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[vsnet-obs 198] Nova Cen 1995,SN1995G,SN1995E (IAUC)


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.

1995 February 25               (6139)              Brian G. Marsden

NOVA CENTAURI 1995
     R. H. McNaught, Anglo-Australian Observatory, communicates the
following precise position by G. J. Garradd (Loomberah, N.S.W.,
0.25-m reflector): R.A. = 13h02m31s.99, Decl. = -60d11'38".1 (equinox
2000.0, uncertainty 0".3 in each coordinate).  On the measured CCD
frame the star is not blended with the GSC star mentioned by W. Liller.
P. M. Kilmartin, Mt. John Observatory, communicates a similar position
(end figures 31s.85, 38".2; residuals of six PPM stars average 0".2),
measured by her from an astrograph film taken on Feb. 25.49 UT by
A. C. Gilmore, who also provides further photometry (cf. IAUC 6139):
Feb. 25.62, V = 8.30, U-B = -0.70, B-V = +0.28, V-R = +1.09, V-I =
+1.23 (airmass 1.04).


SUPERNOVA 1995G IN NGC 1643
     McNaught also reports the following precise position, measured by
him from a 10-min exposure by C. P. Cass with the U.K. Schmidt telescope:
R.A. = 4h43m44s.22, Decl. = -5d18'53".8 (equinox 2000.0, PPM,
uncertainty 0".3 in each coordinate).  The offsets from the galaxy
center are 4".5 east, 16".1 north.  There is a nearby star of mag about
17 at end figures 43s.50, 10".3.


SUPERNOVA 1995E IN NGC 2441
     P. Molaro and G. Vladilo, Trieste Observatory; and N. A.
Walton, Royal Greenwich Observatory, La Palma, report that
spectrograms (range 350-870 nm, resolution FWHM about 0.6 nm)
obtained with the 4.2-m William Herschel Telescope (+ ISIS
spectrograph) on Feb. 23.7 UT confirm this object to be a type Ia
supernova.  The spectrum strongly resembles that of SN 1981B
at maximum.  Major absorption features are Ca II (857.9 nm),
O I (777.3 nm), Mg (448.1 nm) and Si II (635.5, 505.1, 412.9 nm),
observed at expansion velocities between -10 000 and -13 000 km/s.

1995 February 25               (6140)              Brian G. Marsden