CHEERS: The chemical evolution RGS sample

J 2017

CHEERS: The chemical evolution RGS sample

DE PLAA, J., J. S. KAASTRA, Norbert WERNER, C. PINTO, P. KOSEC et. al.

Basic information

Original name

CHEERS: The chemical evolution RGS sample

Authors

DE PLAA, J. (528 Netherlands), J. S. KAASTRA (528 Netherlands), Norbert WERNER (703 Slovakia, guarantor, belonging to the institution), C. PINTO (380 Italy), P. KOSEC (703 Slovakia), Y. Y. ZHANG (156 China), F. MERNIER (56 Belgium), L. LOVISARI (380 Italy), H. AKAMATSU (392 Japan), G. SCHELLENBERGER (276 Germany), F. HOFMANN (276 Germany), T. H. REIPRICH (276 Germany), A. FINOGUENOV (643 Russian Federation), J. AHORANTA (246 Finland), J. S. SANDERS (826 United Kingdom of Great Britain and Northern Ireland), A. C. FABIAN (826 United Kingdom of Great Britain and Northern Ireland), O. POLS (528 Netherlands), A. SIMIONESCU (642 Romania), J. VINK (528 Netherlands) and H. BOHRINGER (276 Germany)

Edition

ASTRONOMY & ASTROPHYSICS, LES ULIS CEDEX A, EDP SCIENCES S A, 2017, 1432-0746

Other information

Language

English

Type of outcome

Článek v odborném periodiku

Field of Study

10308 Astronomy

Country of publisher

France

Confidentiality degree

není předmětem státního či obchodního tajemství

References:

URL URL

Impact factor

Impact factor: 5.565

RIV identification code

RIV/00216224:14310/17:00099808

Organization unit

Faculty of Science

DOI

http://dx.doi.org/10.1051/0004-6361/201629926

UT WoS

000415864100003

Keywords in English

X-rays: galaxies: clusters; galaxies: clusters: intracluster medium; supernovae: general; galaxies: abundances

Abstract

V originále

Context. The chemical yields of supernovae and the metal enrichment of the intra-cluster medium (ICM) are not well understood. The hot gas in clusters of galaxies has been enriched with metals originating from billions of supernovae and provides a fair sample of large-scale metal enrichment in the Universe. High-resolution X-ray spectra of clusters of galaxies provide a unique way of measuring abundances in the hot intracluster medium (ICM). The abundance measurements can provide constraints on the supernova explosion mechanism and the initial-mass function of the stellar population. This paper introduces the CHEmical Enrichment RGS Sample (CHEERS), which is a sample of 44 bright local giant ellipticals, groups, and clusters of galaxies observed with XMM-Newton. Aims. The CHEERS project aims to provide the most accurate set of cluster abundances measured in X-rays using this sample. This paper focuses specifically on the abundance measurements of O and Fe using the reflection grating spectrometer (RGS) on board XMM-Newton. We aim to thoroughly discuss the cluster to cluster abundance variations and the robustness of the measurements. Methods. We have selected the CHEERS sample such that the oxygen abundance in each cluster is detected at a level of at least 5 sigma in the RGS. The dispersive nature of the RGS limits the sample to clusters with sharp surface brightness peaks. The deep exposures and the size of the sample allow us to quantify the intrinsic scatter and the systematic uncertainties in the abundances using spectral modeling techniques. Results. We report the oxygen and iron abundances as measured with RGS in the core regions of all 44 clusters in the sample. We do not find a significant trend of O/Fe as a function of cluster temperature, but we do find an intrinsic scatter in the O and Fe abundances from cluster to cluster. The level of systematic uncertainties in the O/Fe ratio is estimated to be around 20-30%, while the systematic uncertainties in the absolute O and Fe abundances can be as high as 50% in extreme cases. Thanks to the high statistics of the observations, we were able to identify and correct a systematic bias in the oxygen abundance determination that was due to an inaccuracy in the spectral model. Conclusions. The lack of dependence of O/Fe on temperature suggests that the enrichment of the ICM does not depend on cluster mass and that most of the enrichment likely took place before the ICM was formed. We find that the observed scatter in the O/Fe ratio is due to a combination of intrinsic scatter in the source and systematic uncertainties in the spectral fitting, which we are unable to separate. The astrophysical source of intrinsic scatter could be due to differences in active galactic nucleus activity and ongoing star formation in the brightest cluster galaxy. The systematic scatter is due to uncertainties in the spatial line broadening, absorption column, multi-temperature structure, and the thermal plasma models.

Citovat

DE PLAA, J., J. S. KAASTRA, Norbert WERNER, C. PINTO, P. KOSEC, Y. Y. ZHANG, F. MERNIER, L. LOVISARI, H. AKAMATSU, G. SCHELLENBERGER, F. HOFMANN, T. H. REIPRICH, A. FINOGUENOV, J. AHORANTA, J. S. SANDERS, A. C. FABIAN, O. POLS, A. SIMIONESCU, J. VINK and H. BOHRINGER. CHEERS: The chemical evolution RGS sample. ASTRONOMY & ASTROPHYSICS. LES ULIS CEDEX A: EDP SCIENCES S A, 2017, vol. 607, November, p. 98-113. ISSN 1432-0746. Available from: https://dx.doi.org/10.1051/0004-6361/201629926.

