期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 490, 期 3, 页码 3882-3907出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stz2742
关键词
supernovae: general; galaxies: distances and redshifts
资金
- NSF
- Richard and Rhoda Goldman Fund
- TABASGO Foundation
- Christopher R. Redlich Fund
- Miller Institute for Basic Research in Science (U.C. Berkeley)
- National Natural Science Foundation of China (NSFC) [11673006]
- Guangxi Science Foundation [2016GXNSFFA380006, 2017AD22006]
- NASA [NNX08AR22G]
- National Science Foundation [AST-1238877]
- Alfred P. Sloan Foundation
- U.S. Department of Energy
- Japanese Monbukagakusho
- Max Planck Society
- University of Chicago
- Fermilab
- Institute for Advanced Study
- Japan Participation Group
- Johns Hopkins University
- Los Alamos National Laboratory
- Max Planck Institute for Astronomy
- Max Planck Institute for Astrophysics
- New Mexico State University
- University of Pittsburgh
- Planck Institute for Astrophysics
- Princeton University
- United States Naval Observatory
- University of Washington
- NASA [95405, NNX08AR22G] Funding Source: Federal RePORTER
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 (3 SN 1991bg-like, 3 SN 1991T-like, 4 SNe Iax, 2 peculiar, and 3 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 d, and the median first observed epoch is similar to 4.6 d 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 data set. We perform an analysis of our light curves with particular focus on using template fitting tomeasure the parameters that are useful in standardizing 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.
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