Query : 2014A&A...572A..28H

2014A&A...572A..28H - Astronomy and Astrophysics, volume 572A, 28-28 (2014/12-1)

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


Abstract (from CDS):

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 10–15erg/s/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 ∼9000deg2, 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 ∼400deg2. These surveys would demand a moderate-to-high cost in terms the optical follow-ups, requiring determination of redshifts of ∼105 (XMM-Newton) to ∼3x106 objects (eROSITA, ATHENA+, and WFXT) in these sky areas.

Abstract Copyright:

Journal keyword(s): galaxies: active - X-rays: galaxies - cosmology: theory - large-scale structure of Universe

Simbad objects: 3

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Number of rows : 3
N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
1 NAME Chandra Deep Field-South reg 03 32 28.0 -27 48 30           ~ 2063 1
2 NAME COSMOS Field reg 10 00 28.60 +02 12 21.0           ~ 2869 0
3 NAME Chandra Deep Field-North reg 12 36.8 +62 13           ~ 657 0

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