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Статті в журналах з теми "Intra Cluster Medium"
Domainko, Wilfried, Wolfgang Kapferer, Sabine Schindler, Eelco van Kampen, Stefan Kimeswenger, and Maximilian Ruffert. "The Chemical Evolution of the Intra-Cluster Medium." Symposium - International Astronomical Union 217 (2004): 464–65. http://dx.doi.org/10.1017/s0074180900198195.
Повний текст джерелаSchindler, S. "Metal Enrichment in the Intra-Cluster Medium." EAS Publications Series 24 (2007): 121–32. http://dx.doi.org/10.1051/eas:2007019.
Повний текст джерелаMoretti, A., L. Portinari, and C. Chiosi. "Chemical evolution of the intra-cluster medium." Astronomy & Astrophysics 408, no. 2 (September 2003): 431–53. http://dx.doi.org/10.1051/0004-6361:20031012.
Повний текст джерелаBignamini, A., P. Tozzi, S. Borgani, S. Ettori, and P. Rosati. "Intra cluster medium properties and AGN distribution in high-zRCS clusters." Astronomy & Astrophysics 489, no. 3 (August 1, 2008): 967–79. http://dx.doi.org/10.1051/0004-6361:200809437.
Повний текст джерелаBonafede, Annalisa, Chiara Stuardi, Federica Savini, Franco Vazza, and Marcus Brüggen. "Constraining magnetic fields in galaxy clusters." Proceedings of the International Astronomical Union 14, A30 (August 2018): 299–302. http://dx.doi.org/10.1017/s1743921319004459.
Повний текст джерелаCucchetti, E., N. Clerc, E. Pointecouteau, P. Peille, and F. Pajot. "Towards mapping turbulence in the intra-cluster medium." Astronomy & Astrophysics 629 (September 2019): A144. http://dx.doi.org/10.1051/0004-6361/201935677.
Повний текст джерелаKotecha, Sachin, Charlotte Welker, Zihan Zhou, James Wadsley, Katarina Kraljic, Jenny Sorce, Elena Rasia, et al. "Cosmic filaments delay quenching inside clusters." Monthly Notices of the Royal Astronomical Society 512, no. 1 (February 10, 2022): 926–44. http://dx.doi.org/10.1093/mnras/stac300.
Повний текст джерелаSchindler, S., W. Kapferer, W. Domainko, M. Mair, E. van Kampen, T. Kronberger, S. Kimeswenger, M. Ruffert, O. Mangete, and D. Breitschwerdt. "Metal enrichment processes in the intra-cluster medium." Astronomy & Astrophysics 435, no. 2 (April 29, 2005): L25—L28. http://dx.doi.org/10.1051/0004-6361:200500107.
Повний текст джерелаPuchwein, E., and M. Bartelmann. "Three-dimensional reconstruction of the intra-cluster medium." Astronomy & Astrophysics 455, no. 3 (August 16, 2006): 791–801. http://dx.doi.org/10.1051/0004-6361:20054717.
Повний текст джерелаClerc, Nicolas, Edoardo Cucchetti, Etienne Pointecouteau, and Philippe Peille. "Towards mapping turbulence in the intra-cluster medium." Astronomy & Astrophysics 629 (September 2019): A143. http://dx.doi.org/10.1051/0004-6361/201935676.
Повний текст джерелаДисертації з теми "Intra Cluster Medium"
Ghirardini, Vittorio <1990>. "Mapping of the intra-cluster medium out to the virial radius." Doctoral thesis, Alma Mater Studiorum - Università di Bologna, 2019. http://amsdottorato.unibo.it/8775/1/thesis.pdf.
Повний текст джерелаLECCARDI, ALBERTO. "Thermodynamic and chemical properties of the intra-cluster medium in the outer regions of galaxy clusters." Doctoral thesis, Università degli Studi di Milano, 2009. http://hdl.handle.net/2434/72734.
Повний текст джерелаFabjan, Dunja. "The effect of star formation and feedback on the X-ray properties of simulated galaxy clusters." Doctoral thesis, Università degli studi di Trieste, 2010. http://hdl.handle.net/10077/3434.
