Emission-line diagnostics of core-collapse supernova host HII regions including interacting binary population. Issue Volume 14:Issue S346(2019) (August 2018)

• Record Type: Journal Article
• Authors: Xiao, Lin; Eldridge, J. J.; Galbany, L.; Stanway, E.
• Editors: Oskinova, Lidia M.; Bozzo, Enrico; Bulik, Tomasz; Gies, Douglas R.
• Is Part Of: Proceedings of the International Astronomical Union. Volume 14:Issue S346(2019)
• Page Start: 342
• Page End: 343
• Publication Date: 2018-08
• Subjects: binaries:general, -- supernovae:general, -- HII regions; Astronomy -- Congresses; Astronomy -- Periodicals; 520
• DOI: 10.1017/S1743921318008062
• Languages: English
• ISSNs: 1743-9213

Abstract

Abstract: Considering as many as 70% of massive stars interact with a binary companion (Sana et al. 2012, 2014 ), we created a new model of the optical nebular emission of HII regions by combining the results of the Binary Population and Spectral Synthesis (BPASS, Eldridge, Stanway et al. 2017 ) code with the photoionization code (CLOUDY). This is discussed more in detail in Xiao et al. 2018 a. Then we use this model to explore a variety of emission-line diagnostics of CCSN host HII regions from the PMAS/PPAK Integral-field Supernova hosts COmpilation (PISCO, Galbany et al. 2018 ). We determine the age, metallicity and gas parameters for H II regions associated with CCSNe, contrasting the above variables to distribution type II and type Ibc SNe. We find their nebular emission and CCSN progenitor types are largely determined by past and ongoing binary interactions, for example mass loss, mass gain and stellar mergers. However we note these two types SNe have little preference in their host environment metallicity measured by oxygen abundance or in progenitor initial mass, except that at lower metallicities supernovae are more likely to be of type II. The BPASS and nebular emission models are available from bpass.auckland.ac.nz and warwick.ac.uk/bpass .