skip to content

Guiderdoni, B. (Bruno)

Overview
Works: 24 works in 47 publications in 4 languages and 295 library holdings
Genres: Conference papers and proceedings 
Roles: Editor, Author, Interviewee, Thesis advisor, Opponent, 958, 956, Other
Classifications: QB806.5, 523.019
Publication Timeline
Key
Publications about B Guiderdoni
Publications by B Guiderdoni
Most widely held works by B Guiderdoni
Starbursts : triggers, nature, and evolution : Les Houches School, September 17-27, 1996 by Haute-Savoie, France) Ecole d'été de physique théorique (Les Houches( Book )
8 editions published in 1998 in English and held by 130 libraries worldwide
Starbursts are regions of unusually rapid star formation, often located in the central parts of galaxies. They differ from more normal regions of star formation in terms of the throughput of mass and the rapidity with which the gas is consumed. In the last twenty years, extensive observational data at most wavelengths have become available on starbursts, but many important issues remain to be addressed, observationally as well as theoretically. How are strong episodes of star formation triggered? What is the quantity of gas converted into stars during bursts? What is the initial mass function of stars in these events? How does the feedback from stars influence the interstellar medium and self-regulate star formation? What is the subsequent chemical and photometric evolution? How do starbursts rule the formation and evolution of galaxies? In recent years, many observational data at different wavelengths (optical, radio, infrared, X-ray) have become available. However, these observations are still fragmentary in the sense that different classes of objects have been observed in different ways, and the coverage is not consistently deep or complete. As a consequence, an overall observational picture of starburst galaxies is missing, and theoretical understanding and modelling have remained highly tentative. The purpose of the school Starbursts: Triggers, Nature, and Evolution was to gather theorists and observers with complementary approaches to the starburst phenomenon, in order to summarize the state-of-the-art of the observations and models, emphasizing the consistency of the various viewpoints
Dark matter in cosmology : clocks and tests of fundamental laws : proceedings of the XXXth Rencontre de Moriond, Villars sur Ollon, Switzerland, January 22-29, 1995 by Rencontre de Moriond( Book )
9 editions published in 1995 in English and French and held by 76 libraries worldwide
L'homme entre science et religion by Caroline Puig-Grenetier( visu )
2 editions published between 2007 and 2008 in French and held by 8 libraries worldwide
Extrait du résumé figurant sur la jaquette : Depuis la nuit des temps, l'Homme s'interroge sur l'origine de ce monde qui l'entoure et qui l'a engendré. Pendant de longs siècles les scientifiques attribuaient l'origine du monde à une succession de hasards, alors que les chrétiens voyaient en Dieu leur créateur et décideur unique. Aujourd'hui la science et la religion, loin du débat polémique des certitudes, entament un dialogue intelligent, où chacun apporte son regard, ses questions, ses hypothèses, ses convictions ... Six scientifiques, théologiens, chercheurs de sens, croyant avant tout à un ordre possible de l'univers, témoignent
Evolution photometrique des galaxies : evolution des spirales d'amas, previsions pour les galaxies lointaines by B Guiderdoni( Book )
3 editions published in 1986 in French and held by 6 libraries worldwide
LA PREMIERE PARTIE CONCERNE L'EVOLUTION DES GALAXIES SPIRALES DANS LES AMAS. LES PROPRIETES STATISTIQUES DE 107 SPIRALES DE VIRGO, DEDUITES DE LEUR CONTENU EN GAZ ET DE LEUR PHOTOMETRIE, REVELENT UNE CORRELATION ENTRE UNE FORTE DEFICIENCE EN GAZ NEUTRE ET LES TYPES MORPHOLOGIQUES LES PLUS EVOLUES. ON PROPOSE UN SCENARIO POUR L'EVOLUTION DES SPIRALES D'AMAS. LA SECONDE PARTIE TRAITE DE L'EVOLUTION PHOTOMETRIQUE DES GALAXIES LOINTAINES. ON PRESENTE UN MODELE NUMERIQUE POUR L'EVOLUTION SPECTROPHOTOMETRIQUE PERMETTANT D'OBTENIR LES MAGNITUDES ET LES COULEURS POUR TOUT DECALAGE SPECTRAL, EN TENANT COMPTE DE L'EVOLUTION INTERNE ET DE LA COSMOLOGIE
Proceedings of the XXXth Rencontre de Moriond by Rencontre de Moriond( Book )
2 editions published in 1995 in English and held by 5 libraries worldwide
Proceedings of the XXXIst Rencontres de Moriond by Rencontre de Moriond( Book )
