Reproducibility of Non-X-Ray Background for the X-Ray Imaging Spectrometer aboard Suzaku

Tawa, Noriaki; Hayashida, Kentaro; Nagai, Michiko; Nakamoto, Hidetaka; Tsunemi, H.; Yamaguchi, Hiroya; Ishisaki, Yoshitaka; Miller, Eric D.; Mizuno, T.; Dotani, Tadayasu; Ozaki, Masanori; Katayama, Haruyoshi

doi:10.1093/pasj/60.sp1.s11

Cited by 290 publications

(142 citation statements)

References 17 publications

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“…We start with the particle background. The reproducibility of this background component for Suzaku is better than about 3% (e.g., Tawa et al 2008). Here, we conservatively assumed 5% and found best fit temperatures and errors for the third bin as 4.66 +0.81 −0.65 keV and 4.32 +0.77 −0.54 keV.…”

Section: Discussionmentioning

confidence: 86%

“…For Chandra and XMM-Newton, temperature measurements in the low surface brightness cluster outskirts are strongly affected by the uncertainty in the particle background. We tested the influence of the particle background on the Suzaku results by artificially changing the normalization of the Night Earth spectra by a very conservative (e.g., Tawa et al 2008) ±10% and repeating the fitting procedure. We found that the new best fit temperatures are consistent with the statistical uncertainty of the standard fit (Fig.…”

Section: Resultsmentioning

confidence: 99%

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Suzakumeasurement of Abell 2204's intracluster gas temperature profile out to 1800 kpc

Reiprich

Hudson

Zhang

et al. 2009

A&A

105

102

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Context. Measurements of intracluster gas temperatures out to large radii, where much of the galaxy cluster mass resides, are important for using clusters for precision cosmology and for studies of cluster physics. Previous attempts to measure robust temperatures at cluster virial radii have failed. Aims. The goal of this work is to measure the temperature profile of the very relaxed symmetric galaxy cluster Abell 2204 out to large radii, possibly reaching the virial radius. Methods. Taking advantage of its low particle background due to its low-Earth orbit, Suzaku data are used to measure the outer temperature profile of Abell 2204. These data are combined with Chandra and XMM-Newton data of the same cluster to make the connection to the inner regions, unresolved by Suzaku, and to determine the smearing due to Suzaku's point spread function. Results. The temperature profile of Abell 2204 is determined from ∼10 kpc to ∼1800 kpc, close to an estimate of r 200 (the approximation to the virial radius). The temperature rises steeply from below 4 keV in the very center up to more than 8 keV in the intermediate range and then decreases again to about 4 keV at the largest radii. Varying the measured particle background normalization artificially by ±10% does not change the results significantly. Several additional systematic effects are quantified, e.g., those due to the point spread function and astrophysical fore-and backgrounds. Predictions for outer temperature profiles based on hydrodynamic simulations show good agreement. In particular, we find the observed temperature profile to be slightly steeper but consistent with a drop of a factor of 0.6 from 0.3 r 200 to r 200 , as predicted by simulations. Conclusions. Intracluster gas temperature measurements up to r 200 seem feasible with Suzaku, after a careful analysis of the different background components and the effects of the point spread function. Such measurements now need to be performed for a statistical sample of clusters. The result obtained here indicates that numerical simulations capture the intracluster gas physics well in cluster outskirts.

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Section: Discussionmentioning

confidence: 86%

Section: Resultsmentioning

confidence: 99%

Suzakumeasurement of Abell 2204's intracluster gas temperature profile out to 1800 kpc

Reiprich

Hudson

Zhang

et al. 2009

A&A

105

102

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“…We also discarded pixels adjacent to the flickering pixels. Non X-ray backgrounds (NXBs) were estimated by xisnxbgen (Tawa et al 2008). Redistribution matrix files and ancillary response files were produced by xisrmfgen and xissimarfgen (Ishisaki et al 2007) We then fitted the relation between the true energies and the centroid energies of the Gaussians with a first-order polynomial.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Toward the Understanding of the Physical Origin of Recombining Plasma in the Supernova Remnant IC 443

