Hubble Space Telescope Daily Report #3117 – 15 May 2002

HUBBLE SPACE TELESCOPE

DAILY REPORT # 3117

PERIOD COVERED: 0000Z (UTC) 05/14/02 – 0000Z (UTC) 05/15/02

OBSERVATIONS SCHEDULED AND ACCOMPLISHED:

NICMOS 8790

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.

STIS/CCD 8902

The Space Telescope Imaging Spectrograph (CCD) was used to monitor the darks.

STIS/CCD 8904

The Space Telescope Imaging Spectrograph (CCD) was used to 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 in order
to build up high-S/N superbiases and track the evolution of hot columns.

STIS/CCD 8906

The Space Telescope Imaging Spectrograph (CCD) was used to measure the
effectiveness of the CCD hot pixel annealing process 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.

WFPC2 8938

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 8940

The WF/PC-2 was used to monitor flatfield stability by obtaining sequences of
Earth streak flats to construct high quality flat fields for the WF/PC-2 filter
set. These flat fields will allow mapping of the OTA illumination pattern and
will be used in conjunction with previous internal and external flats to
generate new pipeline superflats.

ACS/WFC/HRC 8947

The Advanced Camera for Surveys (WFC and HRC) was used to perform basic
tests to
monitor, the read noise, the development of hot pixels and test for any source
of noise in ACS CCD detectors. This program will be executed at least once
a day
for the entire lifetime of ACS.

NICMOS 1/2 8985

This proposal obtains sequences of NICMOS camera 1 & 2 medium and wide band
filter flat fields, plus one orbit for selected Camera 3 filters. The
observations will be used to build high S/N NICMOS flat fields to enable the
start of science observations.

NICMOS 8993

The purpose of this program is to obtain images that display the panchromatic
capability of HST with refurbishment of NICMOS. We will obtain images of two
targets using NICMOS, and if possible, ACS as well. Images will be obtained
in J
and H and Paschen alpha. If ACS is unavailable images will be taken in K as
well. Two targets will be imaged. The ULIRG IRAS19297-0406 will be observed
under all circumstance. And one object from the list of the Cone Nebula {NGC
2264} and NGC 1241 will be observed. The latter will depend upon the result of
ground-based IR imaging of NGC 2264.

ACS 9027

This activity will obtain a series of images to evaluate the geometric
distortion over the field of view of the ACS SBC channel, after its image
quality has been optimized with the corrector mechanism. Images will be
obtained
in filter F125LP, with a pattern of POS-TARG offsets in each axis. These data
will be complemented by the images of the same field obtained in proposal 9024,
“ACS SBC Flat Field Strability”, which utilizes a similar image offsetting
technique at larger spatial scales. The observations may be scheduled
back-to-back with those from proposal 9024. NGC 6681 {18.7 h, -32 deg} will be
the target, as this star field has been used extensively by the STIS
program for
UV PSF measurement and photometry

FGS/1 9034

Fine Guidance Sensor 11R was used to observe the mass-luminosity relation {MLR}
of Population II stars of which very little is currently known. With the advent
of the Hipparcos Catalogue, improved distances to many spectroscopic binaries
known to be Pop II systems are now available. After surveying the
literature and
making reasonable estimates of the secondary masses, we find 13 systems whose
minimum separation should be larger than the resolution limit of FGS #1.

STIS/FUV-MAMA 9159

Proposal will measure amplitude versus wavelength for the 20 known ell=1 and 9.
known ell=2 modes in PG1159-035 using the STIS FUV- MAMA.

STIS/CCD 9317

The Space Telescope Imaging Spectrograph (CCD) was used to perform the default
archival pure parallel program for STIS during cycle 10.

WF/PC-2 9318

The WF/PC-2 was used to perform the generic target version of the WFPC2
Archival
Pure Parallel program. The program was used to take parallel images of random
areas of the sky, following the recommendations of the Parallels Working
Group.

ACS/WFC 9575

The Advanced Camera for Surveys (WFC) was used to test ACS pure parallels in
POMS.

FLIGHT OPERATIONS SUMMARY:

HSTARs:

8648 – GSAcq (1,3,1) 135/14:12:28z failed to FL

backup on FGS1 14:16:33z due to ssl on FGS3.

COMPLETED OPS REQs:

16768-2 – FSW 2.1B RAM Installation @ 135/2249z

OPS NOTES EXECUTED:

Battery 3 Limits Following Capacity Testing @ 135/2156z

                         SCHEDULED                  SUCCESSFUL    FAILURE

TIMES

FGS GSacq                   7                          7

FGS REacq                   6                          6

FHST Update                18                         18

LOSS of LOCK         None

Operations Notes:

none

SIGNIFICANT FORTHCOMING EVENTS:

Continuation of Servicing Mission Orbital Verification and the gradual
resumption of normal science observations and calibrations.