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IAUC 5708: alpha Ori; GRB 930131; 2CG 135+01; P/SCHWASSMANN-WACHMANN 1

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                                                  Circular No. 5708
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Postal Address: Central Bureau for Astronomical Telegrams
Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
Telephone 617-495-7244/7440/7444 (for emergency use only)
TWX 710-320-6842 ASTROGRAM CAM     EASYLINK 62794505
MARSDEN@CFA or GREEN@CFA (.SPAN, .BITNET or .HARVARD.EDU)


alpha ORIONIS
     E. Guinan, B. Deeney, and K. Miller report:  "Photoelectric
photometry being carried out at Villanova University Observatory
shows that alpha Ori is undergoing a rapid decrease in brightness.
Beginning in 1992 October the star's brightness has decreased about
0.45 mag, to V about +0.87 in early 1993 February.  The last time
alpha Ori was this faint occurred about 4-4.5 yr ago.  We encourage
complementary observations over the next few months."


GRB 930131
     W. Wenzel and J. Greiner, Sonneberg Observatory, report that
they have made blink comparison of pairs of plates taken Feb. 3.2
and 4.2 UT of a 2-degree radius surrounding the gamma-ray burst
reported on IAUC 5702.  No suspicious object was found down to
threshold mag about 15.


2CG 135+01
     The Compton Observatory EGRET Team (C. von Montigny, K.
Brazier, G. Kanbach, and H. A. Mayer-Hasselwander, Max-Planck-
Institut fur Extraterrestrische Physik; D. L. Bertsch, B. L. Dingus,
C. E. Fichtel, R. C. Hartman, S. D. Hunter, J. R. Mattox, P.
Sreekumar, and D. J. Thompson, Goddard Space Flight Center, NASA;
D. A. Kniffen, Hampden-Sydney College; J. Chiang, J. Fierro, Y. C.
Lin, P. F. Michelson, and P. L. Nolan, Stanford University; and E.
Schneid, Grumman Aerospace Corporation) reports the detection of
the COS-B source 2CG 135+01.  The EGRET position excludes the quasar
0241+622 from being the counterpart, but is consistent with the
variable radio source GT 0236+610 (Gregory et al. 1989, Ap.J. 339,
1054).  No flux variation is evident, but the observation (1991
Nov. 28-Dec. 12) does not cover the phase of the radio outburst.
Additional EGRET exposure is planned for the period 1993 Feb. 25-
Mar. 9, which corresponds to the phase interval 0.26-0.71 of the
26.5-day period.  The radio outburst normally occurs at phase 0.5-
0.7.  Simultaneous observations at other wavelengths would be of
interest.  Those planning observations should contact Carl Fichtel
at fichtel@lheavx.gsfc.nasa.gov.


PERIODIC COMET SCHWASSMANN-WACHMANN 1
     Total V CCD magnitude estimates by H. Mikuz, Ljubljana, Slovenia,
using 0.2-m cameras:  Jan. 25.94 UT, [17.7; Feb. 8.76, 12.8.


1993 February 13               (5708)            Daniel W. E. Green

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