XMM-Newton Spectroscopy of the Cluster of Galaxies 2a 0335+096

Werner, Norbert; Plaa, J de; Kaastra, J S; Vink, Jacco; Bleeker, J; Peterson, J R; Verbunt, F

doi:10.2172/878003

Cited by 4 publications

(11 citation statements)

References 45 publications

(68 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…But the actual uncertainties in the measured calcium abundance might be bigger than the statistical error indicated here. This calcium overabundance is also seen in the analysis of 2A 0335+096 (Werner et al 2006), confirming that the overabundance is probably not a statistical deviation. Every other abundance is consistent with the model within the error bars.…”

Section: Abundances and Snia/snii/population-iii Modelssupporting

confidence: 73%

“…This might be an indication that the SNII and SNIa models have difficulties predicting the right yield for this element, but the actual uncertainties in our measured value might also be bigger than the quoted statistical error. When we compare the supernova fractions found by Werner et al (2006) in 2A 0335+096, we see that the SNIa contribution in Sérsic 159-03 tends to be 5-25% higher.…”

Section: Abundance Distribution and Enrichment By Supernova Types Ia/mentioning

confidence: 86%

“…In the core region all fits are acceptable when we use the condition χ 2 r < 1.5. However, the χ 2 r for the single temperature model in the core is much less than in Werner et al (2006) in the cluster 2A 0335+096. In the outer parts multitemperature fitting still results in a better fit, but we do not see significant differences between the models.…”

Section: Radial Profiles Using Thermal Dem Modelsmentioning

confidence: 88%

“…However, their background subtraction method and handling of spectral excess is different, which can lead to systematic differences. Also projection effects can have an influence on the broadness of the DEM distribution, but as Kaastra et al (2004) and Werner et al (2006) show, multi-temperature models are also needed for fitting deprojected spectra.…”

Section: Temperature Structurementioning

confidence: 99%

See 3 more Smart Citations

Chemical Evolution in Sersic 159-03 Observed with Xmm-Newton

Plaa¹,

Werner²,

Bykov³

et al. 2006

Self Cite

View full text Add to dashboard Cite

Abstract. Using a new long X-ray observation of the cluster of galaxies Sérsic 159-03 with XMM-Newton, we derive radial temperature and abundance profiles using single-and multi-temperature models. The fits to the EPIC and RGS spectra prefer multi-temperature models especially in the core. The radial profiles of oxygen and iron measured with EPIC/RGS and the line profiles in RGS suggest that there is a dip in the O/Fe ratio in the centre of the cluster compared to its immediate surroundings. A possible explanation for the large scale metallicity distribution is that SNIa and SNII products are released in the ICM through ram-pressure stripping of in-falling galaxies. This causes a peaked metallicity distribution. In addition, SNIa in the central cD galaxy enrich mainly the centre of the cluster with iron. This excess of SNIa products is consistent with the low O/Fe ratio we detect in the centre of the cluster. We fit the abundances we obtain with yields from SNIa, SNII and Population-III stars to derive the clusters chemical evolution. We find that the measured abundance pattern does not require a Population-III star contribution. The relative contribution of the number of SNIa with respect to the total number of SNe which enrich the ICM is about 25-50%. Furthermore, we discuss the possible presence of a non-thermal component in the EPIC spectra. A potential source of this non-thermal emission can be inverse-Compton scattering between Cosmic Microwave Background (CMB) photons and relativistic electrons, which are accelerated in bow shocks associated with ram-pressure stripping of in-falling galaxies.

show abstract

Section: Abundances and Snia/snii/population-iii Modelssupporting

confidence: 73%

Section: Abundance Distribution and Enrichment By Supernova Types Ia/mentioning

confidence: 86%

Section: Radial Profiles Using Thermal Dem Modelsmentioning

confidence: 88%

Section: Temperature Structurementioning

confidence: 99%

See 2 more Smart Citations

Chemical Evolution in Sersic 159-03 Observed with Xmm-Newton

Plaa¹,

Werner²,

Bykov³

et al. 2006

Self Cite

View full text Add to dashboard Cite

show abstract

“…With the first generation of satellites it was just possible to determine the radial metallicity profiles [4]. With deep observations of bright clusters of galaxies by the Chandra and XMM-Newton satellites it is now possible to extract the metallicities in certain regions of a galaxy cluster and to construct X-ray weighted metallicity maps [5,6,7,8,9,10,11,12,13,14].…”

Section: Introductionmentioning

confidence: 99%

XMM Observations of Metal Abundances in Galaxy Clusters

Lovisari¹,

Schindler²,

Kapferer³

2011

Acta Polytech

View full text Add to dashboard Cite

The hot gas that fills the space between galaxies in clusters is rich in metals. Due to their large potential well, galaxy clusters accumulate metals over the whole history of the cluster, and retain important information on cluster formation and evolution.We derive detailed metallicity maps for a sample of 5 clusters, observed with XMM-Newton, to study the distribution of metals in the Intra-Cluster Medium (ICM). We show that even in relaxed clusters the distribution of metals shows many inhomogeneities with several maxima separated by low metallicity regions. We also found a deviation from the expected temperature-metallicity relation.

show abstract

High-resolution X-ray spectroscopy of astrophysical plasmas with X-ray microcalorimeters

Ezoe

Ohashi

Mitsuda

2021

Rev. Mod. Plasma Phys.

View full text Add to dashboard Cite

High spectral resolution with a resolving power, $$E/\Delta E \gtrsim 1000$$ E / Δ E ≳ 1000 at 6 keV, is now available in X-ray astronomy. X-ray observations are particularly effective for plasma studies since major atomic transitions appear as spectral features in the X-ray band. High-resolution spectroscopy enables us to probe a wide variety of astrophysical plasmas, which are not obtainable from ground experiments, regarding their temperature, density, magnetic field, gravity, and velocity. In this review, we describe what are the X-ray emitting plasmas in the Universe, along with basic plasma diagnostics, and depict historical development of the techniques used for the X-ray spectroscopy. We outline the X-ray microcalorimeter instrument, soft X-ray spectrometer (SXS), onboard the ASTRO-H satellite. Despite the short lifetime of the satellite in orbit for about a month, observations with the SXS have shown the remarkable power of high-resolution spectroscopy in X-ray astronomy. Observed spectrum of the hot plasma in the core region of the Perseus cluster showed He-like Fe K-line to be clearly resolved into resonance, forbidden and intercombination lines for the first time. The line width indicates that the turbulent pressure amounts to only 4% of the thermal pressure of the plasma. We also describe new findings and constraints obtained from the superb spectrum of the Perseus cluster, which all indicate a great potential of X-ray spectroscopy. The recovery of the spectroscopy science of ASTRO-H is aimed at with XRISM, a Japanese mission planned for launch in early 2020s. In further future, Athena will expand the rich science with its high sensitivity and spectral resolution in early 2030s.

show abstract

XMM-Newton Spectroscopy of the Cluster of Galaxies 2a 0335+096

Cited by 4 publications

References 45 publications

Chemical Evolution in Sersic 159-03 Observed with Xmm-Newton

Chemical Evolution in Sersic 159-03 Observed with Xmm-Newton

XMM Observations of Metal Abundances in Galaxy Clusters

High-resolution X-ray spectroscopy of astrophysical plasmas with X-ray microcalorimeters

Contact Info

Product

Resources

About