Hubble Space Telescope Daily Report #3170 – 5 Aug 2002

HUBBLE SPACE TELESCOPE

DAILY REPORT       # 3170
PERIOD COVERED: DOY 213
OBSERVATIONS SCHEDULED (see HSTARS below for possible observation problems)
STIS/CCD 8902
Dark Monitor-Part 2.
The Space Telescope Imaging Spectrograph (CCD) was used to monitor the

darks.
STIS/CCD 8904
Bias Monitor-Part 2.
The Space Telescope Imaging Spectrograph (CCD) was used to monitor the bias

in

the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1 at gain = 4 in

order

to build up high-S/N superbiases and track the evolution of hot columns.
WFPC2 8938
WFPC2 CYCLE 9 SUPPLEMENTAL DARKS pt3/3.
This dark calibration program obtains 3 dark frames every day to provide

data

for monitoring and characterizing the evolution of hot pixels.
WF/PC-2 9058
Trigonometric Parallax of the Globular Cluster 47 Tucanae.
The WF/PC-2 was used measure the trigonometric parallax of 47 Tuc, which is

about 1/4 milliarcsec, to an accuracy of 10%. By repeating a field that was

observed in 1995, we will measure the secular motion of the cluster stars

with

respect to the SMC background with sufficient accuracy that the parallax can

be

measured directly from the displacements within Cycle 10. Constraints of

orientation, and the shape of the WFPC2 footprint, require that we take

images

at 3-month intervals, rotating 90 degrees each time.
WF/PC-2 9118
Tracing the Cosmic Expansion to z>1 with Type Ia Supernovae.
The WF/PC-2 was used to observe type Ia supernovae in order to provide

evidence

for an accelerating universe. The case for cosmic acceleration rests almost

entirely on the observation that the observed SN Ia at z~0.5 are 0.25

magnitudes

fainter than expected for a non-accelerating Universe. It is proposed to

follow

five SN Ia in the range 0.95<z<1.2 using the 850LP filter. When combined

with a

ground-based J-band follow-up campaign, the proposers can expect to measure

the

mean luminosity distance of the sample at z~ 1.05 to better than 5. At these

redshifts, the effect of Omega_Lambda has all but vanished and the Universe

was

decelerating due to its known matter content. Because any simple systematic

error will deviate substantially from the non-monotonic effect of a

Omega_Lambda

 > 0 cosmology, this experiment is a powerful and straightforward way to

assess

the reliability of the SN Ia measurements. In addition, if SN Ia are

reliable

standard candles, the proposed observations will significantly increase the

precision with which Omega_Lambda and Omega_M are measured.
STIS/CCD 9317
Pure Parallel Imaging Program: Cycle 10.
The Space Telescope Imaging Spectrograph (CCD) was used to perform the

default

archival pure parallel program for STIS during cycle 10.
FGS/1 9407
Astrometry of a Star Hosting an Extrasolar Planet: The Mass of Upsilon

Andromedae.
Fine Guidance Sensor #1 was used to determine the astrometric elements

{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. The proposed observations

will

yield a planetary mass, rather than, as previous investigations have done,

only

suggest a planetary mass companion.
ACS 9425
The Great Observatories Origins Deep Survey: Imaging with ACS
We propose a Treasury program of ACS imaging as part of the Great

Observatories

Origins Deep Survey {GOODS}, covering 320{square}', or 32* the area of the

two

original WFPC2 HDFs, to within 0.5--0.8 mag of their depth in four ACS

bands,

BViz. The two GOODS fields, the Hubble Deep Field North and Chandra Deep

Field

South, are the premier deep survey areas from X-- ray to radio wavelengths.

ACS

data will provide unique angular resolution, sensitivity, and wavelength

coverage to close the gap between the deepest Chandra and SIRTF

observations.

Supported by extensive imaging and spectroscopy from the VLT, Keck, Subaru,

NOAO, Gemini, VLA, JCMT, and other facilities, the combined GOODS data set

will

make it possible to map the evolution of the Hubble sequence with redshift,

reconstruct the history of galaxy mass assembly, star formation and nuclear

activity from the epoch of reionization to the present, trace the growth of

density perturbations via cosmic shear, and, with properly phased z--band

observations, detect ~ 12 Type Ia supernovae at 1.2<z<1.8 to test the cosmic

acceleration and the presence of dark energy. All HST, SIRTF, Chandra, and

supporting GOODS data are non-- proprietary, with science--quality images

and

catalogs released on a timescale of months. This will constitute the

deepest,

largest, and most uniform panchromatic data set ever assembled to study the

distant universe.
ACS 9472
A Snapshot Survey for Gravitational Lenses among z >= 4.0 Quasars
Over the last few years, the Sloan Digital Sky Survey has revolutionized the

study of high-redshift quasars by discovering over 200 objects with redshift

greater than 4.0, more than doubling the number known in this redshift

interval.

