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IAUC 6139: N Cen 1995; 1995G; 7P

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                                                  Circular No. 6139
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Postal Address: Central Bureau for Astronomical Telegrams
Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions)
Phone 617-495-7244/7440/7444     TWX 710-320-6842 ASTROGRAM CAM
MARSDEN@CFA.HARVARD.EDU or GREEN@CFA.HARVARD.EDU (science)


NOVA CENTAURI 1995
     W. Liller, Instituto Isaac Newton, Vina del Mar, reports
his discovery of a probable nova with PROBLICOM on Feb. 23 and
his CCD confirmation on Feb. 24, the latter yielding the position
R.A. = 13h02m32s.07, Decl. = -60d11'39".8 (equinox 2000.0; blend with
GSC 8909.2001 at end figures 33s.52, 53".7, mag 12.4).  Magnitudes and
colors: Jan. 27, [12 (Liller); Feb. 23.31 UT, 7.2 (Liller; Kodak TP
film + orange filter); 24.04, V = 7.59 (Liller; CCD, comparison
HD 113012, assumed V = 8.13, B-V = +0.11); 24.15, V = 7.70 (Liller);
25.03, mv = 8.0 (D. Overbeek, Edenvale, South Africa); 25.41, V = 8.14,
U-B = -0.68, B-V = +0.31, V-R = +1.01, V-I = +1.17 (A. C. Gilmore,
Mt. John Observatory; comparisons Cousins F218 and F205, airmass 1.53).

     J. B. Hearnshaw and L. C. Watson, Mt. John University Observatory,
obtained several blue and red CCD spectra with the medium-resolution
spectrograph on the 1-m telescope around Feb. 25.43 UT.  These showed
strong Balmer emission lines with P-Cyg profiles.  The FWHM of the
H-gamma and H-delta lines was 5.5 nm.


SUPERNOVA 1995G IN NGC 1643
     A. V. Filippenko, University of California at Berkeley, reports
that D. Schlegel obtained CCD spectra (range 335-730 nm, resolution
0.7 nm) on Feb. 25 with the 3-m Shane reflector at the Lick
Observatory.  Inspection of the uncalibrated data reveals that SN
1995G is a peculiar type II supernova bearing a close resemblance to
SN 1994W shortly after discovery (cf. IAUC 6046, 6057).  Strong,
relatively narrow (FWHM 1200 km/s), hydrogen Balmer emission lines
are superposed on broader bases (FWZI 7000 km/s).  Narrow, weaker
Fe II emission lines are also present.  The Balmer lines exhibit
narrow (FWHM 300 km/s) P-Cyg absorption components with minima
displaced by about 700 km/s from the emission-line cores.  Similar
features are seen in the Fe II multiplets; they are probably produced
by a dense circumstellar shell.


COMET 7P/PONS-WINNECKE
     CCD magnitude estimates: 1994 Dec. 31.46 UT, R =  20.1 (S. M.
Larson and C. W. Hergenrother, Catalina, 1.5-m reflector); 31.49,
V = 20.9 (J. V. Scotti, Kitt Peak, 0.9-m Spacewatch telescope;
stellar appearance); 1995 Jan. 7.49, V = 20.6 (Scotti); 28.30, R = 20.7
(Larson and Hergenrother, Kitt Peak, 2.3-m reflector).


1995 February 25               (6139)              Brian G. Marsden

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