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SN2003bh 20030110.52 <207C PAL SN2003bh 20030221.32 199C PAL # SN 2003bh (10:00:06.27, +28:16:52.0 (J2000.0), offset = 7"W, 2"N) is # hosted by an apparent spiral galaxy. The UCB team with the Keck I # telescope revealed that it is type Ia SN, about 1 month after # maximum on Feb. 27. The recession velocity of the host galaxy is # about 26700 km/s. SN2003bi 20030128.52 <204C PAL SN2003bi 20030222.43 196C PAL SN2003bi 20030223.49 196C PAL # SN 2003bi (10:44:05.97, +12:31:34.7 (J2000.0), offset = 2"E, 3"N) is # hosted by MAPS-NGP O_492_0145839, a small disk(?) galaxy. The UCB # team also revealed that it is type Ia SN near maximum on Feb. 28. # The recession velocity of the host galaxy is about 28000 km/s. SN 2003aw: In [vsnet-campaign-dn 3511]:SN2003aw = helium dwarf nova? > According to IAUC No. 8084, "SN2003aw" looks like to be a hydrogen-deficient >dwarf nova resembling KL Dra = SN1998di. The duration of the current bright >state suggests a superoutburst, if this type classification is correct. >Further observations are naturally encouraged! SN 2003aa: In [vsnet-campaign-sn 552] (Feb. 4): > The CfA team has revealed that it is type Ic supernova. The >spectrum taken on Feb. 2.31 resembles that of SN Ic 1994I four days >before maximum. The UCB team suggests that it is rather a subluminous SN Ia. SN 2003bg: In [vsnet-campaign-sn 568] (Feb. 28): >SN2003bg 20021107.0 <180:C CHA >SN2003bg 20030225.7 150:C CHA >SN2003bg 20030226.6 150:C CHA > ># SN 2003bg (4:10:59.42, -31:24:50.3 (J2000.0), offset = 16"W, 24"S) ># is hosted by MCG -05-10-15, a nearby barred-spiral (SB(s)c) galaxy. ># The expected maximum for typical SN Ia is mag about 13.0(!), but ># considering that it has remained constant for one day, it seems not ># in the rapid rising phase. Anyway, further photometry and spectral ># classification is urged. The UCB team suggest that its spectrum resembles to that of peculiar type Ic SN (or type-Ic hypernova) about 2 weeks after explosion! SN 2003bg is quite nearby object (comparable to the Virgo cluster), the followup magnitude estimates and drawing the light curve is encouraged. Sincerely Yours, Hitoshi Yamaoka, Kyushu Univ., Japan yamaoka@rc.kyushu-u.ac.jp
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