Повний текст джерелаThe aim of this Thesis was to study the X--ray properties of the IntraCluster Medium (ICM) in a cosmological context resorting to high resolution hydrodynamical simulations. The thermodynamical and chemical properties of the ICM were inspected and studied within a set of galaxy clusters that were simulated with the TREE-SPH Gadget2 code (Springel 2005). This code included a detailed model of chemical evolution (Tornatore et al. 2007) as well as prescriptions for different physical processes: star formation, galactic winds and AGN feedback. We use this large set of simulated galaxy clusters with a twofold aim. First, we study the effect of different sources of feedback on the ICM observable properties, in particular on its metal enrichment and on thermo and chemo--dynamical properties when AGN feedback is at work. Second, we test the robustness of cluster mass proxies against the different physical processes included in the simulations. When exploring the effect on metal enrichment and its evolution we found that among different prescriptions for the stellar Initial Mass Function (IMF), the best results on Iron abundance profiles and global Iron evolution are found when applying the Salpeter IMF (Salpeter 1955). We also found that the positive evolution of the metal abundance in the central regions of simulated clusters can not be simply interpreted as a consequence of an excess of low--redshift star formation. Instead the evolution of the metallicity pattern is driven by the combined action of gas--dynamical processes, which redistribute already enriched gas, and of star formation, which acts both as a source and as a sink of metals (Fabjan et al. 2008, Borgani et al. 2008). Our analysis on the AGN feedback effect on ICM properties lends further support to the idea that a feedback source associated to gas accretion onto super-massive BHs is required by the observational properties of the ICM (e.g. McNamara & Nulsen 2007). However, our results also show that there are still a number of discrepancies between observations and the predictions made by simulations. This is especially true within the core regions of massive clusters, where a more efficient way of extracting and/or thermalising energy released by AGN is required. Our results further demonstrate that different astrophysical feedback sources leave distinct signatures on the pattern of chemical enrichment of the ICM. These differences are much more evident in the outskirts of galaxy clusters, which retain memory of the past efficiency that energy feedback had in displacing enriched gas from star-forming regions and in regulating star formation itself (Fabjan et al. 2010). The characterization of thermal and chemical properties in cluster external regions requires X--ray telescopes with large collecting area and an excellent control of the background, characteristics which should be eventually met by a future generation of X--ray satellites. In the last part of this Thesis we studied the effect that different physical processes included in the simulations have on the mass--observable scaling relations and their evolution with redshift. We focused on two cluster mass proxies, the gas mass M_gas and a new Y_X proxy defined by Kravtsov et al. (2006) as the product of gas mass and cluster temperature and test the robustness of the two relations, M_tot-M_gas and M_tot-Y_X, in simulations before including any observational effect. Furthermore we test the relations against the change of prescription for the physics that describes the ICM, such as viscosity, thermal conduction, star formation, galactic winds and AGN feedback. We found that the evolutions of both relations do not show any significant deviation from the predictions of the simple self--similar model. However we found that the Y_X proxy is less sensitive to the change of physical processes included in simulations. Since Y_X is by definition a measure of the thermal pressure support in the ICM, once the central cluster region is excised, the relation M_tot-Y_X is more stable against the change of physical processes included in the simulations (Fabjan et al., in preparation). In the future, the improved numerical resolution expected to be reached in simulations of the next generation needs to be accompanied by a suitable description of the subresolution physics, both concerning the star formation physics and and the AGN feedback. Within the latter, the inclusion of the jet injection by AGN would of course provide a physically meaningful description of the interplay between BH accretion and ICM properties. While Chandra, XMM and Suzaku will be pushed to their limits in these studies in the next few years, there is no doubt that a detailed knowledge of the ICM out the cluster virial boundaries and reaching very high redshift has to await for the advent of the next generation of X--ray telescopes (Giacconi et al. 2009, Arnaud et al.2009).
