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IAUC 8292: 2004aa; C/2002 T7; (1313); 2004 DW

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IAUC number

                                                  Circular No. 8292
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 617-495-7440/7244/7444 (for emergency use only)

     Further to IAUC 8276, A. Udalski reports the OGLE-III
discovery of an apparent supernova located at R.A. = 4h34h02s.90,
Decl. = -67o54'11".7 (equinox 2000.0), which is 1".0 west of the
center of the apparent host galaxy.  Approximate I-band OGLE-III-
survey magnitudes for SN 2004aa:  Feb. 14.0 UT, [22; 16.0, 20.2;
18.0, 19.6; 20.0, 19.1; 22.0, 18.7.

     W. J. Altenhoff, F. Bertoldi, and K. Menten, Max-Planck-
Institut fuer Radioastronomie, Bonn; and C. Thum, Institut de
Radio-Astronomie Millimetrique (IRAM), Granada, report the
detection of 250-GHz continuum emission from comet C/2002 T7 with
the MAMBO bolometer array at the IRAM 30-m telescope, yielding the
following flux densities:  Feb. 13.636 UT, S = 6.5 +/- 1.1 mJy/beam;
16.697, 8.0 +/- 1.3.  These photometric observations with a beam of
11" register emission at the level of 1 mJy also in neighboring
channels, suggesting that full-width-at-half-maximum emission
extends to a distance of about 20".  Around the time of the comet's
closest approach to the earth in May, the flux density per beam is
expected to increase by a factor 10, and the total flux density by
> 100.

(1313) BERNA
     R. Behrend, Geneva Observatory, writes (on behalf of R. Roy,
S. Sposetti, N. Waelchli, D. Pray, N. Berger, C. Demeautis, D.
Matter, R. Durkee, A. Klotz, D. Starkey, and V. Cotrez) that
photometric observations obtained of the minor planet (1313) on
eight nights during Feb. 6-16 show a lightcurve of amplitude 0.25
mag and suggest that this is a binary system with an orbital period
of 1.061 +/- 0.005 days, showing mutual eclipses and/or
occultations near both rotational lightcurve minima with a duration
of about 0.09 day and depth about 0.7 mag, the first being centered
on Feb. 7.85 UT.  The regular-appearing lightcurve is synchronized
with the eclipse events, indicating that at least one of the two
bodies is elongated and rotates synchronously with the orbital
motion; the sharp eclipse/occultation events indicate that both
components have approximately the same size.  The maximum orbital
separation observed from earth would be about 0".03.

2004 DW
     Corrigendum.  On IAUC 8291, line 5, FOR  albedo  READ
phase-function slope

                      (C) Copyright 2004 CBAT
2004 February 23               (8292)            Daniel W. E. Green

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