Статья

Systematics in the X-ray cluster mass estimators

E. RasiaDipartimento di Astronomia, Università di Padova, vicolo dell'Osservatorio 2, I-35122 Padova, ItalyS. EttoriINAF, Osservatorio Astronomico di Bologna, via Ranzani 1, I-40127 Bologna, ItalyL. MoscardiniDipartimento di Astronomia, Università di Bologna, via Ranzani 1, I-40127 Bologna, ItalyP. MazzottaDipartimento di Fisica, Università di Roma Tor Vergata, via della Ricerca Scientifica 1, I-00133 Roma, ItalyS. BorganiDipartimento di Astronomia, Università di Trieste, via Tiepolo 11, I-34131 Trieste, ItalyK. DolagMax-Planck-Institut für Astrophysik, Karl-Schwarzschild Strasse 1, D-85748 Garching bei München, GermanyG. TormenDipartimento di Astronomia, Università di Padova, vicolo dell'Osservatorio 2, I-35122 Padova, ItalyL. M. ChengInstitute of Theoretical Physics, Chinese Accademy of Sciences, Beijing 100080, ChinaA. DiaferioDipartimento di Fisica Generale ‘Amedeo Avogadro’, Università di Torino, via Giuria 1, I-10125 Torino, Italy

2006en

ABI

Аннотация

We examine the systematics affecting the X-ray mass estimators applied to a set of five galaxy clusters resolved at high resolution in hydrodynamic simulations, including cooling, star formation and feedback processes. These simulated objects are processed through the X-ray Map Simulator, X-MAS, to provide Chandra-like long exposures that are analysed to reconstruct the gas temperature, density and mass profiles used as input. These clusters have different dynamic state: we consider a hot cluster with temperature T = 11.4 keV, a perturbed cluster with T = 3.9 keV, a merging object with T = 3.6 keV, and two relaxed systems with T = 3.3 keV and T = 2.7 keV, respectively. These systems are located at z = 0.175 so that their emission fits within the Chandra ACIS-S3 chip between 0.6 and 1.2 R 500 .

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Идентификаторы

DOI: 10.1111/j.1365-2966.2006.10466.x

Цитирования и источники

Цитирований: 2Использованных источников: 0

Показатели — AkademScholar