Discovery of Molecular and Atomic Clouds Associated with the Gamma-Ray Supernova Remnant Kesteven 79

• DOI: 10.3847/1538-4357/aad7be
• Publication Date: 2018-09-12T13:13:31Z
• Authors: M. Kuriki; H. Sano; N. Kuno; M. Seta; Y. Yamane; T. Inaba; T. Nagaya; S. Yoshiike; K. Okawa; D. Tsutsumi; Y. Hattori; M. Kohno; S. Fujita; A. Nishimura; A. Ohama; M. Matsuo; Y. Tsuda; K. Torii; T. Minamidani; T. Umemoto; G. Rowell; A. Bamba; K. Tachihara; Y. Fukui
• Keywords: High Energy Astrophysical Phenomena (astro-ph.HE); 13. Climate action; Astrophysics of Galaxies (astro-ph.GA); 0103 physical sciences; FOS: Physical sciences; Astrophysics - High Energy Astrophysical Phenomena; Astrophysics - Astrophysics of Galaxies; 01 natural sciences; 7. Clean energy

Abstract We carried out 12 CO( J = 1–0) observations of the Galactic gamma-ray supernova remnant (SNR) Kesteven 79 using Nobeyama Radio Observatory 45 m radio telescope, which has an angular resolution ∼20 arcsec. identified molecular and atomic gas interacting with 79, whose radial velocity is ∼80 km s −1 . The gases show good spatial correspondence X-ray shells, have expanding motion ∼4 associated peaks also exhibits a high intensity ratio CO 3–2/1–0 > 0.8, suggesting kinematic temperature ∼24 K, owing to heating by shock. determined distance SNR be ∼5.5 kpc radius ∼8 pc. average interstellar proton density inside ∼360 cm −3 , protons comprise only ∼10%. Assuming hadronic origin for emission, total cosmic-ray energy above 1 GeV estimated ∼5 × 10 48 erg.