ALMA CO Observations of Gamma-Ray Supernova Remnant N132D in the Large Magellanic Cloud: Possible Evidence for Shocked Molecular Clouds Illuminated by Cosmic-Ray Protons

被引：24

作者：

Sano, H. ^{[1
,2
,3
]}

Plucinsky, P. P. ^{[4
]}

Bamba, A. ^{[5
,6
]}

Sharda, P. ^{[7
,8
]}

Filipovic, M. D. ^{[9
]}

Law, C. J. ^{[4
]}

Alsaberi, R. Z. E. ^{[9
]}

Yamane, Y. ^{[2
]}

Tokuda, K. ^{[1
]}

Acero, F. ^{[11
]}

Sasaki, M. ^{[12
]}

Vink, J. ^{[13
]}

Inoue, T. ^{[2
]}

Inutsuka, S. ^{[2
]}

Shimoda, J. ^{[2
]}

Tsuge, K. ^{[2
]}

Fujii, K. ^{[5
]}

Voisin, F. ^{[14
]}

Maxted, N. ^{[15
]}

Rowell, G. ^{[14
]}

Onishi, T. ^{[10
]}

Kawamura, A. ^{[1
]}

Mizuno, N. ^{[1
]}

Yamamoto, H. ^{[2
]}

Tachihara, K. ^{[2
]}

Fukui, Y. ^{[2
,3
]}

机构：

[1] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan

[2] Nagoya Univ, Dept Phys, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648601, Japan

[3] Nagoya Univ, Inst Adv Res, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648601, Japan

[4] Harvard & Smithsonian, Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA

[5] Univ Tokyo, Grad Sch Sci, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan

[6] Univ Tokyo, Sch Sci, Res Ctr Early Universe, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan

[7] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia

[8] Australian Res Council, Ctr Excellence All Sky Astrophys 3 Dimens ASTRO 3, Canberra, ACT, Australia

[9] Western Sydney Univ, Locked Bag 1797, Penrith, NSW 1797, Australia

[10] Osaka Prefecture Univ, Grad Sch Sci, Dept Phys Sci, Naka Ku, 1-1 Gakuen Cho, Sakai, Osaka 5998531, Japan

[11] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France

[12] Friedrich Alexander Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte Erlangen Ctr Astroparti, Sternwartstr 7, D-96049 Bamberg, Germany

[13] Univ Amsterdam, GRAPPA, Anton Pannekoek Inst, POB 94249, NL-1090 GE Amsterdam, Netherlands

[14] Univ Adelaide, Sch Phys Sci, North Terrace, Adelaide, SA 5005, Australia

[15] Univ New South Wales, Australian Def Force Acad, Sch Sci, Canberra, ACT 2600, Australia

来源：

ASTROPHYSICAL JOURNAL | 2020年 / 902卷 / 01期

基金：

美国国家科学基金会; 澳大利亚研究理事会;

关键词：

Supernova remnants; Interstellar medium; Cosmic ray sources; Gamma-ray sources; X-ray sources; Large Magellanic Cloud; SPACE-TELESCOPE OBSERVATIONS; X-RAY; NOVA REMNANT; ATOMIC DATA; GAS; SPECTROSCOPY; YOUNG; ACCELERATION; ABUNDANCES; DUST;

D O I：

10.3847/1538-4357/abb469

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

N132D is the brightest gamma-ray supernova remnant (SNR) in the Large Magellanic Cloud (LMC). We carried out(12)CO(J = 1-0, 3-2) observations toward the SNR using the Atacama Large Millimeter/submillimeter Array (ALMA) and Atacama Submillimeter Telescope Experiment. We find diffuse CO emission not only at the southern edge of the SNR as previously known, but also inside the X-ray shell. We spatially resolved nine molecular clouds using ALMA with an angular resolution of 5 '', corresponding to a spatial resolution of similar to 1 pc at the distance of the LMC. Typical cloud sizes and masses are similar to 2.0 pc and similar to 100M, respectively. High intensity ratios of COJ = 3-2/1-0 > 1.5 are seen toward the molecular clouds, indicating that shock heating has occurred. Spatially resolved X-ray spectroscopy reveals that thermal X-rays in the center of N132D are produced not only behind a molecular cloud but also in front of it. Considering the absence of a thermal component associated with the forward shock toward one molecular cloud located along the line of sight to the center of the remnant, this suggests that this particular cloud is engulfed by shock waves and is positioned on the near side of the remnant. If the hadronic process is the dominant contributor to the gamma-ray emission, the shock-engulfed clouds play a role as targets for cosmic rays. We estimate the total energy of cosmic-ray protons accelerated in N132D to be similar to 0.5-3.8 x 10(49)erg as a conservative lower limit, which is similar to that observed in Galactic gamma-ray SNRs.

引用

页数：14

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