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IAUC 6105: 1994ae; GX 1+4; 1994r

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                                                  Circular No. 6105
Central Bureau for Astronomical Telegrams
Postal Address: Central Bureau for Astronomical Telegrams
Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions)
Phone 617-495-7244/7440/7444     TWX 710-320-6842 ASTROGRAM CAM

SUPERNOVA 1994ae IN NGC 3370
    S. D. Van Dyk and R. R. Treffers, University of California at
Berkeley (UCB); M. W. Richmond, Princeton University; and A. V.
Filippenko and Y. B. Paik, UCB, report their discovery of an
apparent supernova in NGC 3370 (R.A. = 10h44m23s, Decl. = +17o32'.3,
equinox 1950.0).  Observations were conducted as part of the
Leuschner Observatory Supernova Search (LOSS), which uses an
automated 0.76-m telescope equipped with the Lawrence Berkeley
Laboratory CCD camera.  The supernova is located about 30".3 west
and 6".1 north of the galaxy's nucleus.  The discovery image was
taken on Nov. 14 UT, and the object is visible at R = 15.4 +/- 0.4.
A second image taken nearly 2 hr later shows the object at the same
position; it is not present to a limiting R magnitude of about 17
in previous LOSS images of the galaxy, the most recent one having
been obtained on Nov. 3.

GX 1+4
     D. Chakrabarty and T. A. Prince, California Institute of
Technology; M. H. Finger, Universities Space Research Association;
and R. B. Wilson, Marshall Space Flight Center, NASA, report for
the Compton Gamma Ray Observatory BATSE team:  "The accreting x-ray
pulsar GX 1+4 has resumed spinning up, reversing the steady spindown
trend that had been observed since 1987.  We observed a smooth
decrease in the spin-down rate, from (3.8 +/- 0.1) x 10E-12 sE-2 on
June 20 to zero on about Oct. 30.  During the interval Nov. 8-11,
the spin-up rate was (2.7 +/- 0.3) x 10E-12 sE-2, with a mean
barycentric pulse frequency of (8.19033 +/- 0.00003) x 10E-3 sE-1.
The pulsed flux has increased by a factor of three since Oct. 17,
when the spin-down rate was (1.5 +/- 0.2) x 10E-12 sE-2.  On Nov.
10, the 20- to 100-keV phase-averaged pulsed flux was 95 +/- 10
mCrab, with a spectrum well fit by an optically-thin thermal
bremsstrahlung model F(E) = (A/E)exp(-E/kT), with temperature kT =
35 +/- 2 keV and F(50 keV) = (2.6 +/- 0.1) x 10E-4.  The pulsed
emission is brighter and harder than observed during a previous
outburst (IAUC 5859), and is continuing to increase in intensity."

     Total visual magnitude estimates by C. S. Morris, Pine
Mountain Club, CA (0.26-m reflector):  Oct. 29.32 UT, 10.6; 30.34,
10.5; Nov. 12.47, 10.7.

1994 November 16               (6105)            Daniel W. E. Green

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