The sample includes eight of the ten highest redshift quasars known. We

propose

a snapshot imaging survey of a well-defined sample of 250 z > 4.0 quasars in

order to find objects which are gravitationally lensed. Lensing models

including

magnification bias predict that at least 4% of quasars in a flux-limited

sample

at z > 4 will be multiply lensed. Therefore this survey should find of order

10

lensed quasars at high redshift; only one gravitationally lensed quasar is

currently known at z > 4. This survey will provide by far the best sample to

date of high-redshift gravitational lenses. The observed fraction of lenses

can

put strong constraints on cosmological models, in particular on the

cosmological

constant Lambda. In addition, magnification bias can significantly bias

estimates of the luminosity function of quasars and the evolution thereof;

this

work will constrain how important an effect this is, and thereby give us a

better understanding of the evolution of quasars and black holes at early

epochs, as well as constrain models for black hole formation.
ACS 9480
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/WFPC2 9481
Pure Parallel Near-UV Observations with WFPC2 within High-Latitude ACS

Survey

Fields
In anticipation of the allocation of ACS high-latitude imaging survey{s}, we

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<z<1. We will determine the

morphological

k-correction, and the location of star formation within galaxies, using a

sample

that is likely to be nearly complete with multi-wavelength photometry and

spectroscopic redshifts. The results can be used to interpret observations

of

higher redshift galaxies by ACS.
ACS/WFPC2 9488
Cosmic Shear - with ACS Pure Parallel Observations
The ACS, with greater sensitivity and sky coverage, will extend our ability

to

measure the weak gravitational lensing of galaxy images caused by the large

scale distribution of dark matter. We propose to use the ACS in pure

parallel

{non- proprietary} mode, following the guidelines of the ACS Default Pure

Parallel Program. Using the HST Medium Deep Survey WFPC2 database we have

measured cosmic shear at arc-min angular scales. The MDS image parameters,

in

particular the galaxy orientations and axis ratios, are such that any

residual

corrections due to errors in the PSF or jitter are much smaller than the

measured signal. This situation is in stark contrast with ground-based

observations. We have also developed a statistical analysis procedure to

derive

unbiased estimates of cosmic shear from a large number of fields, each of

which

has a very small number of galaxies. We have therefore set the stage for

measurements with the ACS at fainter apparent magnitudes and smaller, 10

arc-second scales corresponding to larger cosmological distances. We will

adapt

existing MDS WFPC2 maximum likelihood galaxy image analysis algorithms to

work

with the ACS. The analysis would also yield an online database similar to

that

in archive.stsci.edu/mds/
ACS/CAL 9558
ACS weekly Test
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 9657
ACS Internal Flat Field Stability
The flat field stability and characterization obtained during the ground

calibration and SMOV phases will be tested and verified through a sub-sample

of

the filter set. Only internal exposures with the calibration lamps will be

required.
WFPC2 9676
POMS Test Proposal: 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.
FLIGHT OPERATIONS SUMMARY:
HSTARS: (For details see http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf)
Operations Notes:
SIGNIFICANT EVENTS FLIGHT OPERATIONS SUMMARY:
HSTARS: (For details see http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf)
HSTARs:

8751  Temporary Loss of Network Connection @ 214/05:10:00z.HSTfsb3 was

           inaccessible at the SIMOR from approximately 214/05:10:10Z -

05:17Z.

           Confirmed on more than one PC.  Problem spontaneously resolved

itself.

           Under investigation.
8752  Rejected
COMPLETED OPS REQs:

16816-0  Set CCC K51 to L5 and K52 to L2 @ 213/1503z
OPS NOTES EXECUTED:

1025-4  CCC K51 Level 5, K52 Level 2 Limits Operations Notes:
                           SCHEDULED     SUCCESSFUL    FAILURE TIMES

FGS GSacq                8                        8

FGS REacq                7                        7

FHST Update              15                      1D

LOSS of LOCK
Operations Notes:

1. SMS for SA217M00_F1 approved @ 213/1630z.
SIGNIFICANT EVENTS FLIGHT OPERATIONS SUMMARY:
Successfully completed real-time commanding to change CCC K51 to Level 5

and K52 to Level 2 @ 213/15:05Z (OR 16816 and COP 4.23, Case 6).  Battery

5 continues to operate at an elevated temperature and exhibit higher

load-share

than the other batteries, as a result, Batteries 1 - 4 are experiencing a

gradual capacity decline.  HSTAR 8678 and 8723 are related to these

conditions.  OR 16807 adjusted K52 to Level 5 on Day 211.
Successfully completed CCS-O-004X - 486 FSW Loads and Dumps testing

213/11:00Z - 16:40Z.  Verified routine operational procedures and CCS

capabilities to support HST 486 SPC load uplink, dump and compare.

Verified FSW transfer of HST 486 loads from NTPRIMARY and uplinked,

dumped and compared table, software and hardware loads.  Also, verified

CCS capabilities to support HST 486 ESB dump, 32kbps memory dump and

partial table parameter uplink.
HST "B" String Command test scheduled 214/12:00Z - 20:00Z with GDOC,

SOC, HITT, and CCS using CCS "B" String with Release 4.0.1 and PRD

D06100R2.  Objective of test is to verify CCS Release 4.0.1 properly

handles command scenarios between the "B" String and the SOC.
HST On-Orbit Check-out of Real-Time DSMC Interface from IP Packet

Filters scheduled 214/15:00Z - 19:00Z with GDOC, HITT, I&C, and CCS

using CCS "G" String with CCS Release 4.0.1 and PRD D06100R2.  The

purpose of this testing is to verify CCS Release 4.0.1 (IP) is

capable of interfacing through the IP Packet Filters to the DSMC

for ODMs and GCMRs