Mapping the hot gas temperature in galaxy clusters using X-ray and Sunyaev-Zel'dovich imaging

被引：26

作者：

Adam, R. ^{[1
,2
]}

Arnaud, M. ^{[3
]}

Bartalucci, I. ^{[3
]}

Ade, P. ^{[4
]}

Andre, P. ^{[3
]}

Beelen, A. ^{[5
,6
]}

Benoit, A. ^{[7
,8
]}

Bideaud, A. ^{[4
]}

Billot, N. ^{[9
]}

Bourdin, H. ^{[10
]}

Bourrion, O. ^{[2
]}

Calvo, M. ^{[7
,8
]}

Catalano, A. ^{[2
]}

Coiffard, G. ^{[11
]}

Comis, B. ^{[2
]}

D'Addabbo, A. ^{[7
,8
,12
]}

Desert, F. -X. ^{[13
,14
]}

Doyle, S. ^{[4
]}

Ferrari, C. ^{[1
]}

Goupy, J. ^{[7
,8
]}

Kramer, C. ^{[9
]}

Lagache, G. ^{[15
]}

Leclercq, S. ^{[11
]}

Macias-Perez, J. -F. ^{[2
]}

Maurogordato, S. ^{[1
]}

Mauskopf, P. ^{[4
,16
,17
]}

Mayet, F. ^{[2
]}

Monfardini, A. ^{[7
,8
]}

Pajot, F. ^{[5
,6
]}

Pascale, E. ^{[4
]}

Perotto, L. ^{[2
]}

Pisano, G. ^{[4
]}

Pointecouteau, E. ^{[18
,19
]}

Ponthieu, N. ^{[13
,14
]}

Pratt, G. W. ^{[3
]}

Reveret, V. ^{[3
]}

Ritacco, A. ^{[2
]}

Rodriguez, L. ^{[3
]}

Romero, C. ^{[11
]}

Ruppin, F. ^{[2
]}

Schuster, K. ^{[11
]}

Sievers, A. ^{[9
]}

Triqueneaux, S. ^{[7
,8
]}

Tucker, C. ^{[4
]}

Zylka, R. ^{[11
]}

机构：

[1] Univ Cote dAzur, Lab Lagrange, Observ Cote dAzur, CNRS, Blvd Observ,CS 34229, F-06304 Nice 4, France

[2] Univ Grenoble Alpes, CNRS, IN2P3, Lab Phys Subatom & Cosmol, 53 Ave Martyrs, F-38400 Grenoble, France

[3] Univ Paris Diderot, Lab AIM, IRFU, Dept Astrophys,CEA,DRF,CNRS,CEA Saclay, Bat 709, F-91191 Gif Sur Yvette, France

[4] Cardiff Univ, Astron Instrumentat Grp, Cardiff CF10 3XQ, S Glam, Wales

[5] CNRS, IAS, F-91400 Orsay, France

[6] Univ Paris Sud, F-91400 Orsay, France

[7] CNRS, Inst Neel, F-38400 Grenoble, France

[8] Univ Grenoble Alpes, F-38400 Grenoble, France

[9] IRAM, Granada 18012, Spain

[10] Univ Roma Tor Vergata, Dipartimento Fis, Via Ric Sci 1, I-00133 Rome, Italy

[11] IRAM, F-38406 Grenoble, France

[12] Sapienza Univ Roma, Dipartimento Fis, Piazzale Aldo Moro 5, I-00185 Rome, Italy

[13] CNRS, IPAG, F-38406 St Martin Dheres, France

[14] Univ Grenoble Alpes, F-38406 St Martin Dheres, France

[15] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France

[16] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA

[17] Arizona State Univ, Dept Phys, Tempe, AZ 85287 USA

[18] Univ Toulouse, UPS OMP, IRAP, F-31400 Toulouse, France

[19] CNRS, IRAP, 9 Ave Colonel Roche,BP 44346, F-31028 Toulouse 4, France

来源：

ASTRONOMY & ASTROPHYSICS | 2017年 / 606卷

基金：

欧洲研究理事会;

关键词：

techniques: high angular resolution; galaxies: clusters: individual: MACS J0717.5+3745; X-rays: galaxies: clusters; galaxies:clusters: intracluster medium; ARRAY;

D O I：

10.1051/0004-6361/201629810

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We propose a method to map the temperature distribution of the hot gas in galaxy clusters that uses resolved images of the thermal Sunyaev-Zel'dovich (tSZ) effect in combination with X-ray data. Application to images from the New IRAM KIDs Array (NIKA) and XMM-Newton allows us to measure and determine the spatial distribution of the gas temperature in the merging cluster MACS J0717.5+3745, at z = 0.55. Despite the complexity of the target object, we find a good morphological agreement between the temperature maps derived from X-ray spectroscopy only - using XMM-Newton (T-XMM) and Chandra (T-CXO) - and the new gas-mass-weighted tSZ+X-ray imaging method (T-SZX). We correlate the temperatures from tSZ+X-ray imaging and those from X-ray spectroscopy alone and find that T-SZX is higher than T-XMM and lower than T-CXO by similar to 10% in both cases. Our results are limited by uncertainties in the geometry of the cluster gas, contamination from kinetic SZ (similar to 10%), and the absolute calibration of the tSZ map (7%). Investigation using a larger sample of clusters would help minimise these effects.

引用

页数：8

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