Diffuse γ-ray emission from the vicinity of young massive star cluster RSGC 1

被引：15
|
作者：
Sun, Xiao-Na [1 ,2 ]
Yang, Rui-Zhi [3 ,4 ,5 ]
Wang, Xiang-Yu [1 ,2 ]
机构：
[1] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Peoples R China
[2] Nanjing Univ, Key Lab Modern Astron & Astrophys, Minist Educ, Nanjing 210093, Peoples R China
[3] Univ Sci & Technol China, Sch Phys Sci, Dept Astron, Hefei 230026, Anhui, Peoples R China
[4] Univ Sci & Technol China, CAS Key Lab Res Galaxies & Cosmol, Hefei 230026, Anhui, Peoples R China
[5] Univ Sci & Technol China, Sch Astron & Space Sci, Hefei 230026, Anhui, Peoples R China
来源：
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2020年 / 494卷 / 03期
基金：
中国国家自然科学基金;
关键词：
open clusters and associations: individual: RSGC1; gamma-rays: ISM; MILKY-WAY; POPULATION; DISCOVERY;
D O I：
10.1093/mnras/staa947
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
We report the Fermi Large Area Telescope (Fermi-LAT) detection of the gamma-ray emission towards the young massive star cluster RSGC 1. Using the latest source catalogue and diffuse background models, we found that the diffuse gamma-ray emission in this region can be resolved into three different components. The GeV gamma-ray emission from the region HESS J1837-069 has a photon index of 1.83 +/- 0.08. Combining with the HESS and MAGIC data, we argue that the gamma-ray emission in this region likely originates from a pulsar wind nebula. The gamma-ray emission from the north-west part (region A) can be modelled by an ellipse with the semimajor and semiminor axes of 0.5 degrees and 0.25 degrees, respectively. The GeV emission has a hard spectrum with a photon index of about -2 and partially coincides with the TeV source MAGIC J1835-069. The possible origin of the gamma-ray emission in this region is the interaction of the cosmic rays (CRs) accelerated by SNR G24.7+0.6 or/and the OB cluster G25.18+0.26 with the surrounding gas clouds. The GeV gamma-ray emission from the south-east region (region B) can be modelled as an ellipse with the semimajor and semiminor axes of 0.9 degrees and 0.5 degrees, respectively, and also reveals a hard gamma-ray spectrum. We argue that the most probable origin is the interaction of the accelerated protons in the young massive star cluster RSGC 1 with ambient gas clouds, and the total CR proton energy is estimated to be as high as similar to 1 x 10(50) erg.
引用
收藏
页码：3405 / 3412
页数：8
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