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Daily Report #4287



 
 
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Old January 29th 07, 10:36 PM posted to sci.astro.hubble
Lynn Bassford
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Default Daily Report #4287

HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science

DAILY REPORT # 4287

PERIOD COVERED: UT January 26,27,28, 2007 (DOY 026,027,028)

OBSERVATIONS SCHEDULED

NIC1/NIC2/NIC3 8794

NICMOS Post-SAA calibration - CR Persistence Part 5

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/HRC 11041

ACS CCDs daily monitor

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. For cycle 15 the program will cover 18
months 12.1.06- 05.31.08 and it has been divied into three different
proposal each covering six months. The three proposals are
11041-11042-11043.

WFPC2 10915

ACS Nearby Galaxy Survey

Existing HST observations of nearby galaxies comprise a sparse and
highly non-uniform archive, making comprehensive comparative studies
among galaxies essentially impossible. We propose to secure HST's
lasting impact on the study of nearby galaxies by undertaking a
systematic, complete, and carefully crafted imaging survey of ALL
galaxies in the Local Universe outside the Local Group. The resulting
images will allow unprecedented measurements of: {1} the star
formation history {SFH} of a 100 Mpc^3 volume of the Universe with a
time resolution of Delta[log{t}]=0.25; {2} correlations between
spatially resolved SFHs and environment; {3} the structure and
properties of thick disks and stellar halos; and {4} the color
distributions, sizes, and specific frequencies of globular and disk
clusters as a function of galaxy mass and environment. To reach these
goals, we will use a combination of wide-field tiling and pointed deep
imaging to obtain uniform data on all 72 galaxies within a
volume-limited sample extending to ~3.5 Mpc, with an extension to the
M81 group. For each galaxy, the wide-field imaging will cover out to
~1.5 times the optical radius and will reach photometric depths of at
least 2 magnitudes below the tip of the red giant branch throughout
the limits of the survey volume. One additional deep pointing per
galaxy will reach SNR~10 for red clump stars, sufficient to recover
the ancient SFH from the color-magnitude diagram. This proposal will
produce photometric information for ~100 million stars {comparable to
the number in the SDSS survey} and uniform multi- color images of half
a square degree of sky. The resulting archive will establish the
fundamental optical database for nearby galaxies, in preparation for
the shift of high- resolution imaging to the near-infrared.

ACS/WFC 10881

The Ultimate Gravitational Lensing Survey of Cluster Mass and
Substructure

We propose a systematic and detailed investigation of the mass,
substructure, and thermodynamics of one hundred X-ray luminous galaxy
clusters at 0.15z0.3. The primary goal is to test our recent
suggestion that this population is dominated by dynamically immature
disturbed clusters, and that the observed mass-temperature relation
suffers strong structural segregation. If confirmed, this would
represent a paradigm shift in our observational understanding of
clusters, that were hitherto believed to be dominated by mature,
undisturbed systems. The key observation to this endeavor is Hubble
imaging of cluster cores to identify robustly tangential and radial
multiple arcs and measure the shape of faint galaxies. These strong
and weak lensing signals will give an accurate measure of the total
mass and structure of the dark matter distribution that we will
subsequently compare with X-ray and Sunyaev Zeldovich Effect
observables. The broader applications of our project include 1} the
calibration of mass-temperature and mass-SZE scaling relations which
will be critical for the calibration of proposed dark energy
experiments, and 2} the low redshift baseline study of the
demographics of massive clusters to aid interpretation of future high
redshift {z1} cluster samples. For this ultimate cluster survey, we
request ACS SNAPSHOTS through the F606W filter drawn from a target
list of 143 clusters.

NIC3 10874

Search for Extremely Faint z7 Galaxy Population with Cosmic Lenses

Deep UDF/NICMOS observations find a significant decrease in the number
of galaxy candidates between redshift z=6 and 7, but the sample at z7
is too small to draw conclusions. From our observations of 15 clusters
we have found a number of bright z- dropouts, aided by the lensing
amplification. We propose deep NICMOS observations of the best cases
of cluster centers where a rare combination of a significant lensing
effect and the richness in z-band dropouts in background may
dramatically increase the discovery rate. The NICMOS images will reach
an unprecedented depth of AB~27.8, or AB~30 in nonlensed intrinsic
magnitude, and may find many faint {~0.05L*} galaxies at z=7-10, at a
level that the UDF reaches for z~6 objects. We produce precision mass
distribution maps from weak-lensing models, which enable us to derive
the candidates' intrinsic magnitudes and their luminosity function.
The knowledge of such faint galaxy population at z7 will facilitate
the models of the IGM reionization and future JWST planning.

