Central Bureau for Astronomical Telegrams
IAUC 5467: 1992J; N Cyg 1992
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Circular No. 5467
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Postal Address: Central Bureau for Astronomical Telegrams
Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
Telephone 617-495-7244/7440/7444 (for emergency use only)
TWX 710-320-6842 ASTROGRAM CAM EASYLINK 62794505
MARSDEN or GREEN@CFA.BITNET MARSDEN or GREEN@CFAPS2.SPAN
SUPERNOVA 1992J IN ANONYMOUS GALAXY
J. Maza, University of Chile; and M. Hamuy, Cerro Tololo
Interamerican Observatory, report the discovery by M. Wischnjewsky (
University of Chile) of a supernova located about 11" west and 13"
north of the nucleus of an anonymous spiral galaxy located at R.A. =
10h06m43s, Decl. = -26 24'.0 (equinox 1950.0). The supernova was
found on a 20-min unfiltered IIa-O plate taken by L. Wells and R. C.
Smith (CTIO) with the CTIO Curtis Schmidt telescope on Mar. 3.149
UT. Confirmation was made by K. Janes (Boston University) from V
and I CCD images obtained on Mar. 5.3 with the CTIO 0.91-m
telescope, the supernova being at V = 18.35.
NOVA CYGNI 1992
Y. Andrillat and L. Houziaux, Observatoire de Haute Provence,
communicate: "A dozen CCD spectrograms (resolution 0.13 nm) of Nova
Cyg 1992 have been obtained at the 1.93-m telescope from Feb. 22
(just before maximum light) to Feb. 24, covering the regions of H-
alpha, O I at 777.2 nm, 844.3-878 nm, and P7. In all regions the
spectrum is very rapidly changing, with a strong increase in the
emission. H-alpha shows a typical P-Cyg profile (absorption at -920
km/s), with an equivalent width in emission reaching 16 nm on Feb.
24. On Feb. 22, P7 appears as a P-Cyg emission with absorption at
-915 km/s, while on Feb. 23 a second strong absorption system appears
at -1530 km/s. Also on Feb. 23, He II at 1023.4 nm exhibits a
P-Cyg profile with an emission width of 1300 km/s. The spectrum is
complex between 835 and 878 nm, where N I (mult. 1, 8) is present,
Ca II is probably present as emission, and two absorption systems
are seen at -960 and -1350 km/s. O I at 844.6 nm develops a similar
scheme, as well as higher members of the Paschen series, most of the
individual components being lost in the somewhat chaotic appearance
of the spectrum."
H. Mikuz, Ljubljana, forwards the following additional photometry
by A. Dolzan, Litija, Slovenia (cf. IAUC 5463): Feb. 25.171
UT: V = 4.63 +/- 0.03, B-V = +0.48 +/- 0.05, U-B = -0.39 +/- 0.07;
Mar. 2.163, 5.68 +/- 0.01, +0.31 +/- 0.03, -0.66 +/- 0.06; 5.169,
5.87 +/- 0.02, +0.33 +/- 0.04, -0.63 +/- 0.05. J. Borovicka,
Ondrejov Observatory, reports the following CCD photometry: Feb.
28.15 UT, V = 4.73; 29.16, V = 5.01, V-R = +1.01; Mar. 1.13, 5.35,
+0.92; 2.13, 5.70, +1.21; 3.08, 5.73, +1.17 (probable errors 0.06
mag in V, 0.09 in V-R).
1992 March 5 (5467) Daniel W. E. Green
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