Rozprawy doktorskie na temat „Galaxies”

La distribution et l'abondance du gaz atomique et moleculaire dans les galaxies permettent l'etude de leur histoire et de la formation stellaire. Nous nous sommes interesses a la galaxie spirale messier 81, qui est consideree comme un prototype ideal pour tester la theorie des ondes de densite. Nous avons decouvert la presence d'une emission co dans m81 et une cartographie etendue a revele une deficience moleculaire au centre ainsi qu'une distribution annulaire. Des observations a plus haute resolution spatiale nous ont aussi permis de comparer les distributions relatives du co et d'autres traceurs de bras spiraux. M81 etant le membre principal d'un groupe de galaxies nous avons etudie son interaction gravitationnelle avec ses 2 plus proches compagnons et nous avons cherche a simuler les distributions observees du gaz interstellaire

Grace au satellite iras, on a decouvert un type de galaxies dont le rapport luminosite infrarouge sur bleue peut atteindre 100 ou plus; ces galaxies qu'on suppose subir des flambees de formation d'etoile sont l'objet de cette these. Un modele photometrique simple a ete construit pour rendre compte des proprietes ir lointain et optique de ces galaxies a flambees. La photometrie ccd d'un certain echantillon de galaxies iras a ete realisee pour tester le modele: l'accord modele-observation est satisfaisant et la force, ainsi que l'extinction des flambees ont pu etre estimees

In this thesis, we employ two numerical tools - semi- analytical models and N-body plus hydrodynamical simulations of large scale structure and individual galaxies - to explore the underlying physics governing the formation and evolution of groups of galaxies, and the role of environment in generating polar structures around disk galaxies. Using phenomenological models of baryonic physics imposed upon large-scale dissipationless simulations of the Universe, semi-analytic models (SAMs) are one of the principal methods used to model large samples of model galaxies. We sought to examine the properties of groups of galaxies with a range of densities using SAMs applied specifically to the industry-standard Millennium Run; for this work, we make use of the well-known Munich and Durham models, and their descendants. We are especially interested in how group properties change as we change the linking length of our Friends- of-Friends group finder. We compare the group populations and richness in these models and compare them both with observations and high-resolution N- body simulations. This leads us to the conclusion that the Durham models produce a much larger population of compact objects than the Munich models. We also explore the group dynamics and morphology as a function of density. We compare the luminosity distributions of galaxy groups using publicly available SAMs in order to explore

L’évolution de la luminosité infrarouge et de l’UV peut s’expliquer par une chute de la formation stellaire entre les décalages spectraux de 0. 4 à 1, c’est-à-dire depuis 7 à 10 milliards d’années. Cette chute est due à deux types de galaxies : les galaxies infrarouges et les galaxies compactes lumineuses. Au cours de cette thèse, j’ai particulièrement étudié un échantillon de spectres de ces galaxies compactes observées au VLT. Ces objets sont très importants : il y a environ 7 milliards d’années ces galaxies représentaient la population dominante. De plus, malgré leur petite taille, elles rayonnent de l’ordre de 100 fois plus d’énergie que les galaxies locales irrégulières auxquelles les études précédentes les ont assimilées du fait de leurs caractéristiques photométriques et dynamiques semblables. Pour quelques objets, il existe des images prises par le télescope spatial, elles montrent que la plupart de ces galaxies sont en interaction ou du moins possèdent une seconde composante à moins de 10 kpc. L’ensemble des indices réunis que ces objets pourraient être non pas les progéniteurs des galaxies naines compactes locales mais ceux des galaxies spirales
The evolution of the luminosity function in UV is related to the increase in the global star formation rate density up to z ~ 1. This increase is mainly due to two differents types of galaxies : the luminous infrared galaxies (LIRGs) and the luminous compacts galaxies (LCGs). In this thesis, I study a representative sample of LCGs using VLT and HST data at redshift 0. 4-0. 9. About 7 Giga years ago, these galaxies were the dominant galaxy population in number density. Despite their relative small size, they radiate near 100 times more energy than the population of star-forming Blue Compact Galaxies. Spectroscopic analysis show LCGs are composed of a mixed stellar populations, which includes at least : a young burst (less than 10 8 years) superimposed to an older population (more than 1 Giga year). HST images reveal these galaxies are often in interaction or have a multiple component at less than 10 kpc. Our study suggest that these objects may be the progenitors of today’s population of spirals galaxies

