gsh7w@astsun.astro.Virginia.EDU (Greg Hennessy) (12/05/90)
During the last shift the ASTRO telescopes became a working observatory. The shift started with an observation of Capella, which while none of the 3 UV telescopes were able to observe (the star is so bright that it confuses the star trackers, which are more sensitive than the designers thought), the BBXRT was able to use Capella to align its optics. BBXRT had problem in that it would drift off source, the origionally thought was a bad gyro, but it turned out to be a software bug. After the software for the Two Axis Pointing System (TAPS) was fixed, the tracking was fine. The principle investagator of BBXRT has pronounced BBXRT was working as designed. In the past shift BBXRT observed the Large Magellenic Cloud (LMC), the crab nebula, and several quasars and BL Lac objects. In the incoming shift, they will be observing the SMC, M87, M81, among others. The UV instruments are taking data, but while the star trackers are working somewhat, they are still rather fussy. It was thought that 4 minutes would be enough for setup before each operation, but a special operation still needs to be done to insure that the star tracker will work. A new version of the software will be sent up, and a test on the star trackers done. The loss of one terminal means that the two mission scientist have to take turns entering the data, which means that it takes longer to set up. It seems to take at least 10 minutes before an observation can begin, and many observations were scheduled for about 20 minutes or so. These have NOT ben sucessful. However, longer exposures have worked. The instuments have been collecting data for 17% of the time this shift, a dissapointingly low value, but much better than the 0% of data taken from last shift. UIT was able to take deep exposures of 3 objecs, M92 (a globular cluster), Betlegeuse, and Gam Gem (a standard star). In these exposures, UIT achieved about 50% of the nominal exposure times. Changes will be made to allow more efficient use of the scheduled time. Collection efficency should rise to about 50% in the next shift, and if the software patch and test works, should rise to about 75%, which the loss of a terminal in the shuttle will make it hard to do better than. The WUPPE telescope observed 6 stars, getting nice spectra. The instrument is not properly calibrated though, due to th eearlier problems. The calibration will be done this shift, and all of the data taken will be able to be fully calibrated. The HUT telescope has observed five stars, but none of those were stars that they had picked out, rather they were WUPPE stars. The HUT failed to get any time on any of the 4 stars they specified. The reason for this is unknown, but WUPPE observes brightter stars than HUT does, and it may be easier for the star trackers to track the brighter stars. The HUT is known to be out of focus a bit, with the stars being 5 arc seconds in diameter, rather than 2 seconds. The HUT will be focused at the same time as WUPPE, and this should iimprove their operating efficiency. During the last shift the UV instruments observed, SS Cyg (a flare star), M92, the Cygnus Loop super nove remnamt, and my favorite, the Perseus cluster. Since the Perseus cluster is the UIT's most important target,this observation will be repeated to try to ensure the best possible images. In the next shift, objects to be observed include M81, M87, the cluster in Abell 1795, and several sources in the small Magellenic cloud, Eta Carina, and Ez Cma. -- -Greg Hennessy, University of Virginia USPS Mail: Astronomy Department, Charlottesville, VA 22903-2475 USA Internet: gsh7w@virginia.edu UUCP: ...!uunet!virginia!gsh7w