Progenitor mass constraints for the type Ib intermediate-luminosity SN 2015ap and the highly extinguished SN 2016bau

Abstract

Photometric and spectroscopic analyses of the intermediate-luminosity Type Ib supernova (SN) 2015ap and of the heavily reddened Type Ib SN 2016bau are discussed. Photometric properties of the two SNe, such as colour evolution, bolometric luminosity, photospheric radius, temperature, and velocity evolution, are also constrained. The ejecta mass, synthesized nickel mass, and kinetic energy of the ejecta are calculated from their light-curve analysis. We also model and compare the spectra of SN 2015ap and SN 2016bau at various stages of their evolution. The P Cygni profiles of various lines present in the spectra are used to determine the velocity evolution of the ejecta. To account for the observed photometric and spectroscopic properties of the two SNe, we have computed 12 M⊙ zero-age main-sequence (ZAMS) star models and evolved them until the onset of core-collapse using the publicly available stellar-evolution codeMESA. Synthetic explosions were produced using the public version of STELLA and another publicly available code, SNEC, utilizing the MESA models. SNEC and stella provide various observable properties such as the bolometric luminosity and velocity evolution. The parameters produced by SNEC/STELLA and our observations show close agreement with each other, thus supporting a 12 M⊙ ZAMS star as the possible progenitor for SN 2015ap, while the progenitor of SN 2016bau is slightly less massive, being close to the boundary between SN and non-SN as the final product.

Photometric, polarimetric, and spectroscopic studies of the luminous, slow-decaying Type Ib SN 2012au

“…3). The T BB and R BB values for iPTF13bvn and SN 2015ap are taken from Fremling et al (2014) and Aryan et al (2021), respectively, whereas they are calculated independently for SN 2007Y and SN 2009jf using the SUPERBOL code (Nicholl 2018a). Near the peak, SN 2012au exhibits lower temperature in comparison with SN 2007Y, iPTF13bvn, and SN 2015ap and higher than SN 2009jf, although after +20 d all the SNe presented manifest a nearly similar trend of temperature evolution (see middle panel of Fig.…”

“…This is the luminosity that we inject into the whole ejecta above the mass cut uniformly in mass. The explosion using the magnetar model is simulated using another publicly available code SNEC (Morozova et al 2015) by following the methods of Aryan et al (2021). For the initial spin-down luminosity, we assume L sdi = 2.2 × 10 43 erg s −1 , while for the initial spin-down time we assume t sd = 25 d (close to the value obtained from MINIM).…”

“…Upper left: He I, Ca II NIR, and the Fe II line velocities of SN 2012au. The line velocities of SN 2012au are also compared with those of SN 2007Y(Stritzinger et al 2009), SN 2009jf (Sahu et al 2011, iPTF13bvn(Srivastav, Anupama & Sahu 2014), and SN 2015ap (Prentice et al 2019Aryan et al 2021) in the other three panels.…”

SN 2016iyc: a Type IIb supernova arising from a low-mass progenitor

“…Here, we provide the set-up of the explosions to incorporate the Ni-Co decay model. The set-ups for simulating the synthetic explosion using SNEC and STELLA closely follow Ouchi & Maeda ( 2019 ) and Aryan et al ( 2021 ), respectively. Here, we briefly summarize the important parameters and modifications made to Ouchi & Maeda ( 2019 ) and Aryan et al ( 2021 ).…”

“…Owing to the abo v e-mentioned difficulties, only a handful of such studies including progenitor modelling followed by their synthetic e xplosions hav e been performed in the case of stripped or partially stripped CCSNe, including the Type Ib SN iPTF13bvn (Cao et al 2013 ;Bersten et al 2014 ;Paxton et al 2018 ), the famous Type IIb SN 2016gkg (Bersten et al 2018 ), a few other Type IIb SNe including SN 2011dh (Bersten et al 2012), SN 2011fu (Morales-Garoffolo et al 2015, two Type Ib SNe 2015ap and 2016bau (Aryan et al 2021), and another Type Ib SN 2012au (P ande y et al 2021.…”