[IAUC] IAUC 9099: V496 Sct; S/2009 (317) 1 [25139-2010/01-R1]

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                                                  Circular No. 9099
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
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V496 SCUTI
     R. J. Rudy and T. R. Prater, The Aerospace Corporation; R. C.
Puetter, University of California at San Diego; and R. B. Perry,
NASA, report 0.9- to 2.5-micron spectroscopy of V496 Sct (cf. IAUCs
9093, 9097) on Nov. 27.08 UT using the Aerospace Corporation's Near-
Infrared Imaging Spectrograph on the 3-m Shane reflector at Lick
Observatory.  The nova displays very strong emission from the first
overtone of carbon monoxide; this is a rare and extremely short-
lived feature in novae and occurs just before dust formation.  The
nova also displays several C I lines that are among the brightest
emission lines in the spectrum.  The strongest of these display P-
Cyg profiles, behavior not observed previously in novae.  Very
strong C I emission in early novae spectra is a common occurrence
in novae that form dust.  The authors believe that dust formation
in V496 Sct is almost certain and that there is a good probability
that it will occur within the next week.  K. Baker helped in
acquiring the measurements.


S/2009 (317) 1
     W. J. Merline, Southwest Research Institute (SwRI); P. M.
Tamblyn, Binary Astronomy, Dillon, CO, U.S.A., and SwRI; J. D.
Drummond, Starfire Optical Range, Air Force Research Laboratory;
J. C. Christou, Gemini Observatory; A. R. Conrad, W. M. Keck
Observatory; B. Carry, Observatoire de Paris; C. R. Chapman, SwRI;
C. Dumas, European Southern Observatory (Chile); D. D. Durda, SwRI;
W. M. Owen, Jet Propulsion Laboratory; and B. L. Enke, SwRI, report
the discovery on Nov. 24.4 UT of a satellite of minor planet (317)
Roxane from K_p-band imaging using the 8-m Gemini-North telescope
(+ Altair/NIRI adaptive-optics system).  On Nov. 24.39992, the
satellite was at separation 0".27 (projected separation 245 km) and
position angle 76 deg.  The satellite was imaged in K_p-, H-, and
J-bands and was tracked for more than 26 hours.  The brightness
difference in the K_p band is about 2.7 mag, giving an estimated
diameter (primary diameter assumed of 19 km) of the satellite of 5
km.  This binary has characteristics that are very similar to the
other wide binaries previously reported by the authors (see IAUCs
7827, 8075, 8232, 8293, 8297), all being consistent with the EEB
formation mechanism of Durda et al. (2004, Icarus 170, 243).  Among
binaries that can be resolved by imaging, this appears to be the
first of type E.  Given the recent detection of dual lightcurve
periods in (1509) Esclangona (CBET 2020), it is possible that
separate spin periods could be extracted from lightcurve data of
(317).

                      (C) Copyright 2009 CBAT
2009 December 1                (9099)            Daniel W. E. Green