HST Daily Report # 3352

HUBBLE SPACE TELESCOPE

DAILY REPORT # 3352

PERIOD COVERED: DOY 119 (partial day observations due to safemode
event-see
SIGNIFICANT EVENTS section)

OBSERVATIONS SCHEDULED

NICMOS 8791

NICMOS Post-SAA calibration – CR Persistence Part 2

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.

ACS/WFC 9351

Determining Hubble’s Constant from Observations of Cepheids in the Host
Galaxy
of SN Ia 1994ae

the host spiral galaxy NGC 3370. Modern CCD photometry has yielded an
extremely
tight Hubble diagram for SNe Ia with a precisely determined intercept
{i.e.,
Delta H_0/H_0} 1 measurement of the true Hubble constant is still limited
by the
calibration. The HST calibration of all but a few SNe Ia observed to date
is
significantly compromised by the systematics of photographic photometry
and
host
galaxy extinction, as well as by the photometric uncertainties associated
with
WFPC2. In contrast, SN 1994ae is one of the very best-observed SNe Ia
with CCD
photometry. The exquisite B, V, R, and I light curves are well-sampled
beginning
10 days before maximum brightness, and they indicate little reddening.
From our
supernova photometry and the current provisional SN Ia calibration we
would
find
a distance of 30 +/- 2.1 Mpc, well within the range where ACS can
accurately
observe Cepheid light curves and distinguish Cepheids from nonvariable
stars.

HST 9382

A Large Targeted Survey for z < 1.6 Damped Lyman Alpha Lines in SDSS QSO
MgII-FeII Systems.

We have searched the first public release of SDSS QSO spectra for low-z
{z<1.65}
metal absorption lines and found over 200 large rest equivalent width
MgII-FeII
systems. Previously, we empirically showed that such systems are good
tracers of
large neutral gas columns, with ~50% being classical damped Lyman alpha
{DLA}
systems {N_HI>=2*10^20 cm^-2}. Here we propose to follow up a
well-defined
subset of 79 of them to search for DLAs with 0.47<z<1.60. Only QSOs
brighter
than g’=19 were selected. The QSO emission and DLA absorption redshifts
were
constrained to virtually eliminate data loss due to intervening Lyman
limit
absorption. Consequently, we expect to discover ~40 new DLAs, which is a
three-fold increase in this redshift interval. This will significantly
improve
our earlier low-z DLA statistical results on their incidence,
cosmological mass
density, and N_HI distribution. The results will also allow us to better
quantify the empirical DLA — metal-line correlation. With this improved
understanding, the need for follow-up UV spectroscopy will lessen and,
with the
release of the final database of SDSS QSO spectra {an ~25-fold increase},
the
number of low-z DLAs could be increased arbitrarily. Thus, the power of
the
large and statistically-sound SDSS database in combination with a proven
technique for finding low-z DLAs will, over the next few years,
essentially
solve the problem of making an accurate determination of the cosmic
evolution of
the neutral gas component down to z~0.4.

ACS 9454

The Nature of the UV Continuum in LINERs: A Variability Test

LINERs may be the most common AGNs, and the signposts of accretion onto
the
massive black holes present in most galaxies. However, the LINER spectrum
is the
result of UV excitation, and, in at least some LINERs, a nuclear cluster
of hot
stars, rather than an AGN, dominates the energetics in the UV. Thus, it
is
still
unknown if the UV continuum, or the optical emission lines it excites,
have
anything to do with an AGN. The demographics and accretion physics of
low-luminosity AGNs hinge on this question. We propose to search for
variability
in a sample of 17 LINERs with compact UV nuclei. Variability can reveal
an AGN
component in the UV continuum, even when its light is not dominant. We
will
test
systematically the handful of non-definitive reports of UV variability,
and
potentially quantify the AGN contribution to the UV emission. Variability
in all
or most objects will be strong evidence that LINERs mark dormant AGNs in
most
galaxies. Alternatively, a general null detection of variability will
suggest
that, even in LINERs with additional AGN signatures, the UV continuum is
stellar
in origin. Contemporaneous monitoring with the VLA/VLBA of 11 objects
which
have
radio cores {five of which we already know are radio-variable} will
reveal the
relations between UV and radio variations. The UV-variable objects will
be
targeted for future, better-sampled, monitoring.

