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IAUC 5182: 1991D; 1987A; 1991b

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                                                  Circular No. 5182
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. Remillard, Massachusetts Institute of Technology; R.
Brissenden, Center for Astrophysics; and J. Halpern and M.
Eracleous, Columbia University, report their discovery, on CCD
images obtained on Feb. 6 and 7 UT with the 1.3-m McGraw-Hill
telescope of Michigan-Dartmouth-MIT Observatory, of an apparent
supernova (V about 16.5) in a Seyfert 1 galaxy located at R.A. =
13h38m31s.8, Decl. = -14 23'32" (equinox 1950.0; cf. Maza et al.
1989, Ap.J. Suppl. 69, 349).  SN 1991D is offset about 15" east-
southeast of the galaxy nucleus, in what appears to be a faint
spiral arm on the Palomar Sky Survey E print.  A brief spectrogram
(range 710-990 nm) was obtained with the Kitt Peak 4-m telescope on
Feb. 7.  This range does not include H-alpha, though broad features
with possible P-Cyg profiles were detected near 760 and 810 nm.

     L. Wang and E. J. Wampler, European Southern Observatory, report:
"We made recent observations of the ring nebula near SN 1987A.
The observations were obtained on 1990 Aug. 30 and 1991 Jan. 17 with
CASPEC in slitless mode.  Many new narrow nebular lines are observed,
among these being lines of [Fe VII].  The measured fluxes (in units
of 10E-15 erg sE-1 cmE-2) of the [Fe VII] 515.9-nm line are 0.75 and
0.76 for the Aug. 30 and Jan. 17 observations, respectively; the
measured flux of the [Fe VII] + [Ca V] 608.7-nm line on Aug. 30 is
0.38, and the line is still present in the Jan. 17 observation.  The
[Fe VII] 572.1-nm line is present in both observations, but flux
calibration is currently not available.  The width of [Fe VII]
515.9-nm is comparable to the strong metal lines such as [O III] and
[N II].  As is the case for the other narrow lines, it is plausible
that these weak [Fe VII] lines are from photoionization by the initial
ultraviolet event.  However, shock interaction could be a contributing
mechanism and cannot be ruled out by these observations."

COMET ARAI (1991b)
     Total visual magnitude estimates (cf. IAUC 5165):  Jan. 19.24
UT, 9.6 (C. S. Morris, Pine Mountain Club, CA, 0.26-m reflector);
Feb. 3.80, 11.0 (H. Mikuz, Ljubljana, Yugoslavia, 0.20-m reflector);
5.21, 11.3 (A. Hale, Las Cruces, NM, 0.41-m reflector).

1991 February 7                (5182)             Daniel W. E. Green

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