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IAUC 7446: 2000cs; 4U 2206+54; SUNGRAZING COMETS

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                                                  Circular No. 7446
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
Phone 617-495-7244/7440/7444 (for emergency use only)

SUPERNOVA 2000cs IN MCG +7-34-15
     T. Puckett, Mountain Town, GA, reports the discovery of an apparent
supernova (mag 17.8) on an unfiltered CCD frame (limiting mag 20.5) taken
with the Puckett Observatory 0.60-m automated supernova patrol telescope
on June 30.25 UT.  The candidate is located at R.A. = 16h23m32s.24, Decl.
= +39o07'29".1 (equinox 2000.0), which is 5".5 west and 11".9 north of the
center of MCG +7-34-15.  The new object was also present on an unfiltered
CCD frame taken by Puckett on July 1.13.  The candidate was also confirmed
by J. Newton, Newton Observatory B & B, Osoyoss, BC, on unfiltered CCD
images taken with a 0.40-m refelctor on July 1.23.  The candidate does
not appear on Palomar Sky Survey images taken on 1993 Apr. 30, 1989 May 31
and 1953 May 19 (limiting mag about 21.0, 21.0 and 20.0, respectively).

4U 2206+54
     R. Corbet, Goddard Space Flight Center (GSFC) and Universities Space
Research Association; R. Remillard, Massachusetts Institute of Technology
(MIT); and A. Peele, University of Melbourne, report on behalf of the RXTE
ASM team at GSFC and MIT: "We have found that the RXTE ASM lightcurve of
the Be star and x-ray source 4U 2206+54 had previously been made using a
position differing by 0.5 deg from the correct location of R.A. =
22h07m57s.0, Decl. = +54o31'06" (equinox 2000.0; Steiner et al. 1984,
Ap.J. 280, 688).  We have now produced and analyzed a revised lightcurve.
The mean source flux is about 5 mCrab, and we find quasisinusoidal
modulation at a period of 9.570 +/- 0.004 days with a semiamplitude of
about 1.5 mCrab.  There was a maximum on 1998 July 12.1 +/- 0.2 UT.  If this
periodicity is due to orbital motion, then it would be one of the shortest
known for a Be-star x-ray source.  However, the relatively low luminosity
(< 10**35 ergs/s at 2.5 kpc) would run counter to the general trend for
short-orbital-period Be/neutron-star systems to have higher luminosities.
Observations at other wavelengths, including optical spectroscopy and
photometry, are encouraged."

     Further to IAUC 7445, it should be noted that comets C/1998 J4 and
C/2000 L4 showed tails, while C/1998 J3 did not.  C/2000 L5 was independently
reported (mag 4-5) to the Central Bureau by A. Mimeev.  The correct
transliteration of the name of the observer of C/2000 M1 is P. Shkreby.

                      (C) Copyright 2000 CBAT
2000 July 1                    (7446)              Brian G. Marsden

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