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Resonant scattering of X-rays by the warm intergalactic medium | | E.Churazov
; M.Haehnelt
; O.Kotov
; R.Sunyaev
; | | Date: |
25 Feb 2000 | | Journal: | Mon.Not.Roy.Astron.Soc. 323 (2001) 93 | | Subject: | astro-ph | | Affiliation: | MPA,IKI), M.Haehnelt (MPA,ITP), O.Kotov (IKI,MPA), R.Sunyaev (MPA,IKI | | Abstract: | For the low density filamentary and sheet-like structures in the warm ($sim 10^4$ to $sim 10^6$ K) IGM predicted by numerical simulations the resonant line scattering of X-ray background (XRB) photons by He and H-like ions of heavy elements can exceed the ``local’’ thermal emission by a factor of a few or more. Due to the conservative nature of scattering this resonantly scattered radiation can only be identified if a significant fraction of the XRB is resolved and removed. While the combined spectrum of the resolved sources will contain X-ray absorption features, the residual background will contain corresponding emission features with the same intensity. At the relevant densities and temperatures the lines of He and H-like oxygen at 0.57 and 0.65 keV are most promising. These lines (which have a typical width of $sim$ 1-2 eV) may contain up to 50% of the total 0.5-1 keV emission of the filament. For a nearby ($z la 0.1$) filament with a Thomson optical depth of $10^{-4}$ XMM should detect about 200 photons in the OVII line during a $10^5$ s exposure if the metallicity of the gas is as large as observed in galaxy clusters. On average up to a few percent of the soft XRB could be resonantly scattered by this phase of the IGM and resonantly scattered photons should account for a significant fraction of the truly diffuse background at low energies. Close to bright X-ray sources like galaxy clusters or AGN the flux of scattered radiation will be further enhanced. Off-line blazars are the most promising illuminating sources. The scattered emission from AGN may also constrain the duration of the active phase of these objects. | | Source: | arXiv, astro-ph/0002479 | | Services: | Forum | Review | PDF | Favorites | |
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