NAME AT 2017erv , the SIMBAD biblio

2019MNRAS.486.3041K - Mon. Not. R. Astron. Soc., 486, 3041-3046 (2019/July-1)

H α emission in the nebular spectrum of the Type Ia supernova ASASSN-18tb.

KOLLMEIER J.A., CHEN P., DONG S., MORRELL N., PHILLIPS M.M., KUSHNIR D., PRIETO J.L., PIRO A.L. and SIMON J.D.

Abstract (from CDS):

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 d 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 α emission line (L_H α_ = 2.2 ± 0.2 x 1038 ergs s–1) with FWHM ≃ 1100 km s–1 in the nebular-phase spectrum of this SN Ia. High-luminosity H α emission (L_H α_ >= 1040 ergs s–1) has previously been discovered in a rare class of SNe Ia-like objects showing circum-stellar medium (CSM) interactions (SNe Ia-CSM). They predominantly belong to overluminous (Mmax < -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 (MB,max ∼ -17.7 mag) found in an early-type galaxy dominated by old stellar populations. We discuss possible origins for the observed hydrogen. Of the 75 SNe Ia for which we have so far obtained nebular spectra in 100IAS, no other SN shows a ∼1000 km s–1 H α 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 α emission could be as high as ∼10 per cent among sub-luminous SNe Ia.

Abstract Copyright: © 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): techniques: spectroscopic - supernovae: general - supernovae: individual: (ASASSN-18tb/SN2018fhw)

Simbad objects: 21

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2020.09.29-19:18:27

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