Угловые флуктуации космического рентгеновского фона: томография крупномасштабной структуры Вселенной при помощи флуоресцентной линии железа 6.4 кэВ.
М.Р.Гильфанов, Р.А.Сюняев

На конкурс представлена статья:
G.Huetsi, M.Gilfanov, R.Sunyaev
Angular fluctuations in the CXB: Is Fe 6.4 keV line tomography of the large-scale structure feasible?
Astronomy and Astrophysics, 2012, accepted for publication

AGN are known to account for a major fraction, if not all, of the Cosmic X-ray background radiation. The dominant sharp spectral feature in their spectra is the 6.4 keV fluorescent line of iron, which may contribute as much as ~ 5-10% to the CXB spectral intensity at ~ 2-6 keV. Due to cosmological redshift, the line photons detected at the energy E carry information about objects located at the redshift z=6.4/E-1. In particular, imprinted in their angular fluctuations is the information about the large-scale structure at redshift z. This opens a possibility to perform the Fe K_alpha line tomography of the cosmic large-scale structure. We investigate the feasibility of the Fe K_alpha line tomography of the large-scale structure and show that detection of the tomographic signal at a ~100 sigma confidence requires an all-sky survey by an instrument with effective area of ~10 m^2 and field of view of ~1 deg^2. The signal is strongest for objects located at the redshift z~1, and at the angular scales corresponding to l ~ 100-300, therefore an optimal detection can be achieved with an instrument having a rather modest angular resolution of ~ 0.1-0.5 deg. For such an instrument, the CCD-type energy resolution of ~ 100-200 eV FWHM is entirely sufficient for the optimal separation of the signals originating at different redshifts. The gain in the signal strength which could potentially be achieved with energy resolution comparable to the line width, is nullified by the photon counting and AGN discreteness noise. Among the currently planned and proposed missions, these requirements are best satisfied by LOFT, despite the fact that it was proposed for entirely different purpose. Among others, clear detection should be achieved by WFXT (~ 20-35 sigma) and ATHENA (~ 10-20 sigma).