Central Bureau for Astronomical Telegrams
IAUC 6043: 1994W; P83l-57
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Circular No. 6043
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@CFA or GREEN@CFA (.SPAN, .BITNET or .HARVARD.EDU)
SUPERNOVA 1994W IN NGC 4041
C. Pollas, Observatoire de la Cote d'Azur, reports the following
accurate position for SN 1994W from a 5-min exposure taken on
July 30.90 UT (cf. IAUC 6042): R.A. = 11h59m37s.67, Decl. =
+62o25'14".6 (equinox 1950.0); the corresponding offset from the
center of the galaxy is 7".8 west and 17".5 north. The estimated
magnitude of SN 1994W is mpv about 14. A nearby star (mpv about
14.7) has position end figures 53s.68, 26'42".8.
M. W. Richmond, Princeton University; and R. R. Treffers, A. V.
Filippenko, and S. D. Van Dyk, University of California at Berkeley,
report that four R-band images of NGC 4041 were obtained in July as
part of the Leuschner Observatory Supernova Search (observing
conditions generally poor), yielding magnitudes with respect to a
comparison star about 94" east and 96" north of the nucleus (in the
sense SN 1994W - comparison star): July 7, [+3.6; 13, [+3.1; 18,
+1.2; 26, 0.0:. SN 1994W is measured as 6".7 west and 16".1 north
of the galaxy's nucleus.
P83l-57
A. W. Rodgers and W. H. Roberts, Mount Stromlo and Siding
Spring Observatories, report the discovery of a subdwarf O-type
star with Balmer-line and Ca II H- and K-line emission: ''The
emission-line systems have variable intensity and radial velocity.
The star is in the Rodgers et al. catalogue of high-latitude,
early-type stars (1993, A.J. 106, 591) and is designated there as
P83l-57 (R.A. = 3h34m34s.23, Decl. = -64o00'56".1, equinox 2000.0;
magnitude V = 14.2). A series of slit spectra (range 385-438 nm,
and sometimes to 510 nm; resolution 0.12 nm) have been obtained in
1991, 1992, and 1993. No well-defined periodicity in the emission-
line intensity or velocity has been identified, but variations
occur on a timescale of hours, and we encourage other observers to
help obtain more complete coverage of these variations. The
emission-line system presumably arises from an accretion disk
associated with a companion in orbit about the subdwarf O star. The
variations in the intensities of the Balmer emission do not correlate
with those of the Ca II emission. The subdwarf O absorption
spectrum appears constant, with lines of Fe III and He II detected,
and an equivalent width of H-delta of 1.10 +/- 0.07 nm, implying an
effective temperature > 21 000 K. The heliocentric radial velocity
is +160 +/- 28 km/s. The emission-line system of the Balmer and Ca
II H and K lines varies in radial velocity, with an amplitude of 70
km/s. The emission-line widths vary from unresolvable (< 60 km/s)
to about 160 km/s."
1994 August 1 (6043) Daniel W. E. Green
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