ACS/SBC 10862

Comprehensive Auroral Imaging of Jupiter and Saturn during the
International Heliophysical Year

A comprehensive set of observations of the auroral emissions from
Jupiter and Saturn is proposed for the International Heliophysical
Year in 2007, a unique period of especially concentrated measurements
of space physics phenomena throughout the solar system. We propose to
determine the physical relationship of the various auroral processes
at Jupiter and Saturn with conditions in the solar wind at each
planet. This can be accomplished with campaigns of observations, with
a sampling interval not to exceed one day, covering at least one solar
rotation. The solar wind plasma density approaching Jupiter will be
measured by the New Horizons spacecraft, and a separate campaign near
opposition in May 2007 will determine the effect of large-scale
variations in the interplanetary magnetic field {IMF} on the Jovian
aurora by extrapolation from near-Earth solar wind measurements. A
similar Saturn campaign near opposition in Jan. 2007 will combine
extrapolated solar wind data with measurements from a wide range of
locations within the Saturn magnetosphere by Cassini. In the course of
making these observations, it will be possible to fully map the
auroral footprints of Io and the other satellites to determine both
the local magnetic field geometry and the controlling factors in the
electromagnetic interaction of each satellite with the corotating
magnetic field and plasma density. Also in the course of making these
observations, the auroral emission properties will be compared with
the properties of the near-IR ionospheric emissions {from ground-based
observations} and non thermal radio emissions, from ground-based
observations for Jupiter?s decametric radiation and Cassini plasma
wave measurements of the Saturn Kilometric Radiation {SKR}.

NIC3 10861

An ACS Treasury Survey of the Coma cluster of galaxies

We propose to use the unique spatial resolution of HST and ACS to
construct a Treasury imaging survey of the core and infall region of
the richest local cluster, Coma. We will observe samples of thousands
of galaxies down to magnitude B=27.3 with the aim of studying in
detail the dwarf galaxy population which, according to hierarchical
models of galaxy formation, are the earliest galaxies to form in the
universe. Our initial scientific objectives a 1} A study of the
structure of the dwarf galaxies, including scaling laws, nuclear
structure and morphology, to compare with hierarchical and
evolutionary models of their formation. 2} A study of the stellar
populations from colors and color gradients, and how the internal
chemical evolution of galaxies is affected by interaction with the
cluster gaseous and galaxy environment. 3} To determine the effect of
the cluster environment upon morphological features, disks, bulges and
bars, by comparing these structure in the Coma sample with field
galaxy samples. 4} Identification of dwarf galaxy samples for further
study with the new generation of multi-object and integral-field
spectrographs on 8-10 metre class telescopes such as Keck, Subaru,
Gemini, and GTC. This is the first such survey of a nearby rich
cluster. It will provide a key database for studies of galaxy
formation and evolution, and a very needed reference for comparison
with similar galaxy surveys both in lower density environments in the
nearby universe, and in high density environments at high redshifts.

ACS/WFC 10813

MgII Absorption Line Systems: Galaxy Halos or the Metal-Enriched IGM?

