Central Bureau for Astronomical Telegrams
IAUC 7271: 1999ed; GM Sgr
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Circular No. 7271
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
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SUPERNOVA 1999ed IN UGC 3555
M. Modjaz and W. D. Li, University of California at Berkeley
(UCB), on behalf of the Lick Observatory Supernova Search (cf. IAUC
6627, 7126), report their discovery of an apparent supernova (mag
about 17.8) on Oct. 5.5 UT with the 0.8-m Katzman Automatic Imaging
Telescope (KAIT). SN 1999ed is located at R.A. = 6h50m00s.95,
Decl. = +25o37'54".5 (equinox 2000.0), which is 17".4 east and 9".0
south of the nucleus of UGC 3555. A KAIT image taken on 1998 Nov.
21 showed nothing at the position of SN 1999ed (limiting mag 19.5).
Q. Y. Qiao, Y. L. Qiu, and J. Y. Hu, Beijing Astronomical
Observatory (BAO), report the independent discovery of this object
during the course of the BAO Supernova Survey. It was found (mag
about 18.5) in an unfiltered CCD image taken on Oct. 6.88 UT with
the BAO 0.6-m telescope, and confirmed in an image taken on Oct.
7.83. CCD frames taken on Mar. 28.53 (limiting mag about 19.0)
showed nothing at the position of the supernova.
A. V. Filippenko and R. T. Chornock, UCB, report that CCD
spectra (range 330-1000 nm) obtained on Oct. 8 UT with the Shane
3-m reflector at Lick Observatory reveal that the object is a
normal type-II supernova, probably < 2 months after the explosion;
there are strong Balmer lines with P-Cyg profiles. The redshift,
measured from narrow emission lines in the host galaxy, is 0.016.
GM SAGITTARII
M. R. Garcia and J. E. McClintock, Harvard-Smithsonian Center
for Astrophysics, and P. J. Callanan, University College, Cork,
report: "We have obtained a total of 25 spectra (range 380-750 nm,
resolution 0.6 nm) with the Whipple Observatory 1.52-m reflector (+
FAST spectrograph) of GM Sgr, centered on the nights of Sept. 17.2,
18.2, and 19.1 UT. During this time, the H-alpha line transitioned
from emission to absorption. Equivalent widths were -7(1), -3(1),
and +0.45(5) nm, respectively. The strong emission line seen on
Sept. 17.2 had FWHM = 3.3(3) nm and a complex structure with two
prominent peaks on the blue wing. The remainder of the Balmer
series lines (through H16) are visible in each of the spectra; they
are more narrow (1.0 nm < FWHM < 2.0 nm) than the H-alpha emission
line and were always in absorption. The continuum and absorption-
line spectrum resembles that of an A star. The velocities of the
Balmer absorption lines measured on the three consecutive nights
were +320(20), 0(40), and 80(20) km/s, respectively."
(C) Copyright 1999 CBAT
1999 October 8 (7271) Daniel W. E. Green
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