Search

Les amas des galaxies sont l’une des plus grandes structures liées gravitationnellement de l’univers. Leur dynamique est complexe et bien que plusieurs études multi-longueur d’onde ont été effectuées depuis la fin du 20ème siècle, il persiste plusieurs incertitudes sur les subtilités de leur dynamique. À ce jour, le consensus scientifique est que les trous noirs supermassifs actifs au centre des amas ont un impact important sur l’évolution de ces structures. Le trou noir central agit comme centre gravitationnel, mais lorsque ce trou noir est actif, son rôle ne se limite pas seulement à son impact gravitationnel. D’une part, les trous noirs actifs ont un rôle crucial dans l’émission thermique des amas. En effet, les jets radio influencent l’émission rayons-X des amas en poussant mécaniquement le milieu intra-amas qui émet en rayons-X via l’émission Bremsstrahlung. Ce phénomène engendre la formation de cavités rayons-X qui constituent une preuve de la rétroaction énergétique du trou noir sur l’ensemble de l’amas. Un tel phénomène est nécessaire afin d’expliquer les résultats observationnels qui témoignent d’un refroidissement moins important que prédit théoriquement au centre des amas à cœur froid. D’autre part, il existe de plus en plus d’études qui supportent l’hypothèse que les trous noirs actifs ont un rôle dans la (ré-)accélération de particules relativistes responsables de l’émission synchrotron au cœur des amas à cœur froid. Ces structures appelées mini-halos sont typiquement diffuses en radio et donc difficiles à détecter. Dans ce mémoire, nous étudierons en détail l’émission radio de l’amas de galaxies massif à cœur froid MS 0735.6+7421 (z = 0.216). Cet amas est unique puisqu’il possède les jets radio les plus énergétiques détectés au centre d’un amas à cœur froid. Il s’agit donc d’un exemple de trou noir actif parmi les plus extrêmes connus. Cet objet constitue ainsi une cible parfaite afin d’étudier le lien qui unit la rétroaction du trou noir actif central et l’émission synchrotron au centre des amas à cœur froid. Pour réaliser cette étude, nous avons effectué une analyse radio exhaustive de MS 0735.6+7421 à l’aide de données acquises sur le Karl G. Jansky Very Large Array. Cette analyse a permis de détecter une nouvelle structure radio diffuse jamais détectée auparavant. Cette nouvelle structure possède une puissance radio à 1.4 GHz qui concorde avec celles des mini-halos les plus lumineux. Le résultat principal de notre étude supporte donc l’hypothèse selon laquelle il existe un lien fondamental entre la rétroaction du trou noir actif central et la formation de mini-halos au centre des amas à cœur froid., Galaxy clusters are one of the largest gravitationally bound structures in the universe. They exhibit complex dynamics and even though several multi-wavelength studies have been conducted since the end of the 20th century, there are still a lot of uncertainties concerning their evolution. To this day, the scientific consensus is that the active supermassive black hole at the center of the cluster has a profound impact on the cluster’s evolution. Indeed, the central supermassive black hole has a substantial gravitational impact, but when the black hole actively accretes material, its role goes beyond its gravitational influence. Active supermassive black holes have a crucial role in terms of the thermal emission in clusters. Indeed, the radio jets influence the X-ray emission of clusters by mechanically pushing the intracluster medium which emits in X-ray via Bremsstrahlung emission. This leads to the formation of X-ray cavities which are proof of the energetic feedback of the central supermassive black hole on the cluster. Such a phenomenon is required to reconcile the observational results that report less cooling at the center of cool core clusters than what is theoretically predicted. Moreover, there are more and more studies that support the hypothesis that active supermassive black holes have a crucial role in the (re-)acceleration of seed particles responsible for synchrotron emission at the center of cool core clusters. These structures are named mini-halos and are usually difficult to detect because they are diffuse. In this Master’s thesis, we will study the radio emission of the massive cool core galaxy cluster MS 0735.6+7421 (z = 0.216). This cluster is unique because it exhibits the most powerful radio jets ever detected at the center of a cool core cluster. It thus contains one of the most powerful active supermassive black holes known. This object is a perfect target to study the link between active black hole feedback and synchrotron emission in cool core clusters. To conduct this study, we performed a radio analysis of MS 0735.6+7421 with new data obtained with the Karl G. Jansky Very Large Array. This analysis led to the discovery of an extended diffuse radio structure. This newly detected structure has a radio power at 1.4 GHz that matches the most luminous mini-halos known in the literature. The principal result of our study argues in favor of the hypothesis that there is a fundamental link between active black hole feedback and the formation of mini-halos at the center of cool core clusters.

