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IAUC 7887: 2002cp; V4741 Sgr

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                                                  Circular No. 7887
Central Bureau for Astronomical Telegrams
Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions)
URL http://cfa-www.harvard.edu/iau/cbat.html  ISSN 0081-0304
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SUPERNOVA 2002cp IN NGC 3074
     M. Ganeshalingam and W. D. Li, University of California at
Berkeley, report the LOTOSS (cf. IAUC 7514) discovery of an
apparent supernova on unfiltered CCD images taken with the 0.8-m
Katzman Automatic Imaging Telescope (KAIT) on Apr. 28.2 (mag about
17.9) and 30.2 UT (mag about 17.7).  SN 2002cp is located at R.A. =
9h59m35s.95, Decl. = +35o23'57".4 (equinox 2000.0), which is 64".1
west and 23".2 north of the nucleus of NGC 3074.  KAIT images taken
on Apr. 11.2 (limiting mag about 18.0) and Apr. 3.2 (limiting mag
about 19.0) showed nothing at this position.

     E. Gosset, Institut d'Astrophysique, Liege, writes that a
high-resolution spectrum (range 380-900 nm; resolution 48000) of
V4741 Sgr, acquired on Apr. 19.4 UT using the European Southern
Observatory 1.5-m telescope (+ FEROS) at La Silla, shows the
following full widths at zero intensity (FWZI) and at half-maximum
(FWHM) for the lower Balmer lines:  H-alpha, FWZI = 4100 km/s, FWHM
= 2800 km/s; H-beta, FWZI = 3850 km/s; H-gamma, FWZI = 3800 km/s.
H-beta and the upper members of the series are comparatively faint,
suggesting marked reddening (cf. IAUC 7879).  The interstellar
absorption lines related to the Na resonance doublet exhibit a
rather complex structure that can be partitioned into three
families.  The first one is composed of a broad, damped line at
about -2 km/s, blended with a narrow line at about -30 km/s.  The
second family is composed of a narrow line at about -107 km/s with
a faint line in the blue wing.  The third family is made of three
partly blended lines at about -143, -150, and -160 km/s.  A fourth
family at about -190 km/s could possibly be present.  The first
three families are also visible, with less resolution, in the Ca**+
H and K doublet.  Gosset adds:  "The existence of features up to
such velocities is interesting.  If these lines were considered as
being due to interstellar material showing galactic rotation, we
could conclude that the object is situated at a distance quite
comparable to that of the Galactic center or even beyond, in good
agreement with the reported reddening.  However, high-velocity
shells are known to exist in the Carina region.  The first family
component at -2 km/s is also detected for K, CH, and CH**+."
     Visual magnitude estimates:  Apr. 16.606 UT, 9.8 (A. Pearce,
Nedlands, W. Australia); 18.134, 10.3 (R. Y. Shida, Sao Paulo,
Brazil); 18.776, 10.6 (Pearce); 19.755, 10.7 (Pearce).

                      (C) Copyright 2002 CBAT
2002 April 30                  (7887)            Daniel W. E. Green

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