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108 results on '"Lovisari L"'

101. Extending the LX - T relation from clusters to groups.

Author

Bharadwaj, V., Reiprich, T. H., Lovisari, L., and Eckmiller, H. J.

Subjects
GALAXIES, GALAXY clusters, BLACK holes, GASES, X-rays
Abstract

Aims. We aim to investigate the bolometric LX - T relation for galaxy groups, and to study the impact of gas cooling, feedback from super-massive black holes, and the selection effects on it. Methods. With a sample of 26 galaxy groups, we obtained the best-fit LX - T relation for five different cases depending on the intracluster medium (ICM) core properties and central active galactic nuclei (AGN) radio emission, and determined the slopes, normalisations, and intrinsic and statistical scatters for both temperature and luminosity. We undertook simulations to correct for selection effects (e.g. Malmquist bias) and compared the bias-corrected relations for groups and clusters. Results. The slope of the bias-corrected LX - T relation is marginally steeper, but consistent with clusters (~3). Groups with a central cooling time of less than 1 Gyr (SCC groups) show indications of having the steepest slope and the highest normalisation. For the groups, the bias-corrected intrinsic scatter in LX is larger than the observed scatter for most cases, and this is reported here for the first time. We see indications that the groups with an extended central radio source (CRS) have a much steeper slope than those groups that have a CRS with only core emission. Additionally, we see indications that the more powerful radio AGN are preferentially located in non strong cool core (NSCC) groups rather than strong cool core (SCC) groups. [ABSTRACT FROM AUTHOR]

Published
2015
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102. On the dynamical and morphological state of the CHEX-MATE clusters

Author

Campitiello Maria Giulia, Ettori Stefano, and Lovisari Lorenzo

Subjects
Physics, QC1-999
Abstract

The CHEX-MATE sample was built to provide an overview of the statistical properties of the underlying cluster population and to set the stage for future X-ray missions. In this work, we perform a morphological analysis of the 118 clusters included in the sample with the aim to provide a classification of their dynamical state which will be useful for future studies of the collaboration.

Published
2022
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103. The Cluster HEritage project with XMM-Newton: Mass Assembly and Thermodynamics at the Endpoint of structure formation. I. Programme overview