MISTRAL is a millimetric camera working in the W-band (78–103 GHz) which will take data from the Sardinia Radio Telescope, the Italian 64-m radio telescope located 50 km form Cagliari, at 600m above the sea level, in Sardinia. It is being built as a facility instrument by the Sapienza University for INAF, that manages the radio telescope, under a PON contract. It will consist of a compact cryostat hosting the re–imaging optics, cooled at 4K, and a 408–pixel array of photon–noise limited lumped element kinetic inductance detectors fabricated at CNR-IFN and cooled at a base temperature lower than 300mK. MISTRAL will be able to investigate a long list of scientific targets spanning from extragalactic astrophysics to solar system science, with high angular resolution (~ 12 arcsec), including Sunyaev Zel’dovich effect measurements and the study of the Cosmic Web.

Lokken et al., The cosmic web contains filamentary structure on a wide range of scales. On the largest scales, superclustering aligns multiple galaxy clusters along intercluster bridges, visible through their thermal Sunyaev–Zel'dovich signal in the cosmic microwave background. We demonstrate a new, flexible method to analyze the hot gas signal from multiscale extended structures. We use a Compton y-map from the Atacama Cosmology Telescope (ACT) stacked on redMaPPer cluster positions from the optical Dark Energy Survey (DES). Cutout images from the y-map are oriented with large-scale structure information from DES galaxy data such that the superclustering signal is aligned before being overlaid. We find evidence of an extended quadrupole moment of the stacked y signal at the 3.5σ level, demonstrating that the large-scale thermal energy surrounding galaxy clusters is anisotropically distributed. We compare our ACT × DES results with the Buzzard simulations, finding broad agreement. Using simulations, we highlight the promise of this novel technique for constraining the evolution of anisotropic, non-Gaussian structure using future combinations of microwave and optical surveys., J.R.B. was funded by the Natural Sciences and Engineering Research Council of Canada Discovery Grant Program and a fellowship from the Canadian Institute for Advanced Research (CIFAR) Gravity and Extreme Universe program. A.D.H. acknowledges support from the Sutton Family Chair in Science, Christianity and Cultures. R.H. is a CIFAR Azrieli Global Scholar, Gravity and the Extreme Universe Program, 2019, and a 2020 Alfred P. Sloan Research Fellow. R.H. is supported by the Natural Sciences and Engineering Research Council of Canada Discovery Grant Program and the Connaught Fund. The Dunlap Institute is funded through an endowment established by the David Dunlap family and the University of Toronto. J.P.H. acknowledges funding for SZ cluster studies from NSF AAG No. AST-1615657. M.L. acknowledges the support of the National Sciences and Engineering Research Council of Canada (NSERC) [PGSD - 559296 - 2021] and the Queen Elizabeth II / Graduate Scholarships in Science and Technology (QEII-GSST). K.M. acknowledges support from the National Research Foundation of South Africa. This work was supported by the U.S. National Science Foundation through awards AST-0408698, AST-0965625, and AST-1440226 for the ACT project, as well as awards PHY-0355328, PHY-0855887, and PHY-1214379. Funding was also provided by Princeton University, the University of Pennsylvania, and a Canada Foundation for Innovation (CFI) award to UBC. ACT operates in the Parque Astronómico Atacama in northern Chile under the auspices of the Comisión Nacional de Investigación (CONICYT). The development of multichroic detectors and lenses was supported by NASA grants NNX13AE56G and NNX14AB58G. Detector research at NIST was supported by the NIST Innovations in Measurement Science program. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l'Espai (IEEC/CSIC), the Institut de Física d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NFS' NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF's NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grant Nos. ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Program (FP7/2007-2013), including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). We thank the anonymous referee for providing valuable comments which improved the quality of the manuscript. This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. This work received support from the U.S. Department of Energy under contract No. DE-AC02-76SF00515 at SLAC National Accelerator Laboratory. This research used computing resources at SLAC National Accelerator Laboratory and at the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility located at Lawrence Berkeley National Laboratory, operated under contract No. DE-AC02-05CH11231.

