Central Bureau for Astronomical Telegrams
IAUC 5454: N Cyg 1992; EXO 2030+375; N Sgr 1992
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Circular No. 5454
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 or GREEN@CFA.BITNET MARSDEN or GREEN@CFAPS2.SPAN
NOVA CYGNI 1992
Peter Collins, Boulder, CO, reports his visual discovery of an
apparent nova. B. A. Skiff, Lowell Observatory, provides the
following precise position measured from a plate taken by S. J. Bus
with the 0.33-m astrograph on Feb. 20.094 UT, upon which images were
slightly trailed and the star's magnitude was estimated as B = 5.5:
R.A. = 20h30m31s.76, Decl. = +52 37'52".9 (equinox 2000.0). Visual
magnitude estimates, communicated in part by J. Mattei, AAVSO, and
G. M. Hurst, Basingstoke, England: Feb. 19.07, 6.8: (Collins);
19.54, 6.0: (Collins); 20.07, 5.5: (Collins); 20.19, 5.3 (D. Moore,
Dublin, Ireland); 20.42, 5.0 (J. E. Bortle, Stormville, NY); 20.43,
5.0 (C. Scovil, Stamford, CT); 20.44, 5.3 (P. Sventek, Houston, TX);
20.51, 5.0 (Collins); 20.53, 5.2 (D. Levy, Tucson, AZ).
EXO 2030+375
R. B. Wilson, B. A. Harmon, G. J. Fishman, and C. A. Meegan,
Marshall Space Flight Center, NASA; M. H. Finger, Computer Sciences
Corporation; W. S. Paciesas, University of Alabama at Huntsville;
and T. A. Prince, J. M. Grunsfeld, and D. Chakrabarty, California
Institute of Technology, report for the BATSE team: "Pulsed hard x-
ray emission from the transient x-ray pulsar EXO 2030+375 is being
detected by the BATSE instrument onboard the Compton Observatory.
The pulsed emission was first detected at 20-60 keV on Feb. 9. The
pulsed flux has been increasing daily. On Feb. 10, the pulsations
were detected from 25 to 100 keV. Approximate fluxes measured, in
units of 10E-5 photons cmE-2 sE-1, were: 44.0 +/- 6.8, 10.0 +/-
5.1, 5.9 +/- 1.9, and 1.5 +/- 0.9, in the energy ranges 30-40, 40-
50, 50-70, and 70-100 keV, respectively. The spectral index is 3.9
+/- 0.8. The pulse period has increased steadily at a rate of 2.7
ms/day, with the barycentric period on Feb. 10.0057 UT being 41.6794
+/- 0.0006 s. No binary corrections have yet been applied, since
the orbital phase is unknown. The source has also been detected using
Earth occultation, but the measured flux of EXO 2030+375 is
currently not separable from that of Cyg X-3."
NOVA SAGITTARII 1992
Photometry by A. C. Gilmore with the 0.6-m Boller & Chivens
Cassegrain telescope at Mt. John University Observatory: Feb. 16.681
UT, V = 8.99 +/- 0.02, U-B = -0.13 +/- 0.05, B-V = +0.75 +/- 0.02.
1992 February 20 (5454) Daniel W. E. Green
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