Probing large-scale structure with large samples of X-ray selected AGN: I. Baryonic acoustic oscillations

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作者：
Hütsi, Gert [1 ,2 ]
Gilfanov, Marat [1 ,3 ,4 ]
Kolodzig, Alexander [1 ]
Sunyaev, Rashid [1 ,3 ]
机构：
[1] [1,Hütsi, Gert
[2] 1,3,Gilfanov, Marat
[3] Kolodzig, Alexander
[4] 1,Sunyaev, Rashid
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| 1600年 / EDP Sciences卷 / 572期
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We investigate the potential of large X-ray-selected AGN samples for detecting baryonic acoustic oscillations (BAO). Though AGN selection in X-ray band is very clean and efficient; it does not provide redshift information; and thus needs to be complemented with an optical follow-up. The main focus of this study is (i) to find the requirements needed for the quality of the optical follow-up and (ii) to formulate the optimal strategy of the X-ray survey; in order to detect the BAO. We demonstrate that redshift accuracy of σ0 = 10-2 at z = 1 and the catastrophic failure rate of ffail ? 30% are sufficient for a reliable detection of BAO in future X-ray surveys. Spectroscopic quality redshifts (σ0 = 10-3 and ffail ∼ 0) will boost the confidence level of the BAO detection by a factor of ∼2. For meaningful detection of BAO; X-ray surveys of moderate depth of Flim ∼ few 10-15 erg? s-1/cm2 covering sky area from a few hundred to ∼ten thousand square degrees are required. The optimal strategy for the BAO detection does not necessarily require full sky coverage. For example; in a 1000 day-long survey by an eROSITA type telescope; an optimal strategy would be to survey a sky area of ∼9000 deg2; yielding a ∼16σ BAO detection. A similar detection will be achieved by ATHENA+ or WFXT class telescopes in a survey with a duration of 100 days; covering a similar sky area. XMM-Newton can achieve a marginal BAO detection in a 100-day survey covering ∼400 deg2. These surveys would demand a moderate-to-high cost in terms the optical follow-ups; requiring determination of redshifts of ∼105 (XMM-Newton) to ∼3 × 106 objects (eROSITA; ATHENA+; and WFXT) in these sky areas. © ESO; 2014;
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