We report the results of combined analyses of X-ray and optical data of two galaxy clusters, CL 0024$+$1654 and RX J0152.7$-$1357 at redshift $z = 0.395$ and $z = 0.830$, respectively, which offer a holistic physical description of the two clusters. Our X-ray analysis yields temperature and density profile of the gas in the intra-cluster medium (ICM). Using optical photometric and spectroscopic data, complemented with mass distribution from gravitational lensing study, we investigate any possible correlation between the physical properties of the galaxy members, i.e., their color, morphology, and star formation rate (SFR) with their environments. We quantify the properties of the environment of each galaxy by galaxy number density, ICM temperature, and mass density. Although our result shows that the two clusters exhibit a weaker correlation compared to relaxed clusters, it still confirms the significant effect of the ICM on the SFRs in the galaxies. The closer relation between galaxy physical property and the condition of its immediate environment found in this work indicates the locality of galaxy evolution, even within a larger bound system such as cluster. Various physical mechanisms are suggested to explain the relation between the properties of galaxies and their environment., 24 pages, 10 figures, 4 tables, accepted for publication in J. Math. Fund. Sci

We provide the first combined cosmological analysis of South Pole Telescope (SPT) and Planck cluster catalogs. The aim is to provide an independent calibration for Planck scaling relations, exploiting the cosmological constraining power of the SPT-SZ cluster catalog and its dedicated weak lensing (WL) and X-ray follow-up observations. We build a new version of the Planck cluster likelihood. In the $\nu \Lambda$CDM scenario, focusing on the mass slope and mass bias of Planck scaling relations, we find $\alpha_{\text{SZ}} = 1.49_{-0.10}^{+0.07}$ and $(1-b)_{\text{SZ}} = 0.69_{-0.14}^{+0.07}$ respectively. The results for the mass slope show a $\sim 4 \, \sigma$ departure from the self-similar evolution, $\alpha_{\text{SZ}} \sim 1.8$. This shift is mainly driven by the matter density value preferred by SPT data, $\Omega_m = 0.30 \pm 0.03$, lower than the one obtained by Planck data alone, $\Omega_m = 0.37_{-0.06}^{+0.02}$. The mass bias constraints are consistent both with outcomes of hydrodynamical simulations and external WL calibrations, $(1-b) \sim 0.8$, and with results required by the Planck cosmic microwave background cosmology, $(1-b) \sim 0.6$. From this analysis, we obtain a new catalog of Planck cluster masses $M_{500}$. We estimate the ratio between the published Planck $M_{\text{SZ}}$ masses and our derived masses $M_{500}$, as a "measured mass bias", $(1-b)_M$. We analyse the mass, redshift and detection noise dependence of $(1-b)_M$, finding an increasing trend towards high redshift and low mass. These results mimic the effect of departure from self-similarity in cluster evolution, showing different dependencies for the low-mass high-mass, low-z high-z regimes., Comment: 22 pages, 10 figures, the catalogs can be found at http://pole.uchicago.edu/public/data/sptplanck_cluster

