Circular No. 7947
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
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SUPERNOVA 2002eh IN NGC 917
     Independent reports have been received of the discoveries of
an apparent supernova on unfiltered KAIT CCD images obtained by
LOTOSS (cf. IAUC 7906), via B. Swift and W. D. Li, University of
California at Berkeley, on Aug. 1.5 and Aug. 3.4 UT (mag about 16.4)
and by T. Boles, Coddenham, England, in the course of the U.K.
Nova/Supernova patrol on Aug. 2.10 (mag 16.5) and 3.00 UT with a
0.35-m reflector. SN 2002eh is located at R.A. = 2h26m08s.45,
Decl. = +31o54'45".2 (equinox 2000.0), which is 9".3 east and 1".0
north of the nucleus of NGC 917 (measurements by Li). A KAIT image
taken on Feb. 1.2 UT showed nothing at this position (limiting mag
about 19.0). Boles adds that SN 2002eh is not present on earlier
images taken by himself or on second Palomar Sky Survey blue and
red images.


SUPERNOVA 2002ed IN NGC 5468
     M. Salvo and P. Price, Research School of Astronomy and
Astrophysics, Australian National University (ANU), report that a
spectrum (range 340-920 nm, resolution about 0.4 nm) of SN 2002ed
taken at the ANU 2.3-m (+ Double Beam Spectrograph) at Siding Spring
Observatory on July 30.41 UT shows it to be similar to the type-IIP
SN 1992H at early phases, according to the spectra published in
Clocchiatti et al. (1996, A.J. 111, 1286) and shows a blue continuum
with a broad H-alpha emission and H-beta with a P-Cyg profile. The
expansion velocity measured from the blueshifted minimum of H-beta
is about 11 500 km/s, adopting the NED recession velocity of 2845 km/s
for the host galaxy.


V2274 CYGNI
     R. J. Rudy, D. K. Lynch, S. Mazuk and C. C. Venturini, The
Aerospace Corporation; R. C. Puetter, Center for Astrophysics and
Space Sciences, University of California at San Diego; and R. B. Perry,
NASA Langley Research Center, report 0.8-2.5 micron spectroscopy of
the nova V2274 Cyg using the Aerospace Corporation Near-Infrared
Imaging Spectrograph and the Lick Observatory 3-m telescope on
July 18.4 UT (about 370 days after discovery): "He I at 1.0830 micron
is the dominant line in the spectrum. H I and He II lines are also
present at moderate strength. [S VIII] at 0.9911 $\mu$m is the only
coronal line detected. The FWHM of the emission lines is about
1400 km/s. The spectrum is very red, and the H I lines indicate a
reddening value of E(B-V) = 1.5, but there is no obvious emission
from hot dust."

                      (C) Copyright 2002 CBAT
2002 August 3                  (7947)          Carl W. Hergenrother