### Abstract

Deep pencil beam surveys (<1 deg^{2}) are of fundamental importance for studying the high-redshift universe. However, inferences about galaxy population properties (e.g., the abundance of objects) are in practice limited by "cosmic variance." This is the uncertainty in observational estimates of the number density of galaxies arising from the underlying large-scale density fluctuations. This source of uncertainty can be significant, especially for surveys which cover only small areas and for massive high-redshift galaxies. Cosmic variance for a given galaxy population can be determined using predictions from cold dark matter theory and the galaxy bias. In this paper, we provide tools for experiment design and interpretation. For a given survey geometry, we present the cosmic variance of dark matter as a function of mean redshift z̄ and redshift bin size Δz. Using a halo occupation model to predict galaxy clustering, we derive the galaxy bias as a function of mean redshift for galaxy samples of a given stellar mass range. In the linear regime, the cosmic variance of these galaxy samples is the product of the galaxy bias and the dark matter cosmic variance. We present a simple recipe using a fitting function to compute cosmic variance as a function of the angular dimensions of the field, z̄, Δz, and stellar mass m _{*}. We also provide tabulated values and a software tool. The accuracy of the resulting cosmic variance estimates (δσ_{v}/ σ_{v}) is shown to be better than 20%. We find that for GOODS at z̄ = 2 and with Δz = 0.5, the relative cosmic variance of galaxies with m _{*}>10^{11} M _{⊙} is ∼38%, while it is ∼27% for GEMS and 12% for COSMOS. For galaxies of m _{*} 10^{10} M _{⊙}, the relative cosmic variance is ∼19% for GOODS, ∼13% for GEMS, and ∼6% for COSMOS. This implies that cosmic variance is a significant source of uncertainty at z̄ = 2 for small fields and massive galaxies, while for larger fields and intermediate mass galaxies, cosmic variance is less serious.

Original language | English (US) |
---|---|

Article number | 113 |

Journal | Astrophysical Journal |

Volume | 731 |

Issue number | 2 |

DOIs | |

State | Published - Apr 20 2011 |

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### All Science Journal Classification (ASJC) codes

- Nuclear and High Energy Physics
- Space and Planetary Science
- Astronomy and Astrophysics

### Keywords

- cosmology: theory
- galaxies: high-redshift
- galaxies: statistics
- galaxies: stellar content
- large-scale structure of universe

### Cite this

*Astrophysical Journal*,

*731*(2), [113]. https://doi.org/10.1088/0004-637X/731/2/113

}

*Astrophysical Journal*, vol. 731, no. 2, 113. https://doi.org/10.1088/0004-637X/731/2/113

**A cosmic variance cookbook.** / Moster, Benjamin P.; Somerville, Rachel; Newman, Jeffrey A.; Rix, Hans Walter.

Research output: Contribution to journal › Article

TY - JOUR

T1 - A cosmic variance cookbook

AU - Moster, Benjamin P.

AU - Somerville, Rachel

AU - Newman, Jeffrey A.

AU - Rix, Hans Walter

PY - 2011/4/20

Y1 - 2011/4/20

N2 - Deep pencil beam surveys (<1 deg2) are of fundamental importance for studying the high-redshift universe. However, inferences about galaxy population properties (e.g., the abundance of objects) are in practice limited by "cosmic variance." This is the uncertainty in observational estimates of the number density of galaxies arising from the underlying large-scale density fluctuations. This source of uncertainty can be significant, especially for surveys which cover only small areas and for massive high-redshift galaxies. Cosmic variance for a given galaxy population can be determined using predictions from cold dark matter theory and the galaxy bias. In this paper, we provide tools for experiment design and interpretation. For a given survey geometry, we present the cosmic variance of dark matter as a function of mean redshift z̄ and redshift bin size Δz. Using a halo occupation model to predict galaxy clustering, we derive the galaxy bias as a function of mean redshift for galaxy samples of a given stellar mass range. In the linear regime, the cosmic variance of these galaxy samples is the product of the galaxy bias and the dark matter cosmic variance. We present a simple recipe using a fitting function to compute cosmic variance as a function of the angular dimensions of the field, z̄, Δz, and stellar mass m *. We also provide tabulated values and a software tool. The accuracy of the resulting cosmic variance estimates (δσv/ σv) is shown to be better than 20%. We find that for GOODS at z̄ = 2 and with Δz = 0.5, the relative cosmic variance of galaxies with m *>1011 M ⊙ is ∼38%, while it is ∼27% for GEMS and 12% for COSMOS. For galaxies of m * 1010 M ⊙, the relative cosmic variance is ∼19% for GOODS, ∼13% for GEMS, and ∼6% for COSMOS. This implies that cosmic variance is a significant source of uncertainty at z̄ = 2 for small fields and massive galaxies, while for larger fields and intermediate mass galaxies, cosmic variance is less serious.

AB - Deep pencil beam surveys (<1 deg2) are of fundamental importance for studying the high-redshift universe. However, inferences about galaxy population properties (e.g., the abundance of objects) are in practice limited by "cosmic variance." This is the uncertainty in observational estimates of the number density of galaxies arising from the underlying large-scale density fluctuations. This source of uncertainty can be significant, especially for surveys which cover only small areas and for massive high-redshift galaxies. Cosmic variance for a given galaxy population can be determined using predictions from cold dark matter theory and the galaxy bias. In this paper, we provide tools for experiment design and interpretation. For a given survey geometry, we present the cosmic variance of dark matter as a function of mean redshift z̄ and redshift bin size Δz. Using a halo occupation model to predict galaxy clustering, we derive the galaxy bias as a function of mean redshift for galaxy samples of a given stellar mass range. In the linear regime, the cosmic variance of these galaxy samples is the product of the galaxy bias and the dark matter cosmic variance. We present a simple recipe using a fitting function to compute cosmic variance as a function of the angular dimensions of the field, z̄, Δz, and stellar mass m *. We also provide tabulated values and a software tool. The accuracy of the resulting cosmic variance estimates (δσv/ σv) is shown to be better than 20%. We find that for GOODS at z̄ = 2 and with Δz = 0.5, the relative cosmic variance of galaxies with m *>1011 M ⊙ is ∼38%, while it is ∼27% for GEMS and 12% for COSMOS. For galaxies of m * 1010 M ⊙, the relative cosmic variance is ∼19% for GOODS, ∼13% for GEMS, and ∼6% for COSMOS. This implies that cosmic variance is a significant source of uncertainty at z̄ = 2 for small fields and massive galaxies, while for larger fields and intermediate mass galaxies, cosmic variance is less serious.

KW - cosmology: theory

KW - galaxies: high-redshift

KW - galaxies: statistics

KW - galaxies: stellar content

KW - large-scale structure of universe

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UR - http://www.scopus.com/inward/citedby.url?scp=79954990305&partnerID=8YFLogxK

U2 - 10.1088/0004-637X/731/2/113

DO - 10.1088/0004-637X/731/2/113

M3 - Article

AN - SCOPUS:79954990305

VL - 731

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2

M1 - 113

ER -