Volume 547, November 2012
|Number of page(s)||12|
|Section||Cosmology (including clusters of galaxies)|
|Published online||22 October 2012|
Angular fluctuations in the CXB: is Fe 6.4 keV line tomography of the large-scale structure feasible?
Max-Planck-Institut für Astrophysik,
2 Tartu Observatory, 61602 Tõravere, Estonia
3 Space Research Institute of Russian Academy of Sciences, Profsoyuznaya 84/32, 117997 Moscow, Russia
Accepted: 28 August 2012
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 ~5−10% of the CXB spectral intensity at ~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 Kα line tomography of the cosmic large-scale structure.
Aims. The goal of this paper is to investigate the feasibility of the Fe Kα 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 ≳100σ confidence requires an all-sky survey by an instrument with an effective area of ~10 m2 and field of view of ~1deg2. 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 ~0.1−0.5deg. For such an instrument, the CCD-type energy resolution of ~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 (~25−40σ) and ATHENA (~20−30σ).
Key words: cosmology: theory / large-scale structure of Universe / X-rays: diffuse background
© ESO, 2012
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