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IAUC 5905: N Cas 1993; PSR 1706-44

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                                                  Circular No. 5905
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)


NOVA CASSIOPEIAE 1993
     B. Schmidt, Harvard-Smithsonian Center for Astrophysics,
reports that a spectrogram (range 380-900 nm) taken on Dec. 13.3 UT
with the Multiple Mirror Telescope confirms that this object (cf.
IAUC 5902, 5904) is indeed an iron-rich nova.  H-alpha and H-beta
are very strong in emission; H-gamma is also seen.  A multitude of
lines exist, the strongest ones including those at 589.3 nm (Na I
D); 777.3 and 844.6 nm (O I); 850.0 and 854.6 nm (Ca II); and many
Fe II lines (442.0, 458.9, 463.2, 467.1, 473.4, 492.4, 501.8,
516.9, 519.7, 523.7, 527.8, 531.8, 536.6, 616.1, and 625.0 nm).
     Photoelectric photometry:  Dec. 12.70 UT, V = 6.39 +/- 0.02,
B-V = +0.98 +/- 0.0 (H. Mikuz, Ljubljana, Slovenia; comparison star
HR 9010); 13.1, V = 6.461, b-y (Stromgren) = +0.557 (B. Skiff,
Lowell Observatory; based on V = 6.246 and b-y = +0.630 for HR 8985,
and on V = 7.213, b-y = +0.112 for HD 222514).
     Visual magnitude estimates:  Dec. 13.70 UT, 6.4 (L. Kiss,
Szeged, Hungary); 14.25, 6.4 (G. M. Hurst, Basingstoke, U.K.).


PSR 1706-44
     T. Kifune, N. Hayashida, T. Tamura, and M. Teshima, Institute
of Cosmic Ray Research, University of Tokyo; T. Tanimori, S. Ogio,
F. Kakimoto, T. Tsukagoshi, and T. Yoshikoshi, Department of
Physics, Tokyo Institute of Technology; Y. Matsubara and Y. Muraki,
Solar and Terrestrial Environmental Laboratory, Nagoya University;
Y. Mizumoto and T. Suda, Department of Physics, Kobe University; T.
Hara, Yuge National College of Maritime Technology; H. Fujii, S.
Kabe, and Y. Watase, National Laboratory for High Energy Physics
(KEK), Japan; M. Fujimoto, National Astronomical Observatory,
Japan; and P. G. Edwards, J. R. Patterson, G. P. Rowell, M. D.
Roberts, and G. J. Thornton, Department of Physics, University of
Adelaide, communicate:  "Photons of energy 1 TeV have been detected
from the Gamma Ray Observatory source PSR 1706-44.  Observations
were made using the 3.8-m imaging telescope of Project CANGAROO
which is located at Woomera, South Australia.  After cuts, a clear
peak was seen in the alpha distribution (see Punch et al. 1992,
Nature 358, 477).  The signal was seen in July and August 1992 and
1993 with a combined significance as large as 10 sigma.  The excess
corresponds to a constant flux of about 10E-11 cmE-2 sE-1 above the
1-TeV telescope threshold."


1993 December 14               (5905)            Daniel W. E. Green

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