We present an analysis of the diversity of V-band light-curves of hydrogen-rich type II supernovae. Analyzing a sample of 116 supernovae, several magnitude measurements are defined, together with decline rates at different epochs, and time durations of different phases. It is found that magnitudes measured at maximum light correlate more strongly with decline rates than those measured at other epochs: brighter supernovae at maximum generally have faster declining light-curves at all epochs. We find a relation between the decline rate during the 'plateau' phase and peak magnitudes, which has a dispersion of 0.56 mag, offering the prospect of using type II supernovae as purely photometric distance indicators. Our analysis suggests that the type II population spans a continuum from low-luminosity events which have flat light-curves during the 'plateau' stage, through to the brightest events which decline much faster. A large range in optically thick phase durations is observed, implying a range in progenitor envelope masses at the epoch of explosion. During the radioactive tails, we find many supernovae with faster declining light-curves than expected from full trapping of radioactive emission, implying low mass ejecta. It is suggested that the main driver of light-curve diversity is the extent of hydrogen envelopesmore » retained before explosion. Finally, a new classification scheme is introduced where hydrogen-rich events are typed as simply 'SN II' with an 's {sub 2}' value giving the decline rate during the 'plateau' phase, indicating its morphological type.« less

https://iopscience.iop.org/article/10.1088/0004-637X/786/1/67/pdf

Characterizing the V-band light-curves of hydrogen-rich type II supernovae

We present a compilation of UBV RIz light curves of 51 type II supernovae discovered during the course of four different surveys during 1986 to 2003: the Cerro Tololo Supernova Survey, the Calan/Tololo Supernova Program (C&T), the Supernova Optical and Infrared Survey (SOIRS), and the Carnegie Type II Supernova Survey (CATS). The photometry is based on template-subtracted images to eliminate any potential host galaxy light contamination, and calibrated from foreground stars. This work presents these photometric data, studies the color evolution using different bands, and explores the relation between the magnitude at maximum brightness and the brightness decline parameter (s) from maximum light through the end of the recombination phase. This parameter is found to be shallower for redder bands and appears to have the best correlation in the B band. In addition, it also correlates with the plateau duration, being thus shorter (longer) for larger (smaller) s values.

/pdf/ubvriz-light-curves-of-51-type-ii-supernovae-595iziqrjw.pdf

UBVRIz Light Curves of 51 Type II Supernovae

Author(s): Galbany, L; Hamuy, M; Phillips, MM; Suntzeff, NB; Maza, J; Jaeger, TD; Moraga, T; Gonzalez-Gaitan, S; Krisciunas, K; Morrell, NI; Thomas-Osip, J; Krzeminski, W; Gonzalez, L; Antezana, R; Wishnjewski, M; McCarthy, P; Anderson, JP; Gutierrez, CP; Stritzinger, M; Folatelli, G; Anguita, C; Galaz, G; Green, EM; Impey, C; Kim, YC; Kirhakos, S; Malkan, MA; Mulchaey, JS; Phillips, AC; Pizzella, A; Prosser, CF; Schmidt, BP; Schommer, RA; Sherry, W; Strolger, LG; Wells, LA; Williger, GM | Abstract: We present a compilation of UBVRIz light curves of 51 type II supernovae discovered during the course of four different surveys during 1986-2003: the Cerro Tololo Supernova Survey, the Calan/Tololo Supernova Program (CaT), the Supernova Optical and Infrared Survey (SOIRS), and the Carnegie Type II Supernova Survey (CATS). The photometry is based on template-subtracted images to eliminate any potential host galaxy light contamination, and calibrated from foreground stars. This work presents these photometric data, studies the color evolution using different bands, and explores the relation between the magnitude at maximum brightness and the brightness decline parameter (s) from maximum light through the end of the recombination phase. This parameter is found to be shallower for redder bands and appears to have the best correlation in the B band. In addition, it also correlates with the plateau duration, being shorter (longer) for larger (smaller) s values.

/pdf/ubvriz-light-curves-of-51-type-ii-supernovae-3werkxu1ip.pdf

W. Li

Papers

Supernovae 2003cj, 2003ck, 2003cl, 2003cm, 2003cn

Supernovae 2002ev, 2002ew, 2002ex, 2002ey