This work of thesis aims to investigate the process of dark matter (DM) annihilation in galaxy clusters (CG). In particular, the search for DM signal was conducted in the Perseus CG in the very-high-energy (VHE) -ray range. Using data of the Perseus CG collected by MAGIC (Major Atmospheric Gamma Imaging Cherenkov Telescopes), we analyze 45.1 h of data. The morphology of the cluster is taken into account by ad-hoc simulations using a method known as donut Monte Carlo (MC). In order to address properly this study for the annihilation case, J-factors were calculated and a surface brightness profile (SBP) of Perseus was created for this specific work. The annihilating DM J-factor (smooth component only considering spherical halo) calculated in this work is 8:72 1017GeV2cm􀀀5 as well as the decaying DM D-factor with value of 2:84 1018GeVcm􀀀2 and are used for morphology study. An investigation of the skymaps and 2 plots of the analysed sample is used to suppress the signal from the AGN (Active Galactic Nuclei) present in the centre of the field of view, NGC 1275. The applied set of cuts successfully excludes NGC 1275 from the data sample. Future prospects include the calculation of the sensitivity of the search and the estimation of the dark matter annihilation crosssection for different channels.

As the most massive bound structures in the universe, galaxy clusters are a powerful probe of the impact of environment on galaxy evolution. In this work, I present AMASCFI, a new cluster finder algorithm using photometric redshifts I developed during the PhD and use the cluster catalogue obtained on the Canada France Hawaii Telescope Legacy Survey (CFHTLS) to investigate the role played by clusters and their environment on galaxy evolution. We show the good performances of AMASCFI on Euclid and the CFHTLS using mock data. In particular AMASCFI is 90% pure and 70% complete to z

As the most massive bound structures in the universe, galaxy clusters are a powerful probe of the impact of environment on galaxy evolution. In this work, I present AMASCFI, a new cluster finder algorithm using photometric redshifts I developed during the PhD and use the cluster catalogue obtained on the Canada France Hawaii Telescope Legacy Survey (CFHTLS) to investigate the role played by clusters and their environment on galaxy evolution. We show the good performances of AMASCFI on Euclid and the CFHTLS using mock data. In particular AMASCFI is 90% pure and 70% complete to z

