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IAUC 6777: N IN NGC 205; SMC X-3; 1997dp

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                                                 Circular No. 6777
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions)
BMARSDEN@CFA.HARVARD.EDU or DGREEN@CFA.HARVARD.EDU (science)
URL http://cfa-www.harvard.edu/iau/cbat.html
Phone 617-495-7244/7440/7444 (for emergency use only)


NOVA IN NGC 205
     Q. Y. Qiao, Y. L. Qiu, J. Y. Hu, and W. D. Li, Beijing
Astronomical Observatory (BAO); A. Esamdin, Urumqi Astronomical
Station; and Y. Zhang, Beijing Normal University, report their
discovery of a nova in NGC 205 on Nov. 21.54 UT, in the course of
the BAO supernova survey, using the 0.6-m reflector at Xinglong
Station.  The nova is at R.A. = 0h40m23s.26, Decl. = +41o43'27".0
(equinox 2000.0), which is 13".2 east and 139".9 north of the
nucleus of NGC 205.  Unfiltered CCD magnitudes:  Nov. 21.54, 18.8;
22.50, 18.4; 23.44, 18.5.  The nova was not present on a CCD image
taken on Nov. 4.  A low-resolution spectrogram of the nova was
obtained with the 2.16-m telescope at Xinglong on Nov. 23.4 by J.
Y. Wei, L. Cao (BAO), and Q. S. Gu (Nanjing University); the
spectrum shows typical features of a nova after maximum.  The
Balmer emission lines are very strong (equivalent width of H-beta
is -142.4 km/s).  There are also strong Fe II emission lines
(492.4, 451.5, 458.4, 516.9, 527.6, 532.6, and 590.1 nm), He I
emission lines (492.2 and 501.6 nm), and O I emission lines (615.8
and 777.6 nm).  The emission lines show blueshift with a velocity
of 224 km/s, which is similar to that of NGC 205.  The V magnitude
derived from the flux at 550.0 nm continuum is 18.1, yielding an
absolute V magnitude of -6.6 (24.7 adopted as the distance modulus
of NGC 205).


SMC X-3
     F. E. Marshall, Goddard Space Flight Center (GSFC); and J. C.
Lochner and T. Takeshima, GSFC and Universities Space Research
Association, report the detection with the RXTE PCA of an outburst
from the x-ray transient SMC X-3 and the discovery of a period of
92 +/- 1.5 s with a complex pulse profile:  "First detected on Nov.
15.44 UT with a 2-10-keV flux of 1.5 mCrab, the source flux had
increased to about 4 mCrab by Nov. 25.44.   Further RXTE
observations are planned, and observations of the suggested optical
counterpart are encouraged."


SUPERNOVA 1997dp IN NGC 969
     Unfiltered CCD magnitude estimate of SN 1997dp by S. Moretti
and S. Tomaselli, Forli, Italy:  Nov. 3.89 UT, 17.9 (GSC reference
stars).

                      (C) Copyright 1997 CBAT
1997 November 26               (6777)            Daniel W. E. Green

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