Central Bureau for Astronomical Telegrams
IAUC 6314: 1994Y; GRO J1744-28
The following International Astronomical Union Circular may be linked-to from your own Web pages, but must not otherwise be redistributed (see these notes on the conditions under which circulars are made available on our WWW site).
Read IAUC 6315
.dvi or
.ps format.
Circular No. 6314
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)
BMARSDEN@CFA.HARVARD.EDU or DGREEN@CFA.HARVARD.EDU (science)
Phone 617-495-7244/7440/7444 (for emergency use only)
SUPERNOVA 1994Y IN NGC 5371
P. Garnavich, Harvard-Smithsonian Center for Astrophysics; A.
Noriega-Crespo, Infrared Processing and Analysis Center; and A.
Moro-Martin, Maria Mitchell Observatory, write: "Infrared
photometry with the Apache Point 3.5-m telescope (+ GRIM-II array)
shows that the peculiar type-II supernova 1994Y (IAUC 6058) has
developed a strong infrared excess. Magnitude estimates for Jan.
14 are K = 15.6, H = 17.1, and J = 18.9. The excess is similar to
that seen in SN 1980K (Dwek et al. 1983, Ap.J. 274, 168) and
suggests dust formation or a strong infrared echo from an existing
dust shell. The difference in distance between the host galaxies
implies that, during this dust emission phase, SN 1994Y is
intrinsically brighter than was SN 1980K by at least 3 magnitudes
in the K band."
GRO J1744-28
A. Zytkow, Institute of Astronomy, Cambridge; and M. Irwin,
Royal Greenwich Observatory, Cambridge, communicate: "The APM
facility in Cambridge was used to analyze the area covering the
position of GRO J1744-28 on glass copies of a U.K. Schmidt
Telescope (UKST) photographic sky survey IIIa-J plate and a
European Southern Observatory (ESO) R plate. For each plate, an
approximately 4'x4' region centered on the VLA position (IAUC 6307)
was measured. Our examination of the data clearly suggests a
candidate for an optical counterpart that is within 1" of the VLA
position. The estimated magnitude of this candidate on the ESO R
plate is about 19.5, whereas on the IIIa-J sky survey plate, it
cannot be brighter than Bj about 22, as it is close to the plate
limit. The derived positions (equinox 2000.0) are: R.A. =
17h44m36s.92, Decl. = -28o45'38".0 (UKST Bj); 36s.78, 37".6
(position end figures; ESO R). The coordinates derived from the
ESO R plate are more reliable, since the object is well above the
plate limit (estimated errors +/- 0".5); for the IIIa-J plate, the
errors are about 1". Thus, the candidate optical counterpart has
an observed probable Bj-R > 2.5, equivalent to B-V > 1.9. In
addition, visual inspection of the region on a UKST sky survey film
copy in the I band (IV-N emulsion), shows the candidate optical
counterpart of the VLA source to be significantly redder than
neighboring objects, with estimated mag I = 17.5. If the above
optical candidate proves to be related to GRO J1744-28, then it may
be a new candidate for a class of neutron star/M star binaries
similar to HD 154791."
(C) Copyright 1996 CBAT
1996 February 15 (6314) Daniel W. E. Green
Read IAUC 6315
.dvi or
.ps format.
Our Web policy. Index to the CBAT/MPC/ICQ pages.
