Central Bureau for Astronomical Telegrams
IAUC 3736: N Sgr 1982; NGC 2346
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Read IAUC 3737
Circular No. 3736
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
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
NOVA SAGITTARII 1982
H. Drechsel, J. Rahe and W. Wargau, Remeis Observatory, Bamberg;
and J. C. Blades, C. Cacciari and W. Wamsteker, European Space Agency,
Villafranca, report that low-dispersion spectra in the range 120-300
nm were obtained using IUE during Oct. 18.64-18.75 UT. From the
interstellar 220-nm feature the reddening was estimated to be
compatible with E(B-V) ~0.3 +/- 0.1. The continuum flux decreases
steeply between 170 and 160 nm toward zero level at shorter wavelengths,
while it increases toward the optical range: it also exhibits a hump
between ~170 and 220 nm, which might be due to the blending of numerous
strong emission lines. The line spectrum consists of a wealth of
strong emission and absorption lines of mainly unidentified transitions.
Mg II (280 nm) appears as a pronounced P-Cyg-type feature, with a
terminal velocity of the order of 3000 km/s. The fine-error-sensor
520-nm magnitude was 9.2 +/- 0.1.
Precise positions (equinox 1950.0) have been reported for
this object as follows: R.A. = 18h31m32s46, Decl. = -26deg28'25".2
(J. Churms, South African Astronomical Observatory); end figures
32.95, 25.1 (M. Honda and H. Kosai, Kurashiki and Tokyo); 32.7, 25
(A. C. Gilmore and P. M. Kilmartin, Mt. John Observatory); 33.1,
25 (Drechsel et al., IUE).
Churms also communicates the following photoelectric magnitudes
(~V) by J. Hers, Sedgefield, South Africa: Oct. 14.85 UT,
8.00; 16.80, 8.48; 17.80, 8.41.
NGC 2346
W. A. Feibelman, Laboratory for Astronomy and Solar Physics,
Goddard Space Flight Center: and L. H. Aller, Astronomy Department,
University of California at Los Angeles, have determined an
orbital period for the eclipsing-binary nucleus of the bipolar
planetary nebula NGC 2346. Assuming a primary minimum on 1982
Feb. 10.35 UT (Kohoutek 1982, Inf. Bull. Variable Stars No. 2113)
and utilizing five observations made with the IUE fine-error sensor
between Feb. 24 and Sept. 5, when no ground-based observations
were possible, they derived an orbital period of 16.0 days (uncertainty
+0.00, -0.04 day) with a range of 1.8 in V. This agrees
with the radial-velocity period determined by Mendez but differs
from the photometric period of 17.2 days suggested by Kohoutek.
1982 October 20 (3736) Brian G. Marsden
Read IAUC 3737
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