Central Bureau for Astronomical Telegrams
IAUC 4788: N LMC 1988 No. 2; N Vul 1987
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Circular No. 4788
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 IN THE LARGE MAGELLANIC CLOUD 1988 No. 2
R. Gonzalez-Riestra and A. Cassatella, IUE ESA Observatory,
Madrid, report: "Nova LMC 1988-2 was observed by the International
Ultraviolet Explorer on May 21.00 UT (range 120-195 nm) and 25.00
(195-335 nm). The image in the long-wavelength range indicates the
existence of two stars within the large entrance aperture (10" x 20")
of the spectrograph at an approximate distance of 4".4 along the
direction perpendicular to the dispersion. The level of the continuum
is very similar in the two spectra. One spectrum shows a strong Mg II
absorption feature at 280 nm with an equivalent width of 1 nm, while
the other shows emissions at 264.3 and 279.2 nm that therefore
refer to the nova. The spectrum at the shorter wavelength
perpendicular to the dispersion is wider than expected from a point
source, and the position of the emission lines is slightly displaced
with respect to the continuum. However, the spatial resolution in the
short-wavelength range is not sufficient to separate the two stars.
After correction for the presence of the contaminating star, the
fluxes at 144 nm and 300 nm are 2 and 1 x 10**-15 erg cm-2 s-1 A-1,
respectively, values that are fainter by a factor of about 6-7 than
was shown by previous IUE observations on 1988 Dec. 29. The strongest
lines in the short-wavelength range are N V 124.0 nm, N IV] 148.6 nm
and an unidentified feature at 158.4 nm. The intensities of the N V
and N IV] lines have decreased by about the same amount as the
continuum, contrary to the Mg II + [Mg V] blend around 280 nm, which
has decreased by a factor of at least 200."
NOVA VULPECULAE 1987
R. D. Gehrz, University of Minnesota, provides the following
infrared photometry, obtained with the 2.3-m Wyoming telescope on
May 27.5 UT: 3.6 microns, 8.7 +/- 0.3; 4.9 microns, 7.5 +/- 0.4;
7.8 microns, 4.5 +/- 0.4; 8.7 microns, 3.7 +/- 0.3; 9.8 microns,
3.1 +/- 0.3; 10 (7-14) microns, 3.5; 10.3 microns, 3.1 +/- 0.2;
11.6 microns, 3.0 +/- 0.3; 12.5 microns, 3.0 +/- 0.2; 18.5
microns, 2.0 +/- 0.3. These imply a continuum of about 420 K,
with possible silicate emission features at 10 and 20 microns.
Visual magnitude estimates: Mar. 23.17 UT, 13.4 (A. Boattini,
Florence, Italy); 28.12, 13.4 (Boattini); Apr. 30.07, 13.8 (P. Schmeer,
Bischmisheim, West Germany); May 4.09, 13.7 (S. Korth, Dusseldorf, West
Germany); 9.06, 13.4 (Boattini); 15.10, 13.9 (M. Verdenet, Bourbon-
Lancy, France); 17.10, 13.9 (Verdenet); 26.01, 13.9 (Schmeer).
1989 June 2 (4788) Brian G. Marsden
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