XXII Ciclo
1979
Ruppin, Florian. "Cosmologie via les observations d'amas de galaxies par effet Sunyaev-Zel'dovich avec NIKA2." Thesis, Université Grenoble Alpes (ComUE), 2018. http://www.theses.fr/2018GREAY029/document.
Повний текст джерелаThe mass distribution in the Universe, as traced by galaxy clusters is a powerful cosmological probe. The characterization of the processes associated with the origin and the growth of the large scale structures enables constraining cosmological parameters by studying the distribution of clusters according to their mass and redshift. However, a tension is observed between the cosmological constraints established by the study of the primary anisotropies of the cosmological background and those resulting from the analysis of the distribution of galaxy clusters. This may imply that our cosmological model is incomplete. The observation of clusters from the Sunyaev-Zel'dovich (SZ) effect allows us to constrain their gas pressure. This observable can be directly linked to the mass of galaxy clusters via a scaling relation and a pressure profile. It is thus essential to characterize the latter precisely in order to limit the potential bias and systematic effects affecting cosmological analyses. This thesis presents the work carried out to this end. It covers topics ranging from SZ observations made with the NIKA2 camera installed at the IRAM 30-metre telescope to the estimation of cosmological parameters, and including the analysis of NIKA2 raw data and the SZ maps produced.Part of the thesis work presented in this document is dedicated to the study and the improvement of the different tasks carried out, from the observations of galaxy clusters with the NIKA2 camera to the production of maps of the SZ effect. The procedures developed to estimate the NIKA2 instrumental performance are detailed and the analysis pipeline used to analyze the raw data is presented.The work carried out in this thesis also consisted in characterizing the thermodynamic properties of galaxy clusters using joint analyzes that combine the NIKA2 SZ maps with X-ray data measured by the XMM-Newton satellite. We detail the methods used in the SZ data processing software created for the NIKA2 SZ large program, the non-parametric deprojection procedure developed to characterize the pressure profile of galaxy clusters and the results of the first SZ observation with NIKA2.The last activities presented are dedicated to the analyses carried out to quantify the impact of the NIKA2 SZ large program on cosmology. We analyze the effect of dynamic disturbances of the intracluster medium on the characterization of the pressure profile with NIKA2 via the use of clusters from the MUSIC N-body simulation. Finally, we detail the study realized in order to estimate the impact of a modification of the universal pressure profile on the estimation of cosmological parameters derived from the power spectrum of the SZ effect measured by Planck
Balestra, Italo [Verfasser]. "Elemental abundances in the intra-cluster medium and in active galactic nuclei / Italo Balestra." 2007. http://d-nb.info/987922483/34.
Повний текст джерелаRhea, Carter. "Nouvelles observations et techniques d'apprentissage automatique appliquées aux galaxies et aux amas de galaxies." Thesis, 2020. http://hdl.handle.net/1866/24376.
Повний текст джерелаGalaxy clusters are one of the largest structures in the universe and host several complex physical phenomena. Although a wealth of knowledge already exists on their formation and evolution, the recent advent of machine learning in the astronomical sciences has allowed us to probe questions heretofore unanswered. While this thesis does focus heavily on the application of machine learning techniques to X-ray observations of galaxy clusters, it takes the techniques applied there to galaxy cluster's smaller counterparts: the individual galaxies themselves. Although the three papers presented here focus on distinct physics, scales, and techniques, they all form a basis of studies that I will continue during my doctorate: using new techniques to probe the underlying physics of galactic and extragalactic regions. The first paper introduced is a study of a galaxy cluster near the beginning of the epoch of cluster formation exhibiting peculiar attributes such as an elevated stellar formation rate (∽ 900M⊙/yr). In this paper, we employ traditional techniques in X-ray astronomy to determine whether or not the prodigious formation rate is due to an uninhibited cooling core. Since the object is so distant (z=1.7), we must execute our calculations with relatively few photons and thus rely on proxy measures. We determine that there exists a strong cooling flow offset by over 50 kpc from the