Electronic Telegram No. 1073
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)
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(45) EUGENIA
     J. Berthier and P. Descamps, Institut de Mecanique Celeste et de Calcul
des Ephemerides, Paris; and F. Marchis and M. Baek, Carl Sagan Center, SETI
institute, communicate predictions for occultations by (45) Eugenia and its
satellite (45) Eugenia I (Petit-Prince; cf. IAUCs 7129, 7503) on 2007 Oct.
18.81, 2007 Dec. 20.09, and 2008 Mar. 9.23 UT and visible in Ukraine/Russia/
Kazakhstan/China/Indonesia, Angola/Atlantic Ocean/northern Brazil/Peru, and
California/northern Mexico/Pacific Ocean/Indonesia, respectively.  The 2008
Mar. 9 occultation involves the 6th-magnitude star HR 1585 = HD 31539.
The orbital model employed was refined with recent obervations recorded on
2007 Sept. 9.596 at the W. M. Keck telescope (and its AO system) by I. de
Pater (University of California, Berkeley), H. Hammel (Space Science
Institute), and M. Showalter (Carl Sagan Center at SETI); the Keck images
showed the satellite at a distance of 0".50 from the primary in p.a. 32 deg.
The paths of the occultation of the primary and the secondaries will be
regularly updated based on additional data at the following website URL:
http://www.imcce.fr/page.php?nav=en/ephemerides/phenomenes/occult/
stellarocc.php?query=predoc.  The orbital model of the second satellite,
S/2004 (45) 1 (cf. IAUC 8817), is not well constrained yet.  Berthier et al.
encourage observations of the stellar occultations involving Petit-Prince to
constrain its size and shape.


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                         (C) Copyright 2007 CBAT
2007 September 19                (CBET 1073)              Daniel W. E. Green