Planck intermediate results II. Comparison of Sunyaev-Zeldovich measurements from Planck and from the Arcminute Microkelvin Imager for 11 galaxy clusters

被引：16

作者：

Ade, P. A. R. ^{[83
]}

Aghanim, N. ^{[56
]}

Arnaud, M. ^{[72
]}

Ashdown, M. ^{[6
,69
]}

Aumont, J. ^{[56
]}

Baccigalupi, C. ^{[82
]}

Balbi, A. ^{[35
]}

Banday, A. J. ^{[9
,91
]}

Barreiro, R. B. ^{[65
]}

Battaner, E. ^{[93
]}

Battye, R. ^{[68
]}

Benabed, K. ^{[57
,90
]}

Benoit, A. ^{[54
]}

Bernard, J. -P. ^{[9
]}

Bersanelli, M. ^{[32
,48
]}

Bhatia, R. ^{[7
]}

Bikmaev, I. ^{[3
,20
]}

Boehringer, H. ^{[78
]}

Bonaldi, A. ^{[68
]}

Bond, J. R. ^{[8
]}

Borrill, J. ^{[14
,86
]}

Bouchet, F. R. ^{[57
,90
]}

Bourdin, H. ^{[35
]}

Brown, M. L. ^{[68
]}

Bucher, M. ^{[1
]}

Burenin, R. ^{[84
]}

Burigana, C. ^{[34
,47
]}

Butler, R. C. ^{[47
]}

Cabella, P. ^{[36
]}

Carvalho, P. ^{[6
]}

Catalano, A. ^{[71
,73
]}

Cayon, L. ^{[29
]}

Chamballu, A. ^{[52
]}

Chary, R. -R. ^{[53
]}

Chiang, L. -Y. ^{[61
]}

Chon, G. ^{[78
]}

Clements, D. L. ^{[52
]}

Colafrancesco, S. ^{[44
]}

Colombi, S. ^{[57
,90
]}

Coulais, A. ^{[71
]}

Crill, B. P. ^{[67
,80
]}

Cuttaia, F. ^{[47
]}

Da Silva, A. ^{[12
]}

Dahle, H. ^{[11
,63
]}

Davies, R. D. ^{[68
]}

Davis, R. J. ^{[68
]}

de Bernardis, P. ^{[31
]}

de Gasperis, G. ^{[35
]}

de Rosa, A. ^{[47
]}

de Zotti, G. ^{[43
,82
]}

机构：

[1] Univ Paris Diderot, APC, CNRS, CEA,Irfu,Observ Paris,IN2P3, F-75205 Paris 13, France

[2] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland

[3] Acad Sci Tatarstan, Kazan 420111, Republic Of Tat, Russia

[4] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy

[5] Agenzia Spaziale Italiana, Rome, Italy

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

[7] ALMA Santiago Cent Off, Santiago, Chile

[8] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada

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

[10] CALTECH, Pasadena, CA 91125 USA

[11] Univ Oslo, Ctr Math Applicat, Oslo, Norway

[12] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal

[13] CEFCA, Teruel 44001, Spain

[14] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA

[15] CSIC, Madrid, Spain

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

[17] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark

[18] Univ Geneva, Dept Phys Theor, CH-1211 Geneva 4, Switzerland

[19] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain

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

[21] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands

[22] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada

[23] Univ So Calif, Dept Phys & Astron, Dana & David Dornsife Coll Letter Arts & Sci, Los Angeles, CA 90089 USA

[24] Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England

[25] Univ Helsinki, Dept Phys, Helsinki, Finland

[26] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA

[27] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA

[28] Univ Illinois, Dept Phys, Urbana, IL USA

[29] Purdue Univ, Dept Stat, W Lafayette, IN 47907 USA

[30] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy

[31] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy

[32] Univ Milan, Dipartimento Fis, Milan, Italy

[33] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy

[34] Univ Ferrara, Dipartmento Fis, I-44100 Ferrara, Italy

[35] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy

[36] Univ Roma Tor Vergata, Dipartimento Matemat, I-00173 Rome, Italy

[37] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark

[38] ULL, Dpto Astrofis, Tenerife 38206, Spain

[39] ESO Vitacura, European So Observ, Santiago, Chile

[40] European Space Agcy, ESAC, Planck Sci Off, Madrid, Spain

[41] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands

[42] Aalto Univ, Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland

[43] INAF Osservatorio Astron Padova, Padua, Italy

[44] INAF Osservatorio Astron Roma, Monte Porzio Catone, Italy

[45] INAF Osservatorio Astron Trieste, Trieste, Italy

[46] INAF Ist Radioastron, I-40129 Bologna, Italy

[47] INAF IASF Bologna, Bologna, Italy

[48] INAF IASF Milano, Milan, Italy

[49] Univ Roma La Sapienza, Sez Roma 1, INFN, I-00185 Rome, Italy

[50] Univ Paris 11, INRIA, Lab Rech Informat, F-91405 Orsay, France

来源：

ASTRONOMY & ASTROPHYSICS | 2013年 / 550卷

关键词：

cosmology: observations; galaxies: clusters: general; galaxies: clusters: intracluster medium; cosmic background radiation; X-rays: galaxies: clusters; PRE-LAUNCH STATUS; X-RAY-PROPERTIES; DISCRETE OBJECT DETECTION; FAST BAYESIAN-APPROACH; MHZ SKY SURVEY; RADIO-SOURCES; HYDRODYNAMICAL SIMULATIONS; PRESSURE PROFILE; COMPLETE SAMPLE; GAS FRACTION;

D O I：

10.1051/0004-6361/201219361

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

A comparison is presented of Sunyaev-Zeldovich measurements for 11 galaxy clusters as obtained by Planck and by the ground-based interferometer, the Arcminute Microkelvin Imager. Assuming a universal spherically-symmetric Generalised Navarro, Frenk and White (GNFW) model for the cluster gas pressure profile, we jointly constrain the integrated Compton-Y parameter (Y-500) and the scale radius (theta(500)) of each cluster. Our resulting constraints in the Y-500 - theta(500) 2D parameter space derived from the two instruments overlap significantly for eight of the clusters, although, overall, there is a tendency for AMI to find the Sunyaev-Zeldovich signal to be smaller in angular size and fainter than Planck. Significant discrepancies exist for the three remaining clusters in the sample, namely A1413, A1914, and the newly-discovered Planck cluster PLCKESZ G139.59+24.18. The robustness of the analysis of both the Planck and AMI data is demonstrated through the use of detailed simulations, which also discount confusion from residual point (radio) sources and from diffuse astrophysical foregrounds as possible explanations for the discrepancies found. For a subset of our cluster sample, we have investigated the dependence of our results on the assumed pressure profile by repeating the analysis adopting the best-fitting GNFW profile shape which best matches X-ray observations. Adopting the best-fitting profile shape from the X-ray data does not, in general, resolve the discrepancies found in this subset of five clusters. Though based on a small sample, our results suggest that the adopted GNFW model may not be sufficiently flexible to describe clusters universally.

引用

页数：20

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