X-ray hot spots in the eastern ear of the supernova remnant W 50 and the microquasar SS 433 system

Author:

Hayakawa Ryota1ORCID,Yamada Shinya12ORCID,Suda Hirotaka1,Ichinohe Yuto2ORCID,Higurashi Ryota2ORCID,Sakemi Haruka34ORCID,Machida Mami4ORCID,Ohmura Takumi5ORCID,Katsuda Satoru6ORCID,Uchiyama Hideki7ORCID,Sato Toshiki2,Akamatsu Hiroki8,Axelsson Magnus9ORCID

Affiliation:

1. Department of Physics, Tokyo Metropolitan University , 1-1 Minami-Osawa, Hachioji, Tokyo 192-0397 , Japan

2. Department of Physics, Rikkyo University , 3-34-1 Nishi-Ikebukuro, Toshima-ku, Tokyo 171-8501 , Japan

3. Graduate School of Science and Engineering, Kagoshima University , 1-21-35 Korimoto, Kagoshima, Kagoshima 890-0065 , Japan

4. National Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588 , Japan

5. Institute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582 , Japan

6. Graduate School of Science and Engineering, Saitama University , 255 Shimo-Okubo, Sakura, Saitama, Saitama 338-8570 , Japan

7. Faculty of Education, Shizuoka University , 836 Ohya, Suruga-ku, Shizuoka, Shizuoka 422-8529 , Japan

8. Netherlands Institute for Space Research (SRON) , Sorbonnelaan 2, 3584 CA Utrecht , the Netherlands

9. Department of Physics and Oskar Klein Center, Stockholm University , 106 91 Stockholm , Sweden

Abstract

Abstract We examined the X-ray and radio spatial structure at the eastern ear of the W 50/SS 433 system to clarify a characteristic feature of the termination region of the SS 433 jet, and found that a hot spot ahead of the filament structure, which is considered to be a terminal shock of the SS 433 eastern jet, is clearly different from a single point source. The detailed spatial structure of the X-ray emission is finely resolved by Chandra observations, showing that there are two sources. By comparing the point-spread function of Chandra with the radial profiles of the two sources, the northern one is clearly more extended than a point source while the other seems marginally extended. Since there are no point sources nearby, the northern hot spot is likely a localized diffuse source. The northern hot spot spatially corresponds to the peak of the radio emission. Its spatial correlation is confirmed by an X-ray image using XMM-Newton. The X-ray spectra of the two sources are reproduced by a single absorbed power-law but the column density of the northern part is larger by a factor of ∼3. When a radiation model comprising synchrotron emission and inverse Compton emission is applied to the spectral energy distribution of the northern hot spot, the emission from this spot can be explained by the radiation from an electron population accelerated up to 30 TeV in a magnetic field strength of B ≲ 50 μG. This model also agrees with the radio and X-ray data, as well as the upper limit of gamma-ray emission obtained by the Fermi satellite.

Funder

ESA Member States

NASA

National Radio Astronomy Observatory

National Science Foundation

Associated Universities, Inc.

JSPS

NWO

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

Reference59 articles.

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