[vsnet-chat 1402] SN 1998eg in UGC 12133

[Hitoshi YAMAOKA <yamaoka@rc.kyushu-u.ac.jp>]

cf. vsnet-chat 1400
http://vsnet.kusastro.kyoto-u.ac.jp/vsnet/Mail/vsnet-chat/msg01400.html
cf. vsnet-chart 111
http://vsnet.kusastro.kyoto-u.ac.jp/vsnet/Mail/vsnet-chart/msg00111.html

Dear SN watchers,

  Successively to SN 1998ef, a supernova has discovered which is
brighter than it is expected from the recession velosity of the host.
According to IAUC 7033, English amateur Tom Boles has discovered a
supernova 1998eg in UGC 12133.  It is located at R.A. = 22h39m30s.26,
Decl. = +8 36'21".3 (2000.0), which is about 26" west and 25" south
from the nucleus of the host edge-on spiral galaxy UGC 12133.  The new
star locates on the thin disk, and the star at the northwest from the
nucleus is a foregroud star.  Spectroscopic confirmation has not been
reported yet.  Note that this galaxy had produced another SN II 1990Z
(about 19 mag). 

The SN 1998eg images are accessable at: 
http://astrowww.phys.uvic.ca/~balam/sn97do.html (D. Balam)
http://ftp.kusastro.kyoto-u.ac.jp/pub/vsnet/SNe/sn1998eg/u12133-1.jpg
(Y. Sano)

Finding chart based on USNO A1.0 are available at:
http://vsnet.kusastro.kyoto-u.ac.jp/vsnet/Mail/vsnet-chart/msg00111.html

  The host galaxy is a further one.  Estimated with its recession
velocity, typical SNeIa on this galaxy would be expected to be 16.7
mag or so on their maximum (vsnet-chat 1400).  However, the early
photometries of this SN, 

  Sept.17     >18
  Oct. 19.896  15.7C  M. Armstrong
  Oct. 19.906  16.0C  T. Boles (discovery image)
  Oct. 20.88   16.4:R S. Benetti et al, La Palma
  Oct. 20.995  15.5C  M. Armstrong
  Oct. 21.25   17.6R  D. Balam
  Oct. 21.385  16.2C  Y. Sano

show already brighter magnitudes than expected.  As same as the
case of SN 1998ef, it can be caused by the error of the distance, but
it is possible that this SN 1998eg is intrinsically bright one, or
something with unknown nature.  I have checked the BATSE trigger, but
no gamma-ray event has detected around this galaxy since September. 
Further magnitude estimates are strongly encouraged. 

Sincerely Yours,
Hitoshi Yamaoka, Kyushu Univ., Japan
yamaoka@rc.kyushu-u.ac.jp

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