[IAUC] IAUC 8936: 2005 NB_7; V2468 Cyg; V459 Vul [25139-2008/05-R1]

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                                                  Circular No. 8936
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
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2005 NB_7
     M. K. Shepard, Bloomsburg University of Pennsylvania; M. C.
Nolan, National Astronomy and Ionosphere Center; L. A. M. Benner,
J. D. Giorgini, and S. J. Ostro, Jet Propulsion Laboratory, and C.
Magri, University of Maine at Farmington, report:  "Arecibo delay-
Doppler images (2380 MHz, 12.6 cm) obtained on Apr. 11-12 show that
the Apollo-type object 2005 NB_7 (e.g., MPECs 2005-N32, 2005-T82,
2008-F18; MPO 135910) is a binary system.  Preliminary estimates of
average diameters, based on range estimates at 7.5-m resolution,
are 0.5 and 0.2 km (+/- 0.1) km.  The rotation period of the
primary has not been determined, but based on the estimated
diameter and observed bandwidth is >/= 2.5 h.  The semi-major axis
of the relative orbit is >/= 0.6 km; the system orbital period is
not known."


V2468 CYGNI
     R. J. Rudy, R. W. Russell, and D. K. Lynch, The Aerospace
Corporation; and C. E. Woodward, University of Minnesota, report on
SpeX observations (wavelength range 0.8-2.5 microns) made with the
Infrared Telescope Facility (IRTF) on Mar. 13 and Apr. 12 UT:  "The
object continues to display a very rich emission-line spectrum.
Although features of C I, N I, O I, and Fe II still persist, the Ca
II infrared triplet, which was very strong in March, is nearly
undetectable in the April spectrum.  The He I lines are now quite
strong, and He II features are beginning to emerge.  The O I lines
indicate a reddening of E(B-V) = 0.77.  There is no indication yet
of dust formation."


V459 VULPECULAE
     R. W. Russell, D. K. Lynch, R. J. Rudy, The Aerospace
Corporation; and C. E. Woodward, University of Minnesota, report on
IRTF SpeX observations, obtained as above on Apr. 12.62 UT:  "V459
Vul is one of the small number of classical novae to display C I
and coronal lines simultaneously.  Of the latter, [S IX] at 1.25
microns is the highest-excitation and [Si VI] at 1.96 microns is
the strongest.  He II lines and the unidentified novae lines are
present as well.  The O I lines, which are still quite strong,
indicate a reddening of E(B-V) = 1.0, some of which is probably
local to the nova since the spectrum exhibits thermal emission from
dust beyond 1.5 microns."

                      (C) Copyright 2008 CBAT
2008 April 17                  (8936)            Daniel W. E. Green