Author

Alina Streblyanska, Raphael Gavazzi, I. Bartalucci, Mathilde Jauzac, P. S. Corasaniti, Paolo Tozzi, R. F. J. van der Burg, Jack Sayers, Mario Nonino, Dominique Eckert, Franco Vazza, M. Rossetti, S. Molendi, Christine Jones, A. Saro, Stefano Ettori, E. Rasia, A. Ferragamo, Nicolas Clerc, Jean-Baptiste Melin, Jose Alberto Rubino-Martin, Barbara Sartoris, Nobuhiro Okabe, R. T. Duffy, A. Iqbal, Sandrine Pires, F. Andrade-Santos, S. De Grandi, Rossella Cassano, F. Gastaldello, G. Schellenberger, Gustavo Yepes, Annalisa Bonafede, R. Barrena, Mauro Sereno, M. De Petris, Keiichi Umetsu, Etienne Pointecouteau, Paula Tarrío, Hervé Bourdin, Jean-Charles Cuillandre, Klaus Dolag, Chris P. Haines, Pasquale Mazzotta, S. Zarattini, Mario Radovich, Stefano Borgani, L. Salvati, Tiziana Venturi, M. Arnaud, Florian Kéruzoré, Simona Ghizzardi, David J. Barnes, Megan Donahue, Massimo Gaspari, S. Paltani, G. W. Pratt, Myriam Gitti, A. M. C. LeBrun, L. Perotto, S. Burkutean, F. Mayet, Scott T. Kay, Melanie Johnston-Hollitt, Lorenzo Lovisari, Herve Aussel, S. Maurogordato, Ben J Maughan, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), Istituto Nazionale di Astrofisica (INAF), University of Geneva [Switzerland], INAF-IASF Milano, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université de Genève = University of Geneva (UNIGE), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Arnaud, M., Ettori, S., Pratt, G. W., Rossetti, M., Eckert, D., Gastaldello, F., Gavazzi, R., Kay, S. T., Lovisari, L., Maughan, B. J., Pointecouteau, E., Sereno, M., Bartalucci, I., Bonafede, A., Bourdin, H., Cassano, R., Duffy, R. T., Iqbal, A., Maurogordato, S., Rasia, E., Sayers, J., Andrade-Santos, F., Aussel, H., Barnes, D. J., Barrena, R., Borgani, S., Burkutean, S., Clerc, N., Corasaniti, P. -S., Cuillandre, J. -C., De Grandi, S., De Petris, M., Dolag, K., Donahue, M., Ferragamo, A., Gaspari, M., Ghizzardi, S., Gitti, M., Haines, C. P., Jauzac, M., Johnston-Hollitt, M., Jones, C., Keruzore, F., Lebrun, A. M. C., Mayet, F., Mazzotta, P., Melin, J. -B., Molendi, S., Nonino, M., Okabe, N., Paltani, S., Perotto, L., Pires, S., Radovich, M., Rubino-Martin, J. -A., Salvati, L., Saro, A., Sartoris, B., Schellenberger, G., Streblyanska, A., Tarrio, P., Tozzi, P., Umetsu, K., Van Der Burg, R. F. J., Vazza, F., Venturi, T., Yepes, G., Zarattini, S., Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), UAM.Departamento de Física Teórica, COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Arnaud M., Ettori S., Pratt G.W., Rossetti M., Eckert D., Gastaldello F., Gavazzi R., Kay S.T., Lovisari L., Maughan B.J., Pointecouteau E., Sereno M., Bartalucci I., Bonafede A., Bourdin H., Cassano R., Duffy R.T., Iqbal A., Maurogordato S., Rasia E., Sayers J., Andrade-Santos F., Aussel H., Barnes D.J., Barrena R., Borgani S., Burkutean S., Clerc N., Corasaniti P.-S., Cuillandre J.-C., De Grandi S., De Petris M., Dolag K., Donahue M., Ferragamo A., Gaspari M., Ghizzardi S., Gitti M., Haines C.P., Jauzac M., Johnston-Hollitt M., Jones C., Keruzore F., Lebrun A.M.C., Mayet F., Mazzotta P., Melin J.-B., Molendi S., Nonino M., Okabe N., Paltani S., Perotto L., Pires S., Radovich M., Rubino-Martin J.-A., Salvati L., Saro A., Sartoris B., Schellenberger G., Streblyanska A., Tarrio P., Tozzi P., Umetsu K., Van Der Burg R.F.J., Vazza F., Venturi T., Yepes G., and Zarattini S.

Subjects
Structure formation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, Dark matter, Population, Thermodynamics, FOS: Physical sciences, observation [Cosmology], Astrophysics, clusters: intracluster medium [Galaxies], Astrophysics::Cosmology and Extragalactic Astrophysics, clusters: general [Galaxies], Cosmology: observation, 01 natural sciences, Observations [Cosmology], law.invention, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, law, 0103 physical sciences, Cluster (physics), Planck, education, 010303 astronomy & astrophysics, Galaxy cluster, Physics, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Settore FIS/05, 010308 nuclear & particles physics, Cosmology: observations, Física, Galaxies: clusters: general, Galaxies: clusters: intracluster medium, Astronomy and Astrophysics, Astronomía, Dark matter halo, [SDU]Sciences of the Universe [physics], Space and Planetary Science, symbols, Hydrostatic equilibrium, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Cluster HEritage project with XMM-Newton - Mass Assembly and Thermodynamics at the Endpoint of structure formation (CHEX-MATE) is a three mega-second Multi-Year Heritage Programme to obtain X-ray observations of a minimally-biased, signal-to-noise limited sample of 118 galaxy clusters detected by Planck through the Sunyaev-Zeldovich effect. The programme, described in detail in this paper, aims to study the ultimate products of structure formation in time and mass. It is composed of a census of the most recent objects to have formed (Tier-1: 0.05 < z < 0.2; 2 x 10e14 M_sun < M_500 < 9 x 10e14 M_sun), together with a sample of the highest-mass objects in the Universe (Tier-2: z < 0.6; M_500 > 7.25 x 10e14 M_sun). The programme will yield an accurate vision of the statistical properties of the underlying population, measure how the gas properties are shaped by collapse into the dark matter halo, uncover the provenance of non-gravitational heating, and resolve the major uncertainties in mass determination that limit the use of clusters for cosmological parameter estimation. We will acquire X-ray exposures of uniform depth, designed to obtain individual mass measurements accurate to 15-20% under the hydrostatic assumption. We present the project motivations, describe the programme definition, and detail the ongoing multi-wavelength observational (lensing, SZ, radio) and theoretical effort that is being deployed in support of the project., 27 pages, 11 figures; A&A, in press

