NASA Hubble Space Telescope Daily Report # 3461
HUBBLE SPACE TELESCOPE
DAILY REPORT # 3461
PERIOD COVERED: DOYs 276-278
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.
STIS/CCD 9981
The Ultra Deep Field – STIS parallels
We propose to obtain slitless spectroscopy of objects in the GEMS and GOODS
area
around the UDF.
WFPC2 9980
The Ultra Deep Field – WFPC2 Parallels
The ACS Ultra Deep Field {UDF} is a survey carried out by using Director’s
NIC3 9979
The Ultra Deep Field – NICMOS Parallels
This is a plan to manage the NICMOS pure parallels of the ACS Ultra Deep
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
FGS 9971
FGS Astrometry of a Star Hosting an Extrasolar Planet: The Mass of Upsilon
We propose observations with HST/FGS to determine the astrometric elements
FGS 9879
An Astrometric Calibration of the Cepheid Period-Luminosity Relation
We propose to measure the parallaxes of 10 Galactic Cepheid variables. There is
NIC/NIC3 9865
The NICMOS Parallel Observing Program
We propose to continue managing the NICMOS pure parallel program. Based on our
ACS/HRC/WFC 9793
The Grism-ACS Program for Extragalactic Science {GRAPES}
We propose an ACS grism spectroscopic survey with a wide component and an
STIS 9786
The Next Generation Spectral Library
We propose to continue the Cycle 10 snapshot program to produce a Next
WFPC2 9712
Pure Parallel Near-UV Observations with WFPC2 within High-Latitude ACS Survey
In anticipation of the allocation of ACS high-latitude imaging survey{s}, we
WFPC2 9709
POMS Test Proposal: WFII parallel archive proposal
This is the generic target version of the WFPC2 Archival Pure Parallel program.
STIS 9629
MAMA Fold Distribution
The performance of MAMA microchannel plates can be monitored using a MAMA fold
WFPC2 9595
WFPC2 CYCLE 11 SUPPLEMENTAL DARKS pt3/3
This dark calibration program obtains 3 dark frames every day to provide data
NIC1/NIC2/NIC3 8792
NICMOS Post-SAA calibration – CR Persistence Part 3
A new procedure proposed to alleviate the CR-persistence problem of NICMOS.
WFPC2 10069
WFPC2 CYCLE 12 Supplemental Darks, Part 1/3
This dark calibration program obtains 3 dark frames every day to provide data
ACS/HRC/WFC 10042
CCD Daily Monitor
This program consists of basic tests to monitor, the read noise, the
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
STIS/CCD 10017
CCD Dark Monitor-Part 1
Monitor the darks for the STIS CCD.
STIS/CCD 10000
STIS Pure Parallel Imaging Program: Cycle 12
This is the default archival pure parallel program for STIS during cycle 12.
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are preliminary reports of
HSTAR 9165: GS Acquisition (2,1,1) @ 279/02:18:07Z resulted in FL backup
COMPLETED OPS REQs: None
OPS NOTES EXECUTED: None
SIGNIFICANT EVENTS: None
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
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.
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.
Andromedae d
{perturbation orbit semimajor axis and inclination} produced by the outermost
extra-solar planet orbiting the F8V star Upsilon Andromedae. These observations
will permit us to determine the actual mass of the planet by providing the
presently unknown sin i factor intrinsic to the radial velocity method which
discovered this object. An inclination, i = 30degrees, within the range of one
very low precision determination using reanalyzed HIPPARCOS intermediate data
products, would produce the observed radial velocity amplitude, K = 66 ms
with a
companion mass of ~8 M_Jupiter. Such a mass would induce in Upsilon
Andromedae a
perturbation semi-major axis, Alpha = 0arcs0012, easily within the reach of
HST/FGS fringe tracking astrometry. The proposed observations will yield a
planetary mass, rather than, as previous investigations have done, only suggest
a planetary mass companion.
no other instrument on or off the earth that can consistently deliver HST FGS
level of precision for critical parallaxes. When these parallaxes {with 1-sigma
precisions of 10% or better} are added to our recent HST FGS parallax
determination of delta Cep {Benedict et al 2002}, we anticipate determining the
Period-Luminosity relation zero point with a 0.03 mag precision. In addition to
permitting the test of assumptions that enter into other Cepheid distance
determination techniques, this calibration will reintroduce Galactic
Cepheids as
a fundamental step in the extragalactic distance scale ladder. A
Period-Luminosity relation derived from solar metallicity Cepheids can be
applied directly to extragalactic solar metallicity Cepheids, removing the need
to bridge with the Large Magellanic Cloud and its associated metallicity
complications.
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
ultradeep single ACS field. The wide component covers the well-imaged GOODS
Chandra Deep Field south and the deepest field will be the Ultra Deep field to
be observed in cycles 11 and 12. The Grism ACS Program for Extra-galactic
Science {GRAPES} will: {1} Probe the reionization epoch by robustly determining
the luminosity function of Lyman-alpha emitters, Lyman break galaxies and low
luminosity AGNs at z~6, and thus the sources of ionizing photons at the end of
the “dark ages”. A similar census of ionizing photon sources at z=4-6 needed to
maintain the ionized state of the IGM will also be achieved. {2} Study galaxy
formation and evolution by finding galaxies in a contiguous redshift range
between z=4-7 and evolution of black holes through a census of low-luminosity
AGNs. {3} Study star-formation and galaxy assembly at its peak at z=1-2 by
identifying star-forming galaxies by their emission lines, old galaxies by the
4000 AA break and any combination of new and old populations showing both lines
and breaks. {4} Allow the deepest unbiased spectroscopy yet, for identification
of objects to I=27. {5} Enhance the value of multiwavelength data in the
UDF and
GOODS field to the astronomical community.
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.
Fields
request a modification of the default pure parallel program for those WFPC2
parallels that fall within the ACS survey field. Rather than duplicate the red
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
The program will be used to take parallel images of random areas of the sky,
following the recommendations of the 2002 Parallels Working Group.
analysis procedure. The fold analysis provides a measurement of the
distribution
of charge cloud sizes incident upon the anode giving some measure of changes in
the pulse-height distribution of the MCP and, therefore, MCP gain. This
proposal
executes the same steps as the STIS MAMA Fold Analysis {8860} during Cycle 9.
for monitoring and characterizing the evolution of hot pixels.
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.
for monitoring and characterizing the evolution of hot pixels.
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.
at gain = 4, to build up high-S/N superbiases and track the evolution of hot
columns.
potential non-nominal performance that will be investigated.)
on FGS 2
due to SSLE (QF2SSLEX) on FGS 2. Following FHST Map
showed errors of
25.192, -6.043, and -2.55a arcsec. Under investigation.
SCHEDULED SUCCESSFUL FAILURE TIMES
FGS GSacq 27 27
FGS REacq 20 20
FHST Update 32 32
LOSS of LOCK