Submitted by Emanuel Varela Cardoso (emanuel.varela@ufcg.edu.br) on 2018-10-18T17:24:51Z No. of bitstreams: 1 LEONARDO RIBEIRO COLAÇO – DISSERTAÇÃO (PPGFísica) 2016.pdf: 3372949 bytes, checksum: 8387f15d435a4dd929618ecca701927e (MD5) Made available in DSpace on 2018-10-18T17:24:51Z (GMT). No. of bitstreams: 1 LEONARDO RIBEIRO COLAÇO – DISSERTAÇÃO (PPGFísica) 2016.pdf: 3372949 bytes, checksum: 8387f15d435a4dd929618ecca701927e (MD5) Previous issue date: 2018 Capes As teorias cosmológicas mais comumente aceitas são baseadas no pressuposto de que as constantes fundamentais da natureza, como a constante gravitacional G, a constante de estrutura fina α, entre outras, são de fato constantes. Sendo assim, a suposição de que essas constantes não variam no espaço-tempo é apenas uma hipótese, precisando então ser comprovada a partir de dados experimentais. Neste trabalho, propomos um novo método, independente de modelo cosmológico, capaz de investigar uma possível variação como redshift da constante de estrutura fina, α=е2 /hc, onde é a carga elementar, h é a constante de Planck dividida por 2 π e c é a velocidade da luz. Para tal fim, mostramos também que a técnica combinada do Efeito Sunyaev-Zel'dovich (ESZ) como Brilho Superficial em raios-X (SX) para se medir Distância de Diâmetro Angular (DDA) dos Aglomerados de Galáxias (AG) é dependente da constante de estrutura fina. Mais precisamente,se = 0 (z), argumentamos que os dados atuais dessa técnica fornecem DobsA (z) = 2(z)DA(z), onde DA(z) é a verdadeira DDA para o aglomerado de galáxias e (z) é o campo escalar Dilaton que governa uma possível variação em α. Considerando uma amostra de 25 medidas de DobsA (z), feitas por De Filippis et al. (2005),via ESZ/SX na faixa de redshift 0; 023 < zAG < 0; 784 e estimando medidas de DA(z) do assim chamado Union 2.1 Compilation de Super nova e tipoIa (SNeIa), onde o redshift das SNeIa foram cuidadosamente selecionados para coincidir como redshift do aglomerado de galáxias associado com a maior diferença de redshift obedece a jzAG zSNej < 0; 005. Portanto, foi possível atribuir algumas restrições sobre uma possível variação de α para uma classe de Modelos Dilaton Run away, (z) =1 ln (1+ z). Nossas análises mostraram que = 0; 037 0; 157 em 1 , ou seja, nossas análises são compatíveis com uma não variação da constante de estrutura fina. The most common accepted cosmological theories are base don the assumption that the fundamental constants of nature, suchas the gravitational constant G, the new structure constant α, and others, are infact constant. Thus, the assumption that these constants do not vary with time or space is only a hypothesis, then it needs to be confirmed from experimental data. In this paper, we propose a new method, independent of cosmological models, which is cap able to investigate a possible variation with redshift of the new structure constant, α = e2=hc, where e is the elementary charge, h is Planck's constant over 2π and c is the speed of light. For that purpose, we also show that the combined technique between Sunyaev-Zel'doviche effect (SZE) and X-ray surface brightness (SX) to measure Angular Diameter Distance (ADD) of Galaxy Clusters (GC), dependents on the new structure constant. More precisely, if α = α0 (z) we argue that the current data of this technique gives DobsA (z) = 2(z)DA(z), where DA(z) is the true ADD for galaxy clustersand (z) is the dilatons calareld that governs a possible variation of α. We considere da sample of 25 measurements of Dobs A (z), made by De Filipp is e tal. (2005),via ESZ/SX in the range of redshift 0:023 < zGC < 0:784 and we also estimated DA(z) from the so-called Union 2.1 Super novaeIa(SNEIa) Compilation,where the SNeIa redshifts were carefully selected to match the one soft he as sociated galaxy cluster with the larger redshiftd iαe rencefollows jzGC � zSNej < 0:005. There for e,it was possible to put some constraints on a possible variation of α for a class of Dilaton Run a way Model, (z) =1 � ln (1+ z). We obtained = �0; 037 0; 157 in1 , i.e.,our analysis is compatible with an on variation of the new structure constant.