central galaxy. Because of this offset, the AGN is not fueled and thus fails to heat up the cooling flow. This is the first example of a galaxy cluster in which we observe the failure of AGN feedback. Additionally, this provides another mechanism for the creation of intracluster light. The second article presented here focuses on X-ray emission from the hot intra-cluster medium within the galaxy cluster. We develop a comprehensive method for determining the number of underlying thermal components in the plasma's spectra. Our novel technique relies on a combination of an unsupervised learning algorithm (principal component analysis) and a supervised learning algorithm (random forest classification). We create a set of 100,000 realistic mock Chandra observations of the hot X-ray emitting gas in nearby galaxy clusters. After reducing our synthetic training set to its 25 most important principal components, we trained a random forest classifier to distinguish between the number of underlying thermal components. After successful testing and hyperparameter optimization, we applied the methodology third paper featured in this thesis once again employs machine learning to solve a previously undetermined question necessary for the accurate characterization of the kinematics of the warm gas in galaxies. We constructed a convolutional neural network to estimate the velocity and broadening parameters from the optical spectra of emission-line nebula and applied it to synthetic data replicating real SITELLE observations from the SIGNALS program. With a trained and optimized network in hand, we apply our methodology to a target of the SIGNALS program: the galaxy M33. Our results indicate our algorithm out-performs previous methods and nicely complements spectral fitting procedures. Moreover, the methodology increases calculation speeds by more than an order of magnitude -- thus greatly reducing the time needed to determine the kinematic parameters. Although the algorithm was trained for SITELLE data, this method can be readily ported to other IFUs such as MUSE. I have led two of the papers presented in this memoire and made major contributions to the third. All three papers have been either accepted for publication or have already been submitted and revised once. to the Perseus Cluster. In addition to creating a map of the cluster indicating the number of thermal components required to accurately model the thermal emission, we developed a suite of analysis routines to determine the temperatures of the underlying components. Our results are in agreement with over a decade of studies on the Perseus cluster and indicate that multiple temperature components are required for the accurate study of its intracluster medium.
Latulippe, Myriam. "Influence du trou noir supermassif central dans l’amas de galaxies MACS J1447.4+0827." Thèse, 2017. http://hdl.handle.net/1866/20312.
Повний текст джерелаGendron-Marsolais, Marie-Lou. "Observations multi-longueur d’onde d’amas et de groupes de galaxies proches." Thèse, 2018. http://hdl.handle.net/1866/21757.
Повний текст джерелаRichard-Laferrière, Annabelle. "L'impact des trous noirs les plus massifs de l’Univers sur le coeur des amas de galaxies." Thèse, 2019. http://hdl.handle.net/1866/22724.
Повний текст джерелаКниги з теми "Intra Cluster Medium"
The environmental impact of intra-cluster medium on the interstellar medium in early type galaxies: Semiannual reports, 1 August 1993-31 January 1994 ... 1 August 1994-31 January 1995, annual report, 1 August 1995-31 July 1996. Cambridge, Mass: Smithsonian Institution, Astrophysical Observatory, 1996.
Знайти повний текст джерелаЧастини книг з теми "Intra Cluster Medium"
Cora, Sofía A., and Simon D. M. White. "Chemical Enrichment of the Intra-Cluster Medium." In The Evolution of Galaxies, 131–34. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-017-3315-1_23.
Повний текст джерелаElbaz, D., and L. Vigroux. "Timescales for Galaxy Formation and Intra-Cluster Medium Enrichment." In New Light on Galaxy Evolution, 370. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0229-9_82.
Повний текст джерелаIapichino, Luigi, Jens C. Niemeyer, Surajit Paul, and Wolfram Schmidt. "Turbulence Modeling and the Physics of the Intra-Cluster Medium." In High Performance Computing in Science and Engineering, Garching/Munich 2009, 383–94. Berlin, Heidelberg: Springer Berlin Heidelberg, 2010. http://dx.doi.org/10.1007/978-3-642-13872-0_32.
Повний текст джерелаUlmer, M. P., R. G. Cruddace, E. Fenimore, W. A. Snyder, and G. Fritz. "Elemental Abundances and Temperature Distributions in the Intra-Cluster Medium of the Perseus Cluster." In Observational Cosmology, 523–26. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-3853-3_51.
