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IAUC 7340: QY Per; 1999ga; 1999gp

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                                                  Circular No. 7340
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)

     J. A. Mattei, AAVSO, informs us that this suspected SU
UMa-type variable is undergoing what may be a superoutburst, as
indicated by the following visual magnitude estimates:  Dec. 19.972
UT, [14.9 (G. Poyner, W. Midlands, England); 28.146, 13.5 (M.
Simonsen, Macomb, MI); 28.166, 13.6 (Simonsen); 29.731, 13.9 (E.
Muyllaert, Oostende, Belgium); 29.828, 13.8 (C. Jones, Essex,
England); 29.901, 13.8 (H. McGee, Surrey, England).  Mattei notes
that high-speed photometry to look for superhumps is recommended.
The last confirmed outburst for QY Per in the AAVSO archive
occurred on 1995 Aug. 21, at peak mag 14.1.  Additional unfiltered
CCD magnitudes:  Dec. 23.190, [17.5 (P. Schmeer, Bischmisheim,
Germany); 28.168, 13.9 (Schmeer); 29.887, 14.2 (G. Masi, Ceccano,
Italy).  Masi also provides the following precise position for QY
Per:  R.A. = 3h15m36s.85, Decl. = +42o28'15".3 (equinox 2000.0).

SUPERNOVA 1999ga IN NGC 2442
     M. Salvo, L. Rizzi, A. Pastorello, and M. Turatto, Padova
Astronomical Observatory, report:  "A spectrum (370-910 nm;
resolution 1.1 nm) of SN 1999ga (cf. IAUC 7316) was taken on Dec.
29.26 UT with the 1.54-m Danish telescope (+ DFOSC) at the European
Southern Observatory.  Preliminary reduction of the spectrum shows
lines of H, Ca II, [Ca II], Na I D, and Fe II, indicating that the
supernova is of type II.  We therefore confirm the suggestion by
Rubenstein (IAUC 7319), which was based on the supernova's location
inside the parent galaxy, although our spectrum shows no strong
evidence of interstellar absorption.  The supernova seems rather
evolved, and the line emissions dominate over the absorptions.
Indeed, an automated comparison with all the spectra in our
supernovae archive shows the best fit to be with the spectrum of SN
1992H at 143 days after maximum (Clocchiatti et al. 1996, A.J. 111,
1286).  The shape of the continuum is also similar, indicating that
the two supernovae suffered comparable reddening.  The strongest
emission line (H-alpha) is flat-topped, suggesting that the
supernova ejecta is interacting with the circumstellar medium."

SUPERNOVA 1999gp IN UGC 1993
     K. Krisciunas and K. Loomis report preliminary infrared
photometry for SN 1999gp, obtained as noted for SN 1999go on
IAUC 7339:  Dec. 27.07 UT, J = 15.92 +/- 0.07, K' = 15.05 +/- 0.08.
They add that SN 1999gp is not the brighter foreground star
located just north of the galaxy's core.

                      (C) Copyright 1999 CBAT
1999 December 30               (7340)            Daniel W. E. Green

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