Status Report

NASA Hubble Space Telescope Daily Report #3865

By SpaceRef Editor
May 24, 2005
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HUBBLE SPACE TELESCOPE – Continuing to collect World Class Science

DAILY REPORT        # 3865




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.

NIC3 10702

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/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


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 10378

ACS Polarimetry Calibration

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


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

NIC3/ACS/WFC 10327

ACS Imaging of a High-Redshift Cluster of Galaxies

This programme uses ACS observations of the high-redshift radio galaxy
MRC1138- 262 {z=2.16} to investigate massive galaxy and cluster
formation in the early Universe. This field is unique in that it is
known to contain overdensities in both line-emitting {both Lyman-alpha
and H-alpha} and continuum {4000A break} objects. Utilizing the
excellent angular-resolution and field-coverage of HST/ACS we can
obtain the colors and morphologies for a substantial fraction of these
protocluster galaxies. These morphologies and colors will be compared
to studies of field galaxies at similar redshifts {e.g., from GOODS}.
In addition, very deep images of the radio galaxy itself, the presumed
central dominant galaxy of this cluster, will allow us to study in
detail the process of formation for the most massive known galaxies.
The properties of continuum and Ly-alpha clumps within the radio
galaxy will be compared in relation to the radio structures.

WFPC2 10276

Resolving Distance Ambiguity toward Westerlund 2

Resolving Distance Ambiguity toward Westerlund 2 – No description
listed in proposal database.

NIC2 10169

Star Formation in Luminous Infrared Galaxies: giant HII Regions and
Super Star

Luminous Infrared Galaxies {LIRGs, LIR = 10^11-10^12Lsol} and
Ultraluminous Infrared Galaxies {LIR>10^12Lsol} account for
approximately 75% of all the galaxies detected in the mid-infrared in
the redshift range z=0-1.5. In the local universe it is found that
LIRGs are predominantly powered by intense star formation {SF}.
However, the physical conditions and processes governing such dramatic
activity over scales of tens to a few hundred parsecs are poorly
known. In the last decade HST has been playing a significant role,
mainly with the discovery of super star clusters {SSCs}, and more
recently, giant HII regions. Based on observations of a few LIRGs, we
found that these giant HII regions and associated SSCs appear to be
more common in LIRGs than in normal galaxies, and may dominate the
star formation activity in LIRGs. A larger sample is required to
address fundamental questions. We propose an HST/NICMOS targeted
campaign of a volume limited sample {v<5200km/s} of 24 LIRGs. This proposal will probe the role of giant HII regions in the overall energetics of the current star formation, their relation to SSCs, and the dependence of star formation properties on other parameters of LIRGs. Such detailed knowledge of the SF properties of LIRGs in the local universe is essential for understanding galaxies at high redshift.

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 10104

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

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.


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’s ultimate
legacy for understanding the evolution of both the visible and dark


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


9825 – GSACQ(2,1,1) results in finelock backup (2,0,2) @140/1338z The
GSACQ(2,1,1) scheduled at 140/13:38:13 – 13:45:38 resulted to finelock
backup (2,0,2) using FGS2, due to scan step limit exceeded indication
flag on FGS2. Prior FM Updates at 140/13:09:23, 140/13:12:08,showed
very low attitude error. The following Map schedule for 140/14:05:09
showed attitude errors of: -8.461, -7.473 and -0.240 ARCSEC.

9826 – GSACQ(2,1,1) results in finelock backup (1,0,1) @140/1516z The
GSACQ(2,1,1) scheduled at 140/15:15:52 – 15:23:17 resulted to finelock
backup (1,0,1) using FGS1, due to scan step limit exceeded indication
flag on FGS2. Prior RD Update at 140/14:48:05 showed very low attitude
error. The following Map schedule for 140/15:41:05 showed attitude
errors of: -7.377, -7.680 and 1.684 ARCSEC.


17433-0 – Off-line +D SPA Trim Relay @140/1618z


1339-0 – Adjust the CCC V/T Disable Yellow Limits @140/1347z

1340-0 – Adjust the PDU 1 current yellow limits @140/1350z

                              SCHEDULED     SUCCESSFUL    FAILURE TIMES 
 FGS Gsacq                   23                       23 
 FGS Reacq                   23                       23 
 FHST Update                34                        34 


SpaceRef staff editor.