Circular No. 5381
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
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
MARSDEN or GREEN@CFA.BITNET    MARSDEN or GREEN@CFAPS2.SPAN
 
 
NOVA OPHIUCHI 1991 No. 2
     R. H. McNaught, Anglo-Australian Observatory, reports the dis-
covery of another nova by Paul Camilleri, Cobram, Victoria.  The no-
va was found on a photo taken Apr. 11, but not until that photo was
used for a comparison on Oct. 28.  Photovisual magnitudes estimated
by Camilleri from his T-Max 400 exposures with a 135-mm lens are as
follows:  1991 Mar. 22.65 UT, [12.5; Apr. 11.60, 9.3; Apr. 16.54,
10.5; Apr. 21.58, 11.0; May 17.45, 11.0: (image may be of a nearby
star); July 11, [12.  Measures by McNaught of an Apr. 11 negative
give the following position:  R.A. = 17h40m07s.44, Decl. =
-20 05'43".1 (equinox 1950.0, uncertainty 4" in each coordinate; co-
matic images).  B, V, R, and I CCD images, taken on Nov. 8.4 by A.
E. Samuel and R. H. McNaught with the 1.0-m reflector at Siding
Spring, confirm the nova at V about 16.5 and show it to be increas-
ingly bright towards the blue and substantially bluer than surround-
ing field stars.  Coordinates measured by McNaught from the R and I
images give end figures 07s.44, 35".0 (uncertainty 0".4 in each co-
ordinate).  No image appears at this position on the SERC J, R, and
I, nor on the ESO B and R, survey films.
 
 
GX 1+4
     R. K. Sood, S. D. James, Australian Defence Force Academy,
Canberra; D. P. Sharma, K. Hill, University of Tasmania, Hobart;
G. Stringfellow, Mt. Stromlo Observatory, Canberra; and R. K.
Manchanda, Tata Institute, Bombay, telex:  "Spectroscopic studies of
the optical counterpart of the binary x-ray pulsar GX 1+4 were car-
ried out on July 2 and 3, at a resolution of 15 nm, when the x-ray
source was in a high intensity state.  Strong emission at the previ-
ously undetected lines of O I (844.6 nm) and Ca II (849.8 nm) was
seen.  The He II (468.6 nm) emission feature was also detected.  No
significant signal was seen in the forbidden transitions of Fe VII
or Fe X.  There was evidence for the Na doublet at 818.3 and 819.5
nm in absorption.  Further observations are planned."
 
 
V1017 SAGITTARII
     Visual magnitude estimates by D. York, Abiquiu, NM (cf. IAUC
5375):  Oct. 19.07 UT, 11.9; 20.07, 11.6; 22.07, 11.5; 23.07, 11.5;
26.07, 11.5; Nov. 2.06, 11.2; 5.07, 11.0; 6.05, 11.0; 7.06, 11.0.
 
 
1991 November 8                                   Daniel W. E. Green