LOSS Photometry of 93 SNe Ia 1 Lick Observatory Supernova Search Follow-Up Program: Photometry Data Release of 93 Type Ia Supernovae Benjamin E. Stahl,1;2?y WeiKang Zheng,1 Thomas de Jaeger,1z Alexei V. Filippenko,1;3 Andrew Bigley,1 Kyle Blanchard,1 Peter K. Blanchard,4 Thomas G. Brink,1 Samantha K. Cargill,1 Chadwick Casper,1 Sanyum Channa,1 Byung Yun Choi,1 Nick Choksi,1 Jason Chu,5 Kelsey I. Clubb,1 Daniel P. Cohen,6 Michael Ellison,1 Edward Falcon,1 Pegah Fazeli,1 Kiera Fuller,1;6 Mohan Ganeshalingam,7 Elinor L. Gates,8 Carolina Gould,1 Goni Halevi,1;9 Kevin T. Hayakawa,8 Julia Hestenes,1 Benjamin T. Jeffers,1 Niels Joubert,10 Michael T. Kandrashoff,1 Minkyu Kim,1 Haejung Kim,1 Michelle E. Kislak,1;11 Io Kleiser,12 Jason J. Kong,1 Maxime de Kouchkovsky,1 Daniel Krishnan,1 Sahana Kumar,1;13 Joel Leja,4 Erin J. Leonard,1;14 Gary Z. Li,15 Weidong Li,1x Philip Lu,2;6 Michelle N. Mason,16 Jeffrey Molloy,1 Kenia Pina,1 Jacob Rex,1 Timothy W. Ross,1 Samantha Stegman,1 Kevin Tang,1 Patrick Thrasher,1 Xianggao Wang,17 Andrew Wilkins,1 Heechan Yuk,18 Sameen Yunus,1 and Keto Zhang1 1Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA 2Department of Physics, University of California, Berkeley, CA 94720-7300, USA 3Miller Senior Fellow, Miller Institute for Basic Research in Science, University of California, Berkeley, CA 94720, USA 4Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 5Gemini Observatory, 670 N. Aohoku Place, Hilo, HI, USA 6Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA 7Lawrence Berkeley National Laboratory, 1 Cyclotron Rd, Berkeley, CA 94720, USA 8Lick Observatory, P.O. Box 85, Mount Hamilton, CA 95140, USA 9 Department of Astrophysical Sciences, Princeton University, 4 Ivy Lane, Princeton, NJ 08544, USA 10Department of Computer Science, Stanford University, 353 Serra Mall, Stanford, CA 94305, USA 11Netflix, Inc., 100 Winchester Cir, Los Gatos, CA 95032, USA 12NASA Jet Propulsion Laboratory, 4800 Oak Grove Dr, Pasadena, CA 91109, USA 13Department of Physics, Florida State University, Tallahassee, FL 32306, USA 14Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, 90025, USA 15Department of Mechanical and Aerospace Engineering, University of California, Los Angeles, 90025, USA 16Department of Physics and Astronomy, University of Wyoming, 1000 E. University, Dept 3905, Laramie, WY 82071, USA 17Department of Physics, Guangxi University, Nanning 530004, China 18Department of Physics and Astronomy, University of Oklahoma, 440 W. Brooks St., Norman, OK 73019, USA arXiv:1909.11140v1 [astro-ph.SR] 24 Sep 2019 Accepted XXX. Received YYY; in original form ZZZ MNRAS 000,1{30 (2019) MNRAS 000,1{30 (2019) Preprint 26 September 2019 Compiled using MNRAS LATEX style file v3.0 ABSTRACT We present BVRI and unfiltered light curves of 93 Type Ia supernovae (SNe Ia) from the Lick Observatory Supernova Search (LOSS) follow-up program conducted between 2005 and 2018. Our sample consists of 78 spectroscopically normal SNe Ia, with the remainder divided between distinct subclasses (three SN 1991bg-like, three SN 1991T-like, four SNe Iax, two peculiar, and three super-Chandrasekhar events), and has a median redshift of 0.0192. The SNe in our sample have a median coverage of 16 photometric epochs at a cadence of 5.4 days, and the median first observed epoch is ∼ 4:6 days before maximum B-band light. We describe how the SNe in our sample are discovered, observed, and processed, and we compare the results from our newly developed automated photometry pipeline to those from the previous processing pipeline used by LOSS. After investigating potential biases, we derive a final systematic uncertainty of 0.03 mag in BVRI for our dataset. We perform an analysis of our light curves with particular focus on using template fitting to measure the parameters that are useful in standardising SNe Ia as distance indicators. All of the data are available to the community, and we encourage future studies to incorporate our light curves in their analyses. Key words: galaxies: distances and redshifts { supernovae: general { super- novae: individual (SN 2005hk, SN 2005ki, SN 2006ev, SN 2006mq, SN 2007F, SN 2007bd, SN 2007bm, SN 2007fb, SN 2007fs, SN 2007if, SN 2007jg, SN 2007kk, SN 2008Y, SN 2008dh, SN 2008ds, SN 2008eg, SN 2008ek, SN 2008eo, SN 2008eq, SN 2008fk, SN 2008fu, SN 2008gg, SN 2008gl, SN 2008go, SN 2008gp, SN 2008ha, SN 2008hs, SN 2009D, SN 2009al, SN 2009an, SN 2009dc, SN 2009ee, SN 2009eq, SN 2009eu, SN 2009fv, SN 2009hn, SN 2009hp, SN 2009hs, SN 2009ig, SN 2009kq, SN 2010ao, SN 2010hs, SN 2010ii, SN 2010ju, SN 2011M, SN 2011bd, SN 2011by, SN 2011df, SN 2011dl, SN 2011dz, SN 2011ek, SN 2011fe, SN 2011fs, SN 2012E, SN 2012Z, SN 2012bh, SN 2012cg, SN 2012dn, SN 2012ea, SN 2012gl, SN 2013bs, SN 2013dh, SN 2013dr, SN 2013dy, SN 