[IAUC] CBET 2020: 20091116 : (1509) ESCLANGONA

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                                                  Electronic Telegram No. 2020
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
M.S. 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
IAUSUBS en CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions)
CBAT en CFA.HARVARD.EDU (science)
URL http://www.cfa.harvard.edu/iau/cbat.html


(1509) ESCLANGONA
     B. D. Warner, Palmer Divide Observatory and Space Science Institute,
Colorado Springs, CO; P. Pravec and P. Kusnirak, Ondrejov Observatory; A.
W. Harris, Space Science Institute, La Canada, CA; R. Durkee, Shed of
Science Observatory, Minneapolis, MN; R. D. Stephens, Goat Mountain Research
Station, Landers, CA; M. Husarik and M. Pikler, Skalnate Pleso Observatory; F.
Marchis and A. E. Reiss, SETI Institute and University of California at
Berkeley; J. Vilagi, S. Gajdos, and L. Kornos, Modra Observatory; W. Cooney,
J. Gross, and D. Terrell, Sonoita Research Observatory, Sonoita, AZ; and F.
Vachier, Institut de Mecanique Celeste et de Calcul des Ephemerides,
Observatoire de Paris, report that photometric observations of minor planet
(1509) obtained during Sept. 9-Oct. 27 reveal two distinct periods:
3.25285 +/- 0.00002 and 6.6423 +/- 0.0003 hr.  The lightcurve components
associated with two periods are linearly additive and have amplitudes of
0.13 and 0.04 mag, respectively.  It appears likely that these two lightcurve
components are due to the rotations of the primary and secondary, respectively,
of the wide binary reported in 2003 by Merline et al. (IAUC 8075).  The
separation of the two objects observed by Merline et al. is so large that
catching mutual events (occultations and/or eclipses) is unlikely.  Previous
CCD observations (Warner 2005, Minor Planet Bull. 32, 54-58) did not show any
indications of a secondary period or mutual events.


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                         (C) Copyright 2009 CBAT
2009 November 16                 (CBET 2020)              Daniel W. E. Green