A dataset provided by the European Space Agency

Name 050101
Title Radio source ageing and the quenching of cooling cores in clusters
URL

http://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0501010101
http://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0501010201

DOI 10.5270/esa-hhiwbo9
Author Dr Elena Belsole
Description We propose to complete the high-quality X-ray observations of a sample of 35 intermediate-redshift bright galaxy clusters by observing 4 with XMM. The sample is unbiased in X-ray morphology and radio-source content, and is of sufficient size to permit us to address the extent to which cooling flows are halted by energy injected by radio sources, and if the dynamical state of the cluster gas correlates with the radio source physical state. This will be achieved by comparing the X-ray-derived temperature, entropy and pressure structures with energy contents, ages and distributions of the radio-sources within the clusters. In addition, complementary observations of SZ effect and weak lensing will allow us to compare 3 mass estimation methods for a statistical galaxy cluster sample.
Publication A serendipitous XMM survey of the SDSS: the evolution of the colour-magnitude diagram of X-ray AGN from z= 0.8 to 0.1 . Georgakakis, Antonis, Nandra, K., . MNRAS . 414-992 . 2011 . 2011MNRAS.414..992G ,
The cosmological analysis of X-ray cluster surveys - II. Application of the CR-HR method to the XMM archive . Clerc, N., Sadibekova, T., et all. . MNRAS . 423-3561 . 2012 . 2012MNRAS.423.3561C ,
Detection of an Unidentified Emission Line in the Stacked X-Ray Spectrum of Galaxy Clusters . Bulbul, Esra, Markevitch, Maxim, et all. . ApJ . 789-13 . 2014 . 2014ApJ...789...13B ,
Serendipitous UV source catalogues for 10 years of XMM and 5 years of Swift . Yershov, V. N., . Ap&SS . 354-97 . 2014 . 2014Ap&SS.354...97Y ,
Obscuration-dependent Evolution of Active Galactic Nuclei . Buchner, Johannes, Georgakakis, Antonis, et all. . ApJ . 802-89 . 2015 . 2015ApJ...802...89B ,
LoCuSS: The Slow Quenching of Star Formation in Cluster Galaxies and the Need for Pre-processing . Haines, C. P., Pereira, M. J., et all. . ApJ . 806-101 . 2015 . 2015ApJ...806..101H ,
Where do the 3.5 keV photons come from? A morphological study of the Galactic Center and of Perseus . Carlson, Eric, Jeltema, Tesla, . JCAP . 2-9 . 2015 . 2015JCAP...02..009C ,
A novel scenario for the possible X-ray line feature at ~3.5 keV. Charge exchange with bare sulfur ions . Gu, L., Kaastra, J., et all. . A&A . 5...
Instrument EMOS1, EMOS2, EPN, OM, RGS1, RGS2
Temporal Coverage 2008-04-23T15:06:22Z/2008-04-24T00:34:11Z
Version 17.56_20190403_1200
Mission Description The European Space Agency's (ESA) X-ray Multi-Mirror Mission (XMM-Newton) was launched by an Ariane 504 on December 10th 1999. XMM-Newton is ESA's second cornerstone of the Horizon 2000 Science Programme. It carries 3 high throughput X-ray telescopes with an unprecedented effective area, and an optical monitor, the first flown on a X-ray observatory. The large collecting area and ability to make long uninterrupted exposures provide highly sensitive observations.
Since Earth's atmosphere blocks out all X-rays, only a telescope in space can detect and study celestial X-ray sources. The XMM-Newton mission is helping scientists to solve a number of cosmic mysteries, ranging from the enigmatic black holes to the origins of the Universe itself. Observing time on XMM-Newton is being made available to the scientific community, applying for observational periods on a competitive basis.
Creator Contact https://www.cosmos.esa.int/web/xmm-newton/xmm-newton-helpdesk
Date Published 2009-06-06T00:00:00Z
Publisher And Registrant European Space Agency
Credit Guidelines European Space Agency, 2009-06-06T00:00:00Z, 050101, 17.56_20190403_1200. https://doi.org/10.5270/esa-hhiwbo9