@article{1406179,
   author = {de Plaa, J. and Kaastra, J. S. and Werner, Norbert and Pinto, C. and Kosec, P. and Zhang, Y. Y. and Mernier, F. and Lovisari, L. and Akamatsu, H. and Schellenberger, G. and Hofmann, F. and Reiprich, T. H. and Finoguenov, A. and Ahoranta, J. and Sanders, J. S. and Fabian, A. C. and Pols, O. and Simionescu, A. and Vink, J. and Bohringer, H.},
   article_location = {LES ULIS CEDEX A},
   article_number = {November},
   doi = {http://dx.doi.org/10.1051/0004-6361/201629926},
   keywords = {X-rays: galaxies: clusters; galaxies: clusters: intracluster medium; supernovae: general; galaxies: abundances},
   language = {eng},
   issn = {1432-0746},
   journal = {ASTRONOMY & ASTROPHYSICS},
   title = {CHEERS: The chemical evolution RGS sample},
   url = {https://arxiv.org/pdf/1707.05076.pdf},
   volume = {607},
   year = {2017}
}

TY  - JOUR
ID  - 1406179
AU  - de Plaa, J. - Kaastra, J. S. - Werner, Norbert - Pinto, C. - Kosec, P. - Zhang, Y. Y. - Mernier, F. - Lovisari, L. - Akamatsu, H. - Schellenberger, G. - Hofmann, F. - Reiprich, T. H. - Finoguenov, A. - Ahoranta, J. - Sanders, J. S. - Fabian, A. C. - Pols, O. - Simionescu, A. - Vink, J. - Bohringer, H.
PY  - 2017
TI  - CHEERS: The chemical evolution RGS sample
JF  - ASTRONOMY & ASTROPHYSICS
VL  - 607
IS  - November
SP  - 98-113
EP  - 98-113
PB  - EDP SCIENCES S A
SN  - 14320746
KW  - X-rays: galaxies: clusters
KW  - galaxies: clusters: intracluster medium
KW  - supernovae: general
KW  - galaxies: abundances
UR  - https://arxiv.org/pdf/1707.05076.pdf
N2  - Context. The chemical yields of supernovae and the metal enrichment of the intra-cluster medium (ICM) are not well understood. The hot gas in clusters of galaxies has been enriched with metals originating from billions of supernovae and provides a fair sample of large-scale metal enrichment in the Universe. High-resolution X-ray spectra of clusters of galaxies provide a unique way of measuring abundances in the hot intracluster medium (ICM). The abundance measurements can provide constraints on the supernova explosion mechanism and the initial-mass function of the stellar population. This paper introduces the CHEmical Enrichment RGS Sample (CHEERS), which is a sample of 44 bright local giant ellipticals, groups, and clusters of galaxies observed with XMM-Newton. Aims. The CHEERS project aims to provide the most accurate set of cluster abundances measured in X-rays using this sample. This paper focuses specifically on the abundance measurements of O and Fe using the reflection grating spectrometer (RGS) on board XMM-Newton. We aim to thoroughly discuss the cluster to cluster abundance variations and the robustness of the measurements. Methods. We have selected the CHEERS sample such that the oxygen abundance in each cluster is detected at a level of at least 5 sigma in the RGS. The dispersive nature of the RGS limits the sample to clusters with sharp surface brightness peaks. The deep exposures and the size of the sample allow us to quantify the intrinsic scatter and the systematic uncertainties in the abundances using spectral modeling techniques. Results. We report the oxygen and iron abundances as measured with RGS in the core regions of all 44 clusters in the sample. We do not find a significant trend of O/Fe as a function of cluster temperature, but we do find an intrinsic scatter in the O and Fe abundances from cluster to cluster. The level of systematic uncertainties in the O/Fe ratio is estimated to be around 20-30%, while the systematic uncertainties in the absolute O and Fe abundances can be as high as 50% in extreme cases. Thanks to the high statistics of the observations, we were able to identify and correct a systematic bias in the oxygen abundance determination that was due to an inaccuracy in the spectral model. Conclusions. The lack of dependence of O/Fe on temperature suggests that the enrichment of the ICM does not depend on cluster mass and that most of the enrichment likely took place before the ICM was formed. We find that the observed scatter in the O/Fe ratio is due to a combination of intrinsic scatter in the source and systematic uncertainties in the spectral fitting, which we are unable to separate. The astrophysical source of intrinsic scatter could be due to differences in active galactic nucleus activity and ongoing star formation in the brightest cluster galaxy. The systematic scatter is due to uncertainties in the spatial line broadening, absorption column, multi-temperature structure, and the thermal plasma models.
ER  -

DE PLAA, J., J. S. KAASTRA, Norbert WERNER, C. PINTO, P. KOSEC, Y. Y. ZHANG, F. MERNIER, L. LOVISARI, H. AKAMATSU, G. SCHELLENBERGER, F. HOFMANN, T. H. REIPRICH, A. FINOGUENOV, J. AHORANTA, J. S. SANDERS, A. C. FABIAN, O. POLS, A. SIMIONESCU, J. VINK and H. BOHRINGER. CHEERS: The chemical evolution RGS sample. \textit{ASTRONOMY \&{} ASTROPHYSICS}. LES ULIS CEDEX A: EDP SCIENCES S A, 2017, vol.~607, November, p.~98-113. ISSN~1432-0746. Available from: https://dx.doi.org/10.1051/0004-6361/201629926.

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