skip to main content
OSTI.GOV title logo U.S. Department of Energy
Office of Scientific and Technical Information

Title: Is HESS J1912+101 Associated with an Old Supernova Remnant?

Abstract

HESS J1912+101 is a shell-like TeV source that has no clear counterpart in multiwavelength. Using CO and H i data, we reveal that V {sub LSR} ∼ +60 km s{sup −1} molecular clouds (MCs), together with shocked molecular gas and high-velocity neutral atomic shells, are concentrated toward HESS J1912+101. The prominent wing profiles up to V {sub LSR} ∼ +80 km s{sup −1} seen in {sup 12}CO ( J = 1–0 and J = 3–2) data, as well as the high-velocity expanding H i shells up to V {sub LSR} ∼ +100 km s{sup −1}, exhibit striking redshifted-broadening relative to the quiescent gas. These features provide compelling evidences for large-scale perturbation in the region. We argue that the shocked MCs and the high-velocity H i shells may originate from an old supernova remnant (SNR). The distance to the SNR is estimated to be ∼4.1 kpc based on the H i self-absorption method, which leads to a physical radius of 29.0 pc for the ∼(0.7–2.0) × 10{sup 5} years old remnant with an expansion velocity of ≳40 km s{sup −1}. The +60 km s{sup −1} MCs and the disturbed gas are indeed found to coincide with the bright TeV emission, supportingmore » the physical association between them. Naturally, the shell-like TeV emission comes from the decay of neutral pions produced by interactions between the accelerated hadrons from the SNR and the surrounding high-density molecular gas.« less

Authors:
; ; ; ; ;  [1];  [2]
  1. Purple Mountain Observatory and Key Laboratory of Radio Astronomy, Chinese Academy of Sciences, Nanjing 210008 (China)
  2. Department of Astronomy, Nanjing University, Nanjing 210023 (China)
Publication Date:
OSTI Identifier:
22663276
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 845; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; CARBON; CARBON MONOXIDE; CLOUDS; COSMIC GASES; DECAY; DENSITY; DISTURBANCES; ELECTRONIC STRUCTURE; EMISSION; EXPANSION; HYDROGEN; INTERACTIONS; PERTURBATION THEORY; RED SHIFT; SELF-ABSORPTION; SUPERNOVA REMNANTS; TEV RANGE; VELOCITY

Citation Formats

Su, Yang, Zhou, Xin, Yang, Ji, Chen, Xuepeng, Gong, Yan, Zhang, Shaobo, and Chen, Yang, E-mail: yangsu@pmo.ac.cn. Is HESS J1912+101 Associated with an Old Supernova Remnant?. United States: N. p., 2017. Web. doi:10.3847/1538-4357/AA7F2A.
Su, Yang, Zhou, Xin, Yang, Ji, Chen, Xuepeng, Gong, Yan, Zhang, Shaobo, & Chen, Yang, E-mail: yangsu@pmo.ac.cn. Is HESS J1912+101 Associated with an Old Supernova Remnant?. United States. doi:10.3847/1538-4357/AA7F2A.
Su, Yang, Zhou, Xin, Yang, Ji, Chen, Xuepeng, Gong, Yan, Zhang, Shaobo, and Chen, Yang, E-mail: yangsu@pmo.ac.cn. Thu . "Is HESS J1912+101 Associated with an Old Supernova Remnant?". United States. doi:10.3847/1538-4357/AA7F2A.
@article{osti_22663276,
title = {Is HESS J1912+101 Associated with an Old Supernova Remnant?},
author = {Su, Yang and Zhou, Xin and Yang, Ji and Chen, Xuepeng and Gong, Yan and Zhang, Shaobo and Chen, Yang, E-mail: yangsu@pmo.ac.cn},
abstractNote = {HESS J1912+101 is a shell-like TeV source that has no clear counterpart in multiwavelength. Using CO and H i data, we reveal that V {sub LSR} ∼ +60 km s{sup −1} molecular clouds (MCs), together with shocked molecular gas and high-velocity neutral atomic shells, are concentrated toward HESS J1912+101. The prominent wing profiles up to V {sub LSR} ∼ +80 km s{sup −1} seen in {sup 12}CO ( J = 1–0 and J = 3–2) data, as well as the high-velocity expanding H i shells up to V {sub LSR} ∼ +100 km s{sup −1}, exhibit striking redshifted-broadening relative to the quiescent gas. These features provide compelling evidences for large-scale perturbation in the region. We argue that the shocked MCs and the high-velocity H i shells may originate from an old supernova remnant (SNR). The distance to the SNR is estimated to be ∼4.1 kpc based on the H i self-absorption method, which leads to a physical radius of 29.0 pc for the ∼(0.7–2.0) × 10{sup 5} years old remnant with an expansion velocity of ≳40 km s{sup −1}. The +60 km s{sup −1} MCs and the disturbed gas are indeed found to coincide with the bright TeV emission, supporting the physical association between them. Naturally, the shell-like TeV emission comes from the decay of neutral pions produced by interactions between the accelerated hadrons from the SNR and the surrounding high-density molecular gas.},
doi = {10.3847/1538-4357/AA7F2A},
journal = {Astrophysical Journal},
issn = {0004-637X},
number = 1,
volume = 845,
place = {United States},
year = {2017},
month = {8}
}