SN 2022ngb: A faint, slowly evolving Type IIb supernova with a low-mass envelope

TL;DR

SN 2022ngb is a faint, slowly evolving Type IIb supernova with a low-mass envelope, providing insights into its explosion parameters, progenitor star, and explosion asymmetries through extensive photometric and spectroscopic analysis.

Contribution

This study presents detailed modeling of SN 2022ngb's photometric and spectroscopic data, revealing its physical parameters and progenitor characteristics for the first time.

Findings

SN 2022ngb has a peak bolometric luminosity of 7.76 x 10^41 erg/s.

Ejecta mass is estimated at 2.9-3.2 solar masses.

Explosion energy is approximately 1.4 x 10^51 erg.

Abstract

An extensive photometric and spectroscopic follow-up campaign of the Type IIb SN 2022ngb is presented in the article. Through detailed modeling of this dataset, we aim to constrain the key physical parameters of the explosion, infer the nature of the progenitor star and its environment, and probe the dynamical properties of the ejecta. We analyze photometric and spectroscopic data of SN 2022ngb. By constructing and modeling the bolometric light curve with semi-analytic models, we estimate the primary explosion parameters. The spectroscopic data are compared with those of well-studied SNe IIb and NLTE models to constrain the properties of the progenitor and the structure of the resulting ejecta. SN 2022ngb is a low-luminosity SN IIb with a peak bolometric luminosity of L_bol = 7.76 (+1.15/-1.00) x 10^41 erg/s and a V-band rising time of 24.32 +/- 0.50 days. Light curve modeling indicates an ejecta mass of ~2.9-3.2 M_sun, an explosion energy of ~1.4 x 10^51 erg, and a low synthesized 56Ni mass of ~0.045 M_sun. Nebular phase spectra exhibit asymmetric line profiles, pointing to a non-spherical explosion and an anisotropic distribution of radioactive material. Our analysis reveals a relatively compact stripped-envelope progenitor with a pre-SN mass of approximately 4.7 M_sun (corresponding to a 15-16 M_sun ZAMS star). Our analysis suggests that SN 2022ngb originated from the explosion of a moderate-mass relatively compact, stripped-envelope star in a binary system. The asymmetries inferred from the nebular phase spectral line features suggest a non-spherical explosion.