Status Report

NASA Hubble Space Telescope Daily Report # 3595

By SpaceRef Editor
April 22, 2004
Filed under , ,
NASA Hubble Space Telescope Daily Report # 3595

HUBBLE SPACE TELESCOPE – Continuing to collect World Class Science




NIC3 9999

The COSMOS 2-Degree ACS Survey NICMOS Parallels

The COSMOS 2-Degree ACS Survey NICMOS Parallels. This program is a
companion to program 9822.

NIC/NIC3 9865

The NICMOS Parallel Observing Program

We propose to continue managing the NICMOS pure parallel program.
Based on our experience, we are well prepared to make optimal use of
the parallel opportunities. The improved sensitivity and efficiency of
our observations will substantially increase the number of
line-emitting galaxies detected. As our previous work has
demonstrated, the most frequently detected line is Halpha at
0.7<z<1.9, which provides an excellent measure of current star
formation rate. We will also detect star-forming and active galaxies
in other redshift ranges using other emission lines. The grism
observations will produce by far the best available Halpha luminosity
functions over the crucial–but poorly observed–redshift range where
galaxies appear to have assembled most of their stellar mass. This key
process of galaxy evolution needs to be studied with IR data; we found
that observations at shorter wavelengths appear to have missed a large
fraction of the star-formation in galaxies, due to dust reddening. We
will also obtain deep F110W and F160W images, to examine the space
densities and morphologies of faint red galaxies. In addition to
carrying out the public parallels, we will make the fully reduced and
calibrated images and spectra available on-line, with some
ground-based data for the deepest parallel fields included.

NIC2 9845

NICMOS Confirmation of a Young Planetary-Mass Companion

We have recently discovered a strong candidate for a planetary-mass
{~10 Mjup} companion to a young Sun-like star, based on near-IR
imaging and spectroscopy with the Keck and Subaru adaptive optics {AO}
systems. While the ground-based data strongly suggest that the
candidate has a very low effective temperature, and hence a very low
mass, they are not definitive. We propose to obtain NICMOS
coronagraphy to measure the companion’s 1.9um water-band absorption.
This feature is a distinct signature of very cool objects and is
unobservable from the ground. The combined ground-based and
space-based data set will determine whether the companion has a very
low temperature, and hence if it is the lowest mass companion found to
date by direct imaging.


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

ACS/WFC 9811

Establishing the Metallicity Distribution in Normal Giant Ellipticals

NGC 3377 and 3379, the Leo Group ellipticals at d=11 Mpc, are the
nearest E galaxies commonly regarded to be structurally"normal", and
as such, they are keystone objects for understanding the evolution and
early star formation history of large ellipticals. The ACS/WFC camera
now gives us the ability to obtain the metallicity distribution
function {MDF} of their stellar population by direct resolution and
photometry of their halo stars. To do this, we will follow the same
highly successful techniques we have previously used for NGC 5128 with
WFPC2 {V, I} imaging: the {V-I} colors of the brightest red-giant
stars are highly sensitive to metallicity, and their locations in the
color-magnitude diagram can be used for direct construction of the
MDF. This will be a major step forward to understanding the formation
history of these cosmologically dominant galaxies.

ACS/WFC 9788

A Narrow-band Snapshot Survey of Nearby Galaxies

We propose to use ACS/WFC to conduct the first comprehensive HST
narrow-band {H-alpha + [N II]} imaging survey of the central regions
of nearby bulge-dominated disk {S0 to Sbc} galaxies. This survey will
cover, at high angular resolution extending over a large field, an
unprecedented number of galaxies representing many different
environments. It will have important applications for many
astrophysical problems of current interest, and it will be an
invaluable addition to the HST legacy. The observations will be
conducted in snapshot mode, drawing targets from a complete sample of
145 galaxies selected from the Palomar spectroscopic survey of nearby
galaxies. Our group will use the data for two primary applications.
First, we will search for nuclear emission-line disks suitable for
future kinematic measurements with STIS, in order to better constrain
the recently discovered relations between black hole mass and bulge
properties. Preliminary imaging of the type proposed here must be
done, sooner or later, if we are to make progress in this exciting new
field. Second, we will investigate a number of issues related to
extragalactic star formation. Specifically, we will systematically
characterize the properties of H II regions and super star clusters on
all galactic scales, from circumnuclear regions to the large-scale

