Spatially resolved molecular gas properties of host galaxy of Type I superluminous supernova SN 2017egm-Reference-Cited by-同舟云学术

Spatially resolved molecular gas properties of host galaxy of Type I superluminous supernova SN 2017egm

Published:2020-06-10 Issue:4 Volume:72 Page:
ISSN:0004-6264
Container-title:Publications of the Astronomical Society of Japan
language:en
Short-container-title:

Author:

Hatsukade Bunyo¹^ORCID,Morokuma-Matsui Kana¹^ORCID,Hayashi Masao²^ORCID,Tominaga Nozomu³⁴^ORCID,Tamura Yoichi⁵^ORCID,Niinuma Kotaro⁶^ORCID,Motogi Kazuhiro⁶^ORCID,Morokuma Tomoki¹^ORCID,Matsuda Yuichi²⁷^ORCID

Affiliation:

1. Institute of Astronomy, Graduate School of Science, The University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan

2. National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan

3. Department of Physics, Faculty of Science and Engineering, Konan University, 8-9-1 Okamoto, Kobe, Hyogo 658-8501, Japan

4. Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583, Japan

5. Department of Physics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8602, Japan

6. Graduate School of Sciences and Technology for Innovation, Yamaguchi University, Yoshida 1677-1, Yamaguchi, Yamaguchi 753-8512, Japan

7. Graduate University for Advanced Studies (SOKENDAI), 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan

Abstract

Abstract We present the results of CO(1–0) observations of the host galaxy of a Type I superluminous supernova (SLSN-I), SN 2017egm, one of the closest SLSNe-I at z = 0.03063, by using the Atacama Large Millimeter/submillimeter Array. The molecular gas mass of the host galaxy is Mgas = (4.8 ± 0.3) × 109 M⊙, placing it on the sequence of normal star-forming galaxies in an Mgas–star-formation rate (SFR) plane. The molecular hydrogen column density at the location of SN 2017egm is higher than that of the Type II SN PTF10bgl, which is also located in the same host galaxy, and those of other Type II and Ia SNe located in different galaxies, suggesting that SLSNe-I have a preference for a dense molecular gas environment. On the other hand, the column density at the location of SN 2017egm is comparable to those of Type Ibc SNe. The surface densities of molecular gas and the SFR at the location of SN 2017egm are consistent with those of spatially resolved local star-forming galaxies and follow the Schmidt–Kennicutt relation. These facts suggest that SLSNe-I can occur in environments with the same star-formation mechanism as in normal star-forming galaxies.

Funder

JSPS

NAOJ

ALMA

ESO

NSF

NINS

NRC

MOST

ASIAA

KASI

Space Telescope Science Institute