Probing the local environment of the supernova remnant HESS J1731-347 with CO and CS observations

被引：20

作者：

Maxted, N. ^{[1
]}

Burton, M. ^{[1
,2
]}

Braiding, C. ^{[1
]}

Rowell, G. ^{[3
]}

Sano, H. ^{[4
]}

Voisin, F. ^{[3
]}

Capasso, M. ^{[5
]}

Puehlhofer, G. ^{[5
]}

Fukui, Y. ^{[4
]}

机构：

[1] Univ New South Wales, Sch Phys, Sydney, NSW 2052, Australia

[2] Armagh Observ & Planetarium, Coll Hill, Armagh BT61 9DG, North Ireland

[3] Univ Adelaide, Sch Phys Sci, Adelaide, SA 5005, Australia

[4] Nagoya Univ, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan

[5] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2018年 / 474卷 / 01期

基金：

澳大利亚研究理事会;

关键词：

cosmic rays; ISM: clouds; ISM: supernova remnants; gamma-rays: ISM; GALACTIC PLANE SURVEY; MOPRA RADIO TELESCOPE; DENSE MOLECULAR GAS; GAMMA-RAY SOURCES; MM LINE SURVEY; VISUAL EXTINCTION; INTERSTELLAR GAS; COSMIC-RAYS; H-I; EMISSION;

D O I：

10.1093/mnras/stx2727

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The shell-type supernova remnant HESS J1731 - 347 emits TeV gamma-rays, and is a key object for the study of the cosmic ray acceleration potential of supernova remnants. We use 0.5-1 arcmin Mopra CO/CS(1-0) data in conjunction with HI data to calculate column densities towards the HESS J1731 - 347 region. We trace gas within at least four Galactic arms, typically tracing total (atomic+molecular) line-of-sight H column densities of 2-3 x 10(22) cm(-2). Assuming standard X-factor values and that most of the H I/CO emission seen towards HESS J1731 - 347 is on the near-side of the Galaxy, X-ray absorption column densities are consistent with H I+CO-derived column densities foreground to, but not beyond, the Scutum-Crux Galactic arm, suggesting a kinematic distance of similar to 3.2 kpc for HESS J1731 - 347. At this kinematic distance, we also find dense, infrared-dark gas traced by CS(1-0) emission coincident with the north of HESS J1731 - 347, the nearby H II region G353.43-0.37 and the nearby unidentified gamma-ray source HESS J1729 - 345. This dense gas lends weight to the idea that HESS J1729 - 345 and HESS J1731 - 347 are connected, perhaps via escaping cosmic-rays.

引用

页码：662 / 676

页数：15

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