ACS/HRC 9747

An Imaging Survey of the Statistical Frequency of Binaries Among
Exceptionally-Young Dynamical Families in the Main Asteroid Belt

We propose an ambitious SNAPSHOT program to determine the frequency of
binaries among two very young asteroid families in the Main Belt, with
potentially profound implications. These families {of C- and S-type}
have recently been discovered {Nesvorny et al. 2002, Nature 417, 720},
through dynamical modeling, to have been formed at 5.8 MY and 8.3 MY
ago in catastrophic impact events. This is the first time such
precise and young ages have been assigned to a family. Main-belt
binaries are almost certainly produced by collisions, and we would
expect a young family to have a significantly higher frequency of
binaries than the background, because they may not yet have been
destroyed by impact or longer-term gravitational instabilities. In
fact, one of the prime observables from such an event should be the
propensity for satellites. This is the best way that new numerical
models for binary production by collisions {motivated largely by our
ground-based discoveries of satellites among larger asteroids}, can be
validated and calibrated. We will also measure two control clusters,
one being an "old" family, and the other a collection of background
asteroids that do not have a family association, and further compare
with our determined value for the frequency of large main-belt
binaries {2%}. We request visits to 180 targets, using ACS/HRC.

ACS 9294

Observations of the Host Galaxy of 3C 273

The highly luminous flat-spectrum QSO 3C 273 {z=0.158, V=12.8,
M_V~-26.4} will be imaged with the WFC in the [O III]5007 and H-alpha
emission lines with the narrow-band filters FR601N and FR782N,
respectively. Off-band images in F475W and F850LP will also be
acquired to accurately subtract the underlying galaxy continuum.
Combined with the broad-band HRC coronagraphic images from the ERO
program 8992, these new images will offer the most complete and
detailed view yet of the host galaxy and environment of this QSO.

NIC1/NIC2/NIC3 8792

NICMOS Post-SAA calibration – CR Persistence Part 3

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.

WFPC2 10070

WFPC2 CYCLE 12 Supplemental Darks Part 2/3

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

WFPC2 10068

WFPC2 CYCLE 12 Standard Darks

This dark calibration program obtains dark frames every week in order
to provide data for the ongoing calibration of the CCD dark current
rate, and to monitor and characterize the evolution of hot pixels.
Over an extended period these data will also provide a monitor of
radiation damage to the CCDs.


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/MA1 10034

Cycle 12 MAMA Dark Monitor

This test performs the routine monitoring of the MAMA detector dark
noise. This proposal will provide the primary means of checking on
health of the MAMA detectors systems through frequent monitoring of
the background count rate. The purpose is to look for evidence of
change in dark indicative of detector problem developing.

STIS/CCD 10022

STIS CCD Hot Pixel Annealing Cycle 12

The effectiveness of the CCD hot pixel annealing process is assessed
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. Follows on from proposal 9612.

STIS/CCD 10020

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.

STIS/CCD 10018

CCD Dark Monitor-Part 2

Monitor the darks for the STIS CCD.


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

HSTAR 9386: GS Acquisition (2,3,2) @ 110/12:17:47Z failed to RGA
control due to SRLE on FGS 2. Primary Search Radius = 30.0 arcsec.
Prior FHST Roll Delay Update (U2,3RD) showed attitude errors: V1 =
20.913, V2 = -89.066, V3 = 15.6714 arcsec. Successful executed
ARU/PRT @ 110/13:19:48Z to save subsequent GS Reacquisition @
110/13:54:58Z (OR 17128 with COP 3.06). Under investigation.

HSTAR 9387: OTA SE review of PTAS TC run for M_SA103O SMS, determined
the GS Reacquisition (2,1,2) @ 105/01:04:57Z required two attempts on
FGS 1 due to SSLEX during the first attempt. Under investigation.

