| Texto completo | |
| Autor(es): Mostrar menos - |
Kiiveri, K.
[1, 2]
;
Gruen, D.
[3, 4]
;
Finoguenov, A.
[1]
;
Erben, T.
[5]
;
van Waerbeke, L.
[6]
;
Rykoff, E.
[3, 4]
;
Miller, L.
[7]
;
Hagstotz, S.
[8]
;
Dupke, R.
[9, 10, 11, 12]
;
Henry, J. Patrick
[13]
;
Kneib, J-P
[14, 15]
;
Gozaliasl, G.
[1, 2]
;
Kirkpatrick, C. C.
[1, 2]
;
Cibirka, N.
[16, 17]
;
Clerc, N.
[18, 19]
;
Costanzi, M.
[20, 21]
;
Cypriano, E. S.
[17]
;
Rozo, E.
[22]
;
Shan, H.
[23]
;
Spinelli, P.
[24]
;
Valiviita, J.
[25, 2]
;
Weller, J.
[16, 26]
Número total de Autores: 22
|
| Afiliação do(s) autor(es): Mostrar menos - | [1] Univ Helsinki, Dept Phys, POB 64, FI-00014 Helsinki - Finland
[2] Univ Helsinki, Helsinki Inst Phys, Gustaf Hallstromin Katu 2, POB 64, FI-00014 Helsinki - Finland
[3] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 - USA
[4] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 - USA
[5] Argelander Inst Astron, Hugel 71, D-53121 Bonn - Germany
[6] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1 - Canada
[7] Univ Oxford, Dept Phys, Keble Rd, Oxford OX1 3RH - England
[8] Stockholm Univ, AlbaNova Univ Ctr, Oskar Klein Ctr, Dept Phys, SE-10691 Stockholm - Sweden
[9] Univ Alabama, Dept Phys & Astron, Box 870324, Tuscaloosa, AL 35487 - USA
[10] Observ Nacl, Rua Gal Jose Cristino, BR-20921400 Rio De Janeiro - Brazil
[11] Univ Michigan, Dept Astron, 311 West Hall 1085 South Univ Ave, Ann Arbor, MI 48109 - USA
[12] Eureka Sci Inc, 2452 Delmer St Suite 100, Oakland, CA 94602 - USA
[13] Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 - USA
[14] Ecole Polytech Fed Lausanne EPFL, Lab Astrophys, Observ Sauverny, CH-1290 Versoix - Switzerland
[15] Aix Marseille Univ, LAM Lab Astrophys Marseille UMR 7326, CNRS, F-13388 Marseille - France
[16] Ludwig Maximilians Univ Munchen, Univ Sternwarte, Fak Phys, Scheinerstr 1, D-81679 Munich - Germany
[17] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, R Matao 1226, BR-05508090 Sao Paulo - Brazil
[18] CNRS, IRAP, 9 Av Colonel Roche, Postal Code 44346, F-31028 Toulouse - France
[19] Univ Toulouse, UPS OMP, Toulouse - France
[20] INAF Osservatorio Astron Trieste, Via GB Tiepolo 11, I-34143 Trieste - Italy
[21] IFPU Inst Fundamental Phys Universe, Via Beirut 2, I-34014 Trieste - Italy
[22] Univ Arizona, Dept Phys, 1118 E Fourth St, Tucson, AZ 85721 - USA
[23] Shanghai Astron Observ SHAO, Nandan Rd 80, Shanghai 200030 - Peoples R China
[24] Museu Astron & Ciencias Afins MAST, Rua Gen Bruce 586, BR-20921030 Rio De Janeiro - Brazil
[25] Univ Jyvaskyla, Dept Phys, POB 35 YFL, FI-40014 Jyvaskyla - Finland
[26] Excellence Cluster ORIGINS, Boltzmannstr 2, D-85748 Garching - Germany
Número total de Afiliações: 26
|
| Tipo de documento: | Artigo Científico |
| Fonte: | Monthly Notices of the Royal Astronomical Society; v. 502, n. 1, p. 1494-1526, MAR 2021. |
| Citações Web of Science: | 0 |
| Resumo | |
The COnstrain Dark Energy with X-ray clusters (CODEX) sample contains the largest flux limited sample of X-ray clusters at 0.35 < z < 0.65. It was selected from ROSAT data in the 10 000 square degrees of overlap with BOSS, mapping a total number of 2770 high-z galaxy clusters. We present here the full results of the CFHT CODEX programme on cluster mass measurement, including a reanalysis of CFHTLS Wide data, with 25 individual lensing-constrained cluster masses. We employ LENSFIT shape measurement and perform a conservative colour-space selection and weighting of background galaxies. Using the combination of shape noise and an analytic covariance for intrinsic variations of cluster profiles at fixed mass due to large-scale structure, miscentring, and variations in concentration and ellipticity, we determine the likelihood of the observed shear signal as a function of true mass for each cluster. We combine 25 individual cluster mass likelihoods in a Bayesian hierarchical scheme with the inclusion of optical and X-ray selection functions to derive constraints on the slope alpha, normalization beta, and scatter sigma(ln lambda vertical bar mu) of our richness-mass scaling relation model in log-space: < In lambda vertical bar mu > = alpha mu + beta, with mu = ln (M-200c/M-piv), and M-piv = 10(14.81)M(circle dot). We find a slope alpha = 0.49(-0.15)(+0.20) , normalization exp(beta) = 84.0(-14.8)(+9.2) , and sigma(ln lambda vertical bar mu) = 0.17(-0.09)(+0.13) using CFHT richness estimates. In comparison to other weak lensing richness-mass relations, we find the normalization of the richness statistically agreeing with the normalization of other scaling relations from a broad redshift range (0.0 < z < 0.65) and with different cluster selection (X-ray, Sunyaev-Zeldovich, and optical). (AU) | |
| Processo FAPESP: | 14/13723-3 - Aglomerados de galáxias como portais para o universo escuro |
| Beneficiário: | Eduardo Serra Cypriano |
| Modalidade de apoio: | Auxílio à Pesquisa - Regular |