Hubble Space Telescope Daily Report #2684 08/11/00
HUBBLE SPACE TELESCOPE
DAILY REPORT #2684
PERIOD COVERED: 0000Z (UTC) 08/10/00 – 0000Z (UTC) 08/11/00
Daily Status Report as of 224/0000Z
1.0 OBSERVATIONS SCHEDULED AND ACCOMPLISHED:
1.1 Completed Two Sets of WF/PC-2 8826 (Cycle 9 Supplemental Darks pt 1)
The WF/PC-2 was used to perform a T dark calibration program that obtains three dark frames every day in order to provide data for monitoring and characterizing the evolution of hot pixels. There were no reported anomalies.
1.2 Completed WF/PC-2 8805 (POMS Test Proposal: WFII Parallel Archive Proposal Continuation)
The WF/PC-2 was used to perform a 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 Parallels Working. The proposal completed with no reported problems.
1.3 Completed STIS/CCD 8439 (Bias Monitor-Part 2 C8)
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, to build up high-S/N superbiases and track the evolution of hot columns. The proposal completed with no reported problems.
1.4 Completed Two Sets of STIS/CCD 8437 (Dark Monitor-Part 2 C8)
The Space Telescope Imaging Spectrograph (CCD) was used to monitor the darks. The proposal completed nominally.
1.5 Completed WF/PC-2 8698 (Identification of the Galaxy’s Missing Mass)
The WF/PC-2 was used to observe the nature of dark matter that is one of the key astrophysical questions of the day. The existence of dark matter and its dynamical dominance in the outer parts of our Galaxy and spiral galaxies with flat rotation curves is well established. The MACHO project has identified ~half of the Milky Way’s dark matter with stellar objects of ~0.5 M_sun, probably white dwarfs. But the location of the microlensing in the halo is disputed. Several have detected two candidate halo white dwarfs of L/L_sun ~ 10^-5 in the Hubble Deep Field with 25 +/- 5 mas/year proper motions. The observations completed with no reported problems.
1.6 Completed Two Sets of STIS/CCD 8808 (POMS Test Proposal: STIS Non-Scripted Parallel Proposal Continuation III)
The Space Telescope Imaging Spectrograph (CCD) was used to make non-scripted, parallel observations as part of a POMS test proposal. The observations completed with no anomalous activity.
1.7 Completed Two Sets of WF/PC-2/STIS/CCD 8675 (The Massive Star Content of NGC 6822)
The WF/PC-2 and the Space Telescope Imaging Spectrograph (CCD) were used to characterize the young, coeval stellar population discovered with WFPC2 multiband imaging in a NGC6822 star forming region, with follow-up spectroscopy of the massive star candidates. The proposal completed with no reported problems.
1.8 Completed STIS/CCD 8844 (Deep Spatial/Spectral PSF Calibration)
The Space Telescope Imaging Spectrograph (CCD) was used to acquire a set of deep spectroscopic images of isolated, point source stars for the purpose of correcting spectroscopic science observations for dispersed residual scattered light along the slit from the point-like central object. Using limited observations from the archive, it is suspected that a dynamic range approaching 10exp7 can be measured from the stellar core to 26" away at the limit of the CCD and aperture edge. The observations completed with no anomalies reported.
1.9 Completed STIS/CCD 8226 (Discerning the Origins of Blue Stragglers: Masses and Rotation Rates)
The Space Telescope Imaging Spectrograph (CCD) was used to study the blue stragglers in globular cluster NGC-104. Conventional wisdom holds that the masses of Blue Straggler Stars in globular clusters are significantly larger than the turnoff mass. A wavelength calibration observation was also taken. The multiple losses-of-lock detailed in 2.1 and HSTARs 7789 and 7780 occurred during the execution of parts of this proposal. Otherwise, the observations were executed as scheduled, and no further anomalies were noted.
1.10 Completed STIS/CCD/MA1 8219 (A Definitive Census of the Cataclysmic Variable Population in 47 Tuc)
The Space Telescope Imaging Spectrograph (CCD and MA1) was used to make deep, far-ultraviolet, time-resolved observations of the cataclysmic variable population in the globular cluster 47 Tuc (a.k.a., NGC-104). A wavelength calibration image was also taken. The multiple losses-of-lock detailed in 2.1 and HSTARs 7789 and 7780 occurred during the execution of parts of this proposal. Otherwise, the observations were executed as scheduled, and no further anomalies were noted.
1.11 Completed WF/PC-2 8822 (Decontaminations and Associated Observations Pt. 1/4)
The Wf/PC-2 was used for the monthly decons. Also included are instrument monitors tied to decons: photometric stability check, focus monitor, pre- and post-decon internals {bias, intflats, kspots, & darks}, UV throughput check, VISFLAT sweep, and internal UV flat check. There were no reported problems.
2.0 FLIGHT OPERATIONS SUMMARY:
2.1 Guide Star Acquisitions:
Scheduled Acquisitions: 8
Successful: 8
Scheduled Re-acquisitions: 8
Successful: 8
As documented in HSTARs 7789 and 7790, following a successful acquisitions at 223/1956Z and at 223/213302Z, there were at least 10 losses-of-lock. These events were anticipated since the guide star was fainter than expected. Proposals described in 1.9 and 1.10 were affected.
2.2 FHST Updates:
Scheduled: 16
Successful: 16
2.3 Operations Notes:
The SSR EDAC error counter was cleared three times per ROP SR-1A.
SI C&DH errors were reset at 223/1244Z, using ROP NS-5.
Operations returned to the GSFC MOR at 223/1742Z. CCS string "B" became the prime operations string at 223/1936Z.
Using ROP DF-18A, the engineering status buffer limits were modified on three occasions.
At 224/071242Z, the STIS low voltage power supply for the CCD electronics box (OPSCB5V) flagged out-of-limits low with a value of 4.375 volts for one 60-second sample. The limit is 4.4 volts.
3.0 SIGNIFICANT FORTHCOMING EVENTS:
The return to the target of opportunity Comet Linear proposal on days 224 and 225.
Continuation of normal science observations and calibrations.
