Optimizing galaxy samples for clustering measurements in photometric surveys

Tanoglidis, Dimitrios; Chang, Chihway; Frieman, Joshua

doi:10.1093/mnras/stz3281

Title: Optimizing galaxy samples for clustering measurements in photometric surveys

Journal Article · Sat Nov 23 00:00:00 EST 2019 · Monthly Notices of the Royal Astronomical Society

DOI:https://doi.org/10.1093/mnras/stz3281· OSTI ID:1569241

^[1];

^[1]; Frieman, Joshua ^[2]

Univ. of Chicago, IL (United States). Kavli Inst. for Cosmological Physics
Univ. of Chicago, IL (United States). Kavli Inst. for Cosmological Physics; Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States). Accelerator Physics Center

When analysing galaxy clustering in multiband imaging surveys, there is a trade-off between selecting the largest galaxy samples (to minimize the shot noise) and selecting samples with the best photometric redshift (photo-$$z$$) precision, which generally includes only a small subset of galaxies. In this paper, we systematically explore this trade-off. Our analysis is targeted towards the third-year data of the Dark Energy Survey (DES), but our methods hold generally for other data sets. Using a simple Gaussian model for the redshift uncertainties, we carry out a Fisher matrix forecast for cosmological constraints from angular clustering in the redshift range $$z$$ = 0.2–0.95. We quantify the cosmological constraints using a figure of merit (FoM) that measures the combined constraints on $Ωm$ and $$σ_8$$ in the context of Λ cold dark matter ($$Λ$$CDM) cosmology. We find that the trade-off between sample size and photo-z precision is sensitive to (1) whether cross-correlations between redshift bins are included or not, and (2) the ratio of the redshift bin width $δz$ to the photo-$$z$$ precision $$σ_z$$. When cross-correlations are included and the redshift bin width is allowed to vary, the highest FoM is achieved when $δz$ ~ $$σ_z$$. We find that for the typical case of 5-10 redshift bins, optimal results are reached when we use larger, less precise photo-z samples, provided that we include cross-correlations. For samples with higher $$σ_z$$, the overlap between redshift bins is larger, leading to higher cross-correlation amplitudes. This leads to the self-calibration of the photo-z parameters and therefore tighter cosmological constraints. These results can be used to help guide galaxy sample selection for clustering analysis in ongoing and future photometric surveys.

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Research Organization:: Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States)

Sponsoring Organization:: USDOE Office of Science (SC), High Energy Physics (HEP)

Grant/Contract Number:: AC02-07CH11359

OSTI ID:: 1569241

Report Number(s):: arXiv:1908.07150; FERMILAB-PUB-19-486-A; oai:inspirehep.net:1750379; TRN: US2001376

Journal Information:: Monthly Notices of the Royal Astronomical Society, Vol. 491, Issue 3; ISSN 0035-8711

Publisher:: Royal Astronomical SocietyCopyright Statement

Country of Publication:: United States

Language:: English

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Cited by: 5 works

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