MgII QSO absorption lines detected in the spectra of background QSOs
were used over a decade ago to infer that all redshift z 0.2
galaxies have gaseous halos of radius ~ 60 kpc. The actual size of the
halo was believed to be proportional to the luminosity of the galaxy.
However, these conclusions are now much harder to understand in light
of the results from numerical simulations which show how gas evolves
in the universe. These models predict that gas and galaxies merely
share the same filamentary structures defined by dark matter. If these
models are correct, how are MgII systems and galaxies really related?
We can better understand the distribution of absorbing gas if we FIRST
select galaxies close to QSO sightlines and THEN search for MgII
absorption at the redshift of the intervening galaxies. This is the
antithesis of the original experiments which sought to find absorbing
galaxies based on known MgII systems. The frequency with which we
detect MgII lines from randomly selected galaxies should enable us to
better understand if absorption arises in the halos of individual
galaxies, or if MgII merely arises in the same IGM that galaxies
inhabit. We have used ground-based telescopes to indentify twenty z =
0.31-0.55 galaxies within 14-51 kpc of a g 20 QSO, and to search for
MgII absorption at the galaxies' redshifts. Surprisingly, we find that
only 50% of our QSOs show MgII absorption. In this proposal, we seek
multi-color ACS images of twelve of the fields to i} correlate the
incidence of MgII with galaxy morphology; ii} determine if absorption
{or lack thereof} is related to galaxy disks or halos; iii} search for
signs of galaxy interactions which may explain the large
cross-sections of MgII systems; and iv} look for faint interloping
galaxies closer to the line of sight than the one we identified. An
important component of the program is to observe each field in the
SDSS g-, r- and i-bands, to permit an estimate of the photometric
redshift of any objects which lie closer to the QSO sightline than the
identified galaxy, and which might actually be responsible for the
absorption.

NIC2, ACS/WFC 10802

SHOES-Supernovae, HO, for the Equation of State of Dark energy

The present uncertainty in the value of the Hubble constant {resulting
in an uncertainty in Omega_M} and the paucity of Type Ia supernovae at
redshifts exceeding 1 are now the leading obstacles to determining the
nature of dark energy. We propose a single, integrated set of
observations for Cycle 15 that will provide a 40% improvement in
constraints on dark energy. This program will observe known Cepheids
in six reliable hosts of Type Ia supernovae with NICMOS, reducing the
uncertainty in H_0 by a factor of two because of the smaller
dispersion along the instability strip, the diminished extinction, and
the weaker metallicity dependence in the infrared. In parallel with
ACS, at the same time the NICMOS observations are underway, we will
discover and follow a sample of Type Ia supernovae at z 1. Together,
these measurements, along with prior constraints from WMAP, will
provide a great improvement in HST's ability to distinguish between a
static, cosmological constant and dynamical dark energy. The Hubble
Space Telescope is the only instrument in the world that can make
these IR measurements of Cepheids beyond the Local Group, and it is
the only telescope in the world that can be used to find and follow
supernovae at z 1. Our program exploits both of these unique
capabilities of HST to learn more about one of the greatest mysteries
in science.

FLIGHT OPERATIONS SUMMARY:

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

HSTARS:

10648 - GSAcq(2,3,3) failed to RGA Hold (Gyro Control)

Upon acquisition of signal at 026/12:48:23, the GSAcq(2,3,3)scheduled
at 026/12:24:55 - 12:33:00 was observed to have failed to RGA Hold due
to stop flag indication on FGS2. Pre-acquisition OBADs (RSS) attitude
correction values not available due to LOS. Post-acquisition OBAD/MAP
showed 3-axis (RSS) error value of 17.93 arcseconds. Subsequent
REacq(2,3,3) at 026/13:56:41 was successful.

10650 - OBAD Failed Identification (ESB 1902)

At 026/00:00:00, OBAD1 using trackers FHST-1 and FHST-3 failed. One
ESB message 1902 (OBAD Failed Identification) was received. ESB 1805
(T2G_MOVING_TARGET_DETECTED) at 026/16:57:57 also ESB 1806
(T2G_OPEN_LOOP_TIMEOUT) was received at 026/16:58:48. OBAD1 had (RSS)
value of 125463.25 arcseconds. OBAD success flag (mnemonic GCHACL09)
returned to the "no success" state (a value of 1). Unable to execute
OPS REQUEST 17543-2 (OBAD Tables 369 & 370 Dump) prior to next OBAD
due to lack of sufficient forward link. Subsequent GSAcq was
successful.

10651 - HST entered Inertial Hold Safemode

Safetest 'Neon Leakage Test' failed. Acquired 4k data at 027/1308z

10654 - GSACQ(1,2,2) failed to RGA Hold due to SRLEX

The GSACQ(1,2,2) failed to RGA Hold at 027/12:25:38 due to a Search
Radius Limit Exceeded Error on FGS-1. Analysis of the digitized Sky
Survey images does not indicate any obvious problem with the guide
stars. The Map immediately following the acquisition reported an ~77
arcsecond error. This acquisition failure does not appear to have
anything to do with the subsequent safemode entry at 12:34.

