The Atacama Cosmology Telescope: Cosmology From Galaxy Clusters Detected via the Sunyaev-Zel'dovich Effect

Sehgal, Neelima; Trac, Hy; Acquaviva, Viviana; Ade, Peter A. R.; Aguirre, Paula; Amiri, M.; Appel, John W.; Barrientos, L. Felipe; Battistelli, E. S.; Bond, J. R.; Brown, Ben; Burger, B.; Chervenak, J. A.; Das, Sudeep; Devlin, Mark J.; Dicker, Simon; Doriese, W. B.; Dunkley, Joanna; Dünner, Rolando; Essinger‐Hileman, T.; Fisher, R. P.; Fowler, Joseph W.; Hajian, Amir; Halpern, M.; Hasselfield, Matthew; Hernández-Monteagudo, C.; Hilton, G. C.; Hilton, Matt; Hincks, Adam D.; Hložek, Renée; Holtz, David; Huffenberger, K. M.; Hughes, D. H.; Hughes, John P.; Infante, L.; Irwin, K. D.; Jones, Andrew; Juin, J. B.; Klein, Jeff; Kosowsky, Arthur; Lau, Judy M.; Limon, M.; Lin, Yen-Ting; Lupton, Robert H.; Marriage, Tobias A.; Marsden, Danica; Martocci, Krista; Mauskopf, Philip Daniel; Menanteau, F.; Moodley, Kavilan; Moseley, H.; Netterfield, C. B.; Niemack, Michael D.; Nolta, Michael R.; Page, Lyman A.; Parker, Lucas; Partridge, B.; Reid, Beth; Sherwin, Blake D.; Sievers, Jonathan; Spergel, David N.; Staggs, Suzanne T.; Swetz, Daniel S.; Switzer, Eric R.; Thornton, Robert J.; Tucker, C.; Warne, Ryan; Wollack, Edward J.; Zhao, Yue

doi:10.1088/0004-637x/732/1/44

Cited by 149 publications

(143 citation statements)

References 76 publications

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“…However, recent work that uses stacked weak lensing analysis for mass calibration (Johnston et al, 2007;Mandelbaum et al, 2008;Sheldon et al, 2009) has allowed optical samples to achieve the same level of precision as X-ray samples , with comparable levels of systematic error. Constraints from SZ selected samples are emerging (Vanderlinde et al, 2010;Sehgal et al, 2011;Reichardt et al, 2013), and while they are currently weak because of the relatively large uncertainty in the SZ-mass scaling relation, the extensive follow-up campaigns that are currently underway will reduce this scaling uncertainty and bring these constraints to a level comparable to those from optical and X-ray cluster catalogs (e.g. High et al, 2012;Hoekstra et al, 2012;Planck Collaboration, 2012;Rozo et al, 2012d).…”

Section: The Current State Of Playmentioning

confidence: 99%

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Observational probes of cosmic acceleration

et al. 2013

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The accelerating expansion of the universe is the most surprising cosmological discovery in many decades, implying that the universe is dominated by some form of "dark energy" with exotic physical properties, or that Einstein's theory of gravity breaks down on cosmological scales. The profound implications of cosmic acceleration have inspired ambitious efforts to understand its origin, with experiments that aim to measure the history of expansion and growth of structure with percent-level precision or higher. We review in detail the four most well established methods for making such measurements: Type Ia supernovae, baryon acoustic oscillations (BAO), weak gravitational lensing, and the abundance of galaxy clusters. We pay particular attention to the systematic uncertainties in these techniques and to strategies for controlling them at the level needed to exploit "Stage IV" dark energy facilities such as BigBOSS, LSST, Euclid, and WFIRST. We briefly review a number of other approaches including redshift-space distortions, the Alcock-Paczynski effect, and direct measurements of the Hubble constant H 0 . We present extensive forecasts for constraints on the dark energy equation of state and parameterized deviations from General Relativity, achievable with Stage III and Stage IV experimental programs that incorporate supernovae, BAO, weak lensing, and cosmic microwave background data. We also show the level of precision required for clusters or other methods to provide constraints competitive with those of these fiducial programs. We emphasize the value of a balanced program that employs several of the most powerful methods in combination, both to cross-check systematic uncertainties and to take advantage of complementary information. Surveys to probe cosmic acceleration produce data sets that support a wide range of scientific investigations, and they continue the longstanding astronomical tradition of mapping the universe in ever greater detail over ever larger scales.

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Section: The Current State Of Playmentioning

confidence: 99%

“…Vanderlinde et al, 2010;Sehgal et al, 2011). The main difficulty that simulation methods face is our incomplete understanding of baryonic physics, particularly galaxy formation feedback processes.…”

Section: Calibrating the Observable-mass Relationmentioning

confidence: 99%

Observational probes of cosmic acceleration

et al. 2013

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“…Observations testing the predicted mass function and cluster baryon ⋆ E-mail: amantz@slac.stanford.edu fraction have largely validated CDM (e.g. White et al 1993;Bahcall & Fan 1998;Reiprich & Böhringer 2002;Ettori et al 2003Ettori et al , 2009Allen et al 2004Allen et al , 2008Allen et al , 2011Vikhlinin et al 2009;Mantz et al 2010Mantz et al , 2015bRozo et al 2010;Sehgal et al 2011;Benson et al 2013;Hasselfield et al 2013;Planck Collaboration 2014, 2015.…”

Section: Introductionmentioning

confidence: 99%

Cosmology and astrophysics from relaxed galaxy clusters – V. Consistency with cold dark matter structure formation

Mantz

Allen

Morris

2016

Mon. Not. R. Astron. Soc.

