NASA Hubble Space Telescope Daily Report # 3467
HUBBLE SPACE TELESCOPE
DAILY REPORT # 3467
PERIOD COVERED: DOY 286
OBSERVATIONS SCHEDULED
ACS 9984
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.
ACS/CCD/WFC 9978
The Ultra Deep Field with ACS
The ACS Ultra Deep Field {UDF} is a survey carried out by using
Director’s Discretionary time. The main science driver are galaxy
evolution and cosmology. The primary instrument is the Advanced Camera
for Surveys but WFPC2 and NICMOS will also be used in parallel. The
data will be made public. The UDF consists of a single ultra-deep
field {410 orbits in total} within the CDF-S GOODS area. The survey
will use four filters: F435W {55 orbits}, F606W {55 orbits}, F775W
{150 orbits}, and F850LP {150 orbits}. The F435W {B} and F606W {V}
exposures will be one magnitude deeper than the equivalent HDF
filters. The F775W {I} exposure will be 1.5 magnitude deeper than the
equivalent HDF exposure. The depth in F775W and F850LP is optimized
for searching very red objects – like z=6 galaxies – at the detection
limit of the F850LP image. The pointing will be RA{J2000}=3 32 40.0
and Decl.{J2000}=-27 48 00. These coordinates may change slightly due
to guide star availability and implementation issues. We will attempt
to include in the field both a spectroscopically confirmed z=5.8
galaxy and a spectroscopically confirmed type Ia SN at z=1.3. The
pointing avoids the gaps with the lowest effective exposure on the
Chandra ACIS image of CDFS. This basic structure of the survey
represents a consensus recommendation of a Scientific Advisory
Committee to the STScI Director Steven Beckwith. A local Working Group
is looking in detail at the implementation of the survey.
ACS/HRC/WFC 10042
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.
ACS/HRC/WFC 10044
ACS internal CTE monitor
The charge transfer efficiency {CTE} of the ACS CCD detectors will
decline as damage due to on-orbit radiation exposure accumulates. This
degradation will be closely monitored at regular intervals, because it
is likely to determine the useful lifetime of the CCDs. 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 {HRC}.
NIC/NIC3 9865
The NICMOS Parallel Observing Program
We propose to continue managing the NICMOS pure parallel program.
NIC1/NIC2/NIC3 8792
NICMOS Post-SAA calibration – CR Persistence Part 3
A new procedure proposed to alleviate the CR-persistence problem of
NIC2 9726
A NICMOS search for obscured supernovae in starburst galaxies
Recent near-IR monitoring campaigns were successful in detecting
NIC3 9979
The Ultra Deep Field – NICMOS Parallels
This is a plan to manage the NICMOS pure parallels of the ACS Ultra
STIS 9383
Probing the Grains Responsible for Extinction Using Small Magellanic
Small Magellanic Cloud sightlines have the greatest potential to
STIS 9786
The Next Generation Spectral Library
We propose to continue the Cycle 10 snapshot program to produce a Next
STIS/CCD 10000
STIS Pure Parallel Imaging Program: Cycle 12
This is the default archival pure parallel program for STIS during
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,
STIS/CCD 9981
The Ultra Deep Field – STIS parallels
We propose to obtain slitless spectroscopy of objects in the GEMS and
WFPC2 10068
WFPC2 CYCLE 12 Standard Darks
This dark calibration program obtains dark frames every week in order
WFPC2 10069
WFPC2 CYCLE 12 Supplemental Darks, Part 1/3
This dark calibration program obtains 3 dark frames every day to
WFPC2 9709
POMS Test Proposal: WFII parallel archive proposal
This is the generic target version of the WFPC2 Archival Pure Parallel
WFPC2 9980
The Ultra Deep Field – WFPC2 Parallels
The ACS Ultra Deep Field {UDF} is a survey carried out by using
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are preliminary
HSTAR 9174: GS Acquisition (2,1,1) @ 286/19:50:09Z resulted in FL
COMPLETED OPS REQs: None
OPS NOTES EXECUTED: None
SIGNIFICANT EVENTS:
Successfully completed Command Timing Comparison testing “D” String
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
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.
obscured supernovae {SNe} in starburst galaxies. The inferred SN rate
is much higher than that obtained in previous optical campaigns, but
it is still significantly lower than expected by the high level star
formation of these systems. One possible explanation for the shortage
of SNe is that most of them occur in the nuclear region, where the
limited angular resolution of groundbased observations prevents their
detection. We propose NICMOS SNAP observations of a sample of
starburst galaxies already observed once by NICMOS, with the goal of
exploiting its sensitivity and angular resolution to detect nuclear
obscured SNe which might have been missed by groundbased surveys.
