Deconstructing the Spectrum of the Soft X‐Ray Background

Küntz, K. D.; Snowden, S. L.

doi:10.1086/317071

Cited by 239 publications

(244 citation statements)

References 56 publications

Supporting

Mentioning

233

Contrasting

Order By: Relevance

“…We modelled the sky background components using the results from Kuntz & Snowden (2000) to account for the Galactic emission, and results from Lumb et al (2002) to account for the CXB. In particular, we used an absorbed power law with photon index Γ = 1.42 for the CXB while for the emission from beyond the Galactic absorption we used absorbed thermal APEC models with temperatures of kT = 0.14 keV and kT = 0.248 keV, respectively.…”

Section: Model Of the Emission Linesmentioning

confidence: 99%

See 1 more Smart Citation

ChandraACIS-I particle background: an analytical model

Bartalucci

Mazzotta

Bourdin

et al. 2014

A&A

101

View full text Add to dashboard Cite

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.

show abstract

Section: Model Of the Emission Linesmentioning

confidence: 99%

“…It can been modelled using twotemperature thermal emission components (Kuntz & Snowden 2000) although its origin and structure are still under debate.…”

Section: Introductionmentioning

confidence: 99%

ChandraACIS-I particle background: an analytical model

Bartalucci

Mazzotta

Bourdin

et al. 2014

A&A

101

View full text Add to dashboard Cite

show abstract

“…For this reason, we decided to model the Galactic foreground emission by the sum of an unabsorbed thermal emission accounting for the local hot bubble (LHB, kT LHB = 0.1 keV, see e.g. Kuntz & Snowden 2000) and three absorbed thermal components accounting for the Galactic "transabsorption emission" (TAE, kT 1 = 0.099 keV, kT 2 = 0.248 keV, see Kuntz & Snowden 2000) and the NPS (see Fig. 2).…”

Section: Foreground and Background Spectral Contributionsmentioning

confidence: 99%

A2163: Merger events in the hottest Abell galaxy cluster

Bourdin

Arnaud

Mazzotta

et al. 2011

A&A

View full text Add to dashboard Cite

Located at z = 0.203, A2163 is a rich galaxy cluster with an intra-cluster medium (ICM) that exhibits extraordinary properties, including an exceptionally high X-ray luminosity, average temperature, and a powerful and extended radio halo. The irregular and complex morphology of its gas and galaxy structure suggests that this cluster has recently undergone major merger events that involve two or more cluster components. In this paper, we study the gas structure and dynamics by means of spectral-imaging analysis of X-ray data obtained from XMM-Newton and Chandra observations. From the evidence of a cold front, we infer the westward motion of a cool core across the E-W elongated atmosphere of the main cluster A2163-A. Located close to a galaxy over-density, this gas "bullet" appears to have been spatially separated from its galaxy (and presumably dark matter component) as a result of high-velocity accretion. From gas brightness and temperature profile analysis performed in two opposite regions of the main cluster, we show that the ICM has been adiabatically compressed behind the crossing "bullet" possibly because of shock heating, leading to a strong departure of the ICM from hydrostatic equilibrium in this region. Assuming that the mass estimated from the Y X proxy best indicates the overall mass of the system and that the western cluster sector is in approximate hydrostatic equilibrium before subcluster accretion, we infer a merger scenario between two subunits of mass ratio 1:4, leading to a present total system mass of M 500 1.9 × 10 15 M . Additional analysis of the spatially-separated northern subcluster A2163-B does not show any evidence of strong interaction with the main cluster A2163-A, leading us to infer that the physical distance separating the northern subcluster and the main component is longer than the projected separation of these components. The exceptional properties of A2163 present various similarities with those of 1E0657-56, the so-called "bullet-cluster". These similarities are likely to be related to a comparable merger scenario.

show abstract

“…In particular, using a molecular cloud located right outside the LHB, it is possible to disentangle the local from the non-local components. This technique, in the X-ray, has been successfully used first with ROSAT (Kuntz & Snowden 2000), then with Chandra, XMM-Newton, and Suzaku (see Gupta et al 2009 for a review) to investigate the nature of the LHB, SWCX, and the GH.…”

Section: Introductionmentioning

confidence: 99%

Studying the Interstellar Medium and the Inner Region of NPS/Loop 1 With Shadow Observations Toward Mbm36

Ursino

Galeazzi

Liu

2015

ApJ

View full text Add to dashboard Cite

We analyzed data from a shadow observation of the high density molecular cloud MBM36 (l∼4°, b∼35°) with Suzaku. MBM36 is located in a region that emits relatively weakly in the 3/4 keV band compared to the surrounding North Polar Spur (NPS)/Loop 1 structure and the Galactic Bulge (GB). The contrast between high and low density targets in the MBM36 area allows one to separate the local and distant contributors to the soft diffuse X-ray background, providing a much better characterization of the individual components compared to single pointing observations. We identify two non-local thermal components, one at kT≈0.12 keV and one at kT≈0.29 keV. The colder component matches well with models of emission from the higher latitude region of the GB. The emission of the warmer component is in agreement with models predicting that the NPS is due to a hypershell from the center of the Milky Way. Geometrical and pressure calculations rule out a nearby bubble as responsible for the emission associated with the NPS. Any Galactic Halo/circumgalactic halo emission, if present, is outshined by the other components. We also report an excess emission around 0.9 keV, likely due to an overabundance of Ne IX.

show abstract

Deconstructing the Spectrum of the Soft X‐Ray Background

Cited by 239 publications

References 56 publications

ChandraACIS-I particle background: an analytical model

ChandraACIS-I particle background: an analytical model

A2163: Merger events in the hottest Abell galaxy cluster

Studying the Interstellar Medium and the Inner Region of NPS/Loop 1 With Shadow Observations Toward Mbm36

Contact Info

Product

Resources

About