Optical and near-infrared photometry of 94 type II supernovae from the Carnegie Supernova Project

¹ European Southern Observatory, Alonso de Córdova 3107, Casilla 19, Santiago, Chile
² Carnegie Observatories, Las Campanas Observatory, Casilla 601, La Serena, Chile
³ Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark
⁴ “Fundación Chilena de Astronomía”, El Vergel 2252 #1501, Santiago, Chile
⁵ George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Department of Physics and Astronomy, Texas A&M University, College Station, TX 77843, USA
⁶ Centre for Astrophysics and Gravitation, Instituto Superior Técnico, University of Lisbon, Av. Rovisco Pais 1, 1049-001 Lisbon, Portugal
⁷ Institut d’Estudis Espacials de Catalunya (IEEC), Edifici RDIT, Campus UPC, 08860 Castelldefels (Barcelona), Spain
⁸ Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans, s/n, E-08193 Barcelona, Spain
⁹ The Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101, USA
¹⁰ Department of Physics, Florida State University, Tallahassee, FL 32306, USA
¹¹ Centro de Astronomía (CITEVA), Universidad de Antofagasta, Av. Angamos 601, Antofagasta, Chile
¹² Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA
¹³ Department of Physics, Yale University, 217 Prospect Street, New Haven, CT 06511, USA
¹⁴ Planetary Science Institute, 1700 East Fort Lowell Road, Suite 106, Tucson, AZ 85719-2395, USA
¹⁵ Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, Germany
¹⁶ Homer L. Dodge Department of Physics and Astronomy, University of Oklahoma, Rm 100 440 W. Brooks, Norman, OK 73019-2061, USA
¹⁷ Facultad de Ciencias Astronomicas y Geofisicas, Universidad Nacional de La Plata, Instituto de Astrofisica de La Plata (IALP), CONICET, Paseo del Bosque SN, B1900FWA La Plata, Argentina
¹⁸ Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583, Japan
¹⁹ Observatoire du Mont-Mégantic, Département de Physique, Université de Montréal, Montréal, Canada
²⁰ Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA
²¹ Data and Artificial Intelligence Initiative (D&IA), University of Chile, Santiago, Chile
²² Millennium Institute of Astrophysics (MAS), Nuncio Monseñor Sótero Sanz, Providencia, Santiago, Chile
²³ Center for Mathematical Modeling, University of Chile, AFB170001 Santiago, Chile
²⁴ Departamento de Astronomía, Universidad de Chile, Casilla 36D, Santiago, Chile
²⁵ Institut d’Estudis Espacials de Catalunya (IEEC), Gran Capità, 2-4, Edifici Nexus, Desp. 201, E-08034 Barcelona, Spain
²⁶ DARK, Niels Bohr Institute, University of Copenhagen, Jagtvej 128, 2200 Copenhagen, Denmark
²⁷ The Oskar Klein Centre, Department of Physics, Stockholm University, SE-106 91 Stockholm, Sweden
²⁸ Infrared Processing and Analysis Center, Caltech/Jet Propulsion Laboratory, Pasadena, CA 91125, USA
²⁹ Lawrence Berkeley National Laboratory, Department of Physics, 1 Cyclotron Road, Berkeley, CA 94720, USA
³⁰ The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, SE-10691 Stockholm, Sweden
³¹ School of Mathematical and Physical Sciences, Macquarie University, Sydney, NSW 2109, Australia
³² Astrophysics and Space Technologies Research Centre, Macquarie University, Sydney, NSW 2109, Australia
³³ Cerro Tololo Inter-American Observatory/NSFs NOIRLab, Casilla 603, La Serena, Chile
³⁴ NOIRLab, Avda Juan Cisternas 1500, La Serena, Chile
³⁵ Gemini Observatory/NSF’s NOIRLab, Casilla 603, La Serena, Chile
³⁶ Department of Physics and Astronomy, University of South Carolina, Columbia, SC, 29208, USA

^⋆ Corresponding author; janderso@eso.org

Received: 1 July 2022
Accepted: 30 August 2024

Abstract

Context. Type II supernovae (SNe II) mark the endpoint in the lives of hydrogen-rich massive stars. Their large explosion energies and luminosities allow us to measure distances, metallicities, and star formation rates into the distant Universe. To fully exploit their use in answering different astrophysical problems, high-quality low-redshift data sets are required. Such samples are vital to understand the physics of SNe II, but also to serve as calibrators for distinct – and often lower-quality – samples.

Aims. We present uBgVri optical and YJH near-infrared (NIR) photometry for 94 low-redshift SNe II observed by the Carnegie Supernova Project (CSP). A total of 9817 optical and 1872 NIR photometric data points are released, leading to a sample of high-quality SN II light curves during the first ∼150 days post explosion on a well-calibrated photometric system.

Methods. The sample is presented and its properties are analysed and discussed through comparison to literature events. We also focus on individual SNe II as examples of classically defined subtypes and outlier objects. Making a cut in the plateau decline rate of our sample (s₂), a new subsample of fast-declining SNe II is presented.

Results. The sample has a median redshift of 0.015, with the nearest event at 0.001 and the most distant at 0.07. At optical wavelengths (V), the sample has a median cadence of 4.7 days over the course of a median coverage of 80 days. In the NIR (J), the median cadence is 7.2 days over the course of 59 days. The fast-declining subsample is more luminous than the full sample and shows shorter plateau phases. Of the non-standard SNe II highlighted, SN 2009A particularly stands out with a steeply declining then rising light curve, together with what appears to be two superimposed P-Cygni profiles of Hα in its spectra. We outline the significant utility of these data, and finally provide an outlook of future SN II science.