L'étude cinématique des galaxies locales et lointaines permet de contraindre les scénarios de formation et d'évolution des galaxies. Pour cela, la spectroscopie à champ intégral permet une étude détaillée de la cinématique des galaxies proches et fournit depuis peu des indices sur la cinématique des galaxies lointaines. Cette thèse s'appuie principalement sur l'utilisation de l'échantillon cinématique de galaxies locales GHASP. Cet échantillon de référence composé de 203 galaxies spirales et irrégulières de l'Univers local dans des environnements peu denses observées par interférométrie de Fabry-Perot autour de la raie Hα (6563 Å) est le plus grand échantillon de données Fabry-Perot à ce jour. Après un passage en revue des principes de l'interférométrie Fabry-Perot et des nouveautés apportées à la réduction des données Fabry-Perot, mon implication dans le développement du 3D-NTT, nouvel instrument utilisant deux Fabry-Perot est exposée de même que ma participation au projet de spectrographe à grand champ pour les ELT, WFSpec, dont l'objectif est l'étude de l'évolution des galaxies. Je présente dans une deuxième partie les données GHASP. Cet échantillon a été entièrement réduit et analysé à l'aide de nouvelles méthodes. L'analyse cinématique de l'échantillon à partir des cartes cinématiques 2D a été initiée en particulier avec l'étude de la distribution des halos de matière sombre, de la forme des courbes de rotation, de l'influence des potentiels barrés et de la dispersion de vitesses du gaz ionisé. Dans une troisième partie, cet échantillon local sert de point de référence pour l'étude de la cinématique des galaxies lointaines. L'échantillon GHASP est projeté à grand décalage spectral (z = 1.7) afin de déterminer les biais observationnels liés au manque de résolution spatiale des données cinématiques de galaxies lointaines obtenues par SINFONI, OSIRIS et GIRAFFE. L'analyse cinématique de nouvelles observations SINFONI y est également présentée, et l'ensemble des données cinématiques 2D de la littérature est mis en regard avec les résultats obtenus sur l'échantillon GHASP, mettant en évidence une évolution du support dynamique des galaxies avec le temps.

