Stephen Shectman and Ian Thompson, Carnegie Observatories, report that
a spectrum (range 370-540 nm) of SN 2002gw, obtained on Oct. 24.25 UT with
Las Campanas Clay 6.5-m telescope (+ B&C spectrograph), shows it to be a
type-II supernova with prominent Balmer lines exhibiting P-Cyg profiles.
The absorption component of the H-alpha line yields an expansion
velocity of 9300 km/s, based on a redshift of 3100 km/s derived from
the narrow Balmer emission lines of the host galaxy.


Mario Hamuy, Carnegie Observatories, reports that a spectrum (range 360-900 nm)
of SN 2002ha, obtained on Oct. 25.03 UT with the Las Campanas Baade 6.5-m
telescope (+ LDSS2), shows it to be a type-Ia supernova about 3 days
before maximum light, very similar to SN 1994D. A narrow interstellar
Na I D absorption line at the redshift of the host galaxy can be seen
with an equivalent width of 1 angstrom.

A spectrum of SN 2002gy obtained with the same instrument on Oct. 25.21
bears resemblance to the type-Ib/c SN 1999ex. A prominent
absorption at rest wavelength 6140 angstroms can be seen, which could be
due to Si II 6355 or high velocity H alpha. A narrow interstellar
Na I D absorption line at the redshift of the host galaxy is present
with an equivalent width of 3.2 angstrom, which suggests significant
reddening. 


A spectrum of the LOTOSS SN in NGC 2559 obtained with the same instrument
on Oct. 25.34 reveals that this is a Type II supernova. A broad  H alpha
line is seen in emission with no significant absorption counterpart. The
spectrum is very similar to that of the linear SN 1979C 43 days past
maximum  (Filippenko, A. 1997, ARAA, 35, 309).