Status Report

NASA Hubble Space Telescope Daily Report # 3442 (part 2)

By SpaceRef Editor
September 8, 2003
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WFPC2 9710

POMS Test Proposal: WFII backup parallel archive proposal

This is a POMS test proposal designed to simulate scientific plans.

WFPC2 9709

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.

ACS 9675

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 9658

ACS Earth Flats

This program will obtain sequences of flat field images by observing the bright Earth. Several UV filters from the interim calibration program {9564} require additional exposures to obtain the required illumination. A few UV filters from this program will be repeated to monitor for changes in the flat fields and to verify the interim results. Since no streaks are observed in the UV, the wavelength coverage is extended to longer wavelengths in order to explore the severity of streaks in the flats from clouds in the FOV. We have added exposures for the HRC in the visible filters to verify the results derived from the L-flat campaign and to explore the severity of streaks. We have also added exposures on WFC using the minimum exposure time and using filters which will not saturate the brightest WFC pixel by more than 10 times the full well.

ACS 9656

Stability of the ACS CCD: geometry, flat fielding, photometry

A moderately crowded stellar field, located ~6′ West of the centre of the cluster 47 Tuc, is observed repeatedly {every three weeks with the WFC, every other month with the HRC} in various filters, spending 1 orbit per epoch. Different filters will be used every time, so that over the course of the year all filters will have been employed at least twice. The most common filters will be checked more frequently. The same field has been observed in the course of the SMOV phase and the positions and magnitudes of the most prominent stars have been accurately measured. Although the field is neither a proper astrometric nor a proper photometric standard one, the positions and magnitudes of the objects in it can be used to monitor any local and large scale variations in the platescale and sensitivity of the detectors. It should be noted that for the filters which have already been used during the SMOV phase it will be sufficient to take one single image, without CR-SPLIT, since the exposure time is always short {20-30 sec} and there will be so many stars that the few of them which are affected by cosmic rays can be discarded as outliers in the photometry. For narrow and medium band filters not exercised on this target in the SMOV phase, however, a baseline will have to be set. This expenditure of time will apply to the current cycle only. At variance with the approach used in SMOV, there is no need for large telescope slews to place the same objects on opposite sides of the detectors, thence allowing the programme to remain compact and efficient. All exposure level parameters are set to their default values, except for the amplifier gain of the WFC exposures in the F606W band, which will be collected with the gain value of 2 for the WFC for compatibility with the SMOV observations. The exposure time is typically 30 seconds for the WFC, 60 sec for the HRC. No attempt will be made to attain a predefined or the same orientation on the sky amongst different epochs. Typically, for the WFC, five exposures will be accommodated in one orbit. For the HRC, about 10 exposures can be fitted within one orbit

STIS 9633

STIS parallel archive proposal – Nearby Galaxies – Imaging and Spectroscopy

Using parallel opportunities with STIS which were not allocated by the TAC, we propose to obtain deep STIS imagery with both the Clear {50CCD} and Long-Pass {F28X50LP} filters in order to make color-magnitude diagrams and luminosity functions for nearby galaxies. For local group galaxies, we also include G750L slitless spectroscopy to search for e.g., Carbon stars, late M giants and S-type stars. This survey will be useful to study the star formation histories, chemical evolution, and distances to these galaxies. These data will be placed immediately into the Hubble Data Archive.

STIS 9608

CCD Bias Monitor – Part 2

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 9606

CCD Dark Monitor-Part 2

Monitor the darks for the STIS CCD.

WFPC2 9595


This dark calibration program obtains 3 dark frames every day to provide data for monitoring and characterizing the evolution of hot pixels.

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


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 10000

STIS Pure Parallel Imaging Program: Cycle 12

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


Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.)

HSTAR 9138: Two FHST Roll Delay Update (U1,3RD) failures @ 249/15:15:50Z with Error Box results reading “1 FAILED”. A second FHST Roll Delay Update (U2RD) failure occurred @ 249/15:42:14Z with Error Box reading “2 FAILED”. Subsequent Update (U1,2FM) @ 249/16:16:17Z occurred while HST was in LOS, results unknown at this time. Second Update (U1,2FM) @ 249/16:19:02Z was successful. GS Acquisition (2,3,2) @ 249/16:22:098Z was successful. Under investigation.

HSTAR 9140: GS Acquisition (1,2,1) @ 250/14:53:35Z failed to gyro control after SRLE on FGS 1. First failure occurred @ 250/14:53:35Z, second @ 250/14:58:20Z. Four STIS 710 Status Buffer messages were received following GS Acquisition failure. Under investigation.

HSTAR 9141: GS Acquisition (3,1,3) @ 251/01:55:36Z resulted in FL backup using FGS 1. Following GS Acquisition (3,1,3) @ 251/02:49:30Z also resulted in FL backup on FGS 1. Prior FM Updates @ 251/01:50:50Z and 251/01:52Z showed good attitude errors. Under investigation.



                          SCHEDULED     SUCCESSFUL    FAILURE TIMES FGS GSacq             27                        26             250/1453z FGS REacq             21                        21 FHST Update           60                        57              249/1228z*, 249/1515z, 249/1542z LOSS of LOCK 

Note: (* Only 2nd of two U2,3FM updates at 249/1228z failed; no HSTAR required)


SpaceRef staff editor.