L’étude cinématique des galaxies locales et lointaines permet de contraindre les scénarios de formation et d’évolution des galaxies. Pour cela, la spectroscopie à champ intégral permet une étude détaillée de la cinématique des galaxies proches et fournit depuis peu des indices sur la cinématique des galaxies lointaines. Cette thèse s’appuie principalement sur l’utilisation de l’échantillon cinématique de galaxies locales GHASP. Cet échantillon de référence composé de 203 galaxies spirales et irrégulières de l’Univers local dans des environnements peu denses observées par interférométrie de Fabry-Perot autour de la raie Ha (6563 Å) est le plus grand échantillon de données Fabry-Perot à ce jour. Après un passage en revue des principes de l’interférométrie Fabry-Perot et des nouveautés apportées à la réduction des données Fabry-Perot, mon implication dans le développement du 3D-NTT, nouvel instrument utilisant deux Fabry-Perot est exposée de même que ma participation au projet de spectrographe à grand champ pour les ELT, WFSpec, dont l’objectif est l’étude de l’évolution des galaxies. Je présente dans une deuxième partie les données GHASP. Cet échantillon a été entièrement réduit et analysé à l’aide de nouvelles méthodes. L’analyse cinématique de l’échantillon à partir des cartes cinématiques 2D a été initiée en particulier avec l’étude de la distribution des halos de matière sombre, de la forme des courbes de rotation, de l’influence des potentiels barrés et de la dispersion de vitesses du gaz ionisé. Dans une troisième partie, cet échantillon local sert de point de référence pour l’étude de la cinématique des galaxies lointaines. L’échantillon GHASP est projeté à grand décalage spectral (z = 1. 7) afin de déterminer les biais observationnels liés au manque de résolution spatiale des données cinématiques de galaxies lointaines obtenues par SINFONI, OSIRIS et GIRAFFE. L’analyse cinématique de nouvelles observations SINFONI y est également présentée, et l’ensemble des données cinématiques 2D de la littérature est mis en regard avec les résultats obtenus sur l’échantillon GHASP, mettant en évidence une évolution du support dynamique des galaxies avec le temps
Kinematical studies of low and high redshift galaxies enables to probe galaxy formation and evolution scenarios. Integral field spectroscopy is a powerful tool to study with accuracy nearby galaxies kinematics. Recent observations also gives a new 2D vision of high redshift galaxies kinematics. This work mostly relies on the kinematical sample of galaxies GHASP. This control sample, composed of 203 local spiral and irregular galaxies in low density environments observed with Fabry-Perot techniques in the Ha line (6563 Å), is by now the largest sample of Fabry-Perot data. After a revue on Fabry-Perot interferometry and a presentation of new data reduction procedures, my implications on both 3D-NTT Fabry-Perot instrument and the wide field spectrograph project (WFSpec) for galaxy evolution study with the european ELT are developed. The second section is dedicated to GHASP data. This sample have been fully reduced and analysed using new methods. The kinematical analysis of 2D kinematical maps has been undertaken with the study of the dark matter distribution, the rotation curves shape, bar signatures and the ionized gas velocity dispersion. In a third section, this local reference sample is used as a zero point for high redshift galaxies kinematical studies. The GHASP sample is projected at high redshift (z = 1. 7) in order to disentangle evolution effects from distance biases in high redshift galaxies kinematical data observed with SINFONI, OSIRIS and GIRAFFE. The kinematical analysis of new SINFONI high redshift observations is also presented and high redshift data found in the literature are compared with GHASP projected sample, suggesting some evolution of the galaxy dynamical support within the ages

Le theme de cette these est l'etude de la formation et de la structure de galaxies elliptiques au sein de groupes et amas de galaxies. Cette etude se divise selon deux approches principales: l'analyse des proprietes physiques et morphologiques de deux amas de galaxies, abell 85 et 2199 ; et l'etude numerique de la formation de galaxies elliptiques par coalescence de galaxies spirales. Les amas de galaxies ont ete analyses a partir de cliches pris par le detecteur ipc a bord du satellite einstein dans le domaine de rayonnement x. Le gaz intra-amas responsable de l'emission x est suppose etre en equilibre avec le potentiel de l'amas et sert de traceur de ce dernier. En utilisant une technique d'ajustement des cliches par des images de synthese, il est possible de determiner le profil radial de densite du gaz emetteur ainsi que sa morphologie et la presence des sous-structures. En tirant profit des proprietes spectrales du detecteur, le profil de temperature du gaz est estime. L'etude de la formation de galaxies elliptiques se fait par le biais de simulations a n-corps, en utilisant un code en arbre et un code de somme directe sur un ordinateur massivement parallele. Trois classes de conditions initiales ont ete realisees: deux galaxies spirales de masse semblable placees soit en orbite circulaire, soit sur une trajectoire de collision de plein fouet ; des groupes de galaxies spirales en equilibre du viriel ; un effondrement sans collision d'un gaz froid. Les galaxies spirales suivent le modele de miyamoto & nagai a trois composantes bulbe, disque et halo. Les simulations ont ete suivies jusqu'a la formation d'un objet elliptique central en equilibre quasi-stationnaire. Les proprietes physiques et morphologiques de l'objet final des simulations sont confrontees a des modeles issus de la physique statistique appliquee a des systemes gravitationnels en equilibre. Les structures fines, variation de l'ellipticite, deformation et rotation des isocontours, ont ete comparees a des donnees observationnelles. Une modification de la mecanique newtonienne a ete aussi consideree dans le cadre de l'etude de la structure du gaz intra-amas

