On the observational behaviour of the highly polarized Type IIn supernova SN 2017hcc

Author:

Kumar Brajesh1ORCID,Eswaraiah Chakali12,Singh Avinash13ORCID,Sahu D K1,Anupama G C1,Kawabata K S4,Yamanaka Masayuki45,Otsubo Ikki6,Pandey S B7,Nakaoka Tatsuya6,Kawabata Miho6,Aryan Amar7,Akitaya Hiroshi4

Affiliation:

1. Indian Institute of Astrophysics, II Block, Koramangala, Bengaluru 560 034, India

2. National Astronomical Observatories, Chinese Academy of Sciences, Datun Road, Chaoyang District, Beijing 100101, P. R. China

3. Joint Astronomy Programme, Department of Physics, Indian Institute of Science, Bengaluru 560 012, India

4. Hiroshima Astrophysical Science Center, Hiroshima University, 1-3-1 Kagamiyama, Higashi-Hiroshima, Hiroshima 739-8526, Japan

5. Okayama Observatory, Graduate School of Science, Kyoto University, 3037-5 Honjo, Kamogata, Asakuchi, Okayama 719-0232, Japan

6. Department of Physical Science, Hiroshima University, Kagamiyama 1-3-1, Higashi-Hiroshima 739-8526, Japan

7. Aryabhatta Research Institute of Observational Sciences, Manora Peak, Nainital 263 001, India

Abstract

ABSTRACT We present the results based on photometric (Swift UVOT), broad-band polarimetric (V and Rbands) and optical spectroscopic observations of the Type IIn supernova (SN) 2017hcc. Our study is supplemented with spectropolarimetric data available in literature for this event. The post-peak light-curve evolution is slow (∼0.2 mag 100 d−1 in b band). The spectrum of ∼+27 d shows a blue continuum with narrow emission lines, typical of a Type IIn SN. Archival polarization data along with the Gaia DR2 distances have been utilized to evaluate the interstellar polarization (ISP) towards the SN direction which is found to be PISP = 0.17 ± 0.02 per cent and θISP = 140° ± 3°. To extract the intrinsic polarization of SN 2017hcc, both the observed and the literature polarization measurements were corrected for ISP. We noticed a significant decline of ∼3.5 per cent (V band) in the intrinsic level of polarization spanning a period of ∼2 months. In contrast, the intrinsic polarization angles remain nearly constant at all epochs. Our study indicates a substantial variation in the degree of asymmetry in either the ejecta and/or the surrounding medium of SN 2017hcc. We also estimate a mass-loss rate of $\dot{M}$ = 0.12 M⊙ yr−1 (for v$\mathrm{ w}$ = 20 km s−1) which suggests that the progenitor of SN 2017hcc is most likely a luminous blue variable.

Funder

Science and Engineering Research Board

National Post-Doctoral Fellowship

National Key R&D Program of China

Chinese Academy of Sciences

Department of Science and Technology, Republic of South Africa

Japan Society for the Promotion of Science

European Space Agency

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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