Radial temperature profiles for a large sample of galaxy  clusters observed with <i>XMM-Newton</i>

Leccardi, A.; Molendi, S.

doi:10.1051/0004-6361:200809538

Cited by 201 publications

(335 citation statements)

References 34 publications

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“…Note the significant improvement over previous XMM-Newton studies, which were typically limited to the region inside R 500 (e.g. Leccardi & Molendi 2008;Pratt et al 2007). …”

Section: Xmm-newton Surface-brightness Profilementioning

confidence: 84%

The XMM cluster outskirts project (X‐COP)

et al. 2017

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Galaxy clusters are thought to grow hierarchically through the continuous merging and accretion of smaller structures across cosmic time. In the Local Universe, these phenomena are still active in the outer regions of massive clusters (R > R500), where the matter distribution is expected to become clumpy and asymmetric because of the presence of accreting structures. We present the XMM-Newton Cluster Outskirts Project (X-COP), which targets the outer regions of a sample of 13 massive clusters (M500 > 3 × 10 14 M ) in the redshift range 0.04-0.1 at uniform depth. The sample was selected based on the signal-to-noise ratio in the Planck Sunyaev-Zeldovich (SZ) survey with the aim of combining high-quality X-ray and SZ constraints throughout the entire cluster volume. Our observing strategy allows us to reach a sensitivity of 3 × 10 −16 ergs cm −2 s −1 arcmin −2 in the [0.5-2.0] keV range thanks to a good control of systematic uncertainties. The combination of depth and field of view achieved in X-COP will allow us to pursue the following main goals: i) measure the distribution of entropy and thermal energy to an unprecedented level of precision; ii) assess the presence of non-thermal pressure support in cluster outskirts; iii) study the occurrence and mass distribution of infalling gas clumps. We illustrate the capabilities of the program with a pilot study on the cluster Abell 2142.

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“…Note the significant improvement over previous XMM-Newton studies, which were typically limited to the region inside R 500 (e.g. Leccardi & Molendi 2008;Pratt et al 2007). …”

Section: Xmm-newton Surface-brightness Profilementioning

confidence: 84%

The XMM cluster outskirts project (X‐COP)

et al. 2017

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“…Among other aspects, the study of the outskirts of galaxy clusters, which is a well-known example for which controlling the systematics of all background components is critical, will strongly benefit from our work (e.g. Ettori & Molendi 2011;Leccardi & Molendi 2008.…”

Section: Discussionmentioning

confidence: 99%

ChandraACIS-I particle background: an analytical model

Bartalucci

Mazzotta

Bourdin

et al. 2014

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Aims. Imaging and spectroscopy of X-ray extended sources require a proper characterisation of a spatially unresolved background signal. This background includes sky and instrumental components, each of which are characterised by its proper spatial and spectral behaviour. While the X-ray sky background has been extensively studied in previous work, here we analyse and model the instrumental background of the ACIS-I detector on board the Chandra X-ray observatory in very faint mode. Methods. Caused by interaction of highly energetic particles with the detector, the ACIS-I instrumental background is spectrally characterised by the superimposition of several fluorescence emission lines onto a continuum. To isolate its flux from any sky component, we fitted an analytical model of the continuum to observations performed in very faint mode with the detector in the stowed position shielded from the sky, and gathered over the eight-year period starting in 2001. The remaining emission lines were fitted to blank-sky observations of the same period. We found 11 emission lines. Analysing the spatial variation of the amplitude, energy and width of these lines has further allowed us to infer that three lines of these are presumably due to an energy correction artefact produced in the frame store. Results. We provide an analytical model that predicts the instrumental background with a precision of 2% in the continuum and 5% in the lines. We use this model to measure the flux of the unresolved cosmic X-ray background in the Chandra deep field south. We obtain a flux of 10.

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“…The knowledge of these components has been growing thanks to the many efforts involved in collecting suitable blank sky fields to be used as template background by the XMM-Newton users [4,5], the analysis of the XMM-Newton Guest Observer Facility leading to the XMMNewton Extended Source Analysis Software [6,7], the efforts of the XMMNewton SOC 1 and the contributions of various research teams, among them our in Milan has been particularly active on this topic [8,9,10]. A summary table of the EPIC instrumental background components is available at this link 2 .…”

Section: The Current Knowledge Of the Xmm-newton Backgroundmentioning

confidence: 99%