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IAUC 8710: 2006cf; V2575 Oph, V2576 Oph,, V2362 Cyg; RS Oph

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                                                  Circular No. 8710
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)
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SUPERNOVA 2006cf IN UGC 6015
     N. Ponticello and J. Burket report the LOSS discovery (cf.
IAUC 8709), on KAIT images taken on May 11.26 and 12.25 UT, of an
apparent supernova (mag about 18) located at R.A. = 10h54m02s.58,
Decl. = +46o01'36".3 (equinox 2000.0), which is 0".2 east and 4".5
south of the nucleus of UGC 6015.  An independent discovery of
2006cf at mag 17.3 has been reported by T. Puckett and D. Toth on
CCD images taken with a 0.60-m reflector at Ellijay, GA, on May
13.12 (cf. IAUC 8709).  Additional unfiltered CCD magnitudes:  Jan.
26, [19.5 (Puckett); Apr. 30.27, [19.0 (KAIT); May 14.19, 17.2 (A.
Sehgal, 0.50-m reflector, Osoyoos, BC).  Puckett provides position
end figures 02s.65, 36".7 for 2006cf.


V2575 OPHIUCHI, V2576 OPHIUCHI, AND V2362 CYGNI
     R. W. Russell, R. J. Rudy, and D. K. Lynch, The Aerospace
Corporation; and C. E. Woodward, University of Minnesota, report
0.8- to 5.4-micron spectroscopy of these three novae on April 30 UT
using SpeX on the Infrared Telescope Facility (IRTF).  All three
objects are similar Fe II-type CO novae, with very low excitation.
They showed strong C I, NI, O I, and Fe II emission lines.  V2575
Oph showed self-absorption in the He I lines at 1.0830 and 2.0581
microns, and the other two objects showed P-Cyg structure in the
same lines.  No CO emission was detected, and there was no
discernable thermal emission from dust.  E(B-V) values:  V2576 Oph,
0.62; V2575 Oph, 1.42; V2362 Cyg, 0.59.  Infrared magnitudes (+/-
0.1) for V2576 Oph:  J = 9.3, H = 9.3, K(short) = 9.2.  Infrared
magnitudes for V2575 Oph:  J = 9.8, H = 9.9, K(short) = 9.0.
Infrared magnitudes for V2362 Cyg: J = 8.4, H = 8.5, K(short) = 8.2.


RS OPHIUCHI
     Rudy, Lynch, Russell, and Woodward also report 0.8- to 5.4-
micron spectroscopy of RS Oph on May 1 UT using SpeX on the IRTF.
The infrared spectrum of RS Oph is a peculiar blend of very low and
very-high-excitation emission lines.  Features of N I, O I, and Fe
II exist together with some of the highest excitation coronal
features seen in the infrared spectra of novae.  Coronal lines of
[Fe XIII], [Si VI], [Si VII], [Si X], [S VIII], [S IX], and [S XI]
are present in the near-infrared; [Mg VIII] and [Si IX] are
prominent in the mid-wavelength infrared.  The hydrogen line
spectrum is very rich, displaying many features from the Pashcen,
Brackett, Pfund, and Humphreys series.  There is no evidence of
thermal emission from dust.

                      (C) Copyright 2006 CBAT
2006 May 14                    (8710)            Daniel W. E. Green

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