2004/09/30 by Akira Hayakawa, Tae Furusho, Noriko Y. Yamasaki +2 · 39 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Cluster (spacecraft) #Cooling flow #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy cluster #Intracluster medium #Mass distribution #Metallicity #RADIUS #Stellar, planetary, and galactic studies #Type-cD galaxy #astro-ph
paper · pdf · doi:10.1093/pasj/56.5.743
published in Publications of the Astronomical Society of Japan 56(5), 743-752 (Oxford University Press) · 10 pages, 11 figures, accepted by PASJ. High resolution version available at http://www-x.phys.metro-u.ac.jp/~akira_h/papers/
arxiv created 2004/09/30 · openalex publication_date 2004/10/01 · arxiv updated 2015/06/24 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Abstract A Chandra observation of the non-cooling flow cluster A 1060 has confirmed that the hot intracluster medium has fairly uniform distributions of temperature and metal abundance from a radius of about 230 kpc to the central 5 kpc region (H0 = 75 km s-1 Mpc-1). The radial temperature profile shows a broad peak at 30–40 kpc from the center at a level ∼ 20% higher than that in the outer region. Assuming spatially uniform temperature and abundance distributions, we derived a 3-dimensional density structure by iteratively correcting the β model, and obtained the central gas density to be 8.2+1.8-1.0 × 10-3 cm-3. The distribution of gravitational mass was estimated from the density profile, and a central concentration of mass within a radius of 50 kpc was indicated. The data also suggest several high-abundance regions. The most significant blob adjacent to the central galaxy NGC 3311 has a radius of about 9 kpc, which indicates a metallicity of ∼ 1.5 solar. We consider that this blob may be produced by the gas stripped off from NGC 3311.