Central Bureau for Astronomical Telegrams
IAUC 8998: 1998 WV_24; V2468 Cyg; V2670 Oph
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Circular No. 8998
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Mailstop 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 ISSN 0081-0304
Phone 617-495-7440/7244/7444 (for emergency use only)
1998 WV_24
S. D. Benecchi, K. S. Noll, and E. A. Barker, Space Telescope
Science Institute; W. M. Grundy, Lowell Observatory; and H. F.
Levison, Southwest Research Institute, report that the
transneptunian object 1998 WV_24 (cf. MPECs 1998-X12 and 1999-V06)
is a binary. The observations were made during 2007 Aug. 27.1069-
27.1375 UT with the Planetary Camera of the Wide Field Planetary
Camera 2 on the Hubble Space Telescope, using the F606W filter
(wide V) with one 260-s exposure at four dithered positions on the
detector. The two components were separated by an angular distance
of 0".051 +/- 0".002, with the secondary fainter by 0.3 magnitude.
The secondary was located at 0".033 +/- 0".003 in R.A. and 0".039
+/- 0".003 in Decl. relative to the primary. Component centroids
were determined by fitting the point-spread function.
V2468 CYGNI
D. K. Lynch, R. W. Russell, and R. J. Rudy, The Aerospace
Corporation; M. Sitko, Space Science Institute; and C. E. Woodward,
University of Minnesota, report 0.8- to 5.5-micron spectroscopy of
the nova V2468 Cyg (cf. IAUC 8927, 8928, 8936) on Oct. 4 UT using
the Infrared Telescope Facility (+ Spex). Though V2468 Cyg had
faded by more than a factor of two since mid-August, the coronal
lines have strengthened significantly. The [Si VI] line at 1.96
microns is among the strongest of the emission features. Lines of
[S VIII], [S IX], [Al IX], and [Ca VIII] are also present. Several
Rydberg lines are present, including those at 0.89, 1.19, 1.11,
1.55, and 2.1 microns.
V2670 OPHIUCHI
M. Sitko, Space Science Institute; D. K. Lynch, R. W. Russell,
and R. J. Rudy, The Aerospace Corporation; and C. E. Woodward,
University of Minnesota, report 0.8- to 5.5-micron spectroscopy of
the nova V2670 Oph (cf. IAUC 88947, 8948, 8949, 8956) on Oct. 4 UT
using the Infrared Telescope Facility (+ Spex). The spectrum
remains low in excitation, still displaying emission lines of Fe II,
N I, and O I. However, the C I lines that were strong in mid-June
are barely detectable, and the He I 1.083-micron line is now the
strongest feature in the infrared spectrum. The broad components
of the emission lines have disappeared entirely. This nova has not
formed dust and is unlikely to do so at this late stage.
(C) Copyright 2008 CBAT
2008 October 29 (8998) Daniel W. E. Green
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