in English and held by 3 libraries worldwide
Membaca alam membaca ayat by B Guiderdoni( Book )
1 edition published in 2004 in Indonesian and held by 3 libraries worldwide
Dark matter in cosmology, clock and tests of fundamental laws by Rencontres de Moriond( Book )
1 edition published in 1996 in English and held by 3 libraries worldwide
The interplay between massive star formation, the ISM and galaxy evolution : proceedings of the 11th IAP Astrophysics Meeting, July 3-8, 1995, Institut d'Astrophysique de Paris by Institut D'Astrophysique Astrophysics Meeting( Book )
1 edition published in 1996 in English and held by 2 libraries worldwide
Formation et évolution des galaxies à grand décalage spectral développement de l'approche hybride by Jérémy Blaizot( Book )
2 editions published between 2003 and 2007 in French and held by 2 libraries worldwide
This thesis presents a model of galaxy formation in which the formation of dark matter structures is described with cosmological N-body simulations and the fate of baryons is treated in a semi-analytic fashion. We show how mock observations can be made in order to directly confront the model's predictions with observations. This method is then applied to a detailed study of high-refshift Lyman break galaxies, and used to investigate the nature of the galaxy spatial distribution in the local universe
Une vision panchromatique de la formation hierarchique des galaxies by JULIEN DEVRIENDT( Book )
1 edition published in 1999 in French and held by 2 libraries worldwide
CETTE THESE PRESENTE UNE PREMIERE TENTATIVE POUR DEVELOPPER UNE VISION PANCHROMATIQUE COHERENTE DE L'UNIVERS, DE L'ULTRAVIOLET LOINTAIN AU SUB-MILLIMETRIQUE. LE MODELE REPOSE SUR LE CADRE COSMOLOGIQUE EXPLICITE DES SCENARIOS DE FORMATION HIERARCHIQUE DES GALAXIES. LA CROISSANCE HIERARCHIQUE DES STRUCTURES A PARTIR DE FLUCTUATIONS PRIMORDIALES, EST GOUVERNEE PAR LES INSTABILITES GRAVITATIONNELLES DE LA MATIERE SOMBRE FROIDE, QUI DOMINE LA DENSITE DE L'UNIVERS EN EXPANSION. DU GAZ BARYONIQUE REFROIDIT RADIATIVEMENT AU CUR DES HALOS DE MATIERE SOMBRE VIRIALISES, FORME UN DISQUE, ET ENGENDRE DES ETOILES : UNE GALAXIE EST NEE. LES ETOILES MASSIVES EXPLOSENT DANS LES GALAXIES, ET ENRICHISSENT LE MILIEU INTERSTELLAIRE EN ELEMENTS LOURDS. EN RESULTE L'EJECTION D'UNE PARTIE DU CONTENU GAZEUX DES GALAXIES DANS LE MILIEU INTERGALACTIQUE ET LA FORMATION DE GRAINS DE POUSSIERE. POUR SONDER LES DIVERSES ETAPES PAR LESQUELLES PASSENT LES GALAXIES DANS UN TEL PARADIGME, IL FAUT DONC MODELISER TOUS CES PROCESSUS COMPLEXES QUI LES FONT EVOLUER, EN RESPECTANT LEUR BUDGET ENERGETIQUE LUMINEUX. UNE APPROCHE SEMI-ANALYTIQUE EST ICI PROPOSEE, COUPLEE A DES MODELES SYNTHETIQUES DE POPULATIONS STELLAIRES ET D'EVOLUTION CHIMIQUE. L'ABSORPTION DE LA LUMIERE DES ETOILES PAR LES GRAINS DE POUSSIERE AINSI QUE SA RE-EMISSION SONT EGALEMENT PRISES EN COMPTE. NOUS UTILISONS ENSUITE NOTRE NOUVELLE APPROCHE POUR ECLAIRER DEUX PROBLEMES COSMOLOGIQUES CAPITAUX, A SAVOIR LA RE-IONISATION DE L'UNIVERS A GRAND DECALAGE SPECTRAL, ET LES COMPTAGES PANCHROMATIQUES DE GALAXIES FAIBLES. FINALEMENT, NOUS EXPLORONS UNE NOUVELLE METHODE, QUI TIRE PARTIE DES CAPACITES PRESENTES DES SUPER-ORDINATEURS A EFFECTUER DES SIMULATIONS N-CORPS A HAUTE RESOLUTION, POUR RAFFINER CERTAINS ASPECTS DE NOTRE MODELISATION, ET PLUS PARTICULIEREMENT LA FUSION DES GALAXIES A L'INTERIEUR DE LEURS HALOS HOTES
The birth of galaxies : proceedings of the Xth rendontres de Blois, Blois June 28 - July 4, 1998 by Rencontres de Blois( Book )
2 editions published between 1998 and 2001 in English and held by 1 library worldwide
Los cazadores de galaxias primordiales by B Guiderdoni( Article )
1 edition published in 1999 in Spanish and held by 1 library worldwide
Compter les galaxies infrarouges, raconter leur histoire : propriétés statistiques des galaxies infrarouges à grand redshift et origine du fond extragalactique infrarouge by Matthieu Bethermin( file )
1 edition published in 2011 in French and held by 1 library worldwide
