Central Bureau for Astronomical Telegrams

IAUC 7786: 2002A; PECULIAR Var IN Mon

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                                                  Circular No. 7786
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions)
CBAT@CFA.HARVARD.EDU (science)
URL http://cfa-www.harvard.edu/iau/cbat.html  ISSN 0081-0304
Phone 617-495-7440/7244/7444 (for emergency use only)


SUPERNOVA 2002A IN UGC 3804
     Y. L. Qiu and J. Y. Hu, Beijing Astronomical Observatory (BAO),
report the discovery by the BAO Supernova Survey of an apparent
supernova in unfiltered images taken with the BAO 0.6-m telescope
on Jan. 1.79 (mag about 17.4), 8.61 (mag about 16.8), and 9.56 UT
(mag about 16.8).  SN 2002A is located at R.A. = 7h22m36s.14, Decl.
= +71o35'41".5 (equinox 2000.0), which is 6".2 east and 14".7 south
of the nucleus of UGC 3804.  An image taken with the same telescope
on 2000 Dec. 27 showed no star at this position (limiting mag about
18.7).


PECULIAR VARIABLE IN MONOCEROS
     M. Della Valle, Osservatorio Astrofisico di Arcetri, Florence;
and T. Iijima, Osservatorio Astronomico di Padova, write:
"Preliminary analysis of spectra (range 400-680 nm, resolution
about 0.5 nm) of the variable star reported on IAUC 7785, obtained
on Jan. 8 with the 1.22-m telescope (+ Boller & Chivens
spectrograph), shows a heavily reddened continuum characterized by
a lack of the typical signatures exhibited by classical novae at
maximum light or during their early decline.  No absorption band of
TiO or C_2 is seen, while we detect faint H-alpha and Na I emission
lines flanked by P-Cyg profiles.  In addition, we note the presence
of three narrow emission lines at 650.2, 614.5, and 585.9 nm, also
flanked by P-Cyg profiles, tentatively identified as Ba II.  The
expansion velocities derived from the minima of the P-Cyg profiles
range between 380 and 500 km/s.  All of this may suggest this
object not to be a normal classical nova, but rather a peculiar
'slow' nova or a post-asymptotic-giant-branch star in flare-up.
Knowledge of the amplitude of the outburst could improve
significantly the classification."
     T. Kato, Kyoto University, forwards the following position for
the variable measured by H. Yamaoka (Kyushu University) from a
V-band CCD image taken on Jan. 9.496 UT by S. Kiyota (Tsukuba,
Ibaraki, Japan; 0.25-m reflector):  R.A. = 7h04m04s.801, Decl. =
-3o50'50".77 (equinox 2000.0; 29 Tycho-2 stars, uncertainty about
0".3).  They suggest that this object is identical to IRAS
07015-0346, or the 2MASS source having position end figures are
04s.82, 50".5 (and magnitudes J = 13.905, H = 13.480, K = 13.347),
noting that the infrared and V-J colors exclude the possibility of
a long-period variable (and that the IRAS color is very unusual
for a stellar object).  Kiyota provides the following additional
magnitudes:  Jan. 9.497, I_c = 8.28; 9.498, V = 10.10, B = 12.16.

                      (C) Copyright 2002 CBAT
2002 January 10                (7786)            Daniel W. E. Green

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