The XMM-Newton EPIC background and the production of background blank sky event files

Carter, Jennifer; Read, A. M.

doi:10.1051/0004-6361:20065882

Cited by 147 publications

(159 citation statements)

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“…We used a simple powerlaw modified by Galactic absorption, frozen at a column density ∼8 × 10 19 cm −2 (Stark et al 1992), and variable intrinsic absorption. We analysed the background spectrum and found an emission feature coincident with the position of the Al line characterising many background spectra at observed-frame energy ∼1.5 keV (Carter & Read 2007). However, this feature is not expected to influence significantly our iron line analysis, as there is only one object at z higher than 3.27, value which would shift the Al feature to 6.4 keV.…”

Section: The X-ray Datamentioning

confidence: 83%

The XMM Deep survey in the CDF-S

Falocco¹,

Carrera²,

Corral³

et al. 2013

A&A

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Context. X-ray spectroscopy of active galactic nuclei (AGN) offers the opportunity to directly probe the inner regions of the accretion disk. Reflection of the primary continuum on the circumnuclear accreting matter produces features in the X-ray spectrum that help to explore the physics and the geometry of the innermost region, close to the central black hole. Aims. We present the results of our analysis of average AGN XMM-Newton X-ray spectra in the Chandra Deep Field South observation (hereafter, XMM CDFS), in order to explore the Fe line features in distant AGN up to z ∼ 3.5. Methods. We computed the average X-ray spectrum of a sample of 54 AGN with spectroscopic redshifts and signal-to-noise ratio in the 2-12 keV rest-frame band larger than 15 in at least one EPIC camera (for a total of 100 X-ray spectra and 181 623 net counts in the 2-12 keV rest-frame band). We have taken the effects of combining spectra from sources at different redshifts and from both EPIC-pn and EPIC-MOS cameras into account, as well as their spectral resolution; we checked our results using thorough simulations. We explored the iron line components of distant AGN focusing on the narrow core which arises from material far from the central BH and on the putative relativistic component emitted in the accretion disk.Results. The average spectrum shows a highly significant iron feature. Estimating its equivalent width (EW) with a model-independent method suggests a higher EW in a broader range. The line, modelled as an unresolved Gaussian, is significant at 6.8σ and has an EW = 95 ± 22 eV for the full sample. We find that our current data can be fitted equally well adding a relativistic profile to the narrow component (in the full sample, EW = 140 ± 120 eV and 67 ± 28 eV respectively for the relativistic and narrow lines). Conclusions. Thanks to the high quality of the XMM CDFS spectra and to the detailed modelling of the continuum and instrumental effects, we have shown that the most distant AGN exhibit a highly significant iron emission feature. It can be modelled both with narrow and broad lines which suggest that the EW becomes higher when a broader energy range around the line centroid is considered, provides tantalising evidence for reflection by material both very close and far away from the central engine. The EW of both features are similar to those observed in individual nearby AGN, hence they must be a widespread characteristic of AGN, since otherwise the average values would be smaller than observed.

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Section: The X-ray Datamentioning

confidence: 83%

The XMM Deep survey in the CDF-S

Falocco¹,

Carrera²,

Corral³

et al. 2013

A&A

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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%

A systematic analysis of the XMM-Newton background: IV

et al. 2017

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“…The sizes of circular areas were determined by visual inspection of an image of each point source in the pn event list. Blank-sky event lists (see Carter & Read 2007) were used for creating background spectrum corresponding to a proper region. For each spectrum response matrices and effective area files were produced.…”

Section: Observationsmentioning

confidence: 99%

Hot gas in Mach cones around Virgo cluster spiral galaxies

Weżgowiec

Vollmer

Ehle

et al. 2011

A&A

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Context. The detailed comparison between observations and simulations of ram-pressure stripped spiral galaxies in the Virgo cluster has led to a 3D view of the galaxy orbits within the hot intracluster medium. The 3D velocities and Mach numbers derived from simulations can be used to derive simple Mach cone geometries for Virgo spiral galaxies. Aims. We search for indications of hot gas within Mach cones in X-ray observations of selected Virgo cluster spiral galaxies (NGC 4569, NGC 4388, and NGC 4501). Methods. Low-resolution maps of diffuse extended emission and X-ray spectra from XMM-Newton observations are presented. Gas densities and temperatures were derived from the X-ray spectra. Results. We find extraplanar diffuse X-ray emission in all galaxies. Based on the 3D velocity vectors from dynamical modeling, a simple Mach cone is fitted to the triangular shape of NGC 4569's diffuse X-ray emission. Assuming that all extraplanar diffuse X-ray emission has to be located inside the Mach cone, we also fit Mach cones to NGC 4388's and NGC 4501's extraplanar X-ray emission. For NGC 4569 it is hard to reconcile the derived Mach cone opening angle with a Mach number based on the sound speed alone. Instead, a Mach number involving the Alfvénic speed seems to be more appropriate, yielding a magnetic field strength of ∼1-3 μG for an intracluster medium density of n ∼ 10 −4 cm −3 . Whereas the temperature of the hot component of NGC 4569's X-ray halo (0.5 keV) is at the high end, but typical of a galactic outflow, the temperature of the hot gas tails of NGC 4388 and NGC 4501 are significantly hotter (0.7-0.9 keV). Conclusions. In NGC 4569 we find direct evidence of a Mach cone that is filled with hot gas from a galactic superwind. We suggest that the high gas temperatures in the X-ray tails of NGC 4388 and NGC 4501 come from the mixing of the stripped ISM into the hot intracluster medium of the Virgo cluster.

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The XMM-Newton EPIC background and the production of background blank sky event files

Cited by 147 publications

References 10 publications

The XMM Deep survey in the CDF-S

The XMM Deep survey in the CDF-S

A systematic analysis of the XMM-Newton background: IV

Hot gas in Mach cones around Virgo cluster spiral galaxies

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