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IAUC 7321: 1999ge; 1999gf; 1999em

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                                                  Circular No. 7321
Central Bureau for Astronomical Telegrams
Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions)
URL http://cfa-www.harvard.edu/iau/cbat.html  ISSN 0081-0304
Phone 617-495-7244/7440/7444 (for emergency use only)

     Y. Sato and W. D. Li, University of California at Berkeley, on
behalf of the Lick Observatory Supernova Search (LOSS; cf. IAUC
6627, 7126), report the discovery with the 0.8-m Katzman Automatic
Imaging Telescope (KAIT) of an apparent supernova on unfiltered
images taken on Nov. 27.2 (mag about 17.2) and 28.2 UT (mag about
16.9).  The new object is located at R.A. = 0h56m43s.76, Decl. =
-9 54'43".0 (equinox 2000.0), which is 16".0 east and 6".7 north of
the nucleus of NGC 309.  A KAIT image of the same field on Oct.
31.3 (limiting mag about 19.0) showed nothing at the position of
SN 1999ge.

SUPERNOVA 1999gf IN UGC 5515
     Sato and Li also report the discovery by the LOSS of another
apparent supernova on an unfiltered image taken on Nov. 27.5 UT
(mag about 18.2), with confirmation coming from earlier images
taken on Nov. 12.5 and 23.5 (when the new object was at mag 17.5
and 18.0, respectively).  SN 1999gf is located at R.A. =
10h13m37s.00, Decl. = -0 56'09".6 (equinox 2000.0), which is 18".5
west and 37".6 south of the nucleus of UGC 5515.  A KAIT image
taken on 1998 Nov. 21.5 (limiting mag about 19.0) shows nothing at
the position of SN 1999gf.  UGC 5515 is a member of Abell cluster

SUPERNOVA 1999em IN NGC 1637
     P. Garnavich, R. P. Kirshner, and P. Challis, Harvard-
Smithsonian Center for Astrophysics, on behalf of the Supernova
Intensive Study collaboration, write:  "Spectra of SN 1999em were
obtained with the Hubble Space Telescope Imaging Spectrograph on
Nov. 5.8 UT.  The data were obtained with three low-resolution
gratings (range 115-550 nm; resolution about 300 km/s).  The
combined spectrum has a peak flux of 3 x 10**-14 erg cm**-2 s**-1
A**-1 at 297 nm, and then drops off rapidly towards the blue,
falling a factor of 6 in flux density by 230 nm.  The ultraviolet
part of the spectrum is characteristic of the 'Iron Curtain'
resulting from the blending of large number of iron and nickel
lines (Hauschildt et al. 1996, Ap.J. 462, 386).  A broad P-Cyg
feature due to Mg II 280-nm is seen, although modified by the Fe
line blanketing.  Narrow interstellar absorption lines due to Mg I
at 286 nm, Mg II at 280-281 nm, Fe II at 261, 260, 239, and 235 nm,
and C IV at 155 nm are also clearly visible at the velocity of the
host galaxy."

                      (C) Copyright 1999 CBAT
1999 November 28               (7321)            Daniel W. E. Green

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