The Deepest Radio Observations of Nearby SNe Ia: Constraining Progenitor Types and Optimizing Future Surveys

Peter Lundqvist,Stuart D Ryder,Miguel A Pérez-Torres,Esha Kundu,Claes-Ingvar Björnsson,Antxon Alberdi,Erik C Kool,Megan K Argo,Robert J Beswick,Javier Moldon

doi:10.3847/1538-4357/ab6dc6

Abstract

Abstract We report deep radio observations of nearby Type Ia supernovae (SNe Ia) with the electronic Multi-Element Radio Linked Interferometer Network and the Australia Telescope Compact Array. No detections were made. With standard assumptions for the energy densities of relativistic electrons going into a power-law energy distribution and the magnetic field strength (ϵ e = ϵ B = 0.1), we arrive at upper limits on mass-loss rate for the progenitor system of SN 2013dy (SN 2016coj, SN 2018gv, SN 2018pv, SN 2019np) of , where v w is the wind speed of the mass loss. To SN 2016coj, SN 2018gv, SN 2018pv, and SN 2019np we add radio data for 17 other nearby SNe Ia and model their nondetections. With the same model as described, all 21 SNe Ia have . We compare those limits with the expected mass-loss rates in different single-degenerate progenitor scenarios. We also discuss how information on ϵ e and ϵ B can be obtained from late observations of SNe Ia and the youngest SN Ia remnant detected in radio, G1.9+0.3, as well as stripped-envelope core-collapse SNe. We highlight SN 2011dh and argue for ϵ e ≈ 0.1 and ϵ B ≈ 0.0033. Finally, we discuss strategies to observe at radio frequencies to maximize the chance of detection, given the time since explosion, the distance to the SN, and the telescope sensitivity.

Highlights

Type Ia supernovae (SNe Ia) have proven to be of fundamental importance as cosmological distance indicators (e.g., Riess et al 1998; Perlmutter et al 1999)
We report five more SNe Ia to add to this list from our ongoing programs on the electronic Multi-Element Radio Linked Interferometer Network and the Australia Telescope Compact Array (ATCA), namely, SN 2013dy, SN 2016coj, SN 2018gv, SN 2018pv, and SN 2019np
We found no evidence of radio emission in the region of SN 2016coj down to a 3σ limit of 126 μJy beam−1, which corresponds to an upper limit of the monochromatic 1.51 GHz luminosity of 6.1 ́ 1025 erg s−1 Hz−1 (3σ)

Summary

Introduction

Type Ia supernovae (SNe Ia) have proven to be of fundamental importance as cosmological distance indicators (e.g., Riess et al 1998; Perlmutter et al 1999). We are still ignorant regarding what progenitor scenario is the correct one for the majority of SNe Ia. Even so, we are still ignorant regarding what progenitor scenario is the correct one for the majority of SNe Ia This compromises their use for precision cosmology. They are key players in the chemical evolution of galaxies, but not knowing the details of progenitor evolution, the explosion, and the nucleosynthesis means that we do not fully understand the timescale over which SNe Ia turn on, adding uncertainty to models for the chemical enrichment in the universe. It is a generally accepted fact that SNe Ia are thermonuclear explosions of white dwarfs (WDs; Hoyle & Fowler 1960).

Results

Discussion

Conclusion