These observation will allow to assess the real SN rate in starbust
galaxies and deliver a sample of SN occurring in the extreme
environment of galactic nuclei. We expect to detect more than 55 SNe
{if the whole sample is observed}. If the number of SNe detected in
the program is much lower than expected it would prompt for a revision
of our understanding of the relation between the star formation rate
and the SN rate.
Deep Survey. We will obtain a mix of F110W and F160W images along
sight-lines within the mosaiced ACS fields of the CDF-S GOODS and GEMS
surveys, with these sight-lines enabling an examination of the space
density and morphologies of the reddest galaxies.
Cloud Sightlines
relate specific interstellar extinction features to distinct grain
properties. The reasons for this are 1} prominent extinction features
such as the 2175 Angstrom bump and the far-ultraviolet rise vary among
SMC targets and 2} grain types may be very different from those in the
Galaxy. Specifically, Welty et al. {2001} recently identified an SMC
sightline that contains dust, but no silicate grains. Silicates are a
dominant source of extinction in all dust models; the SMC may be the
only location where the importance of silicates can be verified or
disproved. We propose to explore the relationship between grain types
and extinction toward 2 SMC stars with very different extinction
curves; AzV 18 lacks a 2175 Angstrom bump and has a strong far-UV rise
while the extinction curve towards the SMC star AzV 456 has a
prominent 2175 Angstrom bump and a much weaker far-UV rise. We will
compare the interstellar abundances of atoms that are prevalent in
silicates {Si, Mg, Fe} toward these 2 stars and use the results to
constrain dust extinction models. These SMC observations, which can
only be obtained with STIS, are the only direct way to probe the
connection between grain types/environments and extinction. The
results from this study will be useful for modeling and understanding
all regions that contain dust {AGN, circumstellar disks, star
formation regions, etc.}.
Generation Spectral Library of 600 stars for use in modeling the
integrated light of galaxies and clusters. This program is using the
low dispersion UV and optical gratings of STIS. The library will be
roughly equally divided among four metallicities, very low {[Fe/H] lt
-1.5}, low {[Fe/H] -1.5 to -0.5}, near-solar {[Fe/H] -0.3 to 0.1}, and
super-solar {[Fe/H] gt 0.2}, well-sampling the entire HR-diagram in
each bin. Such a library will surpass all extant compilations and have
lasting archival value, well into the Next Generation Space Telescope
era. Because of the universal utility and community-broad nature of
this venture, we waive the entire proprietary period.
cycle 12.
and 1×1 at gain = 4, to build up high-S/N superbiases and track the
evolution of hot columns.
GOODS area around the UDF.
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.
provide data for monitoring and characterizing the evolution of hot
pixels.
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.
Director’s Discretionary time. The main science drivers are galaxy
evolution and cosmology. The primary instrument is the Advanced Camera
for Surveys but WFPC2, NICMOS, and STIS will also be used in pure
parallel mode. The data will be made public. The UDF consists of a
single ultra-deep field {410 orbits in total} within the CDF-S GOODS
area. We request a modification of the default pure parallel programs.
Rather than duplicate the redder bands which will be done much better
with ACS, we propose to observe in the near-ultraviolet F300W filter.
These data will enable study of the rest-frame ultraviolet morphology
of galaxies at 0
reports of potential non-nominal performance that will be
investigated.)
backup using FGS 2 due to SSLE flags on FGS 2. Prior FHST Map @
286/19:57:47Z showed errors of 4.247, -8.207, and 4.914 arcsec.
Analysis indicates GS in FGS 2 to be a marginal double star (seen as
obvious double in 1st FL walk down, but succeeded in 2nd). Guide Star
Problem Report T9174 was submitted to STScI. Under investigation.
SCHEDULED SUCCESSFUL FAILURE TIMES
FGS GSacq 8 8
FGS REacq 4 4
FHST Update 16 16
LOSS of LOCK
(Sun). Confirmed real-time commanding on “D” String (Sun) is slightly
faster than the “C” String (SGI).
