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THE ASTRONOMER Electronic Circular No 828       1994 Apr  4 15.08UT
Ed:Guy M Hurst, 16,Westminster Close, Kempshott Rise,  Basingstoke,
Hants, RG22 4PP,England. Telephone/FAX(0256)471074 Int:+44256471074
INTERNET: GMH at AST.STAR.RL.AC.UK  or    GMH at GXVG.AST.CAM.AC.UK
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EDITORIAL ABSENCE
The Editor will be away on holiday from Tuesday Apr 5 returning
Friday Apr 8 during which time he will not be contactable. Martin
Mobberley will deputise during my absence and, given some
uncertainties involving e-mail at present, it is recommended that
for discoveries only, he is telephoned on (0284) 828431 (weekends)
or (0245) 475297 (weekdays).
Routine messages should continue to be sent via e-mail to this
mailbox. Variable star alerts should continue to be directed to
Gary Poyner as per the usual arrangement.

Q1994/016
Further to the discovery announcement on E824, Gary Poyner,
Birmingham reports visual observations of this possible variable:
1994 Mar 29.826UT, 11.4; Apr 2.861, 11.5 (Poyner, 0.40-m refl.)

PECULIAR VARIABLE IN SAGITTARIUS
On Mar. 28 T. Hirayama, National Astronomical Observatory, Tokyo,
reported the discovery by M. Wakuda (Ryuyu, Shizuoka) on Mar.
14.825 UT of an object of mag about 10.7 (T-Max 400 film, green
filter) at R.A. = 18h51m43s, Decl. = -19d45'.9 (equinox 1950.0,
uncertainty 10").
T. Kato, Kyoto University, reports that M. Yamamoto (Okazaki,
Aichi) has photographic records showing the object's apparent
variability over mag 10.5-11.5 (PO0 filter) since 1993 Mar. 29 but
no earlier detection (and no brighter than mag 12.5 through 1992,
according to Wakuda).  Preliminary reduction of photometry by
A. C. Gilmore at Mt. John Observatory on 1994 Mar. 30.72 UT gives
V = 10.61, U-B = -0.23, B-V = +0.50, V-R = +0.35, V-I = +0.60
(uncertainty generally +/- 0.05 but up to +/- 0.1 in U-B).
E. K. Grebel, European Southern Observatory; and H. W. Duerbeck,
Astronomical Institute, Munster, report spectroscopic observations
on Mar. 30.4 with the ESO/MPI 2.2-m telescope and EFOSC-II.  A
low-resolution spectrum (range 340-920 nm, resolution 0.84 nm)
shows emission lines of H alpha, H beta and the infrared Ca II (2)
triplet, superimposed on a somewhat veiled late-K-giant continuum.
A high-resolution spectrum (range 352-547 nm, resolution 0.19 nm)
shows the Ca II H and K lines in absorption, as well as narrow
(FWHM less than +/- 250 km/s) emission lines of H beta and Fe II
lines (multiplets 41, 42, 48 and 49).  The absence of blueshifted
absorption lines and the narrowness of the emission lines suggest
that the object is a symbiotic nova in a slightly progressed state.
IAUC 5961

Guy M Hurst







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