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This is the fifth in a series of papers studying the astrophysics and cosmology of massive, dynamically relaxed galaxy clusters. Our sample comprises 40 clusters identified as being dynamically relaxed and hot in Papers I and II of this series. Here we use constraints on cluster mass profiles from X-ray data to test some of the basic predictions of cosmological structure formation in the Cold Dark Matter (CDM) paradigm. We present constraints on the concentration-mass relation for massive clusters, finding a power-law mass dependence with a slope of κ m = −0.16 ± 0.07, in agreement with CDM predictions. For this relaxed sample, the relation is consistent with a constant as a function of redshift (power-law slope with 1 + z of κ ζ = −0.17 ± 0.26), with an intrinsic scatter of σ ln c = 0.16 ± 0.03. We investigate the shape of cluster mass profiles over the radial range probed by the data (typically ∼ 50 kpc-1 Mpc), and test for departures from the simple Navarro, Frenk & White (NFW) form, for which the logarithmic slope of the density profile tends to −1 at small radii. Specifically, we consider as alternatives the generalized NFW (GNFW) and Einasto parametrizations. For the GNFW model, we find an average value of (minus) the logarithmic inner slope of β = 1.02 ± 0.08, with an intrinsic scatter of σ β = 0.22 ± 0.07, while in the Einasto case we constrain the average shape parameter to be α = 0.29 ± 0.04 with an intrinsic scatter of σ α = 0.12 ± 0.04. Our results are thus consistent with the simple NFW model on average, but we clearly detect the presence of intrinsic, cluster-to-cluster scatter about the average.

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“…Being the most massive bound systems in the universe, they trace the latest stage of structure formation. Their abundance and mass as a function of redshift are thus highly indicative of how the growth of the cosmic density fluctuations occurs and can thus be used to constrain the matter content, the initial power spectrum normalisation and the expansion history of the universe (Eke et al 1998;Borgani et al 2001;Reiprich & Böhringer 2002;Allen et al 2003;Schuecker et al 2003;Henry 2004;Vikhlinin et al 2009;Mantz et al 2010;Rozo et al 2010;Sehgal & et al 2011;Planck Collaboration et al 2014a;Benson et al 2013;Mantz et al 2014). …”

Section: Introductionmentioning

confidence: 99%

Cosmology through arc statistics I: sensitivity to Ω_mand σ₈

Boldrin

Giocoli

Meneghetti

et al. 2016

Mon. Not. R. Astron. Soc.

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The next generation of large sky photometric surveys will finally be able to use arc statistics as a cosmological probe. Here we present the first of a series of papers on this topic. In particular, we study how arc counts are sensitive to the variation of two cosmological parameters: the (total) matter density parameter, Ω m , and the normalisation of the primordial power spectrum, expressed in terms of σ 8 . Both these parameters influence the abundances of collapsed structures and their internal structure. We compute the expected number of gravitational arcs with various length-to-width ratios in mock light cones, by varying these cosmological parameters in the ranges 0.1 Ω m 0.5 and 0.6 σ 8 1. We find that the arc counts dependence on Ω m and σ 8 is similar, but not identical, to that of the halo counts. We investigate how the precision of the constraints on the cosmological parameters based on arc counts depends on the survey area. We find that the constraining power of arc statistics degrades critically only for surveys covering an area smaller than 10% of the whole sky. Finally, we consider the case in which the search for arcs is done only in frames where galaxy clusters have been previously identified. Adopting the selection function for galaxy clusters expected to be detected from photometric data in future wide surveys, we find that less than 10% of the arcs will be missed, with only a small degradation of the corresponding cosmological constraints.

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The Atacama Cosmology Telescope: Cosmology From Galaxy Clusters Detected via the Sunyaev-Zel'dovich Effect

Cited by 149 publications

References 76 publications

Observational probes of cosmic acceleration

Observational probes of cosmic acceleration

Cosmology and astrophysics from relaxed galaxy clusters – V. Consistency with cold dark matter structure formation

Cosmology through arc statistics I: sensitivity to Ω_mand σ₈

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The Atacama Cosmology Telescope: Cosmology From Galaxy Clusters Detected via the Sunyaev-Zel'dovich Effect

Cited by 149 publications

References 76 publications

Observational probes of cosmic acceleration

Observational probes of cosmic acceleration

Cosmology and astrophysics from relaxed galaxy clusters – V. Consistency with cold dark matter structure formation

Cosmology through arc statistics I: sensitivity to Ωmand σ8

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Resources

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Cosmology through arc statistics I: sensitivity to Ω_mand σ₈