ACS 9480

Cosmic Shear With ACS Pure Parallels

Small distortions in the shapes of background galaxies by foreground mass
provide a powerful method of directly measuring the amount and
distribution of
dark matter. Several groups have recently detected this weak lensing by
large-scale structure, also called cosmic shear. The high resolution and
sensitivity of HST/ACS provide a unique opportunity to measure cosmic
shear
accurately on small scales. Using 260 parallel orbits in Sloan textiti
{F775W}
we will measure for the first time: beginlistosetlength sep0cm
setlengthemsep0cm
setlength opsep0cm em the cosmic shear variance on scales <0.7 arcmin, em
the
skewness of the shear distribution, and em the magnification effect.
endlist Our
measurements will determine the amplitude of the mass power spectrum
sigma_8Omega_m^0.5, with signal-to-noise {s/n} ~ 20, and the mass density
Omega_m with s/n=4. They will be done at small angular scales where
non-linear
effects dominate the power spectrum, providing a test of the
gravitational
instability paradigm for structure formation. Measurements on these
scales are
not possible from the ground, because of the systematic effects induced
by PSF
smearing from seeing. Having many independent lines of sight reduces the
uncertainty due to cosmic variance, making parallel observations ideal.

NICMOS 9484

The NICMOS Parallel Observing Program

NICMOS parallel program and the public parallel NICMOS programs in cycle
7
prepared us to make optimal use of the parallel opportunities. The NICMOS
G141
grism remains the most powerful survey tool for HAlpha emission-line
galaxies at
cosmologically interesting redshifts. It is particularly well suited to
addressing two key uncertainties regarding the global history of star
formation:
the peak rate of star formation in the relatively unexplored but critical
1<= z
<= 2 epoch, and the amount of star formation missing from UV
continuum-based
estimates due to high extinction. Our proposed deep G141 exposures will
increase
the sample of known HAlpha emission- line objects at z ~ 1.3 by roughly
an
order
of magnitude. We will also obtain a mix of F110W and F160W images along
random
sight-lines to examine the space density and morphologies of the reddest
galaxies. The nature of the extremely red galaxies remains unclear and
our
program of imaging and grism spectroscopy provides unique information
regarding both the incidence of obscured star bursts and the build up of
stellar
mass at intermediate redshifts. In addition to carrying out the parallel
program
we will populate a public database with calibrated spectra and images,
and
provide limited ground- based optical and near-IR data for the deepest
parallel
fields.

WFPC2 9594

WFPC2 CYCLE 11 SUPPLEMENTAL DARKS pt2/3

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

STIS 9606

CCD Dark Monitor-Part 2

Monitor the darks for the STIS CCD.

STIS 9608

CCD Bias Monitor – Part 2

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, to build up high-S/N superbiases and track the evolution of
hot
columns.

ACS 9658

ACS Earth Flats

This program will obtain sequences of flat field images by observing the
bright
Earth. Several UV filters from the interim calibration program {9564}
require
additional exposures to obtain the required illumination. A few UV
filters from
this program will be repeated to monitor for changes in the flat fields
and to
verify the interim results. Since no streaks are observed in the UV, the
wavelength coverage is extended to longer wavelengths in order to explore
the
severity of streaks in the flats from clouds in the FOV. We have added
exposures
for the HRC in the visible filters to verify the results derived from the
L-flat
campaign and to explore the severity of streaks. We have also added
exposures on
WFC using the minimum exposure time and using filters which will not
saturate
the brightest WFC pixel by more than 10 times the full well.

WFPC2/PC1 9663

Focus Monitoring

The HST focus is monitored using WFPC2/PC1. In principle ACS/HRC should
provide
superior capability for monitoring the HST focus. Since most of the HST
science
will shift to ACS in Cycle 11 trending observations are continued with
this
program to establish the focus of WFPC2/PC1 {and hence HST} and ACS/HRC
{and WFC
to a lessor degree} using exposures over full orbits that are taken in
parallel.
With parallel exposures breathing cancels out for the relative camera
offset.

ACS 9674

CCD Daily Monitor

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.

STIS 9708

STIS Pure Parallel Imaging Program: Cycle 11

WFPC2 9709

POMS Test Proposal: WFII parallel archive proposal

Used to take parallel images of random areas of the sky, following the
recommendations of the 2002 Parallels Working Group.