Matsumura

Tanaka

Uchida

et al. 2017

ApJ

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We perform a spatially resolved spectroscopic analysis of X-ray emission from the supernova remnant (SNR) IC 443 with Suzaku. All the spectra are well reproduced by a model consisting of a collisional ionization equilibrium (CIE) and two recombining plasma (RP) components. Although previous X-ray studies found an RP in the northeastern region, this is the first report on RPs in the other parts of the remnant. The electron temperature kT e of the CIE component is almost uniform at ∼ 0.2 keV across the remnant. The CIE plasma has metal abundances consistent with solar and is concentrated toward the rim of the remnant, suggesting that it is of shocked interstellar medium origin. The two RP components have different kT e : one in the range of 0.16-0.28 keV and the other in the range of 0.48-0.67 keV. The electron temperatures of both RP components decrease toward the southeast, where the SNR shock is known to be interacting with a molecular cloud. We also find the normalization ratio of the lower-kT e RP to higher-kT e RP components increases toward the southeast. Both results suggest the X-ray emitting plasma in the southeastern region is significantly cooled by some mechanism. One of the plausible cooling mechanisms is thermal conduction between the hot plasma and the molecular cloud. If the cooling proceeds faster than the recombination timescale of the plasma, the same mechanism can account for the recombining plasma as well.

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“…The region representing the whole remnant has a size of 4 .85 The background for 3C 391 is a combination of the non-X-ray background (NXB), the cosmic X-ray background (CXB) emission, and the Galactic ridge X-ray emission, GRXE (Koyama et al 1986). First, we estimated the NXB data from night Earth observations using the tool xisnxbgen (Tawa et al 2008), and subtracted the NXB from the spectrum. We selected the background region, the nearby blank sky region (Obs.ID 500009020) on the Galactic plane, consisting of the GRXE and the CXB.…”

Section: Background Estimation and Model Fittingmentioning

confidence: 99%

Recombining Plasma in the Gamma-Ray-Emitting Mixed-Morphology Supernova Remnant 3c 391

Ergin

Sezer

Saha

et al. 2014

ApJ

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A group of middle-aged mixed-morphology (MM) supernova remnants (SNRs) interacting with molecular clouds (MCs) has been discovered to be strong GeV gamma-ray emitters by the Large Area Telescope (LAT) on board the Fermi Gamma-Ray Space Telescope (Fermi-LAT). The recent observations of the Suzaku X-ray satellite have revealed that some of these interacting gamma-ray-emitting SNRs, such as IC443, W49B, W44, and G359.1-0.5, have overionized plasmas. 3C 391 (G31.9+0.0) is another Galactic MM SNR interacting with MCs. It was observed in GeV gamma rays by Fermi-LAT as well as in the 0.3-10.0 keV X-ray band by Suzaku. In this work, 3C 391 was detected in GeV gamma rays with a significance of ∼18σ and we showed that the GeV emission is point-like in nature. The GeV gamma-ray spectrum was shown to be best explained by the decay of neutral pions assuming that the protons follow a broken power-law distribution. We revealed radiative recombination structures of silicon and sulfur from 3C 391 using Suzaku data. In this paper, we discuss the possible origin of this type of radiative plasma and hadronic gamma rays.

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Reproducibility of Non-X-Ray Background for the X-Ray Imaging Spectrometer aboard Suzaku

Cited by 290 publications

References 17 publications

Suzakumeasurement of Abell 2204's intracluster gas temperature profile out to 1800 kpc

Suzakumeasurement of Abell 2204's intracluster gas temperature profile out to 1800 kpc

Toward the Understanding of the Physical Origin of Recombining Plasma in the Supernova Remnant IC 443

Recombining Plasma in the Gamma-Ray-Emitting Mixed-Morphology Supernova Remnant 3c 391

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