H-$\hat{I}\pm$ emission in the nebular spectrum of the Type Ia supernova ASASSN-18tb

Abstract

As part of the 100IAS survey, a program aimed to obtain nebular-phase spectra for a volume-limited and homogeneous sample of Type Ia supernovae (SNe Ia), we observed ASASSN-18tb (SN 2018fhw) at 139 days past maximum light. ASASSN-18tb was a fast-declining, sub-luminous event that fits well within the observed photometric and spectroscopic distributions of the SN Ia population. We detect a prominent H$\hat{I}\pm$ emission line of $L_{\mathrm{H}\hat{I}\pm }=2.2\pm 0.2\times 10^{38}$ ergs s${}^{-1}$ with FWHM $\approx 1100$ km s${}^{-1}$ in the nebular-phase spectrum of this SN Ia. High luminosity H$\hat{I}\pm$ emission ($L_{\mathrm{H}\hat{I}\pm }\gtrsim 10^{40}$ ergs~s${}^{-1}$) has previously been discovered in a rare class of SNe Ia-like objects showing CSM interactions (SNe Ia-CSM). They predominantly belong to over-luminous ($M_{\max }<-19$ mag in optical) 1991T-like SNe Ia and are exclusively found in star-forming galaxies. By contrast, ASASSN-18tb is a sub-luminous SN Ia ($M_{B,\max }\sim -17.7$ mag) found in an early-type galaxy dominated by old stellar populations. We discuss possible origins for the observed hydrogen. Out of 75 SNe Ia for which we have so far obtained nebular spectra in 100IAS, no other SN shows a $\sim 1000\mathrm{km}{\mathrm{s}}^{-1}$ H$\hat{I}\pm$ emission line with comparable line luminosity as ASASSN-18tb, emphasizing the rarity of such emission in the nebular phase. Based on preliminary results from our survey, the rate for ASASSN-18tb-like nebular H$\hat{I}\pm$ emission could be as high as $\sim 10\%$ level among sub-luminous SNe Ia.

Submitted to MNRAS