The extragalactic background light is the relic emission of the process of structure formation in the Universe. About half of this background, called cosmic infrared background, is emitted in the 8-1000 microns interval, peaks near 150 microns, and is essentially due to the star formation processes in the Universe. In fact, the infrared luminosity of a galaxy is linked to the hosted star formation. It is thus necessary to determine the evolution of infrared galaxies to well understand the origin of the cosmic infrared background.A rather simple statistical measurement, enabling to understand the origin of the cosmic infrared background, but also the evolution of the galaxies, consist in counting the sources as a function of their flux. I measured number counts of infrared galaxies using different methods in the data of the Spitzer and Herschel space telescopes, and of the BLAST experiment. The individually detected sources in the 24 microns Spitzer maps are responsible of the main part of the background. But, at larger wavelength, the sensitivity and the angular resolution of the instruments decreases, and the detected sources explain only a small part of the background. The stacking analysis enable to measure the mean far-infrared or sub-millimeter flux of a population detected only in the mid-infrared. This technique provides stringent lower limits on the level of the background, but also enables to count the sources which are too faint to be detected individually. These results are confirmed by the P(D) analysis, which determines the counts from the histogram of the infrared maps.These new measurements constrain the evolution of the infrared galaxies. I built a parametric evolution model to interpret the source counts. This model well reproduces the statistical properties of the infrared galaxies between 15 and 1100 microns. It predicts that the star formation in the young Universe (z>2) mainly happen in ultra-luminous infrared galaxies (LIR> 10^12 Lsun). These galaxies formed stars very quickly (more than 100 Msun/years), and have few equivalents in the local Universe. Nowadays, the star formation rate has decreased by a factor of ten, and the star formation mainly happen in galaxies like ours. This model has been used to interpret the fluctuations of the cosmic infrared background at large wavelength observed by BLAST, Planck, and Herschel
Modélisation de l'émission Lyman-alpha dans les galaxies à grand décalage spectral et simulations cosmologiques by Thibault Garel( file )
1 edition published in 2011 in French and held by 1 library worldwide
Many galaxies have been detected at high redshift since the late nineties thanks to their strong Lyman-alpha emission line. These objects, knows as Lyman-alpha Emitters, allow us to probe galaxies in the first two Gigayears of the Universe. Although a large amount of detections, their statistical and physical properties are still poorly constrained. Indeed, observations are difficult to interpret, mainly due to line transfer effects in the interstellar mediaum and gas kinematics."In addition to observations, theoretical efforts are needed to reach a better understanding of the properties of these objects, their role in the scenario of hierarchical formation of galaxies, and their link with the other main high redshift galaxy population, the so-called Lyman Break galaxies. In this thesis, we model Lyman-alpha Emitters in the cosmological context with an original method."The hierarchical galaxy formation process is described with the GALICS model, which couples a N body simulation of Dark Matter, with semi-analytic prescriptions to model galaxy physics. GALICS can predict the physical properties of a large sample of mock galaxies between z~3 and 7. Lyman-alpha properties are computed thanks to the coupling of GALICS with a library of numerical tranfser models, generated with the MCLya code. With this approach, Lyman-alpha photons escape fractions and line profiles can be predicted, taking into account resonnant scattering effects and gas kinematics. We find a strong dispersion of the escape fraction with respect to the star formation rate of the galaxies. The model predictions are in good agreement with most of the observationnal data, especially the Lyman-alpha luminosity functions between z~3 and 7. The model is able to reproduce UV properties of UV and Lyman-alpha selected galaxies. We find that Lyman-alpha Emitters have moderate mass on average and display asymetric line profiles, as it is shown by the observations. In particular, we predict a strong abundance of faint Lyman-alpha Emitters. These objects will be a main target of the forthcoming MUSE instrument that will be installed at VLT. In order to help preparing future surveys with MUSE, mock fields of Lyman-alpha Emitters have been created with our model to make predictions, especially in terms of number counts and cosmic variance