10655 - FHST OBAD (no maneuver) Failed

OBAD scheduled at 028/07:36:13 using trackers 1 and 3 failed. During
LOS ESB message 1901 " OBAD Too Few Stars" was received.

OBAD scheduled at 028/08:58:03 also failed. ESB message 1901 "OBAD Too
Few Stars" as received at 09:00:50.

OBAD scheduled at 028/10:34:00 failed. ESB 1901 was received at
10:36:50.

COMPLETED OPS REQUEST:
17992-0 - Turn NCS CPL Startup Heater
17993-0 - Turn on PCE
17994-0 - Dump Table 320
17996-0 - Power on GEA
17995-0 - Dump HST486 Table (SPA AREA)
17998-1 - Safemode Recovery from Inertial Hold
17999-0 - Safe NICMOS
18000-1 - Uplink N02Z5630C,Set ATP Pointer, & Clear ENGREPs
18001-0 - Open ACS PDU 2 Relay
17997-1 - Re-enable Neon Leakage Test/Power on FHSTs

COMPLETED OPS NOTES:
16624-0 - Reset NCS Min/Max Buffer (Generic)
17543-2 - Dump OBAD tables after failed OBAD (Generic)
17597-7 - FHST Stuck-on-Bottom Macro Execution (Generic)
17659-0 - ESTR Reconditioning (Generic)
17929-0 - Set TMDIAG Slots to Monitor Aero Torques (Generic)
17946-1 - MA/GN Mode Recorder Dump Test (Generic)
17966-0 - Monitor FHST Sanity Check via TMDIAG Slots 0-2 (Generic)


SCHEDULED SUCCESSFUL
FGS GSacq 07 05
FGS REacq 09 09
OBAD with Maneuver 34 33

SIGNIFICANT EVENTS:

Flash Report - Inertial Hold DOY 07/027

HST entered Inertial Hold Safemode on 2007/027/12:34:38 GMT (Sat,
01/27/97) following a Total Pressure Sensor (TPS) limit violation.
Autonomous safing actions included powering off the FHSTs and the FGS
High Voltage and terminating High Gain Antennae (HGA) tracking. Data
review following the safemode entry revealed: "Structure Current
Safing Test limit was exceeded ~10sec prior to safemode entry, but HST
structure current returned within limits before the test could fail."
ACS safed due to loss of power "NICMOS Cryo-Cooler safed due to a
Total Pressure Sensor (TPS) limit violation. Note: NO Indication of
NEON Leak." All other HST science instruments and spacecraft
subsystems were functioning nominally. At 10:00 am and 1:00 pm EST in
GSFC B3/S107A, Status meetings were held with the Mission Operations
Team, Science Institute and HST Project. HST Project gave approval to
proceed with HST recovery from Inertial Hold safe mode.

Flash Report:
01/28/07, 9am Inertial Hold Status Mtg At 9:00 am, Sun, 01/28/07. HST
Project granted approval to proceed with the following:
1) Re-enable the Neon Leakage Test and power on the FHSTs on 1/28/07
2) Open ACS PDU 2 Relay on 01/28/07
3) Prepare for NCS power on as early as 01/29/07

Flash Report: ACS PDU 2 Relay Open

The ACS PDU 2 relay was opened via Ops Request
18001 at 17:26:36 GMT. No anomalous structure current signature was
observed when the PDU 2 relay was opened.

Flash Report:

Ops Request 17997-1 for re-enabling the Neon Leak Safing test and
powering the FHSTs back on was completed at 2007/028 17:45. The Safing
system is now in its nominal configuration, with all Two-Gyro Science
mode Safing tests and macros enabled. Fixed-Head Star Tracker
performance has been nominal since power-on. Control mode transitions
into T2G Rate Damping and Attitude Hold were performed as expected.
The FHST Maps at 028/19:15 and 028/20:10 both measured less than 1
degree of RSS attitude error.


 




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