Published
2021
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104. Stormy weather in 3C 196.1: nuclear outbursts and merger events shape the environment of the hybrid radio galaxy 3C 196.1

Author

Ralph Kraft, Elisabetta Liuzzo, Francesco Massaro, Grant R. Tremblay, Stefi A. Baum, William R. Forman, Alessandro Paggi, Federica Ricci, Belinda Jane Wilkes, Christopher P. O'Dea, Lorenzo Lovisari, Ricci F, Lovisari L, Kraft R. P., Massaro F., Paggi A., Liuzzo E., Tremblay G., Forman W. R., Baum S., O'Dea C., Wilkes B., Ricci, F., Lovisari, L., Kraft, R. P., Massaro, F., Paggi, A., Liuzzo, E., Tremblay, G., Forman, W. R., Baum, S., O’Dea, C., and Wilkes, B.

Subjects
galaxies: clusters: intracluster medium, Age of the universe, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, ISM [radio continuum], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, clusters: general [galaxies], Surface brightness, Brightest cluster galaxy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Jet (fluid), 010308 nuclear & particles physics, Image (category theory), Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Projection (relational algebra), radio continuum: ISM, 13. Climate action, Space and Planetary Science, clusters: intracluster medium [galaxies], galaxies: clusters: general, X-rays: galaxies: clusters, Astrophysics of Galaxies (astro-ph.GA), active [galaxies], galaxie [radio continuum], galaxies: clusters [X-rays], radio continuum: galaxie, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present a multi-wavelength analysis based on archival radio, optical and X-ray data of the complex radio source 3C 196.1, whose host is the brightest cluster galaxy of a $z=0.198$ cluster. HST data show H$\alpha$+[N II] emission aligned with the jet 8.4 GHz radio emission. An H$\alpha$+[N II] filament coincides with the brightest X-ray emission, the northern hotspot. Analysis of the X-ray and radio images reveals cavities located at galactic- and cluster- scales. The galactic-scale cavity is almost devoid of 8.4 GHz radio emission and the south-western H$\alpha$+[N II] emission is bounded (in projection) by this cavity. The outer cavity is co-spatial with the peak of 147 MHz radio emission, and hence we interpret this depression in X-ray surface brightness as being caused by a buoyantly rising bubble originating from an AGN outburst $\sim$280 Myrs ago. A \textit{Chandra} snapshot observation allowed us to constrain the physical parameters of the cluster, which has a cool core with a low central temperature $\sim$2.8 keV, low central entropy index $\sim$13 keV cm$^2$ and a short cooling time of $\sim$500 Myr, which is $, Comment: 14 pages, 4 figures, ApJ accepted

