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IAUC 5718: 1993G; V1055 Ori; CY UMa

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                                                  Circular No. 5718
Central Bureau for Astronomical Telegrams
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

     R. R. Treffers, B. Leibundgut, and A. V. Filippenko, University
of California at Berkeley; and M. W. Richmond, Princeton University,
report their discovery of an apparent supernova in NGC 3690
(R.A. = 11h25m44s.2, Decl. = +58 50'23", equinox 1950.0).  Observations
were conducted as part of the Leuschner Observatory Supernova
Search (LOSS), which uses an automated 0.76-m telescope equipped
with the Lawrence Berkeley Laboratory CCD camera.  The supernova is
located about 1".5 west and 15" south of the galaxy's eastern,
relatively diffuse, condensation.  The discovery image was taken on
Mar. 5 UT, with confirmation on Mar. 6.  The supernova is not present
in previous LOSS images of the galaxy, the most recent one having
been obtained on Feb. 15.  Data obtained on Mar. 6.26 with the
0.5-m Berkeley Automatic Imaging Telescope (BAIT) yield R = 16.6
+/- 0.2 for the supernova.

     R. M. Wagner, D. L. DePoy, R. D. Blum, and R. Bertram, Ohio
State University; and D. T. Thompson and M. W. Buie, Lowell
Observatory, report:  "V- and K-band imagery of V1055 Ori (IAUC 5717)
were obtained on Mar. 5.1 UT at the Hall 1.1-m and Perkins 1.8-m
telescopes at the Lowell Observatory using the Lowell RCA direct
CCD camera and the newly-commissioned Ohio State Infrared Imaging
System, respectively.  Digital aperture photometry of these data
gives V = 20.0 +/- 0.7 and K = 17.2 +/- 0.3, with the large error
in the V magnitude attributable to the small telescope and a bright
background from the nearly full moon.  Our results are consistent
with previous photometry of V1055 Ori (Machin et al. 1990, MNRAS
247, 205; Gottwald et al. 1991, A.Ap. Suppl. 89, 367), which give a
mean V = 18.9 +/- 0.1, but with some intrinsic variability of about
0.2-0.3 mag.  Our photometry indicates that V1055 Ori appears to be
near its quiescent brightness and not in an unusual high state, but
the observations cover only one epoch.  Additional photometric
observations are encouraged."

     Visual magnitude estimates by P. Schmeer, Bischmisheim,
Germany, of a superoutburst of this SU UMa-type dwarf nova:  Feb.
23.00 UT, [13.2; 24.07, 12.2; 24.84, 12.3; 25.88, 12.5; 28.20,
12.7; Mar. 1.11, 12.7; 3.15, 12.9.

1993 March 6                   (5718)            Daniel W. E. Green

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