Constraints on Cosmological Parameters from Future Galaxy Cluster Surveys

By Zoltán Haiman, Joseph J. Mohr, G. Holder. 2000

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We study the expected redshift evolution of galaxy cluster abundance between 0 ≲ z ≲ 3 in different cosmologies, including the effects of the cosmic equation of state parameter w ≡ p/ρ. Using the halo mass function obtained in recent large-scale numerical simulations, we model the expected cluster yields in a 12 deg2 Sunyaev-Zeldovich effect (SZE) survey and a deep 104 deg2 X-ray survey over a wide range of cosmological parameters. We quantify the statistical differences among cosmologies using both the total number and redshift distribution of clusters. Provided that the local cluster abundance is known to a few percent accuracy, we find only mild degeneracies between w and either Ωm or h. As a result, both surveys will provide improved constraints on Ωm and w. The Ωm-w degeneracy from both surveys is complementary to those found either in studies of cosmic microwave background (CMB) anisotropies or of high-redshift supernovae (SNe). As a result, combining these surveys together with either CMB or SNe studies can reduce the statistical uncertainty on both w and Ωm to levels below what could be obtained by combining only the latter two data sets. Our results indicate a formal statistical uncertainty of ≈3% (68% confidence) on both Ωm and w when the SZE survey is combined with either the CMB or SN data; the large number of clusters in the X-ray survey further suppresses the degeneracy between w and both Ωm and h. Systematics and internal evolution of cluster structure at the present pose uncertainties above these levels. We briefly discuss and quantify the relevant systematic errors. By focusing on clusters with measured temperatures in the X-ray survey, we reduce our sensitivity to systematics such as nonstandard evolution of internal cluster structure.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/d6ff280142d4d5dbb6725f6853f606aabfb5d042

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Citations in the corpus

The X-Ray Luminosity-Mass Relation for Local Clusters of Galaxies (2006, background): “The counts, spatial clustering and bulk properties of the most massive halos in the universe offer a means to test cosmological physics (Wang & Steinhardt 1998; Haiman et al. 2001; Carlstrom et al. 2002; Majumdar & Mohr 2003; Battye & Weller 2003; Wang et al. 2004).”
GALAXY CLUSTERS DISCOVERED VIA THE SUNYAEV–ZEL’DOVICH EFFECT IN THE FIRST 720 SQUARE DEGREES OF THE SOUTH POLE TELESCOPE SURVEY (2012, background): “…current constraints on cosmological parameters, including the equation of state of dark energy and the sum of the neutrino masses (Wang & Steinhardt 1998; Haiman et al. 2001; Holder et al. 2001; Battye & Weller 2003; Molnar et al. 2004; Wang et al. 2004, 2005; Lima & Hu 2007; Shimon et al. 2011).”
The large-scale structure of the Universe (2006, background): “This probes the growth of the mass fluctuation spectrum and the variation of the cosmological volume elemen”
X-RAY PROPERTIES OF THE FIRST SUNYAEV–ZEL'DOVICH EFFECT SELECTED GALAXY CLUSTER SAMPLE FROM THE SOUTH POLE TELESCOPE (2010, background): “…(IKI), Profsoyuznaya 84/32, Moscow, Russia 2 Large area cluster surveys extending to high redshift can be used to study the evolution of the abundance of galaxy clusters, thereby delivering precise constraints on the amount and nature of the dark energy (Wang & Steinhardt 1998; Haiman et al. 2001).”
Planck 2013 results. XX. Cosmology from Sunyaev-Zeldovich cluster counts (2013, background): “…ESA and a scientific consortium led and funded by Denmark. the possibility of using SZ-selected cluster samples to constrain cosmological parameters (Barbosa et al. 1996; Aghanim et al. 1997; Haiman et al. 2001; Holder et al. 2001; Weller et al. 2002; Diego et al. 2002; Battye & Weller 2003).”
CLASH: JOINT ANALYSIS OF STRONG-LENSING, WEAK-LENSING SHEAR, AND MAGNIFICATION DATA FOR 20 GALAXY CLUSTERS (2015, background): “…3RH, UK 7 Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA 8 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21208, USA late the exponential tail of the cosmic mass function of darkmatter (DM, hereafter) halos (Haiman et al. 2001).”
GALAXY CLUSTERS DISCOVERED WITH A SUNYAEV–ZEL'DOVICH EFFECT SURVEY (2008, methodology): “A catalog of clusters with masses and redshifts can be used to constrain the matter density, the density fluctuation amplitude, and the dark energy equation of state (Wang & Steinhardt 1998; Haiman et al. 2001; Holder et al. 2001; Molnar et al. 2004; Wang et al. 2004; Lima & Hu 2007).”
THE ATACAMA COSMOLOGY TELESCOPE: SUNYAEV–ZEL'DOVICH-SELECTED GALAXY CLUSTERS AT 148 GHz IN THE 2008 SURVEY (2010, background): “Galaxy cluster surveys are one of the few methods that probe the growth of structure and interpretation of survey yields has the potential to precisely constrain the equation of state of dark energy (e.g., Bartlett & Silk 1994; Holder et al. 2000; Haiman et al. 2001; Majumdar & Mohr 2004).”
MASS FUNCTION PREDICTIONS BEYOND ΛCDM (2010, background): “Because large and massive halos form very late, the high-mass tail of the mass function – the regime of cluster-scale masses – is exponentially sensitive to dark energyrelated parameters (Haiman et al. 2001).”
The 400 Square Degree ROSAT PSPC Galaxy Cluster Survey: Catalog and Statistical Calibration (2006, methodology): “Clusters also can be used as an independent and complementary Dark Energy probe (Starobinsky 1998; Wang & Steinhardt 1998; Huterer & Turner 2001; Haiman et al. 2001; Battye & Weller 2003; Molnar et al. 2004; Hu & Cohn 2006).”
Sample Variance Considerations for Cluster Surveys (2002, background): “Recently, its use in constraining the density and equation of state of the dark energy using planned Sunyaev-Zel’dovich (SZ) cluster surveys has been the focus of several studies (Haiman et al. 2001; Weller et al. 2001).”
Total mass biases in X-ray galaxy clusters (2008, background): “Measurements of fb at high redshifts can be used to derive constraints on the equation of state of the dark energy (Haiman et al. 2001; Majumdar & Mohr 2004; Allen et al. 2008).”