Published
2018

105. The cavity of 3CR 196.1: H$\alpha$ emission spatially associated with an X-ray cavity

Author

A. Jimenez-Gallardo, E. Sani, F. Ricci, C. Mazzucchelli, B. Balmaverde, F. Massaro, A. Capetti, W. R. Forman, R. P. Kraft, G. Venturi, M. Gendron-Marsolais, M. A. Prieto, A. Marconi, H. A. Peña-Herazo, S. A. Baum, C. P. O’Dea, L. Lovisari, R. Gilli, E. Torresi, A. Paggi, V. Missaglia, G. R. Tremblay, B. J. Wilkes, Ministerio de Ciencia e Innovación (España), Istituto Nazionale di Astrofisica, Jimenez-Gallardo, A., Sani, E., Ricci, F., Mazzucchelli, C., Balmaverde, B., Massaro, F., Capetti, A., Forman, W. R., Kraft, R. P., Venturi, G., Gendron-Marsolais, M., Prieto, M. A., Marconi, A., Pena-Herazo, H. A., Baum, S. A., O'Dea, C. P., Lovisari, L., Gilli, R., Torresi, E., Paggi, A., Missaglia, V., Tremblay, G. R., and Wilkes, B. J.

Subjects
Space and Planetary Science, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract

This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited., We present a multifrequency analysis of the radio galaxy 3CR 196.1 (z=0.198), associated with the brightest galaxy of the cool-core cluster CIZAJ0815.4-0303. This nearby radio galaxy shows a hybrid radio morphology and an X-ray cavity, all signatures of a turbulent past activity, potentially due to merger events and active galactic nuclei (AGN) outbursts. We present results of the comparison between Chandra and Very Large Telescope Multi-Unit Spectroscopic Explorer data for the inner region of the galaxy cluster, on a scale of tens of kpc. We discovered Hα + [N ii]λ6584 emission spatially associated with the X-ray cavity (at ∼10 kpc from the galaxy nucleus) instead of with its rim. This result differs from previous discoveries of ionized gas surrounding X-ray cavities in other radio galaxies harbored in galaxy clusters and could represent the first reported case of ionized gas filling an X-ray cavity, either due to different AGN outbursts or to the cooling of warm (104 < T ≤ 107 K) AGN outflows. We also found that the Hα, [N ii]λλ6548, 6584, and [S ii]λλ6718, 6733 emission lines show an additional redward component, at ∼1000 km s−1 from rest frame, with no detection in Hβ or [O iii]λλ4960, 5008. We believe the most likely explanation for this redward component is the presence of a background gas cloud as there appears to be a discrete difference of velocities between this component and the rest frame. © 2022. The Author(s). Published by the American Astronomical Society., This work is supported by the "Departments of Excellence 2018-2022" Grant awarded by the Italian Ministry of Education, University and Research (MIUR) (L. 232/2016). This research has made use of resources provided by the Ministry of Education, Universities and Research for the grant MASF_FFABR_17_01. This investigation is supported by the National Aeronautics and Space Administration (NASA) grants GO9-20083X and GO0-21110X. A.J. acknowledges the financial support (MASF_CONTR_FIN_18_01) from the Italian National Institute of Astrophysics under the agreement with the Instituto de Astrofisica de Canarias for the "Becas Internacionales para Licenciados y/o Graduados Convocatoria de 2017". F.R. acknowledges support from PRIN MIUR 2017 project "black hole winds and the Baryon Life Cycle of Galaxies: the stone-guest at the galaxy evolution supper", contract No. 2017PH3WAT. G.V. acknowledges support from ANID program FONDECYT Postdoctorado 3200802. A.P. acknowledges financial support from the Consorzio Interuniversitario per la fisica Spaziale (CIFS) under the agreement related to the grant MASF_CONTR_FIN_18_02. W.F. and R.K. acknowledge support from the Smithsonian Institution and the Chandra High Resolution Camera Project through NASA contract NAS8-03060. S.B. and C.O. acknowledge support from the Natural Sciences and Engineering Research Council (NSERC) of Canada., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.

