Comparison of Sunyaev-Zel'dovich measurements from Planck and from the Arcminute Microkelvin Imager for 99 galaxy clusters

被引：18

作者：

Perrott, Y. C. ^{[2
]}

Olamaie, M. ^{[2
]}

Rumsey, C. ^{[2
]}

Brown, M. L. ^{[15
]}

Feroz, F. ^{[2
]}

Grainge, K. J. B. ^{[2
,15
,16
]}

Hobson, M. P. ^{[2
]}

Lasenby, A. N. ^{[2
,16
]}

MacTavish, C. J. ^{[16
]}

Pooley, G. G. ^{[2
]}

Saunders, R. D. E. ^{[2
,16
]}

Schammel, M. P. ^{[2
,10
]}

Scott, P. F. ^{[2
]}

Shimwell, T. W. ^{[2
,5
]}

Titterington, D. J. ^{[2
]}

Waldram, E. M. ^{[2
]}

Aghanim, N. ^{[11
]}

Arnaud, M. ^{[17
]}

Ashdown, M. ^{[2
,16
]}

Aussel, H. ^{[17
]}

Barrena, R. ^{[8
,14
]}

Bikmaev, I. ^{[1
,7
]}

Boehringer, H. ^{[19
]}

Burenin, R. ^{[20
,21
]}

Carvalho, P. ^{[12
,16
]}

Chon, G. ^{[19
]}

Comis, B. ^{[18
]}

Dahle, H. ^{[13
]}

Democles, J. ^{[17
]}

Douspis, M. ^{[11
]}

Harrison, D. ^{[12
,16
]}

Hempel, A. ^{[14
,23
]}

Hurier, G. ^{[11
]}

Khamitov, I. ^{[7
,22
]}

Kneissl, R. ^{[3
,9
]}

Macias-Perez, J. F. ^{[18
]}

Melin, J. -B. ^{[6
]}

Pointecouteau, E. ^{[4
,24
]}

Pratt, G. W. ^{[17
]}

Rubino-Martin, J. A. ^{[8
,14
]}

Stolyarov, V. ^{[2
,16
,21
]}

Sutton, D. ^{[12
,16
]}

机构：

[1] Acad Sci Tatarstan, Kazan 420111, Russia

[2] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England

[3] ALMA Santiago Cent Off, Atacama Large Millimeter Submillimeter Array, Santiago 7630355, Chile

[4] CNRS, IRAP, F-31028 Toulouse 4, France

[5] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Epping, NSW 1710, Australia

[6] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France

[7] Kazan Fed Univ, Dept Astron & Geodesy, Kazan 420008, Russia

[8] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain

[9] ESO Vitacura, Santiago 19001, Chile

[10] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy

[11] Univ Paris 11, Inst Astrophys Spatiale, CNRS, UMR 8617, F-91405 Orsay, France

[12] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England

[13] Univ Oslo, Inst Theoret Astrophys, N-0371 Oslo, Norway

[14] Inst Astrofis Canarias, Tenerife 38205, Spain

[15] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England

[16] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England

[17] Univ Paris Diderot, Lab AIM, IRFU Serv Astrophys, CEA,DSM,CNRS,CEA Saclay, F-91191 Gif Sur Yvette, France

[18] Univ Grenoble 1, Lab Phys Subatom & Cosmol, CNRS IN2P3, Inst Natl Polytech Grenoble, F-38026 Grenoble, France

[19] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany

[20] Moscow Inst Phys & Technol, Moscow 141700, Russia

[21] Russian Acad Sci, Space Res Inst IKI, Moscow 117997, Russia

[22] Tbitak Natl Observ, TR-07058 Antalya, Turkey

[23] Univ Andres Bello, Dept Ciencias Fis, Fac Ciencias Exactas, Astron, Santiago 7591538, Chile

[24] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France

来源：

ASTRONOMY & ASTROPHYSICS | 2015年 / 580卷

关键词：

cosmology: observations; galaxies: clusters: general; galaxies: clusters: intracluster medium; cosmic background radiation; X-rays: galaxies: clusters; DISCRETE OBJECT DETECTION; FAST BAYESIAN-APPROACH; SCALING RELATIONS; MASS FUNCTION; RADIO-SOURCES; 10C SURVEY; CATALOG; SIMULATIONS; COSMOLOGY; REDSHIFTS;

D O I：

10.1051/0004-6361/201424188

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present observations and analysis of a sample of 123 galaxy clusters from the 2013 Planck catalogue of Sunyaev-Zel'dovich sources with the Arcminute Microkelvin Imager (AMI), a ground-based radio interferometer. AMI provides an independent measurement with higher angular resolution, 3 arcmin compared to the Planck beams of 5-10 arcmin. The AMI observations thus provide validation of the cluster detections, improved positional estimates, and a consistency check on the fitted size (theta(s)) and flux (Y-tot) parameters in the generalised Navarro, Frenk andWhite (GNFW) model. We detect 99 of the clusters. We use the AMI positional estimates to check the positional estimates and error-bars produced by the Planck algorithms PowellSnakes and MMF3. We find that Y-tot values as measured by AMI are biased downwards with respect to the Planck constraints, especially for high Planck-S/N clusters. We perform simulations to show that this can be explained by deviation from the universal pressure profile shape used to model the clusters. We show that AMI data can constrain the alpha and beta parameters describing the shape of the profile in the GNFW model for individual clusters provided careful attention is paid to the degeneracies between parameters, but one requires information on a wider range of angular scales than are present in AMI data alone to correctly constrain all parameters simultaneously.

引用

页数：39

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