Methods for cluster cosmology and application to the SDSS in preparation for DES Year 1 release

被引：90

作者：

Costanzi, M. ^{[1
,2
]}

Rozo, E. ^{[3
]}

Simet, M. ^{[4
]}

Zhang, Y. ^{[5
]}

Evrard, A. E. ^{[6
,7
]}

Mantz, A. ^{[8
]}

Rykoff, E. S. ^{[8
,9
]}

Jeltema, T. ^{[10
]}

Gruen, D. ^{[8
,9
]}

Allen, S. ^{[11
]}

McClintock, T. ^{[3
]}

Romer, A. K. ^{[12
]}

von der Linden, A. ^{[13
]}

Farahi, A. ^{[14
]}

DeRose, J. ^{[8
,11
]}

Varga, T. N. ^{[15
,30
]}

Weller, J. ^{[15
,16
,30
]}

Giles, P. ^{[12
]}

Hollowood, D. L. ^{[10
]}

Bhargava, S. ^{[12
]}

Bermeo-Hernandez, A. ^{[12
]}

Chen, X. ^{[7
]}

Abbott, T. M. C. ^{[17
]}

Abdalla, F. B. ^{[18
,19
]}

Avila, S. ^{[20
]}

Bechtol, K. ^{[21
]}

Brooks, D. ^{[18
]}

Buckley-Geer, E. ^{[5
]}

Burke, D. L. ^{[8
,9
]}

Rosell, A. Carnero ^{[22
,23
]}

Kind, M. Carrasco ^{[24
,25
]}

Carretero, J. ^{[26
]}

Crocce, M. ^{[27
,28
]}

Cunha, C. E. ^{[8
]}

da Costa, L. N. ^{[22
,23
]}

Davis, C. ^{[8
]}

De Vicente, J. ^{[29
]}

Diehl, H. T. ^{[5
]}

Dietrich, J. P. ^{[16
,30
]}

Doel, P. ^{[18
]}

Eifler, T. F. ^{[31
,32
]}

Estrada, J. ^{[5
]}

Flaugher, B. ^{[5
]}

Fosalba, P. ^{[27
,28
]}

Frieman, J. ^{[5
,33
]}

Garcia-Bellido, J. ^{[34
]}

Gaztanaga, E. ^{[27
,28
]}

Gerdes, D. W. ^{[6
,7
]}

Giannantonio, T. ^{[4
,30
,35
,36
]}

Gruendl, R. A. ^{[24
,25
]}

机构：

[1] INAF, Osservatorio Astron Trieste, Via GB Tiepolo 11, I-34143 Trieste, Italy

[2] IFPU, Via Beirut 2, I-34014 Trieste, Italy

[3] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA

[4] Univ Calif Riverside, Dept Phys & Astron, 900 Univ Ave, Riverside, CA 92521 USA

[5] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA

[6] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA

[7] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA

[8] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA

[9] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA

[10] Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA

[11] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA

[12] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England

[13] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA

[14] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA

[15] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garrhing, Germany

[16] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany

[17] Natl Opt Astron Observ, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile

[18] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England

[19] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa

[20] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England

[21] LSST, 933 North Cherry Ave, Tucson, AZ 85721 USA

[22] Lab Interinst & Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil

[23] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil

[24] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA

[25] Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA

[26] Barcelona Inst Sci & Technol, IFAE, Campus UAB, E-08193 Bellaterra, Barcelona, Spain

[27] IEEC, Barcelona 08193, Spain

[28] CSIC, Inst Space Sci, ICE, Campus UAB,Carrer Can Magrans S-N, E-08193 Barcelona, Spain

[29] Ctr Invest Energet Medioambientales & Tecnol CIEM, Madrid 28040, Spain

[30] Ludwig Maximilian Univ Munchen, Fak Phys, Univ Sternwarte, Scheinerstr 1, D-81679 Munich, Germany

[31] Steward Observ, Dept Astron, 933 North Cherry Ave, Tucson, AZ 85721 USA

[32] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA

[33] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA

[34] UAM, CSIC, Inst Fis Teor, E-28049 Madrid, Spain

[35] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England

[36] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England

[37] Swiss Fed Inst Technol, Dept Phys, Wolfgang Pauli Str 16, CH-8093 Zurich, Switzerland

[38] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA

[39] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA

[40] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA

[41] Australian Astron Observ, N Ryde, NSW 2113, Australia

[42] Univ Sao Paulo, Inst Fis, Dept Fis Matemat, CP 66318, BR-05314970 Sao Paulo, SP, Brazil

[43] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA

[44] Texas A&M Univ, Dept Phys & Astron, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA

[45] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA

[46] Inst Catalana Recerca & Estudis Avanots, E-08010 Barcelona, Spain

[47] Brookhaven Natl Lab, Bldg 510, Upton, NY 11973 USA

[48] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England

[49] Brandeis Univ, Phys Dept, 415 South St, Waltham, MA 02453 USA

[50] Univ Estadual Campinas, Inst Fis Gleb Wataghin, BR-13083859 Campinas, SP, Brazil

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2019年 / 488卷 / 04期

基金：

欧洲研究理事会; 美国国家科学基金会; 英国科学技术设施理事会; 澳大利亚研究理事会;

关键词：

galaxies: clusters: general; cosmological parameters; large-scale structure of Universe; HALO MASS FUNCTION; BARYON ACOUSTIC-OSCILLATIONS; LARGE-SCALE BIAS; OCCUPATION DISTRIBUTION; PARAMETER CONSTRAINTS; SHEAR CALIBRATION; GALAXY CLUSTERS; POWER-SPECTRUM; JOINT ANALYSIS; ASSEMBLY BIAS;

D O I：

10.1093/mnras/stz1949

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We implement the first blind analysis of cluster abundance data to derive cosmological constraints from the abundance and weak lensing signal of redMaPPer clusters in the Sloan Digital Sky Survey (SDSS). We simultaneously fit for cosmological parameters and the richness-mass relation of the clusters. For a flat Lambda cold dark matter cosmological model with massive neutrinos, we find . This value is both consistent and competitive with that derived from cluster catalogues selected in different wavelengths. Our result is also consistent with the combined probes analyses by the Dark Energy Survey (DES), the Kilo-Degree Survey (KiDS), and with the cosmic microwave background (CMB) anisotropies as measured by Planck. We demonstrate that the cosmological posteriors are robust against variation of the richness-mass relation model and to systematics associated with the calibration of the selection function. In combination with baryon acoustic oscillation data and big bang nucleosynthesis data (Cooke etal.), we constrain the Hubble rate to be h= 0.66 +/- 0.02, independent of the CMB. Future work aimed at improving our understanding of the scatter of the richness-mass relation has the potential to significantly improve the precision of our cosmological posteriors. The methods described in this work were developed for use in the forthcoming analysis of cluster abundances in the DES. Our SDSS analysis constitutes the first part of a staged-unblinding analysis of the full DES data set.

引用

页码：4779 / 4800

页数：22

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