Supernova rates and luminosity functions from ASAS-SN

II. 2014–2017 core-collapse supernovae and their subtypes

¹ European Southern Observatory, Alonso de Córdova 3107, Vitacura, Casilla, 19001 Santiago, Chile
² Instituto de Estudios Astrofísicos, Facultad de Ingeniería y Ciencias, Universidad Diego Portales, Av. Ejército Libertador 441, Santiago, Chile
³ Institute for Astronomy, University of Hawai’i at Mānoa, 2680 Woodlawn Drive, Honolulu, HI 96822, USA
⁴ Millennium Institute of Astrophysics MAS, Nuncio Monsenor Sotero Sanz 100, Off. 104, Providencia, Santiago, Chile
⁵ Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA
⁶ Center for Cosmology and AstroParticle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, USA
⁷ Department of Physics, The Ohio State University, 191 W. Woodruff Ave., Columbus, OH 43210, USA
⁸ Department of Astronomy, School of Physics, Peking University, Yiheyuan Rd. 5, Haidian District, Beijing 100871, China
⁹ Kavli Institute for Astronomy and Astrophysics, Peking University, Yi He Yuan Road 5, Hai Dian District, Beijing 100871, PR China
¹⁰ National Astronomical Observatories, Chinese Academy of Science, 20A Datun Road, Chaoyang District, Beijing 100101, China

^⋆ Corresponding author: Thallis.Pessi@eso.org

Received: 9 August 2025
Accepted: 1 September 2025

Abstract

Aims. The volumetric rates and luminosity functions (LFs) of core-collapse supernovae (ccSN) and their subtypes are important for understanding the cosmic history of star formation and the buildup of ccSNe products. To estimate these rates, we used data of nearby ccSNe discovered by the All-Sky Automated Survey for Supernovae (ASAS-SN) from 2014 to 2017, when all observations were made in the V band.

Methods. The sample is composed of 174 discovered or recovered events, with high spectroscopic completeness from follow-up observations. This allowed us to obtain a statistically precise and systematically robust estimate of nearby rates for ccSNe and their subtypes. The volumetric rates were estimated by correcting the observed number of events for survey completeness, which was estimated through injection recovery simulations using ccSN light curves.

Results. We find a total volumetric rate for ccSNe of 7.0^+1.0_−0.9 × 10⁻⁵ yr⁻¹ Mpc⁻³ h³₇₀, at a median redshift of 0.0149, for absolute magnitudes at peak M_V, peak ≤ −14 mag. This result is in agreement with previous local volumetric rates. We obtain volumetric rates for the different ccSN subtypes (II, IIn, IIb, Ib, Ic, Ibn, and Ic-BL), and find that the relative fractions of Type II, stripped-envelope, and interacting ccSNe are 63.2%, 32.3%, and 4.4%, respectively. We also estimate a volumetric rate for superluminous SNe of 1.5^+4.4_−1.1 yr⁻¹ Gpc⁻³ h³₇₀, corresponding to a fraction of 0.002% of the total ccSN rate. We produced intrinsic V-band LFs of ccSNe and their subtypes, and show that ccSN rates steadily decline for increasing luminosities. We further investigated the specific ccSN rate as a function of their host galaxy stellar mass and find that the rate decreases with increasing stellar mass, with significantly higher rates at lower mass galaxies (log M_* < 9.0 M_⊙).