000150275 001__ 150275
000150275 005__ 20251017144636.0
000150275 0247_ $$2doi$$a10.1111/j.1365-2966.2012.21972.x
000150275 0248_ $$2sideral$$a142477
000150275 037__ $$aART-2012-142477
000150275 041__ $$aeng
000150275 100__ $$0(orcid)0000-0002-6211-499X$$aAsorey, J.
000150275 245__ $$aRecovering 3D clustering information with angular correlations
000150275 260__ $$c2012
000150275 5060_ $$aAccess copy available to the general public$$fUnrestricted
000150275 5203_ $$aWe study how to recover the full 3D clustering information ofP(k, z), including redshift space distortions (RSD), from 2D tomography using the angular auto- and cross-spectra of different redshift bins Cℓ(z, z′). We focus on quasi-linear scales where the minimum scale λmin or corresponding maximum wavenumber kmax = 2π/λmin is targeted to be in the range kmax = {0.05-0.2} h Mpc−1. For spectroscopic surveys, we find that we can recover the full 3D clustering information when the redshift bin width Δz used in the 2D tomography is similar to the targeted minimum scale, i.e. Δz ≃ {0.6.0.8} λminH(z)/c which corresponds to Δz ≃ 0.01-0.05 for z < 1. This value of Δz is optimal in the sense that larger values of Δz lose information, while smaller values violate our minimum-scale requirement. For a narrow-band photometric survey, with photo-z error σz = 0.004, we find almost identical results to the spectroscopic survey because the photo-z error is smaller than the optimal bin width σz < Δz. For a typical broad-band photometric survey with σz = 0.1, we have that σz > Δz and most radial information is intrinsically lost. The remaining information can be recovered from the 2D tomography if we use Δz ≃ 2σz. While 3D and 2D analyses are shown here to be equivalent, the advantage of using angular positions and redshifts is that we do not need a fiducial cosmology to convert to 3D coordinates. This avoids assumptions and marginalization over the fiducial model. In addition, it becomes straightforward to combine RSD, clustering and weak lensing in 2D space.
000150275 540__ $$9info:eu-repo/semantics/openAccess$$aAll rights reserved$$uhttp://www.europeana.eu/rights/rr-f/
000150275 590__ $$a5.521$$b2012
000150275 591__ $$aASTRONOMY & ASTROPHYSICS$$b9 / 56 = 0.161$$c2012$$dQ1$$eT1
000150275 655_4 $$ainfo:eu-repo/semantics/article$$vinfo:eu-repo/semantics/publishedVersion
000150275 700__ $$aCrocce, M.
000150275 700__ $$aGaztanaga, E.
000150275 700__ $$aLewis, A.
000150275 773__ $$g427, 3 (2012), 1891-1902$$pMon. not. R. Astron. Soc.$$tMonthly notices of the Royal Astronomical Society$$x0035-8711
000150275 8564_ $$s661517$$uhttps://zaguan.unizar.es/record/150275/files/texto_completo.pdf$$yVersión publicada
000150275 8564_ $$s2655491$$uhttps://zaguan.unizar.es/record/150275/files/texto_completo.jpg?subformat=icon$$xicon$$yVersión publicada
000150275 909CO $$ooai:zaguan.unizar.es:150275$$particulos$$pdriver
000150275 951__ $$a2025-10-17-14:29:41
000150275 980__ $$aARTICLE