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|Title:||Fossil group origins - VI. Global X-ray scaling relations of fossil galaxy clusters||Authors:||Kundert, A.
Aguerri, J. A. L.
Corsini, E. M.
DE GRANDI, Sabrina
|Issue Date:||2015||Journal:||MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY||Number:||454||Issue:||1||First Page:||161||Abstract:||We present the first pointed X-ray observations of 10 candidate fossil galaxy groups and clusters. With these Suzaku observations, we determine global temperatures and bolometric X-ray luminosities of the intracluster medium (ICM) out to r<SUB>500</SUB> for six systems in our sample. The remaining four systems show signs of significant contamination from non-ICM sources. For the six objects with successfully determined r<SUB>500</SUB> properties, we measure global temperatures in the range 2.8 ≤ T<SUB>X</SUB> ≤ 5.3 keV, bolometric X-ray luminosities of 0.8 × 10<SUP>44</SUP> ≤ L<SUB>X, bol</SUB> ≤ 7.7 × 10<SUP>44</SUP> erg s<SUP>-1</SUP>, and estimate masses, as derived from T<SUB>X</SUB>, of M<SUB>500</SUB> ≳ 10<SUP>14</SUP> M<SUB>☉</SUB>. Fossil cluster scaling relations are constructed for a sample that combines our Suzaku observed fossils with fossils in the literature. Using measurements of global X-ray luminosity, temperature, optical luminosity, and velocity dispersion, scaling relations for the fossil sample are then compared with a control sample of non-fossil systems. We find the fits of our fossil cluster scaling relations are consistent with the relations for normal groups and clusters, indicating fossil clusters have global ICM X-ray properties similar to those of comparable mass non-fossil systems.||Acknowledgments:||This research has made use of data obtained from the Suzaku satellite, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). We thank the anonymous referee for valuable comments, K. Hamaguchi and K. Pottschmidt at the Suzaku Helpdesk for useful advice on multiple aspects of our analysis, and D. Eckert for helpful discussions and for suggesting the flickering pixels issue as an explanation for the excess in the 0.5–0.7 keV range. Support for this research was provided by NASA Grant No. NNX13AE97G, and by the University of Wisconsin-Madison Office of the Vice Chancellor for Research and Graduate Education with funding from the Wisconsin Alumni Research Foundation. FG acknowledges the financial contribution from contract PRIN INAF 2012 (‘A unique data set to address the most compelling open questions about X-ray galaxy clusters’) and the contract ASI INAF NuSTAR I/037/12/0. ED gratefully acknowledges the support of the Alfred P. Sloan Foundation. MG acknowledges funding from MIUR PRIN2010-2011 (J91J12000450001). JALA has been partly funded from MINECO AYA2013-43188-P. EMC is partially supported by Padua University through grants 60A02-4807/12, 60A02-5857/13, 60A02-5833/14, and CPDA133894. JM-A acknowledges support from the European Research Council Starting Grant (SEDmorph; PI: V. Wild).||URI:||http://hdl.handle.net/20.500.12386/23559||URL:||https://academic.oup.com/mnras/article/454/1/161/1118585
|Appears in Collections:||1.01 Articoli in rivista|
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