The Lick Observatory Supernova Search follow-up program: photometry data release of 70 stripped-envelope supernovae

TL;DR

This paper presents a comprehensive photometric dataset of 70 stripped-envelope supernovae from the Lick Observatory, including detailed light curves, data processing methods, and new insights into their physical properties.

Contribution

It provides the first large-scale, publicly available photometric dataset of SESNe with detailed analysis, including rise times and physical parameter estimates.

Findings

SNe Ic have lower ejecta masses and velocities than SNe Ib and IIb.

Produced accurate rise-time measurements for a large SESNe sample.

Derived host-galaxy extinction values using empirical color evolution.

Abstract

We present BVRI and unfiltered Clear light curves of 70 stripped-envelope supernovae (SESNe), observed between 2003 and 2020, from the Lick Observatory Supernova Search (LOSS) follow-up program. Our SESN sample consists of 19 spectroscopically normal SNe~Ib, two peculiar SNe Ib, six SN Ibn, 14 normal SNe Ic, one peculiar SN Ic, ten SNe Ic-BL, 15 SNe IIb, one ambiguous SN IIb/Ib/c, and two superluminous SNe. Our follow-up photometry has (on a per-SN basis) a mean coverage of 81 photometric points (median of 58 points) and a mean cadence of 3.6d (median of 1.2d). From our full sample, a subset of 38 SNe have pre-maximum coverage in at least one passband, allowing for the peak brightness of each SN in this subset to be quantitatively determined. We describe our data collection and processing techniques, with emphasis toward our automated photometry pipeline, from which we derive publicly available data products to enable and encourage further study by the community. Using these data products, we derive host-galaxy extinction values through the empirical colour evolution relationship and, for the first time, produce accurate rise-time measurements for a large sample of SESNe in both optical and infrared passbands. By modeling multiband light curves, we find that SNe Ic tend to have lower ejecta masses and lower ejecta velocities than SNe~Ib and IIb, but higher $^{56}$Ni masses.