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IAUC 4083: 1985e; R Aqr; 1E 1048.1-5937

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                                                  Circular No. 4083
Central Bureau for Astronomical Telegrams
Postal Address: Central Bureau for Astronomical Telegrams
Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
TWX 710-320-6842 ASTROGRAM CAM    Telephone 617-495-7244/7440/7444

     An apparently positive visual detection of this comet was made
by T. Seki, Geisei (0.20-m refractor), on July 8.5 UT at m2 = 10.0-
10.5, and a simultaneous photographic positional observation is
shown below; the positional uncertainty is 10" because of interference
from clouds.  Several observers have reported negative
observations to limiting mag ~ 11 on subsequent nights.

     1985 UT             R.A.   (1950.0)   Decl.        m1

     July  8.4810       8 53 12.4      +22 01 32       11.0

     R. Viotti, Istituto Astrofisica Spaziale, Frascati; L. Piro,
Istituto TESRE, Bologna; M. Friedjung, Institut d'Astrophysique,
Paris; and A. Cassatella, IUE Observatory, Villafranca, telex:
"We have detected weak x-ray emission from the symbiotic Mira
variable R Aqr at maximum.  Observations made with EXOSAT on June
14 give a flux of 0.005 cts/s (+/- 10 percent), suggesting that the
x-ray flux is not correlated with the Mira-type variations.
Coordinated IUE observations on June 18 show a faint emission line
spectrum of intermediate ionization; C IV is the strongest line."

1E 1048.1-5937
     A. P. Smale, P. A. Charles and R. H. D. Corbet, Oxford
University; and F. D. Seward, Center for Astrophysics, report: "We
have performed an EXOSAT observation of the Einstein x-ray pulsar
1E 1048.1-5937 (Seward and Charles 1984, Bull. A.A.S. 16, 983)
lasting 6.5 hr on June 20.  From the medium-energy experiment we
confirm the presence of x-ray pulsations at a period of 6.4407 +/-
0.0009 s, which is slightly but significantly longer than the
Einstein value.  The best fit to the x-ray spectrum is a power law
with photon index 2.3 and, when combined with the observed countrate
in the low-energy telescopes, it indicates a high degree of
obscuration (~ 1.6 x 10**26 atoms m**-2).  The source position is R.A. =
10h48m10s05, Decl. = -59deg37'24" 9 (equinox 1950.0) with an error-circle
radius of 15".  Examination of SRC IIIa-J and ESO blue plates
reveals that the brightest star in this circle has V ~ 19.  The x-
ray obscuration implies a visual extinction  Av ~ 8, and hence this
system can be interpreted as a distant Be binary."

1985 July 17                   (4083)              Brian G. Marsden

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