Photometric Redshift Requirements for Self-Calibration of Cluster Dark Energy Studies
The ability to constrain dark energy from the evolution of galaxy cluster counts is limited by the imperfect knowledge of cluster redshifts. Ongoing and upcoming surveys will mostly rely on redshifts estimated from broad-band photometry (photo-z's). For a Gaussian distribution for the cluster p...
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ftdatacite:10.48550/arxiv.0709.2871 2023-05-15T18:22:45+02:00 Photometric Redshift Requirements for Self-Calibration of Cluster Dark Energy Studies Lima, Marcos Hu, Wayne 2007 https://dx.doi.org/10.48550/arxiv.0709.2871 https://arxiv.org/abs/0709.2871 unknown arXiv https://dx.doi.org/10.1103/physrevd.76.123013 Assumed arXiv.org perpetual, non-exclusive license to distribute this article for submissions made before January 2004 http://arxiv.org/licenses/assumed-1991-2003/ Astrophysics astro-ph FOS Physical sciences article-journal Article ScholarlyArticle Text 2007 ftdatacite https://doi.org/10.48550/arxiv.0709.2871 https://doi.org/10.1103/physrevd.76.123013 2022-04-01T15:26:53Z The ability to constrain dark energy from the evolution of galaxy cluster counts is limited by the imperfect knowledge of cluster redshifts. Ongoing and upcoming surveys will mostly rely on redshifts estimated from broad-band photometry (photo-z's). For a Gaussian distribution for the cluster photo-z errors and a high cluster yield cosmology defined by the WMAP 1 year results, the photo-z bias and scatter needs to be known better than 0.003 and 0.03, respectively, in order not to degrade dark energy constrains by more than 10% for a survey with specifications similar to the South Pole Telescope. Smaller surveys and cosmologies with lower cluster yields produce weaker photo-z requirements, though relative to worse baseline constraints. Comparable photo-z requirements are necessary in order to employ self-calibration techniques when solving for dark energy and observable-mass parameters simultaneously. On the other hand, self-calibration in combination with external mass inferences helps reduce photo-z requirements and provides important consistency checks for future cluster surveys. In our fiducial model, training sets with spectroscopic redshifts for ~5%-15% of the detected clusters are required in order to keep degradations in the dark energy equation of state lower than 20%. : 18 pages, 8 figures, submitted to PRD Text South pole DataCite Metadata Store (German National Library of Science and Technology) South Pole |
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Astrophysics astro-ph FOS Physical sciences |
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Astrophysics astro-ph FOS Physical sciences Lima, Marcos Hu, Wayne Photometric Redshift Requirements for Self-Calibration of Cluster Dark Energy Studies |
topic_facet |
Astrophysics astro-ph FOS Physical sciences |
description |
The ability to constrain dark energy from the evolution of galaxy cluster counts is limited by the imperfect knowledge of cluster redshifts. Ongoing and upcoming surveys will mostly rely on redshifts estimated from broad-band photometry (photo-z's). For a Gaussian distribution for the cluster photo-z errors and a high cluster yield cosmology defined by the WMAP 1 year results, the photo-z bias and scatter needs to be known better than 0.003 and 0.03, respectively, in order not to degrade dark energy constrains by more than 10% for a survey with specifications similar to the South Pole Telescope. Smaller surveys and cosmologies with lower cluster yields produce weaker photo-z requirements, though relative to worse baseline constraints. Comparable photo-z requirements are necessary in order to employ self-calibration techniques when solving for dark energy and observable-mass parameters simultaneously. On the other hand, self-calibration in combination with external mass inferences helps reduce photo-z requirements and provides important consistency checks for future cluster surveys. In our fiducial model, training sets with spectroscopic redshifts for ~5%-15% of the detected clusters are required in order to keep degradations in the dark energy equation of state lower than 20%. : 18 pages, 8 figures, submitted to PRD |
format |
Text |
author |
Lima, Marcos Hu, Wayne |
author_facet |
Lima, Marcos Hu, Wayne |
author_sort |
Lima, Marcos |
title |
Photometric Redshift Requirements for Self-Calibration of Cluster Dark Energy Studies |
title_short |
Photometric Redshift Requirements for Self-Calibration of Cluster Dark Energy Studies |
title_full |
Photometric Redshift Requirements for Self-Calibration of Cluster Dark Energy Studies |
title_fullStr |
Photometric Redshift Requirements for Self-Calibration of Cluster Dark Energy Studies |
title_full_unstemmed |
Photometric Redshift Requirements for Self-Calibration of Cluster Dark Energy Studies |
title_sort |
photometric redshift requirements for self-calibration of cluster dark energy studies |
publisher |
arXiv |
publishDate |
2007 |
url |
https://dx.doi.org/10.48550/arxiv.0709.2871 https://arxiv.org/abs/0709.2871 |
geographic |
South Pole |
geographic_facet |
South Pole |
genre |
South pole |
genre_facet |
South pole |
op_relation |
https://dx.doi.org/10.1103/physrevd.76.123013 |
op_rights |
Assumed arXiv.org perpetual, non-exclusive license to distribute this article for submissions made before January 2004 http://arxiv.org/licenses/assumed-1991-2003/ |
op_doi |
https://doi.org/10.48550/arxiv.0709.2871 https://doi.org/10.1103/physrevd.76.123013 |
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1766202167412129792 |