Central Bureau for Astronomical Telegrams
IAUC 5006: V3890 Sgr; Poss. N IN Sgr; WX Cet
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Read IAUC 5007
Circular No. 5006
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
V3890 SAGITTARII
R. M. Wagner and R. Bertram, Ohio State University; and S. G.
Starrfield, Arizona State University, report: "Optical spectra
obtained of V3890 Sgr on May 2.38 UT, using the OSU CCD spectrograph
(range 597.5-713.0 nm, resolution 0.2 nm) on the Perkins 1.8-m
telescope at the Lowell Observatory, show strong and broad emission
lines of H-alpha, He I (667.8, 706.5 nm), and numerous weaker
features. [Fe VII] at 608.5 nm is present. He I at 706.5 nm exhibits
a weak P-Cyg profile. The FWHM and FWZI of H-alpha emission are
2140 and 8600 km/s, respectively. The interstellar line at 628.4 nm
is present with an equivalent width of about 0.1 nm. The spectrum
is very similar to that of the recurrent nova V745 Sco (IAUC 4822,
4825, 4826) early in its 1989 outburst. A spectrum of V3890 Sgr in
quiescence is presented by Williams (1983, Ap.J. Suppl. 53, 523)."
POSSIBLE NOVA IN SAGITTARIUS
T. Harrison, Mount Stromlo Observatory, reports infrared photometry
of this object (cf. IAUC 4974, 4978), obtained with the Infrared
Photometry System on the 2.3-m reflector at Siding Spring: Mar.
9.7 UT, J = 10.13 +/- 0.02, H = 9.87 +/- 0.04, K = 9.24 +/- 0.03;
Mar. 10.7, 10.36 +/- 0.02, 10.04 +/- 0.02, 9.48 +/- 0.02; Mar. 13.7,
11.78 +/- 0.04, 11.39 +/- 0.02, 10.91 +/- 0.02, L = 9.97 +/- 0.10.
The photometry shows an energy distribution characteristic of free-
free emission.
R. H. McNaught, Siding Spring Observatory, reports that an
Uppsala Schmidt film exposed on Mar. 24.67 UT shows that the star
had then faded to mag about 14. Spectroscopic observations are
still needed to clarify whether or not this is a nova.
WX CETI
D. O'Donoghue, Astronomy Department, University of Cape Town,
writes: "High-speed photometry of WX Cet during its 1989 June outburst
(IAUC 4792, 4793, 4796) reveals superhumps with a period of 76
min, but with uncertainty of a few minutes due to aliasing. Any
other time-resolved photometry during this outburst could resolve
this ambiguity and establish WX Cet as the shortest-period hydrogen-
rich cataclysmic variable, and I would appreciate being contacted
concerning any relevant data (FAX 27-21-650-3726)."
1990 May 4 (5006) Daniel W. E. Green
Read IAUC 5007
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