Type II supernovae from the Carnegie Supernova Project-I

I. Bolometric light curves of 74 SNe II using uBgVriYJH photometry

¹ Instituto de Astrofísica de La Plata (IALP), CCT-CONICET-UNLP. Paseo del Bosque s/n, B1900FWA, La Plata, Argentina
e-mail: laureano@carina.fcaglp.unlp.edu.ar
² Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque s/n, B1900FWA La Plata, Argentina
³ Universidad Nacional de Río Negro. Sede Andina, Mitre 630, 8400 Bariloche, Argentina
⁴ Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583, Japan
⁵ European Southern Observatory, Alonso de Córdova 3107, Casilla 19, Santiago, Chile
⁶ Vice President and Head of Mission of AURA-O in Chile, Avda. Presidente Riesco 5335 Suite 507, Santiago, Chile
⁷ Hagler Institute for Advanced Studies, Texas A&M University, College Station, TX 77843, USA
⁸ CENTRA-Centro de Astrofísica e Gravitaçäo and Departamento de Física, Instituto Superio Técnico, Universidade de Lisboa, Avenida Rovisco Pais, 1049-001 Lisboa, Portugal
⁹ Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, 8000 Aarhus C, Denmark
¹⁰ Carnegie Observatories, Las Campanas Observatory, Casilla 601, La Serena, Chile
¹¹ Finnish Centre for Astronomy with ESO (FINCA), 20014 University of Turku, Finland
¹² Tuorla Observatory, Department of Physics and Astronomy, 20014 University of Turku, Finland
¹³ Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101, USA
¹⁴ Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA
¹⁵ Department of Astronomy, University of California, 501 Campbell Hall, Berkeley, CA 94720-3411, USA
¹⁶ Data and Artificial Intelligence Initiative, Faculty of Physical and Mathematical Sciences, University of Chile, Santiago, Chile
¹⁷ Centre for Mathematical Modelling, Faculty of Physical and Mathematical Sciences, University of Chile, Santiago, Chile
¹⁸ Millennium Institute of Astrophysics, Santiago, Chile
¹⁹ Department of Astronomy, Faculty of Physical and Mathematical Sciences, University of Chile, Santiago, Chile
²⁰ Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans, s/n, 08193 Barcelona, Spain
²¹ Department of Physics, Florida State University, 77 Chieftan Way, Tallahassee, FL 32306, USA
²² Consejo Nacional de Investigaciones Científicas y Tećnicas (CONICET), Argentina
²³ 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

Received: 23 August 2021
Accepted: 25 October 2021

Abstract

The present study is the first of a series of three papers where we characterise the type II supernovae (SNe II) from the Carnegie Supernova Project-I to understand their diversity in terms of progenitor and explosion properties. In this first paper, we present bolometric light curves of 74 SNe II. We outline our methodology to calculate the bolometric luminosity, which consists of the integration of the observed fluxes in numerous photometric bands (uBgVriYJH) and black-body (BB) extrapolations to account for the unobserved flux at shorter and longer wavelengths. BB fits were performed using all available broadband data except when line blanketing effects appeared. Photometric bands bluer than r that are affected by line blanketing were removed from the fit, which makes near-infrared (NIR) observations highly important to estimate reliable BB extrapolations to the infrared. BB fits without NIR data produce notably different bolometric light curves, and therefore different estimates of SN II progenitor and explosion properties when data are modelled. We present two methods to address the absence of NIR observations: (a) colour-colour relationships from which NIR magnitudes can be estimated using optical colours, and (b) new prescriptions for bolometric corrections as a function of observed SN II colours. Using our 74 SN II bolometric light curves, we provide a full characterisation of their properties based on several observed parameters. We measured magnitudes at different epochs, as well as durations and decline rates of different phases of the evolution. An analysis of the light-curve parameter distributions was performed, finding a wide range and a continuous sequence of observed parameters which is consistent with previous analyses using optical light curves.