WFPC2 9710

POMS Test Proposal: WFII backup parallel archive proposal

This is a POMS test proposal designed to simulate scientific plans.

FLIGHT OPERATIONS SUMMARY:

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

HSTAR 9008: Gyro 3 Motor Current (GRG2_3MC) spiked for several samples
@ 119/12:18:09Z, reaching a maximum value of 294
mA
@ 119/12:18:33Z.
Current was running around 193 mA before the
spike,
settle to 201 mA
after the spike.

HSTAR 9010: Zero Gyro Safemode entry @ 119/14:21:39Z. See HSTAR
9008. Gyro 3 Motor
Current spiked @ 119/12:18:33Z, three additional
current spikes were
observed beginning at 119/14:03:22Z, leading to a
large increase in Gyro
3 Motor Current beginning ~ 119/14:19Z. FGS 1
suffered LOL @ 119/14:16:42Z
and recovered FL @ 119/14:18:33Z. After normal LOS
@
119/14:20:15Z for TDRSS
ZOE, when telemetry recovered @ 119/14:35:26Z,
Observatory was in ZGSP.
System Momentum Test failed @ 119/14:21:39Z, Two
Gyro
Test failed @ 119/14:24:37Z.

COMPLETED OPS REQs:

• 16939-0 Contingency GYRO#3 Restart#2 @119/1537z
• 16755-2 Contingency GYRO#1 Power On in ZG Safemode @119/1543z
• 16942-0 Dump ESB Messages @119/1715z
• 16943-0 Power On GEA/TAGS after ZGSP Entry @119/1718z
• 16945-1 Transition NICMOS to SAAOPER @119/1817z
• 16946-0 GYRO 1246 Reconfiguration @119/1949z
• 16947-0 Recovery from ZGSP @119/1954z/Completed @120/0609z
• 16948-0 Transition WFPC-2 from DECON to Standby @119/2100z
• 16949-0 ZGSP Recovery Steps 24 Load name @119/2128z
• 16950-1 R/T Map @119/2233z
• 16951-1 R/T Map @119/2240z
• 16952-1 R/T Map @120/0002z
• 16954-0 LBBIAS Uplink @120/0111z
• 16953-0 R/T Map @120/0132z
• 16955-0 ARU/PRT @120/0204z
• 16956-1 Update PSEA RGA Configuration @120/0250z
• 16957-0 R/T Map @120/0508z
• 16958-0 N02Z9950A Uplink, Set pointer & Clear Safeinit Flags @120/0321z
• 16959-0 LBBIAS Uplink @120/0620z
• 16960-0 ARU/PRT @120/0721z

OPS NOTES EXECUTED:

• 0911-0 Limit Management during WFPCII Decontamination @119/2115z(M001)
• 1095-5 Consolidated PCS Limit Modifications@120/0401z

SCHEDULED SUCCESSFUL FAILURE TIMES
FGS GSacq 2 2
FGS REacq 2 2
FHST Update 1 1
LOSS of LOCK

SIGNIFICANT EVENTS:

Zero gyro Safemode entry 119:14:21:39z due to gyro 3 current spikes. The
Health and
Safety load is scheduled to start at 120/02:00, with the Science Mission
Specification
(science intercept load) starting at 121/00:00.

More detailed safemode descriptions:
Gyro 3 Motor Current (GRG2_3MC) spiked for several samples @
119/12:18:09Z,
reaching
a maximum value of 294 mA @ 119/12:18:33Z. Motor Current was running
around 193 mA
before the spike, settled down around 201 mA after the spike. See HSTAR
9008.

Gyro 3 Motor Current spiked an addition three times beginning @
119/14:19Z. Normal LOS
for TDRSS ZOE occurred @ 119/14:20:15Z. After exit ZOE and telemetry
was
recovered,
data showed Observatory in ZGSP. System Momentum Test failed @
119/14:21:39Z, Two
Gyro Test failed @ 119/14:24:37Z.

Commencing at 14:52 GMT, operations personnel made three unsuccessful
attempts to restart gyro #3.
Commands were sent to start Gyro #1 at 15:42 GMT. Gyro #1 turned on
successfully. Motor
Current stable 120 mA.