Повний текст джерелаТези доповідей конференцій з теми "Intra Cluster Medium"
Molendi, Silvano. "The Intra-Cluster Medium." In PLASMAS IN THE LABORATORY AND IN THE UNIVERSE: New Insights and New Challenges. AIP, 2004. http://dx.doi.org/10.1063/1.1718479.
Повний текст джерелаDomainko, Wilfried, W. Kapferer, M. Gitti, S. Schindler, E. Van Kampen, S. Kimeswenger, M. Mair, T. Kronberger, M. Ruffert, and O. E. Mangete. "Metal enrichment of the Intra-Cluster Medium: Ram-Pressure Stripping and Feedback from Intra-Cluster Supernovae." In Baryons in Dark Matter Halos. Trieste, Italy: Sissa Medialab, 2004. http://dx.doi.org/10.22323/1.014.0074.
Повний текст джерелаMolendi, Silvano, A. Comastri, L. Angelini, and M. Cappi. "The Intra-cluster medium: recent results and future prospects." In X-RAY ASTRONOMY 2009; PRESENT STATUS, MULTI-WAVELENGTH APPROACH AND FUTURE PERSPECTIVES: Proceedings of the International Conference. AIP, 2010. http://dx.doi.org/10.1063/1.3475229.
Повний текст джерелаIapichino, L., A. Maier, W. Schmidt, J. C. Niemeyer, Jean-Michel Alimi, and André Fuözfa. "Turbulence modeling and the physics of the intra-cluster medium." In INVISIBLE UNIVERSE: Proceedings of the Conference. AIP, 2010. http://dx.doi.org/10.1063/1.3462735.
Повний текст джерелаBasu, K., M. W. Sommer, Y. Y. Zhang, A. Comastri, L. Angelini, and M. Cappi. "Joint X-ray∕Sunyaev-Zel’dovich Analysis of the Intra-Cluster Medium." In X-RAY ASTRONOMY 2009; PRESENT STATUS, MULTI-WAVELENGTH APPROACH AND FUTURE PERSPECTIVES: Proceedings of the International Conference. AIP, 2010. http://dx.doi.org/10.1063/1.3475230.
Повний текст джерелаSato, Kosuke, Kazuyo Tokoi, Kyoko Matsushita, Yoshitaka Ishisaki, Noriko Y. Yamasaki, Manabu Ishida, Takaya Ohashi, et al. "Supernovae contributions to metals in intra-cluster medium observed with Suzaku." In ORIGIN OF MATTER AND EVOLUTION OF GALAXIES: The 10th International Symposium on Origin of Matter and Evolution of Galaxies: From the Dawn of Universe to the Formation of Solar System. AIP, 2008. http://dx.doi.org/10.1063/1.2943599.
Повний текст джерелаSchindler, Sabine. "Interaction of galaxies with the intra-cluster medium and ICM metal enrichment." In Baryons in Dark Matter Halos. Trieste, Italy: Sissa Medialab, 2004. http://dx.doi.org/10.22323/1.014.0023.
Повний текст джерелаPančišin, M., C. Kaiser, G. Pavlovski, W. Kapferer, S. Schindler, E. van Kampen, M. Ruffert, Sebastian Heinz, and Eric Wilcots. "Enrichment of the Intra-Cluster Medium Due to AGN Outflows Induced by Late-Type Galaxies." In THE MONSTER’S FIERY BREATH: FEEDBACK IN GALAXIES, GROUPS, AND CLUSTERS. AIP, 2009. http://dx.doi.org/10.1063/1.3293015.
Повний текст джерелаLiu, Wing Kam, and Ashfaq Adnan. "Multiscale Modeling and Simulation for Nanodiamond-Based Therapeutic Delivery." In ASME 2010 First Global Congress on NanoEngineering for Medicine and Biology. ASMEDC, 2010. http://dx.doi.org/10.1115/nemb2010-13273.
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