Giant H II Regions in M101. I. X-ray Analysis of Hot Gas

Дата и время публикации : 2012-10-07T06:13:39Z

Авторы публикации и институты :
Wei Sun (Nanjing University)
Yang Chen (Nanjing University)
Li Feng (Nanjing University)
You-Hua Chu (University of Illinois)
C. -H. Rosie Chen (Max Planck Institut fur Radioastronomie)
Q. Daniel Wang (University of Massachusetts)
Jiang-Tao Li (Nanjing University, University of Massachusetts, CEASaclay)

Ссылка на журнал-издание: Ссылка на журнал-издание не найдена
Коментарии к cтатье: 11 pages, 6 figures, Accepted for publication in the Astrophysical Journal
Первичная категория: astro-ph.HE

Все категории : astro-ph.HE, astro-ph.CO, astro-ph.GA

Краткий обзор статьи: We performed a Chandra X-ray study of three giant H II regions (GHRs), NGC 5461, NGC 5462, and NGC 5471, in the spiral galaxy M101. The X-ray spectra of the three GHRs all contain a prominent thermal component with a temperature of ~0.2 keV. In NGC 5461, the spatial distribution of the soft (< 1.5 keV) X-ray emission is generally in agreement with the extent of H1105, the most luminous H II region therein, but extends beyond its southern boundary, which could be attributed to outflows from the star cloud between H1105 and H1098. In NGC 5462, the X-ray emission is displaced from the H II regions and a ridge of blue stars; the H-alpha filaments extending from the ridge of star cloud to the diffuse X-rays suggest that hot gas outflows have occurred. The X-rays from NGC 5471 are concentrated at the B-knot, a "hypernova remnant" candidate. Assuming a Sedov-Taylor evolution, the derived explosion energy, on the order of 10^52 ergs, is consistent with a hypernova origin. In addition, a bright source in the field of NGC 5462 has been identified as a background AGN, instead of a black hole X-ray binary in M101.

Category: Physics