Central Bureau for Astronomical Telegrams
IAUC 5240: Var OBJECT IN Oph; N Her 1991
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Circular No. 5240
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
VARIABLE OBJECT IN OPHIUCHUS
R. M. Wagner, Ohio State University and Lowell Observatory,
reports: "Examination of reduced and calibrated high signal-to-noise-
ratio (S/N) spectra obtained on Apr. 15 UT (range 440-690 nm,
resolution 1 nm) indicates that the feature identified as broad H-alpha
absorption in unreduced low-S/N spectra obtained on Apr. 14 (cf.
IAUC 5238) is in fact due to TiO absorption at 620.0 nm. Additional
TiO bands as well as Na D are present. If this object is identical
to that reported on IAUC 5238, then it is likely to be a Mira variable
observed at maximum light. Further spectroscopic confirmation
using the accurate coordinates reported on IAUC 5238 is encouraged."
A. C. Gilmore and P. M. Kilmartin, Mt. John University Observatory,
report that this object does not appear on several photographs,
with approximate limiting magnitudes provided (Mt. John astrographic
plates unless noted otherwise): 1970 Sept. 5, mpg [14 (Vehrenberg's
Atlas Stellarum); 1973 June 7, mv [12 (Papadopoulos' True Visual
Atlas); 1984 Oct. 3, mpg [11; 1985 Sept. 13, mpg [14; 1985 Sept. 15,
mpg [13. They note that this region is sparsely populated, and the
star appears to be superposed on a dust cloud.
NOVA HERCULIS 1991
G. S. Rossano, C. J. Selvey, P. Erwin, and R. J. Rudy, Space
Sciences Laboratory, The Aerospace Corporation, communicate: "
Spectrophotometry from 0.75 to 1.65 microns was obtained with the
University of Minnesota 1.5-m telescope at Mt. Lemmon on Apr. 6.5, 7.5,
and 8.5 UT with spectral resolution of 450, using a 20" beam. The
following broad emission features were observed: Pa-beta, Pa-gamma,
Pa-delta, He I at 1083.0 nm (which was significantly self-absorbed),
and very weak O I at 1128.7 nm. No He II lines were detected. He I
1083.0-nm and Pa-beta line profiles showed evidence of a shell geometry,
with the blue peak stronger than the red. Line widths of 4500
km/s were observed. The continuum was weak at 0.75 micron and rose
toward the red. The continuum emission was nearly constant over the
three days observed with a monochromatic 1.25-micron magnitude of
7.5. The line strengths decreased over the three days observed,
with that at 1083.0 nm declining by a factor of 0.68 and the Paschen
lines by a factor of 0.86."
1991 April 16 (5240) Daniel W. E. Green
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