In this thesis, we investigate the luminosity functions (LFs) and projected number density profiles of galactic satellites around isolated primaries of differing luminosity. To this end, we develop a new method to select isolated galactic satellite systems using the Sloan Digital Sky Survey (SDSS) spectroscopic and photometric galaxy samples. For specific luminosity primaries, we are able to stack as many as ~ 50,000 galaxy systems to obtain robust statisitcal results. Based on these samples, we derive accurate satellite luminosity functions extending almost 8 magnitudes fainter than their primaries and accurate projected number densities profiles of satellites down to 4 magnitudes fainter than their primaries. Then, we determine how the satellite luminosity functions and projected number density profiles vary with both the properties of their satellites and their primaries. In addition, we find that the normalized profiles can be well fitted by the NFW profiles in most cases. The dependence of the NFW concentration parameters on the luminosity of the satellites and their primaries are explored. Inspired by the similar independent study, we also explore the dependence of estimates of satellite luminosity functions on two different background subtraction methods. We then measure these quantities for model satellites placed into the Millennium and Millennium II dark matter simulations by the GALFORM semi-analytic galaxy formation model for different bins of primary galaxy magnitude. We compare our model predictions to the data that we previously measured. The generally successful comparison of the GALFORM model with the SDSS data performed here provides a non-trivial validation of the assumptions and framework of this kind of modelling.

