[Date Prev][Date Next][Thread Prev][Thread Next][Search]
[HEASARC Mailing List Archives]
info for Cycle-5 Proposers (Instrument Status Report)
This messages gives updates on hardware status and new capabilities for the
four instruments on the Compton Observatory. For more information, please
contact the instrument teams or feel free to contact me (gehrels@lheavx
.gsfc.nasa.gov) for references.
Compton Project Scientist
INSTRUMENT STATUS AND NEW CAPABILITIES
The BATSE flight instrumentation continues to work extremely well. There
have been no hardware failures or degradation in the detectors since launch.
All components, including photomultiplier tubes, power supplies and the on-
board computer continue to have nominal performance. The on-board software
has undergone two minor modifications since launch, primarily to optimize
the data types and to perform on-board data storage and delayed readout to
overcome the loss of the GRO tape recorders. A 1 kilobit/sec data stream is
being utilized during periods of data gaps. This helps to recover about
half of the data that would otherwise be lost and is especially valuable for
The BATSE all-sky hard x-ray source monitoring capabilities have been
continually improved since launch. Hard x-ray/gamma-ray source detection
and monitoring have become more reliable and quantitative. The results of
these analyses are available to the scientific community quicker than
previously. This is especially important for follow-up observations by
other, more sensitive instruments and observations at other wavelengths.
Unusual events of broad interest are often submitted as IAU Circulars. An
occultation transform imaging technique has been developed which has been
extremely valuable in locating and separating sources. Typical
sensitivities for continuous and pulsed sources can be derived from recent
BATSE publications (e.g. 2nd Compton Symposium and the X-ray Binaries
Conference, Univ. of Md.).
Gamma-ray burst detection and analysis has also improved considerably since
launch. The development of new spectral analysis software has now been
completed and the first deliveries have been made. Burst trigger criteria
have been changed several times since Sept. 1994 in order to better study
other transient phenomena such as the BATSE-discovered atmospheric gamma-ray
flashes. Perhaps the most significant change since launch for the study of
gamma-ray bursts has been the development of the BAtse COordinate
DIstribution NEtwork (BACODINE) system by S. Barthelmy/GSFC, in conjunction
with the BATSE investigators. By intercepting the BATSE data stream in
real-time, this system can recognize a burst, derive its approximate
location, and distribute this information in a matter of seconds of its
occurrence. This permits the search for a candidate burst counterpart by
wide-field instruments sooner than ever before possible. The gamma-ray
burst location software has been considerably improved; location accuracies
of about 2 degrees (for strong bursts) are expected, using the new software.
COMPTEL operations are routine. The instrument is stable and performing
well at 93% of its maximum sensitivity in the energy range from 750 keV to
30 MeV . Individuals requiring additional detail should contact the COMPTEL
instrument manager, John Macri, at UNH. Telephone: (603)862-2793.
In September 94 the GSFC and UNH/COMPTEL teams implemented systems for
automated FTP transfer of selected COMPTEL data sets from the BACODINE BATSE
real-time burst monitor computer to analysis systems at UNH. With this
method the locations of selected bursts are reported in 15 to 30 minutes.
The previous best was 100 minutes. For additional details contact Marc
Kippen. Telephone: (603)862-4378. Internet: email@example.com.
The EGRET instrument, as the others on the Compton Gamma Ray Observatory,
was designed for a two year lifetime with an effective factor of two
contingency. At the present time just a few months before the fourth year
in orbit, the status of the EGRET instrument is reasonably good and the
consumable, the spark chamber gas, is expected to last significantly past
the four year period as will be described in the second paragraph. There
has been only one failure, that being one of the sixteen lower phototubes
in the coincidence system. Since it is on the periphery, the loss in
sensitivity is slightly less that it would be if it were in the middle.
The loss in sensitivity, about 6%, is included in the figures and software
provided to the guest investigators; so there is no need for a guest
investigator to take the matter into account further. There has been a
slight degradation in the spark chamber system in the form of a decreased
efficiency in a few decks; this change has little or no influence on the
final results, and any quantitative effect is included in the normalization
factors provided routinely to the guest investigators.
Regarding the gas life, it is now expected that the present full solid
angle operation mode will continue through the end of cycle 4 with the
exception of a few viewing periods where it does not seem warranted. There
should be enough gas after that to continue to operate through cycle 5 and
probably significantly beyond that in a limited mode which is described
fully in the Cycle 5 NASA Research Announcement in the appendix concerned
with the EGRET instrument. Basically, the recommendation is that most
observations should use only one or occasionally two or three of the nine
basic EGRET instrument telescope modes. Further, EGRET should be shut off
if there is no significant observation for a given pointing. This approach
allows examining a source, several sources close together, or a band of
radiation, but not looking at the full large solid angle.
The OSSE instrument continues to operate normally, with all detector
sub-systems performing as designed. Since launch, OSSE flight software has
been modified several times to improve flight operations and add
flexibility. Most importantly, the On-board Data Storage (ODS) process was
implemented in Phase 2 (following the failure of the on-board tape
recorders) to ensure >95% coverage for the primary source and background
spectral data for each orbit. ODS accumulates spectral data during times
when TDRSS contacts are not available, data that would otherwise be lost.
The one area of concern in flight operations is the status of the motor
drive for detector #1. On three occasions, the drive has failed to step in
response to the motor drive positioning process that, in normal operation,
moves the detectors every two minutes. In all cases, recovery from the
anomaly was made without difficulty. The cause is still under
investigation. It should be noted that each OSSE detector has a redundant
drive motor system in case of hard failure of the primary drive.
In coordination with the BATSE team, a new capability to OSSE's response to
cosmic gamma-ray bursts has recently been added. The burst trigger signal
generated by BATSE now encodes the results of an on-board calculation of the
approximate position of a cosmic gamma-ray burst. If the burst strength and
position meet a specified set of criteria, the encoded scan angle is sent to
OSSE, which then enters a special burst mapping mode. The criteria are
currently (1) count rate greater than 40 counts per 64 ms in the BATSE 100-
300 keV band, (2) azimuth from the OSSE scan plane less than 11 degrees, and
(3) OSSE scan angle within -45 to +135 degrees from the spacecraft's +Z
axis. The OSSE detectors map the region within +-10 degrees of the
estimated burst position for a period of 12 hours to search for persistent
or delayed low-level emission from the burst source. Both the mapping area
and the duration of the response are user-definable. If, in the meantime,
an improved position becomes available via the BACODINE network, e.g. from a
detection by COMPTEL, the OSSE mapping strategy can be updated appropriately
within about one hour with a ground command.