Published
2022

106. CHEX-MATE: Morphological analysis of the sample

Author

M. G. Campitiello, S. Ettori, L. Lovisari, I. Bartalucci, D. Eckert, E. Rasia, M. Rossetti, F. Gastaldello, G. W. Pratt, B. Maughan, E. Pointecouteau, M. Sereno, V. Biffi, S. Borgani, F. De Luca, M. De Petris, M. Gaspari, S. Ghizzardi, P. Mazzotta, S. Molendi, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Campitiello, M. G., Ettori, S., Lovisari, L., Bartalucci, I., Eckert, D., Rasia, E., Rossetti, M., Gastaldello, F., Pratt, G. W., Maughan, B., Pointecouteau, E., Sereno, M., Biffi, V., Borgani, S., De Luca, F., De Petris, M., Gaspari, M., Ghizzardi, S., Mazzotta, P., Molendi, S., M. G. Campitiello, S. Ettori, L. Lovisari, I. Bartalucci, D. Eckert, E. Rasia, M. Rossetti, F. Gastaldello, G. W. Pratt, B. Maughan, E. Pointecouteau, M. Sereno, V. Biffi, S. Borgani, F. De Luca, M. De Petri, M. Gaspari, S. Ghizzardi, P. Mazzotta, and S. Molendi

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxies: clusters: intracluster medium, Settore FIS/05, galaxie, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Cosmology, X-ray, Astrophysic, Space and Planetary Science, X-rays: galaxies: clusters, X-rays, galaxies, astro-ph.CO, clusters, galaxies clusters, intracluster medium, Nongalactic Astrophysics, galaxies cluster, cluster, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

In this work, we performed an analysis of the X-ray morphology of the 118 CHEX-MATE (Cluster HEritage project with XMM-Newton - Mass Assembly and Thermodynamics at the Endpoint of structure formation) galaxy clusters, with the aim to provide a classification of their dynamical state. To investigate the link between the X-ray appearance and the dynamical state, we considered four morphological parameters: the surface brightness concentration, the centroid shift, and the second- and third-order power ratios. These indicators result to be: strongly correlated with each other, powerful in identifying the disturbed and relaxed population, characterised by a unimodal distribution and not strongly influenced by systematic uncertainties. In order to obtain a continuous classification of the CHEX-MATE objects, we combined these four parameters in a single quantity, M, which represents the grade of relaxation of a system. On the basis of the M value, we identified the most extreme systems of the sample, finding 15 very relaxed and 27 very disturbed galaxy clusters. From a comparison with previous analysis on X-ray selected samples, we confirmed that the Sunyaev-Zeldovich (SZ) clusters tend to be more disturbed. Finally, by applying our analysis on a simulated sample, we found a general agreement between the observed and simulated results, with the only exception of the concentration. This latter behaviour, is partially related to the presence of particles with high smoothed-particle hydrodynamics density in the central regions of the simulated clusters due to the action of the idealised isotropic thermal Active Galactic Nuclei (AGN) feedback., 24 pages, 16 figures, 10 tables. Accepted for publication in A&A

Published
2022
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107. The intracluster magnetic field in the double relic galaxy cluster Abell 2345

