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IAUC 5659: EU 1902+20 AND EU 2017-01; 1992t; N LMC 1992

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                                                  Circular No. 5659
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@CFA or GREEN@CFA (.SPAN, .BITNET or .HARVARD.EDU)


EU 1902+20 AND EU 2017-01
     S. Brandt, A. J. Castro-Tirado, and N. Lund, Danish Space
Research Institute, communicate:  "Two new x-ray transients, located
at R.A. = 19h02m, Decl. = +20.0 and R.A. = 20h17m, Decl. = -1.0
(equinox 1950.0; estimated error radius 1 deg), have been discovered
with the WATCH wide-field monitor on the European Space Agency's
EURECA satellite.  The new transients were detected in data
from Nov. 22, but both appear at a lower level of significance
already on Nov. 21.  EU 2017-01 has a hard spectrum, whereas EU
1902+20 has only been detected between 6 and 8 keV, the flux from
both sources being of the order 100 mCrab.  Follow-up at other
wavelengths is encouraged."


PERIODIC COMET SWIFT-TUTTLE (1992t)
     J. Davies, Royal Observatory, Edinburgh, reports:  "A 3.2- to
3.6-micron spectrogram of P/Swift-Tuttle was taken at the U.K.
Infrared Telescope on Nov. 13.15 UT by S. Lumsden on behalf of Davies,
M. Mumma, S. Hoban, H. Weaver, and collaborators.  Preliminary
reduction of the spectrum shows a broad emission feature between 3.3
and 3.45 microns.  There may be substructure within this feature,
most notably appearing as a local peak near 3.427 microns.  There
is a broad emission feature centered at 3.52 microns, with no evidence
of an emission feature at 3.28 microns.  Detailed modeling of
fluorescence from methanol produces a spectrum that explains all of
the flux from 3.3 to 3.4 microns, and also that of the 3.52-micron
feature.  Excess flux is seen from 3.4 to 3.48 microns, probably
due to another species.  The 3.52-micron feature (which we attribute
to methanol) has a flux of 8 x 10E-16 W mE-2 summed over an
area 3".1 x 6".2, implying a methanol production rate of 1.5 x
10E28 molecules sE-1.  The flux in the 3.3- to 3.45-micron region
is about 6 x 10E-15 W mE-2 in excess of the underlying continuum.
The underlying continuum has a flux of 1.15 x 10E-13 W mE-2 micronE-1
near 3.25 microns, rising to 1.4 x 10E-13 near 3.58 microns."


NOVA IN THE LARGE MAGELLANIC CLOUD 1992
     Photometry by A. C. Gilmore with the 0.6-m f/14 Cassegrain
reflector at Mt. John University Observatory:  Nov. 21.58 UT, V =
12.32 +/- 0.06, U-B = -0.86 +/- 0.07, B-V = +0.09 +/- 0.06, V-R =
+0.73 +/- 0.07; Nov. 22.48, 12.39 +/- 0.02, -0.74 +/- 0.02, +0.05
+/- 0.01, +0.74 +/- 0.01.


1992 November 23               (5659)            Daniel W. E. Green

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