HSTAR 9398: Based on PCS SE input and review of PTAS TC run log for
M_SA103O SMS, OTA SE confirms the GS Acquisition (1,2,1) @
106/17:16:23Z achieved FL-DV on both FGSs @ 106/17:20:22Z, but then
went to SSM control @ ~106/17:22:22Z. The LOL Recovery was successful
and no further LOL was seen during the guiding period on these stars.
Under investigation.


  • 17128-0 – ARU/PRT @ 110/1320z
  • 17126-3 – Eclipse Management, GMT 110 @ 110/1843z
  • 17127-1 – Continuation of FSW 2.5B On-Orbit Verification @ 110/1851z
  • 17129-1 – ACS FSW CS4.0 Installation @ 111/2046z
  • 17130-0 -Genslew for proposal 9906 – slot 13 @ 111/2308z
  • 17131-0 -Genslew for proposal 9906 – slot 14 @ 111/2310z
  • 17132-0 -Genslew for proposal 9906 – slot 1 @ 111/2313z
  • 17133-0 – Genslew for proposal 9906 – slot 2 @ 111/2316z
  • 17134-0 – Genslew for proposal 9906 – slot 3 @ 112/0708z


  • 1223-0 – Delivery of ACS FSW CS4.0 Loads @ 110/2100z
  • 1220-0 – Adjust Recharge Ratio Limits for High Sun DOY 2004/110-119 @
  • 110/2208z

                         SCHEDULED     SUCCESSFUL    FAILURE TIMES
FGS GSacq             13                       13              110/1217z 
(HSTAR # 9386)
FGS REacq             19                       19               110/1043z
FHST Update           29                       29


Day 110

Continued FSW 2.5b on-orbit verification (OR 17127-1 with attached
script). FHST 1 was placed in Rate Control under FGS guiding from ~
110/14:21Z – 14:35Z.

FHSTs 1, 2, and 3 were placed in simultaneous Rate Control under FGS
guiding from ~ 110/14:35Z – 14:50Z.

FHST 3 was placed in Rate Control under RGA control from ~ 110/14:50Z
– 15:05Z.

FHST 2 was place in Rate Control under RGA control following the
110/17:00Z FM Update from ~ 110/18:38Z – 18:51Z.

Solar Eclipse 110/13:47Z – 14:05Z and 110/15:36Z – 15:46Z (OR 17126-3
with attached ROP PS-02A and MEGG timeline). Temporarily disable the
Rate of Charge and SA old Protection safemode tests. CCS timer was
modified to prevent software logic from operating as if a CSS failure
occurred due to the eclipse. With Trickle Charge verified, reset the
safemode tests and CSS timer to their nominal state @ 110/18:44Z.
Preliminary results from limited real-time data appear to indicate
Trickle Charge was reached during both eclipse periods.

Successfully executed ARU/PRT @ 110/13:19:48Z to save subsequent GS
Reacquisition @ 110/13:54:58Z (OR 17128 with COP 3.06). See HSTAR

ACS FSW CS4.0 EEPROM installation and verification 111/10:12Z – 20:38Z
(OR 17129-1 with attached script). This FSW change will improve the
ability of the ACS to position its Filter Wheel more reliably. The
FSW will be loaded into EEPROM while the ACS remains in Operate Mode.
ACS will remain under ACS FSW CS3.0CF control until ACS transition to
Anneal Mode @ ~116/09:00Z and then back to Operate Mode @ ~116/22:00Z,
at which time the new FSW CS4.0 will be loaded into EDAC memory and

Day 111

Successfully completed ACS FSW 4.0 uplink (segments 1 – 199) to EEPROM
memory @ 111/20:46Z [OR 17129-1 with attached ACS FSW Version 4.0
Install Procedure (EEPROM)]. No errors or problems were encountered
during the loading process. The new image now resides in the ACS
EEPROM. Post-install memory dump was completed and transferred to the
Payload FSW Team. No discrepancies or differences were found with the
newly loaded ACS FSW CS4.0 image.

When ACS emerges from its monthly anneal cycles ~116/22:00Z, the new
FSW will be activated.

ACS EEPROM dump was executed @097/22:00Z (OR 17120). ACS EEPROM dump
CSIJ04097215708.EFS was collected and transferred to the FSW Team;
analysis completed and contents were verified to match ground image.

SpaceRef staff editor.