Dusty star-forming galaxies (DSFGs) are highly luminous (LFIR ≳ 10¹² L⊙), very distant (z ≳2.5) and ≳ 10x rarer then 'normal', NIR-selected (BzK), star-forming galaxies. Capable of producing a Mstars ≳ 10¹¹-M⊙ galaxy after a tburst ~ 100-Myr burst of late-stage, merger-induced star formation, DSFGs naturally provide extreme laboratories with which to study the formation and evolution of massive structures within the Universe. Thus far, however, theoretical models have struggled to reconcile the observed abundance and redshift distribution of these massive, dust-enshrouded galaxies that occupy the high-end tail of the galaxy stellar mass function. Therefore, it is of paramount importance, from an observational point of view, to both increase the number of known distant (z ≳ 4) DSFGs and to thoroughly explore their extreme environments in order to provide further constraints on such models. Thus, in Chapter 2 of this thesis, I report on efforts to substantially increase the number of distant DSFGs using the uniquely wide H-ATLAS imaging survey. I analysed a sample of 109, so-called 'ultra-red galaxies' selected via their red Herschel-SPIRE flux densities (σ500 > 3.5 and S500 < 100mJy) and flux-density ratios (S500/S250 > 1.5 and S500/S350 > 0.85). Ground-Based continuum imaging at ~ 850 μm with the JCMT and APEX telescopes allowed me to locate the dust peaks of these S500 ≳ 30-mJy ultra-red galaxies and derive a median photometric redshift of zphot = 3.66 (3.30-4.27, IQR) for them (assuming that they can satisfactorily be represented by a Tdust ~ 30-K template SED). Using 25 spectroscopically confirmed DSFGs with SPIRE flux densities matching this ultra-red criteria, I determined that these FIR photometric redshift estimates have a minimum intrinsic scatter of σ = 0.14(1 + zspec) and systematically under-estimate the spectroscopic redshifts below zspec ≲ 5. With over a third of these ultra-red galaxies lying above z > 4, I derived a space density of at least p ≈ 6 x 10⁻⁷Mpc⁻³ for this sample (assuming a tburst = 100-Myr burst of star formation), which is only a factor of 7x less numerous than that of the most massive (Mstars ≳ 10¹¹M⊙), compact, quiescent galaxies selected in the NIR at z ~ 3. Finally, although the space density of z > 4 ultra-red galaxies aligns very well with that of massive (MBH ≳ 10⁸M⊙) AGN at z > 6, none have yet to be uncovered within this sample to date. In the following chapter, I present wide images obtained with LABOCA of a sub-sample of 22, representative ultra-red galaxies to see if these galaxies are signposting over-dense regions in the early Universe, as might be expected if they were to evolve into the most massive, compact, quiescent galaxies at z ~ 0. This LABOCA ultra-red galaxy survey covers an area of ≈ 0.8 deg² down to an average r.m.s. of 3.9mJy beam⁻¹, with the five deepest images going ≈ 2x deeper still. I catalogue 86 galaxies detected above > 3.5σ870 surrounding these 22 ultra-red galaxies, which implies a δ ≈ 100 ± 30% over-density of S870 > 8.5-mJy (LFIR ≈ (7-30) x 10¹² L⊙) DSFGs when compared against LESS. Thus, I am 99.93% confident that these ultra-red galaxies are pinpointing over-dense regions in the Universe, and ≈ 95% confident that these regions are over-dense by a factor of at least ≥ 1.5x. Using the same template SEDs as in the previous chapter, I derived a consistent median photometric redshift of z = 3.2 ± 0.2 with an IQR of z = 2.8-3.6 for these ultra-red galaxies. I constrained the surrounding galaxies likely responsible for this over-density to within |∆z| ≤ 0.65 of their respective ultra-red galaxies. However, on average, I was only able to associate one surrounding galaxy to within |∆z| ≤ 0.5 of its respective ultra-red galaxy. These 'associated' galaxies are radially distributed within (physical) distances of 1.6 ± 0.5Mpc from their ultra-red galaxies, have median SFRs of vI≈ (1.0±0.2)x10³M⊙ yr⁻¹ (assuming a Salpeter stellar IMF) and median gas reservoirs of Mgas ~ 1.7 x 10¹¹M⊙. These candidate proto-clusters have average total SFRs of at least Ψ ≈ (2.3 ± 0.5) x 10³M⊙ yr⁻¹ and a space density of ~ 9 x 10⁻⁷Mpc⁻³, consistent with the idea that their constituents may occupy the centres of rich galaxy clusters seen today. Finally, in Chapter 4 of this thesis, I extracted Herschel-SPIRE photometry at the 850-μm positions of DSFGs detected within in the S2CLS and S2COSMOS imaging surveys. I then analysed the multi-wavelength environmental properties around a robust sample of 64 ultra-red galaxies selected via their 'ultra-red probability'. Similar to the findings in Chapter 3, I found that these ultra-red galaxies are preferentially located in over-dense regions extending over scales of ~ 5' (or ~ 2Mpc at z ~ 3). Furthermore, I found that these candidate, high-redshift proto-clusters have FIR total dust masses and total SFRs of Mdust ~ 10⁹M⊙ and Ψ ~ 10³M⊙ yr⁻¹, respectively. Ground-Based, optical/NIR imaging around a subset of 42 ultra-red galaxies shows a factor of ~ 5x increase in both the stellar mass and the (MB -MI )-colour of associated LBGs as the radial distance decreases from . 500 kpc - consistent with the emergence of a galaxy red sequence at z ~ 3. Furthermore, these data show a 1-σ increase in the fraction of 'green-valley' galaxies within scales of ~ 5' compared to the field - supporting the concept that red-sequence galaxies are appearing at a faster rate around ultra-red galaxies compared to the field. There is a sizeable contribution of Mstars ~ 10¹²M⊙ from these high-redshift LBGs within the environments of ultra-red galaxies. On average, I was able to associate ≈ 28 LBGs to a given ultra-red galaxy (~ 30x the number of associated DSFGs). Although these systems have average optical/NIR/FIR properties that are consistent with their evolution into present-day galaxy clusters with DM halos of mass Mhalo ~ 10¹⁴-10¹⁵M⊙, I am still likely missing a sizeable contribution from unassociated LBGs and DSFGs due to the large photometric redshift uncertainties for the ultra-red galaxies. Therefore, the results presented in this thesis should be regarded as firm lower limits on these environmental properties around ultra-red galaxies, which can now only be improved upon when spectroscopic data increases the accuracy of the photometric redshift estimates presented here.

