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IAUC 3887: SN IN NGC 3227; SSV-13 AND HERBIG-HARO 7-11; 4U 2129+47 = V1727 Cyg

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                                                  Circular No. 3887
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 617-864-5758

     E. P. Aksenov, Sternberg Astronomical Institute, cables that
V. Pronik has discovered a supernova 12" due west of the nucleus
of NGC 3227 (R.A. = 10h20m9, Decl. = +20deg09', equinox 1950.0).
The supernova was at mpg = 12.0 on Nov. 4.04 UT and is of type I.

     R. Liseau, Stockholm Observatory, reports the optical detection
of the exciting source for the objects HH 7-11.  Observations
were made during Oct. 28.88-29.00 UT with a CCD camera (thin
laminated RCA chip) and RG 785 filter mounted at f/5 on the Stockholm
1.0-m reflector.  Bad weather conditions have so far prevented
further observations and the determination of the object's apparent
brightness in the near-infrared.  The optical position, determined
with respect to the 13 stars nearby tabulated by Herbig
and Jones  (1983, A.J. 88, 1040), is R.A. = 3h25m58s22 +/- 0s05,
Decl. = +31deg05'43"5 +/- 0"6 (equinox 1950.0).  Olofsson (unpublished)
gives for the corresponding infrared position the end-figures 58s2 +/-
0s2, 45" +/- 2" , while Haschick et al. (1980, Ap.J. 237, 26) have
given for the H2O maser source 58s2 +/- 0s1, 44" +/- 1" .

4U 2129+47 = V1727 CYGNI
     W. Pietsch and H. Steinle, Max-Planck-Institut fur Extraterrestrische
Physik, Garching; and M. Gottwald, European Space Operations
Center, Darmstadt, telex: "All types of observation by the
EXOSAT satellite for 15 hr on Sept. 29 and Oct. 4 failed to detect
this 5.2-hr-period binary x-ray source.  Simultaneous UBV observations
with the 2.2-m and 1.2-m telescopes at the German-Spanish
Astronomical Center, Calar Alto, showed the star to be in a state
of very low intensity (V = 17.8, B = 18.4), and no variation of
amplitude greater than +/- 0.3 mag was found in the UBV range.  As
with Her X-1 = HZ Her, the 1.5-mag-amplitude optical lightcurve
reported formerly has been interpreted as due to x-ray heating of
the optical star.  Our present optical observations indicate that
V1727 Cyg has been shut off, behavior similar to that of HZ Her
between 1949 and 1956.  Since no previous quiescent state is
known, optical (especially spectroscopic) and x-ray observations
are urged.  The position is R.A. = 21h29m36s2, Decl. = +47deg04'08"
(equinox 1950.0): see Thorstensen et al. (1979, Ap.J. 233, L57)."

1983 November 10               (3887)              Brian G. Marsden

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