[vsnet-alert 3611] SNe 1999ej and 1999ek

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

Dear SN watchers,

  LOSS KAIT team has discovered two supernovae in nearby galaxies,
which can reach 15-mag order.  

  First, SN 1999ej was discovered and confirmed on Oct. 18.3 and 19.3
UT, respectingly.  The position of new object is: R.A. = 1h22m57s.38,
Decl. = +33o27'58".0 (2000.0), which is about 18" east and 20" south 
of the nucleus of NGC 495.  In RC3, NGC 495 is classified as SB0-pec,
but on DSS2 image, it seems to be a face-on SBbc galaxy with very
bright nucleus and rather faint arm.  SN 1999ej is overposed on the
outer edge of southeasetern arm.  No confusing foreground star is
there.  

  NGC 495 makes a pair with S0 galaxy NGC 499 which lies about 3'
east.  In their neighbor (about 4' north), there is another SBc galaxy
NGC 496, but it seems not to be a member of NGC 495-499 group, because
of the difference in the recession velocities (delta_v = 2000 km/s).  

  The recession velocity of NGC 495 is about 4000 km/s, from which it
is expected that a normal SN Ia without absorption will reach 15.3 mag
or so in its maximum.  

  Second, SN 1999ek was discovered and confirmed on Oct. 20.5 and 21.4
UT, respectingly.  The coordinate is: R.A. = 5h36m31s.60, Decl. =
+16o38'17".8 (2000.0), which is about 12" west and 12" south of the
nucleus of Sbc galaxy UGC 3329.  Because of low galactic latitude,
there are many foreground stars. Among them, a 15-mag star is there at
5" east and 9" south og the core of UGC 3329.  Careful identification
is needed.

  The recession velocity of this galaxy is about 5000 km/s, which
implies that a typical SN Ia on it will reach 15.8 mag or so.  The
magnitudes in the discovery and confirmation epoch shows that it is in
the rising phase. 

  For these two SNe, further magnitude estimates are encouraged, as
well as spectroscopic confirmation.  The discovery images which can
find at : 
http://astron.berkeley.edu/~bait/1999/sn99ej.html and
http://astron.berkeley.edu/~bait/1999/sn99ek.html 
should be very helpful for identifications.

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

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