Interaction between supernova remnant G22.7–0.2 and the ambient molecular clouds

Journal Article · Mon Dec 01 04:00:00 EST 2014 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/796/2/122· OSTI ID:22370137

Su, Yang; Yang, Ji; Zhou, Xin ^[1]; Zhou, Ping; Chen, Yang ^[2]

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1. Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008 (China)
2. Department of Astronomy, Nanjing University, 163 Xianlin Avenue, Nanjing 210093 (China)

We have carried out {sup 12}CO (J = 1-0 and 2-1), {sup 13}CO (J = 1-0), and C{sup 18}O (J = 1-0) observations in the direction of the supernova remnant (SNR) G22.7–0.2. A filamentary molecular gas structure, which is likely part of a larger molecular complex with V {sub LSR} ∼ 75-79 km s{sup –1}, is detected and is found to surround the southern boundary of the remnant. In particular, the high-velocity wing (77-110 km s{sup –1}) in the {sup 12}CO (J = 1-0 and J = 2-1) emission shows convincing evidence of the interaction between SNR G22.7–0.2 and the 75-79 km s{sup –1} molecular clouds (MCs). Spectra with redshifted profiles, a signature of shocked molecular gas, are seen in the southeastern boundary of the remnant. The association between the remnant and the 77 km s{sup –1} MCs places the remnant at the near distance of 4.4 ± 0.4 kpc, which agrees with a location on the Scutum-Crux arm. We suggest that SNR G22.7–0.2, SNR W41, and H II region G022.760-0.485 are at the same distance and are associated with GMC G23.0–0.4.

• OSTI ID: 22370137
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 2 Vol. 796; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
CARBON 12
CARBON 13
CARBON MONOXIDE
COSMIC GASES
DISTANCE
ELEMENT ABUNDANCE
EMISSION
INTERACTIONS
MOLECULES
OXYGEN 18
RED SHIFT
SPECTRA
SUPERNOVA REMNANTS
VELOCITY