U okviru ove disertacije ce biti predstavljeni rezultati analize formiranja, rasprostranjenosti i evolucije patuljastih galaksija iz kosmoloških simulacija. Bice predstavljena prva kosmološka simulacija koja je u potpunosti izvedena i analizirana u Srbiji. Iz dobijenih rezultata je pokazano kako se formirala struktura na velikim skalama, pre svega kako se formiraju jata galaksija. Kako su jata galaksija dominantne strukture u svemiru, koje se relativno sporo formiraju u odnosu na postojanje svemira, korišcenjem Ilustris simulacije, u kojoj je ukljucena kompletna fizika, bice pokazano da znacajan deo jata galaksija nije u stanju dinamicke ravnoteže, kako neki autori tvrde, odnosno da su u procesu formiranja i danas. Dobijeni rezultati ce biti iskorišceni da se jata galaksija podele na tri tipa: jata u interakciji, jata koja interaguju sa manjim grupama (slabo interagujuca jata) i jata galaksija koja nisu u interakciji. Kako patuljaste galaksije po svom broju cine najveci broj galaksija u svemiru, a pogotovu u jatima, ovo postavlja pitanje kako trenutni procesi u kojima se jato nalazi uticu na strukturu i rasprostranjenost razlicitog tipa patuljastih galaksija. Nakon kratkog pregleda danas poznatih tipova patuljastih galaksija, pokazacemo da postoji osetljivost rasprostranjenosti patuljastih nepravilnih galaksija u odnosu na to da li je maticno jato galaksija u interakciji ili ne. Kako se pretpostavlja da su patuljaste nepravilne galaksije prethodnici za formiranje najbrojnijih tipova patuljastih galaksija, ovo bi moglo da ukaže na dominantan kanal dopremanja tih galaksija u jata galaksija gde se ocekuje da dožive morfološku transformaciju. Na kraju ce biti predstavljeno otkrice dva kanala formiranja za kompaktne elipticne galaksije u jatima galaksija... Within this dissertation results from the analysis of formation, abundance and evolution of the dwarf galaxies from cosmological simulations will be presented. We will present results from first cosmological simulation which was performed and analyzed in its entirety in Serbia. From the obtained results it was shown how the large scale structure formed, primarily the formation of clusters of galaxies. Since the clusters of galaxies are dominant structures in the universe, which are relatively slowly forming in relation to the existence of the universe, using the Illustris cosmological simulation, with included hydrodynamics, it will be shown that a significant part of the clusters of galaxies are not in the state of dynamic equilibrium, as some authors claim, therefore their formation process continues. The obtained results will be used to divide the clusters of galaxies into three types: interacting clusters, clusters interacting with smaller groups (weakly interacting clusters), and clusters of galaxies that are not interacting. As the dwarf galaxies constitute largest number of galaxies in the universe, notably largest number in the clusters of galaxies, this raises the question how cluster’s interactions affect the structure and abundance of a diverse type of dwarf galaxies within them. After a brief review of today’s known types of dwarf galaxies, we will show that there is susceptibility of the abundance of dwarf irregular galaxies in relation to whether the parent cluster of galaxies is in interaction or not. As it is assumed that the dwarf irregular galaxies are predecessors for the formation of the most numerous types of dwarf galaxies, this could point to the dominant channel of delivering these galaxies to clusters of galaxies where they are expected to undergo morphological transformation. In the end, the discovery of two formation channels for compact elliptical galaxies in the clusters of galaxies will be presented...

In this introductory talk, I place clusters and protoclusters, and their evolution, in the general context of the cosmic web formation. I also give an overview of the technics used to find clusters and their progenitors, and of the coverage of the redshift-mass plane achieved with current samples. I summarize the open questions that can be addressed from local merging cluster observations, statistical studies of the dynamical state of the cluster population, the cluster outskirts and protoclusters., This work was supported by the European Research Council under the European Union's Seventh Framework Pro- gramme (FP7/2007-2013) / ERC grant agreement number 340519.

