H α emission in the nebular spectrum of the Type Ia supernova ASASSN-18tb
Abstract
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 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 (LH α = 2.2 ± 0.2 × 1038 ergs s−1) with FWHM ≈ 1100 km s−1 in the nebular-phase spectrum of this SN Ia. High-luminosity H α emission (LH 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 $${\sim } 1000 \, {\rm km\, s^{-1}}$$ 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 $${\sim } 10{{\ \rm per\ cent}}$$ among sub-luminous SNe Ia.
- Authors:
-
[1];
- Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA
- Kavli Institute for Astronomy and Astrophysics, Peking University, Yi He Yuan Road 5, Hai Dian District, Beijing 100871, China
- Las Campanas Observatory, Carnegie Observatories, Casilla 601, La Serena, Chile
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot 76100, Israel
- Núcleo de Astronomía de la Facultad de Ingeniería y Ciencias, Universidad Diego Portales, Av. Ejército 441 Santiago, Chile, Millennium Institute of Astrophysics, Santiago, Chile
- Publication Date:
- Sponsoring Org.:
- USDOE
- OSTI Identifier:
- 1608141
- Resource Type:
- Published Article
- Journal Name:
- Monthly Notices of the Royal Astronomical Society
- Additional Journal Information:
- Journal Name: Monthly Notices of the Royal Astronomical Society Journal Volume: 486 Journal Issue: 3; Journal ID: ISSN 0035-8711
- Publisher:
- Oxford University Press
- Country of Publication:
- United Kingdom
- Language:
- English
Citation Formats
Kollmeier, Juna A., Chen, Ping, Dong, Subo, Morrell, Nidia, Phillips, M. M., Kushnir, Doron, Prieto, J. L., Piro, Anthony L., and Simon, Joshua D. H α emission in the nebular spectrum of the Type Ia supernova ASASSN-18tb. United Kingdom: N. p., 2019.
Web. doi:10.1093/mnras/stz953.
Kollmeier, Juna A., Chen, Ping, Dong, Subo, Morrell, Nidia, Phillips, M. M., Kushnir, Doron, Prieto, J. L., Piro, Anthony L., & Simon, Joshua D. H α emission in the nebular spectrum of the Type Ia supernova ASASSN-18tb. United Kingdom. https://doi.org/10.1093/mnras/stz953
Kollmeier, Juna A., Chen, Ping, Dong, Subo, Morrell, Nidia, Phillips, M. M., Kushnir, Doron, Prieto, J. L., Piro, Anthony L., and Simon, Joshua D. Wed .
"H α emission in the nebular spectrum of the Type Ia supernova ASASSN-18tb". United Kingdom. https://doi.org/10.1093/mnras/stz953.
@article{osti_1608141,
title = {H α emission in the nebular spectrum of the Type Ia supernova ASASSN-18tb},
author = {Kollmeier, Juna A. and Chen, Ping and Dong, Subo and Morrell, Nidia and Phillips, M. M. and Kushnir, Doron and Prieto, J. L. and Piro, Anthony L. and Simon, Joshua D.},
abstractNote = {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 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 (LH α = 2.2 ± 0.2 × 1038 ergs s−1) with FWHM ≈ 1100 km s−1 in the nebular-phase spectrum of this SN Ia. High-luminosity H α emission (LH 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 ${\sim } 1000 \, {\rm km\, s^{-1}}$ 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 ${\sim } 10{{\ \rm per\ cent}}$ among sub-luminous SNe Ia.},
doi = {10.1093/mnras/stz953},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 3,
volume = 486,
place = {United Kingdom},
year = {Wed Apr 03 00:00:00 EDT 2019},
month = {Wed Apr 03 00:00:00 EDT 2019}
}
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