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@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions) CBAT@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. NOTE: These 'Central Bureau Electronic Telegrams' are sometimes superseded by text appearing later in the printed IAU Circulars. (C) Copyright 2009 CBAT 2009 November 16 (CBET 2020) Daniel W. E. Green