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Chandra Observations of the Luminous IR Galaxy NGC3256 | | P.Lira
; M.Ward
; A.Zezas
; A.Alonso-Herrero
; S.Ueno
; | | Date: |
13 Sep 2001 | | Journal: | Mon.Not.Roy.Astron.Soc. 330 (2002) 259 | | Subject: | astro-ph | | Affiliation: | 1,2), M.Ward , A.Zezas , A.Alonso-Herrero (4,5), S.Ueno( Leicester, U of Chile, CfA, Hertfordshire, Steward Observatory, NASDA | | Abstract: | We present a detailed analysis of high-resolution Chandra observations of the merger system NGC3256, the most IR luminous galaxy in the nearby universe. The X-ray data show that several discrete sources embedded in complex diffuse emission contribute ~>20 of the total emission (L_x^tot ~8E41 ergs/s in the 0.5-10 keV energy range). The compact sources are hard and extremely bright and their emission is probably dominated by accretion driven processes. Both galaxy nuclei are detected with L_x ~3-10E40 ergs/s. No evidence is found for the presence of an active nucleus in the southern nucleus, contrary to previous speculation. Once the discrete sources are removed, the diffuse component has a soft spectrum which can be modelled by the superposition of 3 thermal plasma components with temperatures kT = 0.6, 0.9 and 3.9 keV. Alternatively, the latter component can be described as a power-law with index Gamma ~3. Some evidence is found for a radial gradient of the amount of absorption and temperature of the diffuse component. We compare the X-ray emission with optical, Halpha and NICMOS images of NGC3256 and find a good correlation between the inferred optical/near-IR and X-ray extinctions. Although Inverse Compton scattering could be important in explaining the hard X-rays seen in the compact sources associated with the nuclei, the observed diffuse emission is probably of thermal origin. The observed X-ray characteristics support a scenario in which the powerful X-ray emission is driven solely by the current episode of star formation. | | Source: | arXiv, astro-ph/0109198 | | Services: | Forum | Review | PDF | Favorites | |
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