2013ex, SN 2013fa, SN 2013fw, SN 2013gh, SN 2013gq, SN 2013gy, SN 2014J, SN 2014ai, SN 2014ao, SN 2014bj, SN 2014dt, SN 2015N, SN 2016aew, SN 2016coj, SN 2016fbk, SN 2016ffh, SN 2016gcl, SN 2016gdt, SN 2016hvl, SN 2017cfd, SN 2017drh, SN 2017dws, SN 2017erp, SN 2017fgc, SN 2017glx, SN 2017hbi, SN 2018aoz, SN 2018dem, SN 2018gv) 1 INTRODUCTION become immensely valuable as cosmological distance indica- tors. Indeed, observations of nearby and distant SNe Ia led Type Ia supernovae (SNe Ia) are objects of tremendous in- to the discovery of the accelerating expansion of the Uni- trigue and consequence in astronomy. As individual events, verse and dark energy (Riess et al. 1998; Perlmutter et al. SNe Ia | especially those at the extremes of what has 1999), and they continue to provide precise measurements been previously observed (e.g., Filippenko et al. 1992a,b; of the Hubble constant (Riess et al. 2016, 2019). Foley et al. 2013) | present interesting case studies of high- energy, transient phenomena. Collectively, SNe Ia are prized The aforementioned light-curve\width-luminosity"rela- as \cosmic lighthouses" with luminosities of several billion tions form the basis for the use of SNe Ia as cosmological dis- ∗ Suns, only a factor of 2{3 lower than an L host galaxy tance indicators. To further refine these relationships as well 10 of ∼ 10 L . The temporal evolution of the luminosity of as understand their limitations, extensive datasets of high- a SN Ia, which is powered largely by the radioactive de- precision light curves are required. At low redshift, multiple 56 56 56 cay chain Ni ! Co ! Fe, is codified by light curves groups have answered the call, including the Cal´an/Tololo (typically in several broadband filters). With some variation Supernova Survey with BVRI light curves of 29 SNe Ia between filters, a SN Ia light curve peaks at a value de- (Hamuy et al. 1996), the Harvard-Smithsonian Center for 56 termined primarily by the mass of Ni produced and then Astrophysics (CfA) Supernova Group with > 300 multiband declines at a rate influenced by its spectroscopic/colour evo- light curves spread over four data releases (Riess et al. 1999; lution (Kasen, & Woosley 2007). With the advent of empir- Jha et al. 2006; Hicken et al. 2009a, 2012, henceforth CfA1- ical relationships between observables (specifically, the rate 4, respectively), the Carnegie Supernova Project (CSP) with of decline) and peak luminosity (e.g., Phillips 1993; Riess et > 100 multiband light curves (Contreras et al. 2010; Fo- al. 1996; Jha et al. 2007; Zheng et al. 2018), SNe Ia have latelli et al. 2010; Stritzinger et al. 2011; Krisciunas et al. 2017, henceforth CSP1, CSP1a, CSP2, and CSP3, respec- tively), and our own Lick Observatory Supernova Search ? E-mail: benjamin [email protected] y Marc J. Staley Graduate Fellow (LOSS) follow-up program with BVRI light curves of 165 z Bengier Postdoctoral Fellow SNe Ia (Ganeshalingam et al. 2010, henceforth G10). More x Deceased 2011 December 12 recently, the Foundation Supernova Survey has published © 2019 The Authors LOSS Photometry of 93 SNe Ia 3 its first data release of 225 low redshift SN Ia light curves Electronic Telegrams (CBETs) and the International Astro- derived from Pan-STARRS photometry (Foley et al. 2018). nomical Union Circulars (IAUCs). Whenever possible and Despite these extensive campaigns, there exist many more needed, we spectroscopically classify and monitor newly dis- well-observed light curves for high redshift (z & 0:1) SNe Ia covered SNe Ia with the Kast double spectrograph (Miller & than for those at low redshift (Betoule et al. 2014). As Stone 1993) on the 3 m Shane telescope at Lick Observatory. low-redshift SNe Ia are used to calibrate their high-redshift Discovery and classification references are provided for each counterparts, a larger low-redshift sample will be useful for SN in our sample in Table A1. further improving width-luminosity relations, gauging sys- While the focus in this paper is on SNe Ia, we have tematic errors arising from the conversion of instrumental also built up a collection of images containing SNe II and magnitudes to a uniform photometric system, and for inves- SNe Ib/c (see Filippenko 1997, for a discussion of SN spec- tigating evolutionary effects over large timescales. troscopic classification). These additional datasets have been The LOSS follow-up program has been in continuous processed by our automated photometry pipeline and will be operation for over 20 years. The result is an extensive made publicly available pending analyses (T. de Jaeger et database of SN Ia photometry from images obtained with al. 2019, in prep., & W. Zheng et al. 2019, in prep.; for the the 0.76 m Katzman Automatic Imaging Telescope (KAIT) SN II and SN Ib/c datasets, respectively).