Radio Follow-up Observations of SN 2023ixf by Japanese and Korean Very Long Baseline Interferometers

被引：0

作者：

Iwata, Yuhei ^{[1
,2
]}

Akimoto, Masanori ^{[3
]}

Matsuoka, Tomoki ^{[4
]}

Maeda, Keiichi ^{[5
]}

Yonekura, Yoshinori ^{[6
]}

Tominaga, Nozomu ^{[1
,7
,8
]}

Moriya, Takashi J. ^{[1
,9
]}

Fujisawa, Kenta ^{[10
]}

Niinuma, Kotaro ^{[3
,10
]}

Yoon, Sung-Chul ^{[11
]}

Lee, Jae-Joon ^{[12
]}

Jung, Taehyun ^{[12
]}

Byun, Do-Young ^{[12
]}

机构：

[1] Natl Astron Observ Japan, Div Sci, 2-21-1 Osawa, Tokyo 1818588, Japan

[2] Natl Astron Observ Japan, Mizusawa VLBI Observ, 2-12 Hoshigaoka, Oshu, Iwate 0230861, Japan

[3] Yamaguchi Univ, Grad Sch Sci & Technol Innovat, 1677-1 Yoshida, Yamaguchi, Yamaguchi 7538512, Japan

[4] Acad Sinica, Inst Astron & Astrophys, 1 Sec 4,Roosevelt Rd, Taipei 106216, Taiwan

[5] Kyoto Univ, Dept Astron, Kitashirakawa Oiwake Cho,Sakyo Ku, Kyoto 6068502, Japan

[6] Ibaraki Univ, Ctr Astron, 2-1-1 Bunkyo, Mito, Ibaraki 3108512, Japan

[7] SOKENDAI, Grad Inst Adv Studies, Astron Sci Program, 2-21-1 Osawa, Tokyo 1818588, Japan

[8] Konan Univ, Fac Sci & Engn, Dept Phys, 8-9-1 Okamoto, Kobe, Hyogo 6588501, Japan

[9] Monash Univ, Fac Sci, Sch Phys & Astron, Clayton, Vic 3800, Australia

[10] Yamaguchi Univ, Res Inst Time Studies, 1677-1 Yoshida, Yamaguchi, Yamaguchi 7538511, Japan

[11] Seoul Natl Univ, Dept Phys & Astron, Astron Program, Seoul 08826, South Korea

[12] Korea Astron & Space Sci Inst, 776 Daedeokdae Ro, Daejeon 34055, South Korea

来源：

ASTROPHYSICAL JOURNAL | 2025年 / 978卷 / 02期

基金：

日本学术振兴会; 新加坡国家研究基金会;

关键词：

CIRCUMSTELLAR MATERIAL; RED SUPERGIANT; MASS-LOSS; X-RAY; HYDROGEN-RICH; LIGHT-CURVE; MESSIER; 101; PROGENITOR; EMISSION; DENSE;

D O I：

10.3847/1538-4357/ad9a62

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report on radio follow-up observations of the nearby Type II supernova SN 2023ixf, spanning from 1.7 to 269.9 days after the explosion, conducted using three very long baseline interferometers (VLBIs), which are the Japanese VLBI Network, the VLBI Exploration of Radio Astrometry, and the Korean VLBI Network. In three observation epochs (152.3, 206.1, and 269.9 days), we detected emission at the 6.9 and 8.4 GHz bands, with a flux density of similar to 5 mJy. The flux density reached a peak at around 206.1 days, which is longer than the timescale to reach the peak observed in typical Type II supernovae. Based on an analytical model of radio emission, our late-time detections were inferred to be due to decreasing optical depth. In this case, the mass-loss rate of the progenitor is estimated to have increased from similar to 10(-6)-10(-5)M(circle dot) yr(-1) to similar to 10(-4)M(circle dot) yr(-1) between 28 and 6 yr before the explosion. Our radio constraints are also consistent with the mass-loss rate needed to produce a confined circumstellar medium proposed by previous studies, which suggest that the mass-loss rate increased from similar to 10(-4)M(circle dot) yr(-1) to greater than or similar to 10(-2)M(circle dot) yr(-1) in the last few years before the explosion.

引用

页数：9