Sökning: WFRF:(Saro S.) > Validation of selec...
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000 | 05534naa a2201213 4500 | |
001 | oai:DiVA.org:su-187873 | |
003 | SwePub | |
008 | 210107s2020 | |||||||||||000 ||eng| | |
024 | 7 | a https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-1878732 URI |
024 | 7 | a https://doi.org/10.1093/mnras/staa23332 DOI |
040 | a (SwePub)su | |
041 | a engb eng | |
042 | 9 SwePub | |
072 | 7 | a ref2 swepub-contenttype |
072 | 7 | a art2 swepub-publicationtype |
100 | 1 | a Grandis, S.4 aut |
245 | 1 0 | a Validation of selection function, sample contamination and mass calibration in galaxy cluster samples |
264 | c 2020-08-11 | |
264 | 1 | b Oxford University Press (OUP),c 2020 |
338 | a print2 rdacarrier | |
520 | a We construct and validate the selection function of the MARD-Y3 galaxy cluster sample. This sample was selected through optical follow-up of the 2nd ROSAT faint source catalogue with Dark Energy Survey year 3 data. The selection function is modelled by combining an empirically constructed X-ray selection function with an incompleteness model for the optical follow-up. We validate the joint selection function by testing the consistency of the constraints on the X-ray flux–mass and richness–mass scaling relation parameters derived from different sources of mass information: (1) cross-calibration using South Pole Telescope Sunyaev-Zel'dovich (SPT-SZ) clusters, (2) calibration using number counts in X-ray, in optical and in both X-ray and optical while marginalizing over cosmological parameters, and (3) other published analyses. We find that the constraints on the scaling relation from the number counts and SPT-SZ cross-calibration agree, indicating that our modelling of the selection function is adequate. Furthermore, we apply a largely cosmology independent method to validate selection functions via the computation of the probability of finding each cluster in the SPT-SZ sample in the MARD-Y3 sample and vice versa. This test reveals no clear evidence for MARD-Y3 contamination, SPT-SZ incompleteness or outlier fraction. Finally, we discuss the prospects of the techniques presented here to limit systematic selection effects in future cluster cosmological studies. | |
650 | 7 | a NATURVETENSKAPx Fysik0 (SwePub)1032 hsv//swe |
650 | 7 | a NATURAL SCIENCESx Physical Sciences0 (SwePub)1032 hsv//eng |
653 | a methods: statistical | |
653 | a galaxies: clusters: general | |
653 | a large-scale structure of Universe | |
653 | a X-rays: galaxies: clusters | |
700 | 1 | a Klein, M.4 aut |
700 | 1 | a Mohr, J. J.4 aut |
700 | 1 | a Bocquet, S.4 aut |
700 | 1 | a Paulus, M.4 aut |
700 | 1 | a Abbott, T. M. C.4 aut |
700 | 1 | a Aguena, M.4 aut |
700 | 1 | a Allam, S.4 aut |
700 | 1 | a Annis, J.4 aut |
700 | 1 | a Benson, B. A.4 aut |
700 | 1 | a Bertin, E.4 aut |
700 | 1 | a Bhargava, S.4 aut |
700 | 1 | a Brooks, D.4 aut |
700 | 1 | a Burke, D. L.4 aut |
700 | 1 | a Rosell, A. Carnero4 aut |
700 | 1 | a Kind, M. Carrasco4 aut |
700 | 1 | a Carretero, J.4 aut |
700 | 1 | a Capasso, Raffaellau Stockholms universitet,Fysikum,Oskar Klein-centrum för kosmopartikelfysik (OKC)4 aut0 (Swepub:su)raca1834 |
700 | 1 | a Costanzi, M.4 aut |
700 | 1 | a da Costa, L. N.4 aut |
700 | 1 | a De Vicente, J.4 aut |
700 | 1 | a Desai, S.4 aut |
700 | 1 | a Dietrich, J. P.4 aut |
700 | 1 | a Doel, P.4 aut |
700 | 1 | a Eifler, T. F.4 aut |
700 | 1 | a Evrard, A. E.4 aut |
700 | 1 | a Flaugher, B.4 aut |
700 | 1 | a Fosalba, P.4 aut |
700 | 1 | a Frieman, J.4 aut |
700 | 1 | a García-Bellido, J.4 aut |
700 | 1 | a Gaztanaga, E.4 aut |
700 | 1 | a Gerdes, D. W.4 aut |
700 | 1 | a Gruen, D.4 aut |
700 | 1 | a Gruendl, R. A.4 aut |
700 | 1 | a Gschwend, J.4 aut |
700 | 1 | a Gutierrez, G.4 aut |
700 | 1 | a Hartley, W. G.4 aut |
700 | 1 | a Hinton, S. R.4 aut |
700 | 1 | a Hollowood, D. L.4 aut |
700 | 1 | a Honscheid, K.4 aut |
700 | 1 | a James, D. J.4 aut |
700 | 1 | a Jeltema, T.4 aut |
700 | 1 | a Kuehn, K.4 aut |
700 | 1 | a Kuropatkin, N.4 aut |
700 | 1 | a Lima, M.4 aut |
700 | 1 | a Maia, M. A. G.4 aut |
700 | 1 | a Marshall, J. L.4 aut |
700 | 1 | a Melchior, P.4 aut |
700 | 1 | a Menantcau, F.4 aut |
700 | 1 | a Miquel, R.4 aut |
700 | 1 | a Ogando, R. L. C.4 aut |
700 | 1 | a Palmese, A.4 aut |
700 | 1 | a Paz-Chinchón, E.4 aut |
700 | 1 | a Plazas, A. A.4 aut |
700 | 1 | a Romer, A. K.4 aut |
700 | 1 | a Roodman, A.4 aut |
700 | 1 | a Sanchez, E.4 aut |
700 | 1 | a Saro, A.4 aut |
700 | 1 | a Scarpine, V4 aut |
700 | 1 | a Schubnell, M.4 aut |
700 | 1 | a Serrano, S.4 aut |
700 | 1 | a Sheldon, E.4 aut |
700 | 1 | a Smith, M.4 aut |
700 | 1 | a Stark, A. A.4 aut |
700 | 1 | a Suchyta, E.4 aut |
700 | 1 | a Swanson, M. E. C.4 aut |
700 | 1 | a Tarle, G.4 aut |
700 | 1 | a Thomas, D.4 aut |
700 | 1 | a Tucker, D. L.4 aut |
700 | 1 | a Varga, T. N.4 aut |
700 | 1 | a Weller, J.4 aut |
700 | 1 | a Wilkinson, R.4 aut |
710 | 2 | a Stockholms universitetb Fysikum4 org |
773 | 0 | t Monthly notices of the Royal Astronomical Societyd : Oxford University Press (OUP)g 498:1, s. 771-798q 498:1<771-798x 0035-8711x 1365-2966 |
856 | 4 | u https://doi.org/10.1093/mnras/staa2333y Fulltext |
856 | 4 | u https://academic.oup.com/mnras/article-pdf/498/1/771/33715028/staa2333.pdf |
856 | 4 8 | u https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-187873 |
856 | 4 8 | u https://doi.org/10.1093/mnras/staa2333 |
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