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IAUC 3756: SN IN NGC 5485; VZ Scl; HD 208311: AN UNUSUAL NEW Be STAR

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IAUC number

                                                  Circular No. 3756
Central Bureau for Astronomical Telegrams
Postal Address: Central Bureau for Astronomical Telegrams
Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
TWX 710-320-6842 ASTROGRAM CAM     Telephone 617-864-5758

     R. Wood and J. Sinclair, Royal Greenwich Observatory, telex
and M. Lovas, Konkoly Observatory, confirms that the supernova
reported on IAUC 3754 is in the galaxy NGC 5485, not in the nearby
NGC 5473.  Wood and Sinclair give the accurate position of the
supernova as R.A. = 14h05m25s48, Decl. = +55deg15'21".3 (equinox
1950.0), which is 19" west and 63" north of the galaxy's nucleus.

     B. Schaefer, Massachusetts Institute of Technology; and J.
Patterson, Harvard-Smithsonian Center for Astrophysics, report that
this novalike variable (R.A. = 23h47m33s78, Decl. = -26deg39'32".9,
equinox 1950.0) is in a deep low-state.  On Oct. 20.047 UT it
appeared at mag ~ 20 on an unfiltered IIIa-J exposure with the
Curtis Schmidt telescope at Cerro Tololo.  Visual observations on
Oct. 14.3, 16.2, 18.2 and Nov. 21.2 confirm that VZ Scl was then
fainter than mag 16.6, whereas it is normally around mag 15.6.

     W. P. Bidelman, Warner and Swasey Observatory, writes: "HD
208311 = BD +32 4286, listed as of spectral type B5 and
photographic magnitude 8.9 in the AGK3, has been found to exhibit
strong hydrogen emission of a very unusual character on 10P
objective-prism plates taken with the Burrell Schmidt at the Kitt Peak
Station of the Warner and Swasey Observatory on 1981 Sept. 7 and
1982 Oct. 14.  It had previously been noted (visual survey, in
progress) as a new bright-H-alpha star by C. B. Stephenson on a 4-deg.
plate taken in 1980 Sept.  The star's peculiarity consists of an
extremely flat Balmer emission decrement: emission centered in
strong absorption wings is seen as far as H-19 on the more recent
blue plate.  The spectrum now resembles to some extent that of the
pole-on star 11 Cam, but the helium lines are substantially broader
than those in that object.  Presumably the onset of the emission
has been fairly recent, as Burrell plates in 1952, 1969 and
1971 show no evidence of it.  However, a plate taken on 1972 Sept.
16 suggests that HS emission was somewhat weak at that time, and
H-beta appears slightly filled-in on a plate taken on 1976 Aug. 19.
We have no plates during the following four years."

1982 December 22               (3756)              Brian G. Marsden

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