Author

Franco Vazza, Paola Domínguez-Fernández, R. J. van Weeren, Annalisa Bonafede, C. Stuardi, Lorenzo Lovisari, F. de Gasperin, Marcus Brüggen, Stuardi, C., Bonafede A., Lovisari L., Domínguez-Fernández P., Vazza F., Brüggen M., Van-Weeren, R.J., and De-Gasperin, F.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Radiation Mechanisms, FOS: Physical sciences, Non Thermal, Individual, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Clusters, Radio relics, Abell 2345, 0103 physical sciences, Cluster (physics), 010303 astronomy & astrophysics, Galaxy cluster, Equipartition theorem, Physics, magnetic fields – radiation mechanisms: non thermal – galaxies: clusters: individual: Abell 2345, 010308 nuclear & particles physics, Spectral density, Astronomy and Astrophysics, Radius, Galaxies, Polarization (waves), Astrophysics - Astrophysics of Galaxies, Magnetic field, Magnetic Fields, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Magnetic fields are ubiquitous in galaxy clusters, yet their radial profile, power spectrum, and connection to host cluster properties are poorly known. Merging galaxy clusters hosting diffuse polarized emission in the form of radio relics offer a unique possibility to study the magnetic fields in these complex systems. In this paper, we investigate the intra-cluster magnetic field in Abell 2345. This cluster hosts two radio relics that we detected in polarization with 1-2 GHz JVLA observations. X-ray XMM-Newton images show a very disturbed morphology. We derived the Rotation Measure (RM) of five polarized sources within $\sim$ 1 Mpc from the cluster center applying the RM synthesis. Both, the average RM and the RM dispersion radial profiles probe the presence of intra-cluster magnetic fields. Using the thermal electron density profile derived from X-ray analysis and simulating a 3D magnetic field with fluctuations following a power spectrum derived from magneto-hydrodynamical cosmological simulations, we build mock RM images of the cluster. We constrained the magnetic field profile in the eastern radio relic sector by comparing simulated and observed RM images. We find that, within the framework of our model, the data require a magnetic field scaling with thermal electron density as $B(r)\propto n_e(r)$. The best model has a central magnetic field (within a 200 kpc radius) of $2.8\pm0.1$ $\mu$G. The average magnetic field at the position of the eastern relic is $\sim$0.3 $\mu$G, a factor 2.7 lower than the equipartition estimate., Comment: 20 pages, 13 figures, 6 tables, accepted for publication in MNRAS

Published
2021

108. The radio relic in Abell 2256: overall spectrum and implications for electron acceleration

Author

Hiroki Akamatsu, Tracy Clarke, M. Trasatti, Marcus Brüggen, Annalisa Bonafede, Lorenzo Lovisari, Uli Klein, Daniele Dallacasa, Trasatti, M., Akamatsu, H., Lovisari, L., Klein, U., Bonafede, A., Brüggen, M., Dallacasa, D., and Clarke, T.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Spectral index, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Galaxies: clusters: individual: Abell 2256, Astrophysics, Electron, Astronomy and Astrophysic, Acceleration of particle, Power law, Astrophysics - Astrophysics of Galaxies, Acceleration, Radio relics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Galaxies: clusters: general, Test particle, Astrophysics - High Energy Astrophysical Phenomena, Galaxy cluster, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The galaxy cluster Abell 2256 hosts one of the most intriguing examples in the class of radio relics. It has been found that this radio relic has a rather flat integrated spectrum at low frequencies that would imply an injection spectral index for the electrons that is inconsistent with the flattest allowed by the test particle diffusive shock acceleration (DSA). We performed new high-frequency observations at 2273, 2640, and 4850 MHz. Combining these new observations with images available in the literature, we constrain the radio integrated spectrum of the radio relic in Abell 2256 over the widest sampled frequency range collected so far for this class of objects (63 -10450 MHz). Moreover, we used X-ray observations of the cluster to check the temperature structure in the regions around the radio relic. We find that the relic keeps an unusually flat behavior up to high frequencies. Although the relic integrated spectrum between 63 and 10450 MHz is not inconsistent with a single power law with $\alpha_{63}^{10450}= 0.92\pm 0.02$, we find hints of a steepening at frequencies > 1400 MHz. The two frequency ranges 63-1369 MHz and 1369-10450 MHz are, indeed, best represented by two different power laws, with $\alpha_{63}^{1369}= 0.85\pm 0.01$ and $\alpha_{1369}^{10450}= 1.00\pm 0.02$. This broken power law would require special conditions to be explained in terms of test-particle DSA, e.g., non-stationarity of the spectrum and/or non-stationarity of the shock. On the other hand, the single power law would make of this relic the one with the flattest integrated spectrum known so far, even flatter than what allowed in the test-particle approach to DSA. We find a rather low temperature ratio of $T_2/T_1 \sim 1.7$ across the G region of the radio relic and no temperature jump across the H region., Comment: 18 pages, 11 figures, 9 tables. Accepted for publication in Astronomy & Astrophysics

Published
2014

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