科研之友
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摘要
Context. Active galactic nuclei (AGN) are known to account for a major portion, if not all, of the cosmic X-ray background (CXB) radiation. The dominant sharp spectral feature in their spectra is the 6.4 keV fluorescent line of iron, which may contribute to as much as similar to 5-10% of the CXB spectral intensity at similar to 2-6 keV. Owing 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 the possibility of performing the Fe K-alpha line tomography of the cosmic large-scale structure.
Aims. The goal of this paper is to investigate the feasibility of the Fe K alpha line tomography of the large-scale structure.
Methods. At any observed energy E, the 6.4 keV line photons are blended with continuum emission, which originates in objects located at many different redshifts and therefore contaminates and dilutes the tomographic signal. However, its contribution can be removed by doing observations at two nearby energy intervals and by calculating the power spectrum of the corresponding differential signal map.
Results. We show that detection of the tomographic signal at greater than or similar to 100 sigma confidence requires an all-sky survey by an instrument with an effective area of similar to 10 m(2) and field of view of similar to 1 deg(2). The signal is strongest for objects located at the redshift z similar to 1 and at the angular scales corresponding to l similar to 100-300, therefore an optimal detection can be achieved with an instrument having a rather modest angular resolution of similar to 0.1-0.5 deg. For such an instrument, the CCD-type energy resolution of similar to 100-200 eV FWHM is entirely sufficient for the optimal separation of the signals coming from different redshifts. The gain in the signal strength that 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, even though that it was proposed for an entirely different purpose. Among others, clear detection should be achieved by WFXT (similar to 25-40 sigma) and ATHENA (similar to 20-30 sigma).
- 出版日期2012-11