Thesis (Ph.D) - Swinburne University of Technology, Faculty of Information & Communication Technologies, 2007.
A thesis presented in fulfillment of the requirements of Doctor of Philosophy, Faculty of Information and Communication Technologies, Swinburne University of Technology, 2007. Typescript. Bibliography p. 109-118.

In this thesis, we investigate the evolution of dust mass and chemical composition in different galaxies by means of new detailed chemical evolution models which account for the presence of dust. We adopt updated prescriptions for dust formation in Asymptotic Giant Branch (AGB) stars and Type II SNe, as well as for dust accretion and destruction in the interstellar medium (ISM). We predict in detail the evolution of the abundances of single elements both in the dust and in gas phase of the ISM, and distinguish the contributions from different sources during the galactic time. We study the dust evolution in galaxies of different morphological type, i.e. dwarf irregulars, spirals, Milky Way-type and ellipticals: our model has proven to be very useful to study various dust properties such as dust mass, dust-to-gas (DG) ratio and chemical composition. In our approach, the main difference between galaxies is the star formation history: in ellipticals it is assumed a very fast and intense star formation rate, and this rate decreases going towards spirals, irregulars and smaller galaxies. First, we compare our model predictions for a typical dwarf irregular galaxy with chemical abundances measured in Damped Lyman Alpha (DLA) systems. After having reproduced the abundances of volatile elements S and Zn (unaffected by the presence of dust), we study the depletion patterns of refractory elements (Si and Fe), which tend to be incorporated in the dust phase. Our study suggests that Fe and Si undergo a different history of dust formation and evolution and that Fe is mainly incorporated into iron-rich solid nano-particles, which may form by dust growth in the ISM. We also provide a new method, based on DLA column density measurements and the ratio between volatile and refractory elements, to give for the first time an estimate of the chemical abundance ratios inside dust grains. In this way, we try to disentangle the main dust constituents and predict their evolution: in particular, we focus on the fraction between silicates and metallic particles and between pyroxenes and olivines. Concerning the Milky Way, we present the evolution (in space and time) of the DG ratio in the context of the galactic habitable zone, defined as the region with highly enough metallicity to form planetary systems capable of sustaining life. In this study, we provide theoretical prescriptions of the DG ratio and metallicity for models of planetary systems formation. Then we focus our study on high redshift elliptical galaxies, and we try to disentangle the responsible processes for the sudden appearance of metals and dust observed in those objects. The first metals and dust appear very early since they are both produced by short living massive stars (core-collapse SNe), on the time-scales of few tenths of million years. In their initial burst of star formation, the metallicity can attain almost a solar value after one hundred million years and the same is true for dust, to which also AGB stars contribute on time-scales equal or larger than 30 million years. Finally, we study the cosmic dust rate (CDR) across the Universe by assuming that the cosmic dust abundance results from the contribution of galaxies of different morphological type averaged in a unitary volume of the Universe. These galaxies are assumed to evolve in number density according to their weight in the luminosity function at different redshifts and different cosmological scenarios. Parallel to the CDR we compute the cosmic star formation rate (CSFR) as well as the cosmic rate of metallicity. Our predictions are extreme important to understand the roles of dust production, accretion and destruction in the CDR evolution. Our best scenario predicts a dust rate peak between 2