THE SPECTROSCOPIC DIVERSITY OF TYPE Ia SUPERNOVAE*

摘要

We present 2603 spectra of 462 nearby Type Ia supernovae (SNe?Ia), including 2065 previously unpublished spectra, obtained during 1993-2008 through the Center for Astrophysics Supernova Program. There are on average eight spectra for each of the 313 SNe?Ia with at least two spectra. Most of the spectra were obtained with the FAST spectrograph at the Fred Lawrence Whipple Observatory 1.5?m telescope and reduced in a consistent manner, making this data set well suited for studies of SN?Ia spectroscopic diversity. Using additional data from the literature, we study the spectroscopic and photometric properties of SNe?Ia as a function of spectroscopic class using the classification schemes of Branch et al. and Wang et al. The width-luminosity relation appears to be steeper for SNe?Ia with broader lines, although the result is not statistically significant with the present sample. Based on the evolution of the characteristic Si II?λ6355 line, we propose improved methods for measuring velocity gradients, revealing a larger range than previously suspected, from ~0 to ~400 km s?1 day?1 considering the instantaneous velocity decline rate at maximum light. We find a weaker and less significant correlation between Si II velocity and intrinsic B – V color at maximum light than reported by Foley et al., owing to a more comprehensive treatment of uncertainties and host galaxy dust. We study the extent of nuclear burning and the presence of unburnt carbon in the outermost layers of the ejecta and report new detections of C II?λ6580 in 23 early-time SN?Ia spectra. The frequency of C II detections is not higher in SNe?Ia with bluer colors or narrower light curves, in conflict with the recent results of Thomas et al. Based on nebular spectra of 27 SNe?Ia, we find no relation between the FWHM of the iron emission feature at ~4700 ? and Δm 15(B) after removing the two low-luminosity SN?1986G and SN?1991bg, suggesting that the peak luminosity is not strongly dependent on the kinetic energy of the explosion for most SNe?Ia. Finally, we confirm the correlation of velocity shifts in some nebular lines with the intrinsic B – V color of SNe?Ia at maximum light, although several outliers suggest a possible non-monotonic behavior for the largest blueshifts.