2004IAUC.8453....3F

Further to IAUC 8452, A. V. Filippenko and R. J. Foley write that inspection of CCD Keck I spectra, also obtained on Dec. 12 UT, shows that SN 2004gd (IAUC 8443) is of type IIn, strongly resembling SN 1985G (Pastorello et al. 2002, MNRAS 333, 27). Prominent, relatively narrow (FWHM 1000 km/s) hydrogen-Balmer emission lines are superposed on broader bases and exhibit narrow P-Cyg absorption components with minima displaced by about 700 km/s from the emission-line cores. Similar absorption features are seen in the Fe II multiplets and other lines; they are probably produced by a dense circumstellar shell. SN 2004ge (IAUC 8443) is of type Ic, shortly after maximum brightness; the shape of its continuum argues that it is heavily reddened, and the equivalent width of the narrow interstellar Na I D absorption line at 589 nm is about 0.2 nm. SN 2004gf (IAUC 8444) is of type II, probably within a few weeks past explosion, based on the blue continuum; the H_alpha line is vastly dominated by the emission component (FWHM = 2200 km/s), although all other lines (Balmer, Fe II, O I, Ca II) show more typical P-Cyg profiles. SN 2004gl (IAUC 8446) is of type Ia, three weeks past maximum brightness; the redshift of the host galaxy, measured from narrow emission lines in the nucleus, is 0.0393.