Formation & Evolution of early-types galaxies : Numerical simulations of galaxy mergers by Maxime Bois( file )
1 edition published in 2011 in French and held by 1 library worldwide
A simple morphological classification of the galaxies in the local Universe shows two main families: (1) the disc galaxies, with spiral arms and in two-thirds of these galaxies a stellar bar; and (2) the elliptical and lenticular galaxies, labelled early-type galaxies (ETGs), which are dominated by a spheroidal stellar component. ETGs are among the most massive galaxies of the local Universe and present a red color, meaning that their stars are old. These galaxies also present a large diversity of stellar dynamics: they may have a regular rotation pattern aligned with the photometry or perpendicular to it; they can present no global rotation at all; or may hold a central stellar component with a rotation axis distinct from the outer stellar body called a Kinematically Distinct Core (KDC). These features observed in the dynamics of the ETGs and their large mass are clearly signs of past interactions, especially signs of galaxy mergers. The main goal of my thesis is to analyse a large sample of high-resolution numerical simulations of binary galaxy mergers. These binary mergers are called "idealized" because they do not take into account the full cosmological context of galaxy formation: two isolated spiral galaxies are launched in an orbit resulting in a merger of the galaxies, the final remnant is an ETG. The statistical analysis of this large sample of simulations enables us to link the initial conditions of the merger to the final merger remnant. I demonstrated that the mass ratio between the spiral progenitors and the orientation of their spins of angular momentum are the main drivers for the formation of fast and slow rotating ETGs and the KDCs. The morphology of the initial spiral (Bulge/Disc ratio) seems also to play a major role for the formation of the different types of ETGs but its impact is not completelly clear, and other simulations are planned to clarify this problem. During my thesis, I also studied the importance of the resolution in the numerical simulations of galaxy mergers. I showed that the number of particles and the size of the computational grid have a predominant role in the final product of the merger. A too low resolution (i.e. too few particles and a coarse grid) can not follow the rapid evolution of the gravitational potential during the merger. In this case, the angular momentum is not as efficiently transfered to the outer parts of the galaxy: the merger remnant keeps thus a strong and regular rotation. At higher resolution, the scattering of the orbit is resolved and the merger remnant may end-up with, under some special initial conditions, a slow rotation and may form a KDC
Cosmological RHD simulations of early galaxy formation by Karl Joakim Rosdahl( file )
1 edition published in 2012 in English and held by 1 library worldwide
With the increasing sophistication and efficiency of cosmological hydrodynamics codes, ithas become viable to include ionizing radiative transfer (RT) in cosmological simulations,either in post-processing or in full-blown radiation-hydrodynamics (RHD) simulations. Inspite of the many hurdles involved, there has been much activity during the last decade or soon different strategies and implementations, because a number of interesting problems canbe addressed with RT and RHD, e.g. how and when the Universe became reionized, howradiation from stars and active galactic nuclei plays a part in regulating structure formationon small and large scales, and what predictions and interpretations we can make of observedphenomena such as the Lyman-alpha forest and diffuse sources of radiation.This coincides with the advent of the James Webb space telescope (JWST) and otherstate-of-the-art instruments which are about to give us an unprecedented glimpse into theend of the dark ages of the Universe, when the cosmos switched from a cold and neutralstate to a hot and ionized one, due to the turn-on of ionizing radiative sources.With a primary interest in the problem of radiative feedback in early structure formation,we have implemented an