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IAUC 7401: SAX J1747.0-2853; XTE J1118+480; 1999em

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                                                  Circular No. 7401
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions)
BMARSDEN@CFA.HARVARD.EDU or DGREEN@CFA.HARVARD.EDU (science)
URL http://cfa-www.harvard.edu/iau/cbat.html  ISSN 0081-0304
Phone 617-495-7244/7440/7444 (for emergency use only)


SAX J1747.0-2853
     S. Campana, Brera Observatory, Milan; and G. L. Israel and L.
Stella, Rome Observatory, on a behalf of a larger collaboration,
report on a BeppoSAX observation of the transient source SAX
J1747.0-2853 (IAUC 7377) on Mar. 16.71-17.48 UT:  "The source was
determined to lie at R.A. = 17h47m03s.1, Decl. = -28o52'30"
(equinox 2000.0; error radius 30" at 90-percent confidence level).
During the BeppoSAX observation, a type-I burst was observed,
testifying to the presence of a weakly magnetized neutron star.
Based on the peak flux, we estimate a distance of less than or
about 8000 pc.  The source was clearly detected up to 200 keV in
the PDS instrument, showing a heavily absorbed (10**23 cm**-2)
spectrum modeled with a blackbody (kT = 1 keV) plus a cut-off
(about 200 keV) power law (photon index gamma = 2.6).  The absorbed
0.1-200-keV flux amounts to 2 x 10**-9 erg cm**-2 s**-1."


XTE J1118+480
     C. Mauche, Lawrence Livermore National Laboratory; R. Hynes
and P. Charles, University of Southampton; and C. Haswell, Open
University, on behalf of the EUVE project at the University of
California at Berkeley, report:  "EUVE obtained a 20 500-s exposure
of XTE J1118+480 coincident with RXTE and Hubble Space Telescope
(HST) observations during Apr. 8.10-8.71 UT.  The mean count rate
in the DS photometer was about 1 count/s and the extreme-
ultraviolet (EUV) spectrum is apparent in the SW spectrometer from
the left edge of the detector at about 7.0 nm to about 12.0 nm.  A
crude estimate of the flux density at 9 nm is 4 x 10**-13 erg
cm**-2 s**-1 A**-1.  This is the first EUV spectrum of a blackhole-
candidate x-ray binary.  Additional EUVE observations are planned
during observations by RXTE on Apr. 13 (20 000 s) and by RXTE,
Chandra, and the HST on Apr. 18 (100 000 s)."


SUPERNOVA 1999em IN NGC 1637
     CCD magnitudes, unfiltered unless otherwise noted:  1999 Nov.
4.746 UT, 14.1 (S. Yoshida and K. Kadota, Ageo, Saitama, Japan);
13.591, 14.0 (Yoshida and Kadota); 2000 Jan. 5.267, 14.50 (M.
Martignoni, Milan, Italy); 5.756, V = 13.96 +/- 0.03 (D. Hanzl,
Brno, Czech Rep.); 15.765, 14.59 (Martignoni); 21.774, 14.56
(Martignoni); 30.408, 14.5 (Yoshida and Kadota); Feb. 5.471, 14.2
(Yoshida and Kadota); 12.440, 14.6 (Yoshida and Kadota); Mar.
13.75, 15.7 +/- 0.1 (K. Sarneczky, K. Sziladi, and L. Kiss,
Piszkesteto station, Konkoly Observatory).

                      (C) Copyright 2000 CBAT
2000 April 13                  (7401)            Daniel W. E. Green

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