A comparison between star formation rate diagnostics and rate of core collapse supernovae within 11 Mpc

Abstract

Aims. The core collapse supernova rate provides a strong lower limit for the star formation rate (SFR). Progress in using it as a cosmic SFR tracer requires some confidence that it is consistent with more conventional SFR diagnostics in the nearby Universe. This paper compares standard SFR measurements based on Hα, far ultraviolet (FUV) and total infrared (TIR) galaxy luminosities with the observed core collapse supernova rate in the same galaxy sample. The comparison can be viewed from two perspectives. Firstly, by adopting an estimate of the minimum stellar mass to produce a core collapse supernova one can determine a SFR from supernova numbers. Secondly, the radiative SFR can be assumed to be robust and then the supernova statistics provide a constrain on the minimum stellar mass for core collapse supernova progenitors. Methods. The novel aspect of this study is that Hα, FUV and TIR luminosities are now available for a complete galaxy sample within the local 11 Mpc volume and the number of discovered supernovae in this sample within the last 13 years is high enough to perform a meaningful statistical comparison. We exploit the multi-wavelength dataset from 11 HUGS, a volume-limited survey designed to provide a census of SFR in the Local Volume. There are 14 supernovae discovered in this sample of galaxies within the last 13 years. Although one could argue that this may not be complete, it is certainly a robust lower limit. Results. Assuming a lower limit for core collapse of 8 M (as proposed by direct detections of SN progenitor stars and white dwarf progenitors), the core-collapse supernova rate matches the SFR from the FUV luminosity. However, the SFR based on Hα luminosity is lower than these two estimates by a factor of nearly 2. If we assume that the FUV or Hα based luminosities are a true reflection of the SFR, we find that the minimum mass for core collapse supernova progenitors is 8 ± 1 M and 6 ± 1 M , respectively. Conclusions. The estimate of the minimum mass for core collapse supernova progenitors obtained exploiting FUV data is in good agreement with that from the direct detection of supernova progenitors. The concordant results by these independent methods point toward a constraint of 8 ± 1 M on the lower mass limit for progenitor stars of core collapse supernovae.

Chemoarchaeological downsizing in a hierarchical universe: impact of a top-heavy IGIMF

“…Almost no difference arises between the results of the calibrated models SAGS and SAGTH5B2. The observed rates show a dichotomy at low redshift; while the works of Botticella et al (2012) and Mattila et al (2012) estimate SNe CC rates of almost 2 (10 −4 ) yr −1 Mpc −3 h 3 70 , the works of Cappellaro et al (1999) and Li et al (2011) give SNe CC rates of the order of 0.6 (10 −4 ) yr −1 Mpc −3 h 3 70 . The model outputs are consistent with the higher values of SNe CC rates at z = 0.…”

The rate of supernovae at redshift 0.1–1.0

“…At low redshift we plot the rate estimates of LOSS (Li et al 2011a), which is the largest SN survey to date in the local volume with a total number of core collapse SNe of 440. We also plot the low redshift rates determined by Cappellaro et al (1999), Botticella et al (2012), and Mattila et al (2012). At slightly higher redshifts we plot the results from Botticella et al (2008), which also includes the data presented in Cappellaro et al (2005).…”

“…The use of core collapse supernovae as tracers of recent star formation is thus feasible at low redshifts (e.g. Botticella et al 2012). However, as we go to higher redshifts the bulk of the star formation takes place in dusty galaxies with high infrared luminosities (LIRGs and ULIRGs).…”

“…The rate from Cappellaro et al (1999) has been rescaled from SNu to a volumetric rate by assuming a local B-band luminosity density 2.0 × 10 8 h 70 L Mpc −3 at redshift ∼0. The local CCSN rates from Botticella et al (2012) and Mattila et al (2012) have been measured in small volumes and are likely dominated by inhomogeneity. The star formation rate in the local volume is higher than the average over an extended volume and can therefore cause the SNR to be higher than expected.…”

Observing gravitational waves from core-collapse supernovae in the advanced detector era

“…Within the Local Group (D ≲ 3 Mpc), the CCSN rate is ∼9 × 10 −2 CCSNe yr −1 , with major contributions from Andromeda (M31), Triangulum (M33), and the dwarf irregular galaxy IC 10, IC 1613, and NGC 6822 [82,84,89,90]. Outside of the Local Group, the CCSN rate increases to ∼0.15 CCSNe yr −1 within D ∼ 5 Mpc, including IC 342, the M81 group, M83, and NGC 253 as significant contributors to the CCSN rate [91][92][93][94][95][96]. Within D ¼ 10 Mpc, the CCSN rate is ∼0.47 CCSNe yr −1 , while it increases to ∼2.1 CCSNe yr −1 within D ¼ 20 Mpc [91,[94][95][96].…”