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IAUC 7988: 2002gb; 2001ig, 2002eg, 2002ew, 2002gc; V4743 Sgr

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IAUC number

                                                  Circular No. 7988
Central Bureau for Astronomical Telegrams
Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions)
URL http://cfa-www.harvard.edu/iau/cbat.html  ISSN 0081-0304
Phone 617-495-7440/7244/7444 (for emergency use only)

     M. Hamuy, Carnegie Observatories, reports that a spectrum
(range 380-920 nm) of SN 2002gb (cf. IAUC 7983), obtained on Oct. 8
UT with the Las Campanas Dupont 2.5-m telescope (+ WFCCD), bears
resemblance to the type-Ia SN 1994D, 20 days past maximum, from
which a redshift of approximately 0.074 is derived.
     A. V. Filippenko and R. Chornock, University of California,
Berkeley, also write that CCD spectra (range 310-930 nm) obtained
on Oct. 8 UT with the Keck-I 10-m telescope (+ Low Resolution
Imaging Spectrometer) reveal that SN 2002gb is of type Ia, about 1
month past maximum brightness.  The redshift of the host galaxy,
measured from the narrow (H II region) H-alpha emission line, is

SUPERNOVAE 2001ig, 2002eg, 2002ew, 2002gc
     Filippenko and Chornock add that CCD spectra, obtained as
above on Oct. 8 UT, reveal that SN 2002gc (IAUC 7983) is of type
Ia, but with spectral peculiarities that resemble those of SN
2002eu (IAUC 7965):  the relative strengths of the Ti II/Si II
580-nm and Si II 615-nm features are similar to those of SN 1991bg,
but it lacks the strong Ti II 420-nm absorption characteristic of
SN 1991bg-like objects.  SN 2002eg (IAUC 7944) is of type IIb, as
previously reported (IAUC 7952); He I absorption lines are now
easily visible.  SN 2002ew (IAUC 7964) is of type II, as had been
suspected, but it exhibits some spectral peculiarities, such as
substantial O I 777.4-nm absorption and strong H-alpha emission
(with essentially no absorption).  SN 2001ig (IAUC 7772) has
transformed itself into a type-Ib/c supernova in the nebular phase,
as had been predicted (IAUC 7793).  The [O I] and [Ca II] emission
lines are very prominent, and Mg I] 457.1-nm is the strongest
(relative to [O I] 630-nm) seen thus far in any supernova,
exceeding even its strength in SN 2002ap (Leonard et al. 2002,

     R. J. Ivison, Royal Observatory, Edinburgh, on behalf of the
James Clerk Maxwell Telescope nova-monitoring group, reports the
detection of V4743 Sgr with the SCUBA submillimeter camera.  The
flux density measured on Oct. 3.1 UT in good conditions was 39 +/-
4 mJy at 0.85 mm, with an upper limit of 225 mJy at 0.45 mm.  Very
Large Array observations are planned for Oct. 11, with a flux
density of equal to or greater than 0.05 mJy expected at 3.6 cm.

                      (C) Copyright 2002 CBAT
2002 October 8                 (7988)            Daniel W. E. Green

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