Clusters of galaxies are large and massive structures containing more than 80% of dark matter. In the cluster core, the mass density can reach a critical threshold making the curvature of space-time large enough to bend light path and then allow multiple convergence of images from the same sources to appear on the observer field of view. Thanks to deep photometric coverage of Abell 2744, a lot of multiply-imaged systems were discovered. Nevertheless, finding them remain a challenge and based on the preserved photometric properties by lensing, I developed a robust method to automatically find them. However, measuring the redshifts for each multiple images remains the best way to surely associate them. The deep coverage of the integral field spectrograph MUSE allowed me to identify a large number of sources ( 514 ) among them 83 were multiple images. Thanks to this large spectroscopic coverage, I built one of the most constrained parametric mass model for lensing cluster to date. The sensitivity raised by this model allow me to probe the influence of outskirts substructures ( at 700 kpc distance ), revealing systematic sources of uncertainties related to the mass model parametrisation ( 6% ). Compared to previous studies, I notice a 10% lower mass in the center ( within 100kpc ) showing one of the benefit of large spectroscopic constraints. This benefit, is smaller on the amplification estimation but shows a significant discrepancy between different mass counterparts in the models, up to 2 times the statistical uncertainties, Les amas de galaxies sont des structures massives composées à plus de 80% de matière noire. Leur coeur peut atteindre une densité de masse critique qui en déformant l'espace-temps fait converger les rayons lumineux vers l'observateur. Grâce à des relevés photométriques profonds de l'amas Abell 2744, de nombreux systèmes multiples ont été découverts. Identifier ces systèmes reste un défi, j'ai donc développé une méthode robuste basée sur les propriétés photométriques conservées par l'effet de lentille gravitationnelle qui permet de les détecter automatiquement. Le meilleur moyen de prouver que des images proviennent de la même galaxie reste la mesure de leur distance(redshifts) grâce à leur spectre. En analysant les données collectées par le spectrographe à intégrale de champ MUSE j'ai mesuré un grand nombre de sources (514) dont 83 d'entre elles sont des images multiples. Bénéficiant de cette large couverture spectrale, j'ai créé un modèle paramétrique de masse parmi les plus contraints à ce jour. La sensibilité atteinte par le modèle permet de sonder l'influence de structures périphériques (jusqu'à une distance de 700kpc), révélant ainsi des erreurs systématiques sur la mesure de la masse due à la paramétrisation du modèle (6%). Comparé aux précédentes études, on voit une diminution de 10% de la masse dans un rayon 100 kpc montrant ainsi en partie le gain offert par la spectroscopie. Ce gain, bien que négligeable sur la mesure de l'amplification, s'est avéré pouvoir contraindre la balance en masse entre les différentes composantes de notre modèle, dépassant par endroits 2 fois l'incertitude statistique

We have constrained the spatial variation of the fine structure constant using multi-frequency measurements of the thermal Sunyaev-Zeldovich effect of 618 X-ray selected clusters. Although our results are not competitive with the ones from quasar absorption lines, we improved by a factor 10 and ~2.5 previous results from Cosmic Microwave Background power spectrum and from galaxy clusters, respectively., 10 pages, 1 figures, based on arXiv:1605.03053 and on the oral presentation at VARCOSMOFUN16, accepted for publication in "Universe", Special Issue "Varying Constants and Fundamental Cosmology" for the VARCOSMOFUN16 in Szczecin, Poland, 12-17 September, 2016

Whether the formation of bars is triggered by interactions or by internal processes has been discussed for many decades. In this work, we study differences between both mechanisms by means of numerical simulations. We relate our analysis to fly-by interactions in different mass groups or clusters according to the velocity of the encounters. We find that once the bar is created, the interaction does not much affect its evolution. We also find that bars can be triggered purely by a slow interaction. Those bars affected or triggered by interaction stay for a longer time in the slow regime, i.e., the corotation radius is more than 1.4 times the bar radius., We acknowledge support by the CSIC Open Access Publication Initiative through its Unit of Information Resources for Research (URICI)., Inma Martinez-Valpuesta thanks support from the MINECO through grants AYA2013-46886-P and AYA2014-583308-P

A new type of β model of intracluster gas distribution is established, which is well fitted to the observed X-ray surface brightness profile except for outermost region. It employs the exact King model of the self-gravitating system of collisionless particles instead of the widely used approximated analytical formula for the dark matter distribution. The small difference between the modelled and the observed X-ray surface brightness profiles would disappear if the infall of matter from the intercluster space is taken into account. The number of parameters of our model is the same as for the isothermal β model, but the agreement between our model and data points is satisfactory even when the fitting with the isothermal β model remaines a large central excess. In addition, the enhanced central mass concentration in our model is high enough to resolve the discrepancy between the X-ray and the lensing measurements of cluster mass. These facts suggest that most of the central excess might be no more than a ghost embossed by an inadequate fitting. Therefore the central excess would not necessarily be linked to the existence of cooling flow. It is also shown that the obtained values of β(our model)∼0.5support the theory of non-gravitational intracluster gas heatings comparable to those reached through gravitational collapse. On the other hand, the value of β∼0.6obtained for the isothermal β model is explained as showing the scarcity of matter in the space surrounding each cluster, brobably due to the infall of matter towards it over a long time.

