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Emission-line diagnostics of core-collapse supernova host HII regions including interacting binary population

Published online by Cambridge University Press:  30 December 2019

Lin Xiao ,
J. J. Eldridge ,
L. Galbany  and
E. Stanway
Lin Xiao
Affiliation:
CAS Key Laboratory for Research in Galaxies and Cosmology, Department of Astronomy, University of Science and Technology of China, Hefei, China email: lxiao33@ustc.edu.cn
J. J. Eldridge
Affiliation:
Department of Physics, University of Auckland, Private Bag 92019, Auckland, New Zealand email: j.eldridge@auckland.ac.nz
L. Galbany
Affiliation:
PITT PACC, Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260, USA email: llgalbany@pitt.edu
E. Stanway
Affiliation:
Department of Physics, University of Warwick, Gibbet Hill Road, Coventry, CV4 7AL, UK email: e.r.stanway@warwick.ac.uk
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Abstract

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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.2018a. 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.

Keywords

binaries:generalsupernovae:generalHII regions
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S346: High-mass X-ray Binaries: Illuminating the Passage from Massive Binaries to Merging Compact Objects , August 2018 , pp. 342 - 343
Copyright
© International Astronomical Union 2019 

References

Eldridge, J. J., Fraser, M., Smartt, S. J., Maund, J. R., & Crockett, R. M. 2013, MNRAS, 436, 774 CrossRefGoogle Scholar
Eldridge, J. J., Stanway, E., Xiao, L., McClelland, L. A. S., Taylor, G., Ng, M., Greis, S. M. L., Bray, J. C. et al. 2017, PASA, 34, e058 CrossRefGoogle Scholar
Galbany, L., Anderson, J. P., Sánchez, S. F., et al. 2018, ApJ, 855, 107 CrossRefGoogle Scholar
Sana, H., de Mink, S. E., de Koter, A., Langer, N., Evans, C. J., Gieles, M., Gosset, E., Izzard, R. G., Le Bouquin, J.-B., & Schneider, F. R. N. 2012, Science, 337:444.CrossRefGoogle Scholar
Sana, H., Le Bouquin, J.-B., Lacour, S., Berger, J.-P., Duvert, G., Gauchet, L., Norris, B., Olofsson, J., Pickel, D., Zins, G., Absil, O., de Koter, A., Kratter, K., Schnurr, O., Zinnecker, H., et al. 2014, ApJS, 215, 15 CrossRefGoogle Scholar
Smartt, S. J. 2015, pasa, 32, e016 CrossRefGoogle Scholar
Xiao, L., Stanway, E. R., & Eldridge, J. J. 2018a, MNRAS, 477, 904 CrossRefGoogle Scholar
Xiao, L., Galbany, L., Eldridge, J. J., & Stanway, E. R. 2018b, arXiv:1805.01213Google Scholar