Status Report

NASA Hubble Space Telescope Daily Report # 3567

By SpaceRef Editor
March 11, 2004
Filed under , ,

HUBBLE SPACE TELESCOPE – Continuing to collect World Class Science





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.


Natural Coronagraphic Imaging of KH 15D

We propose to obtain V, H-alpha and [SII] images of the unique,
eclipsing pre-main sequence star KH 15D near minimum light with the
ACS/HRC. This solar-like star in NGC 2264, near the Cone Nebula, is
fortuitously positioned with respect to our line of sight. Every 48.36
days its photosphere and accretion zone are progressively occulted and
then revealed by an eclipsing body, which is evidently non-luminous,
extended circumstellar matter in the star’s vicinity. Dramatic
spectral evolution is seen during these "natural cononagraphic" events
that is revealing the structure of the accretion zone on spatial
scales {~0.01 AU or less} that may not be achieved in other sources
for decades to come, if ever. It is important to know whether this
object is unique only in its orientation and not in its basic
structure. Our observations will test the hypothesis that KH 15D at
minimum light looks like nearly edge-on disk/jet systems around stars
of similar mass and age in closer star forming regions such as Tau/Aur
or MBM 12. We argue that the disk and jet will be resolved and will
provide new constraints on this system. If not resolved, the data will
at least constrain the scattering and jet emission zones to be
remarkably close to the star {~10 AU}. In either case, we will have
important new information on the nature of this unique object.

ACS/WFC 9766

The Globular Cluster Systems of Spiral Galaxies along the Hubble

While the globular cluster {GC} systems of ellipticals and ongoing
mergers have been relatively well-studied with HST, very little is
known about the GC systems of spirals besides the Milky Way and M31.
To constrain GC/galaxy formation models, especially where spirals are
the merger progenitors of ellipticals, it is crucial to understand
their GC properties. We propose to obtain ACS images of three edge-on
spirals, spanning the Hubble sequence, with Keck spectroscopic
follow-up. This will effectively double the number of well-studied
spiral systems. We will detect 100-200 GCs per galaxy, sufficient to
reveal GC subpopulations, their relative numbers, radial trends, and
dependences on Hubble type {e.g., a bulge vs. disk origin for red
GCs}. For half of our GCs we will be able to measure individual sizes.
By providing a much-needed comparative benchmark, these data will
allow researchers to better exploit the large existing HST database of
GCs in E/S0 galaxies.


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

NIC1/NIC2/NIC3 9993

Cycle 12 NICMOS dark current, shading profile, and read noise
monitoring program

The purpose of this proposal is to monitor the dark current, read
noise, and shading profile for all three NICMOS detectors throughout
the duration of Cycle 12. This proposal is an essentially unchanged
continuation of PID 9636 which cover the duration of Cycle 11.

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.


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.

STIS/CCD 10017

CCD Dark Monitor-Part 1

Monitor the darks for the STIS CCD.

STIS/CCD 10019

CCD Bias Monitor – Part 1

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 10085

STIS Pure Parallel Imaging Program: Cycle 12

This is the default archival pure parallel program for STIS during
cycle 12.

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 10084

WFII parallel archive proposal

This is the generic target version of the WFPC2 Archival Pure Parallel
program. The program will be used to take parallel images of random
areas of the sky, following the recommendations of the 2002 Parallels
Working Group.


Significant Spacecraft Anomalies: (The following are preliminary
reports of potential non-nominal performance that will be
investigated.) None



                          SCHEDULED     SUCCESSFUL    FAILURE TIMES
FGS GSacq              11                       11
FGS REacq              09                        09
FHST Update            16                       16


CCS Release Issue Re-test scheduled 071/12:00Z – 21:00Z with
GDOC, SOC, and HITT using CCS "D" String with CCS Release and
PRD O06300ST. The purpose of this testing is to re-test CCS Release issues.

SpaceRef staff editor.