A microscopic origin of dark matter phenomenon is the most plausible hypothesis to explain the mystery of dark matter. The dark matter particle hypothesis necessarily implies an extension of the Standard Model. In this thesis, we undertook a systematic model-independent program of studying the properties of decaying dark matter. By analyzing the experimental data for dwarf spheroidal galaxies it was shown that the X-ray energy range is a preferred region when searching for radiatively decaying dark matter. By analyzing dark matter distributions in different types of galaxies and in galaxy clusters we show that the expected dark matter signal increases slowly with the mass of the object. Therefore, dwarf and spiral galaxies are the observational targets with the optimal signal-to-noise ratio. To probe the theoretically interesting regions of particle physics models we performed a combined analysis of a very large dataset of archival XMM-Newton observations of galaxies. Finally, we discussed an ultimate way to probe the whole parameter space of minimal models of decaying dark matter. We argue that a new X-ray telescope with the narrow energy resolution (comparable to internal width of the line) and large field-of-view is required.

This thesis investigates the influence of ram pressure stripping on the star formation history of cluster spiral galaxies. Ram pressure stripping is the hydrodynamical interaction between the interstellar medium (ISM) of a spiral galaxy that is moving inside the potential well of a cluster, and the intracluster medium (ICM). If the dynamical pressure exerted by the ICM is larger than the restoring force due to the galactic potential, the galaxy loses gas from the outer disk. The Virgo cluster is an ideal laboratory to study environmental effects on galaxy evolution, because it is rich in spirals and dynamically young. From observations we know that the amount of atomic gas in Virgo spirals is less than that of galaxies in the field. In particular cluster spirals show truncated HI disks. For those galaxies that also show a symmetrical stellar distribution, ram pressure stripping is the most probably origin of the gas-disk truncation., Cette these etudie l'influence du balayage par pression dynamique sur l'histoire de la formation stellaire des galaxies spirales qui se trouvent dans des amas. Le balayage par pression dynamique est l'interaction hydrodynamique entre le milieu interstellaire (ISM) d'une galaxie spirale qui evolue dans le puits de potentiel d'un amas, et le milieu intra-amas (ICM). Si la pression dynamique exercee par l'ICM excede la force d'attraction gravitationnelle due au potentiel galactique, la galaxie perd du gaz de sa partie externe. L'amas de la Vierge constitue un laboratoire ideal pour etudier les effets de l'environnement sur l'evolution des galaxies. En effet, cet amas est riche en spirales et dynamiquement jeune. Des observations nous montrent que la quantite de gaz atomique qui se trouve dans les spirales de la Vierge est moins importante que celle des galaxies du champ. En particulier, les spirales des amas presentent des disques HI tronques. Pour celles des galaxies qui presentent aussi une distribution stellaire symetrique, le balayage par pression dynamique semblerait etre l'origine la plus probable de la troncature du gaz du disque.

Interstellar dust, infrared emission from galaxies and measurements of the CMB, De la Poussière Interstellaire, de l'Emission Infrarouge des Galaxies, et des Mesures du rayonnement cosmologique à 3K

We introduce the concept of chemical mass of a galaxy, which is the total mass of stars which have participated to the astration process. This concept is used in chemical evolution models for irregular galaxies, spiral galaxies and cluster of galaxies. In irregular galaxies, we found a good agreement between the luminous and the chemical mass. At the opposite, in cluster of galaxies, we found a good agreement between chemical mass and virial mass. Implications for the cluster of galaxies evolution are presented.