RHD version of the Ramses cosmological code we call RamsesRT,which is moment based and employs the local M1 Eddington tensor closure. This code allowsus to study the effects of ionizing radiation on-the-fly in cosmological RHD simulationsthat take full advantage of the adaptive mesh refinement and parallelization strategies ofRamses. For self-consistent RHD we have also implemented a non-equilibrium chemistry ofthe atomic hydrogen and helium species that interact with the transported radiation.I present in this thesis an extensive description of the RamsesRT implementation andnumerous tests to validate it.Thus far we have used the RHD implementation to study extended line emission fromaccretion streams, which are routinely predicted to exist at early redshift by cosmologicalsimulations but have never been unambiguously verified by observations, and to investigatewhether gravitational heating in those streams could be the dominant power source ofso-called Lyman-alpha blobs, an observed phenomenon which has been much studied anddebated during the last decade or two. Our conclusions from this investigation are thatLyman-alpha blobs can in principle be powered by gravitational heating, and furthermorethat accretion streams are on the verge of being directly detectable for the first time withupcoming instruments.My future intent is to use RamsesRT for high-resolution cosmological zoom simulations ofearly galaxy formation, up to the epoch of reionization, to study how radiative feedbackaffects the formation and evolution of those galaxies and to make observational predictionsthat can be tested with upcoming instruments such as the JWST
Predictabilité, galaxies infrarouges et lentilles gravitationnelles applications de l'approche hybride by Jaime Ernesto Forero Romero( Book )
1 edition published in 2007 in English and held by 1 library worldwide
Formation & Evolution des galaxies par l'approche semi-analytique by Morgane Cousin( file )
1 edition published in 2013 in French and held by 1 library worldwide
Semi-analytical models (SAMs) are currently the best way to understand the formation of galaxies and clusters within the cosmic web dark-matter structures. While they fairly well reproduce the local stellar mass function, correlation function and luminosity function, they fail to match observations at high redshift (z>3) in most cases, particularly in the low-mass range. The inconsistency between models and observations indicates that the history of gas accretion in galaxies, within their host dark-matter halo, and the transformation of gas into stars, is not well followed. In this thesis, we introduce a new version of the GalICS model and we use it to explore the impact, on the star formation and in the low-mass range, of supernovae feedback and photo-ionization. These two mechanisms are commonly used to limit the amount of gas available to form stars.We will show that, even with a strong efficiency, these two process cannot explain the observed stellar mass function, luminosity functions, and the stellar mass versus dark matter halo mass relation. We will thus introduce two ad-hoc modifications of the standard paradigm. We propose first a strong modification of the star formation efficiency as a function of the dark matter halo mass. This model produces good results, especially on the faint end of the stellar mass function, but is, by construction, in disagreement with the well known Kennicutt star formation law. We will thus introduce a deeper change, based on a no star-forming gas component, and a new gas distribution in the galaxy discs. The reservoir in which stays the no star-forming gas generates a delay between the gas accretion and star formation. This model is in very good agreement with a large set of observations. However, it poses the question of the origin of the no star-forming gas. We will discuss its origin in the framework of the large scale disturbed dynamic of high-redshift structures
Building Galaxies : From the Primordial Universe to the Present by Fran?ois Hammer( file )
1 edition published in 2000 in English and held by 0 libraries worldwide
 
moreShow More Titles
fewerShow Fewer Titles
Alternative Names
Guiderdoni, B.
Guiderdoni, Bruno
Languages
English (26)
French (13)
Indonesian (1)
Spanish (1)
Covers
Close Window

Please sign in to WorldCat 

Don't have an account? You can easily create a free account.