity function {PNLF}, the fundamental plane
{FP}, and
the globular cluster luminosity function {GCLF}. As a result, the distance to
the Virgo cluster core remains uncertain by as much as 20 determination is
directly affected by a lingering 0.1 mag {5 uncertainty in the photometric
calibration of the WFPC2. Resolving these issues is essential not only to firm
up the extragalactic distance scale, but also to understand the mass and
velocity structure of the local universe. SBF in particular is emerging as the
method of choice for mapping local velocity fields to 10, 000 kms because it
offers an order of magnitude less Malmquist bias than TF, and SNIa are too rare
to study large scale flows effectively. This project will tighten the
photometric calibration of the WFPC2, and provide a solid Cepheid calibration
for SBF and PNLF.

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.

FGS/1 9234

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

Fine Guidance Sensor #1 was used to calibrate the mass-luminosity relation for
stars less massive than 0.2 Msun, with special emphasis on objects near the
stellar/brown dwarf border.

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.

GO 9276

Localization of Optically-Dark Gamma-Ray bursts by Chandra and HST

We propose Chandra {CXO} observations of 4 GRBs detected by the HETE soft X-ray
camera, with contemporaneous observations with HST. These observations are
“relaxed” TOOs, performed 7-16 days after burst detection. To optimize the
chance of isolating Z>10 GRBs, we will select “dark GRBs” for which no optical
counterpart has been found by ground-based searches within 2 days of GRB onset.
Previous CXO GRB searches have required that observations start within ~24
hours
of burst onset, placing an enormous strain on CXO operations. We have
determined
that 30 ks observations made 7-16 days after burst onset will detect sufficient
photons to allow <0.7" localization of the GRB afterglow. We will immediately place all CXO and HST positions and intensities in the public domain via the GCN.

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. We
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.

STIS/CCD 9317

Pure Parallel Imaging Program: Cycle 10.

The Space Telescope Imaging Spectrograph (CCD) was used to perform the default
archival pure parallel program for STIS during cycle 10.

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.

WF/PC-2 9345

Fundamental Properties of L-type Dwarfs in Binaries.

The WF/PC-2 was used to characterize the physical properties of eight L-dwarfs
in four binary systems. The goal is to obtain astrometric, photometric and
spectroscopic measurements of each component that will yield basic information
on their atmospheric and dynamical properties.

ACS 9352

The Deceleration Test from Treasury Type Ia Supernovae at Redshifts 1.2 to 1.6

Type Ia supernovae {SNe Ia} provide the only direct evidence for an
accelerating
universe, an extraordinary result that needs a rigorous test. The case for
cosmic acceleration rests on the observation that SNe Ia at z ~ 0.5 are ~ 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 SN Ia result attributed to
grey dust or cosmic evolution of the SN Ia peak luminosity would not show this
change of sign. We have demonstrated proof of this concept with a single SN Ia,
SN 1997ff at z = 1.7, found and followed by HST. The results suggest an early
epoch of deceleration, but this is too important a conclusion to rest on just
one object. Here we propose to use HST for observations of six SNe Ia in the
range 1.2 <= z <= 1.6, that will be discovered as a byproduct from proposed Treasury programs for high-latitude ACS surveys. Six objects will provide a much firmer foundation for a conclusion that touches on important questions of fundamental physics.

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.

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)

8693 – Data Server on A/string B/B process count drops from 1.0 to 0.0 @
164/0555z

8694 – NICMOS Detector 3 VSRC voltage OOL high @ 164/1107z
At 164/11:07:47 the mnemonic ND3VSRCV(DETECTOR 3 VSRC VOLTAGE)
flagged out
of limits red high EV=5.40402v and went back in bounds at
11:08:17. Red limits L=-0.1 H=5.15. NICMOS was in observe
configuration.
We were in orbit night and we were not in a SAA. The anomaly
happened during a
continuous scan. Observation NIC 110 at 11:07:59 may have been
affected.

8695 – A-String AppServer home fills up @ 163/1848z

8696 – EquationServer_A not running @ 163/2030z

8697 – Please disregard this entry

8698 – Archive on the A/string was hung @ 164/2313z

8699 – SADE 2 – SADM Temp 3 @ 165/0416z

COMPLETED OPS REQs: None

OPS NOTES EXECUTED: None

                      SCHEDULED     SUCCESSFUL    FAILURE TIMES

FGS GSacq               5                  5

FGS REacq               10                10

FHST Update             8                  8

LOSS of LOCK           None

‘B’ string configured for Prime R/T Operations @ 164/1230z

‘A’ string configured for Prime R/T Operations @ 164/1340z

SIGNIFICANT EVENTS:

Continuation of Servicing Mission Orbital Verification and the gradual
resumption of normal science observations and calibrations.