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IAUC 6941: Poss. N IN Oph; 1998 KY_{26; C/1997 J2

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                                                 Circular No. 6941
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
Phone 617-495-7244/7440/7444 (for emergency use only)

     S. Nakano, Sugano, Japan, reports the discovery of a possible
nova (mag 9.5) by Kesao Takamizawa, Saku-machi, Nagano-ken, which
was found on two T-Max 400 films (each exposure about 4.5 min)
taken on June 15.561 UT with a 0.10-m f/4.0 lens.  Takamizawa
reports the position of the possible nova as R.A. = 17h32m00s.0,
Decl. = -19o13'56" (equinox 2000.0).  No star is present at this
location on 48 previous patrol films taken by Takamizawa between
1994 Feb. 17 and 1998 May 19.  R. and Y. Kushida report the
following position end figures for the variable star from a poor
CCD image obtained on June 16.531, when they estimated V = 10.0:
31m59s.82, 57".0 (uncertainty stated as 1" or more; average of
three frames).  There is a red USNO A1.0 star (B = 18.0, R = 16.8)
at position end figures 59s.79, 55".0.  T. Kato, Kyoto University,
notes that the possible nova lies within the 16" error circle of the
ROSAT source 1RXS 173200.0-191349.

1998 KY_{26
     P. Pravec and L. Sarounova, Ondrejov Observatory, report: "Our
photometric observations of this Apollo-type object from Ondrejov
during June 1.977-2.040 and 2.875-3.037 UT revealed a synodic
period of 10.702 +/- 0.003 min; periods other than half-integer
multiples of this period are apparently ruled out.  The lightcurve
has most of its signal in the second harmonic (i.e., it shows two
maxima/minima pairs per period), and the peak-to-peak amplitude is
0.3 mag.  We interpret the period as being the rotation period of
the asteroid.  This result is in agreement with the radar
observations by Ostro et al. (IAUC 6935).  This rotation period
indicates that the object is a monolithic body.  A body composed of
pieces held together by self-gravitation only (the so-called
'rubble pile' structure; cf. Harris 1996, Lunar Planet. Sci. 27,
493) would require an unrealistic bulk density of more than 340
g/cm**3.  Our composite lightcurve is presented at

     Visual m_1 estimates:  May 1.04 UT, 11.0 (M. Meyer,
Frauenstein, Germany, 0.25-m reflector); 18.00, 11.4 (R. J. Bouma,
Groningen, The Netherlands, 0.25-m reflector); June 3.98, 10.7 (M.
Reszelski, Szamotuly, Poland, 0.25-m refl.); 13.89, 11.2 (A.
Baransky, Kiev, Ukraine, 0.20-m reflector).

                      (C) Copyright 1998 CBAT
1998 June 17                   (6941)            Daniel W. E. Green

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