Academic literature on the topic 'Galaxies : à haute redshift'
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Journal articles on the topic "Galaxies : à haute redshift"
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Mickaelian, A. M., S. K. Balayan, and S. A. Hakopian. "The Byurakan-IRAS Galaxy (BIG) Sample: The Redshift Survey." International Astronomical Union Colloquium 184 (2002): 217–19. http://dx.doi.org/10.1017/s0252921100030724.
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AbstractThe Byurakan-IRAS Galaxy (BIG) sample (1967 galaxies) is based on optical identifications of IRAS PSC sources at δ>+61° and |b| >15° (FBS area). A redshift survey for brighter objects (B<18m) is being carried out with the Byurakan Observatory 2.6m, Special Observatory 6m, and Observatoire de Haute-Provence 1.93m telescopes. 213 objects have been observed, and redshifts in the range 0.008-0.173 have been measured. For this subsample, 15% of the objects are AGNs, and 15% are LIGs and ULIGs.
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Mickaelian, A. M. "Investigation of the Local Universe by Means of IRAS Galaxies." Symposium - International Astronomical Union 204 (2001): 69. http://dx.doi.org/10.1017/s0074180900225904.
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The Byurakan-IRAS galaxy (BIG) sample is based on optical identifications of IRAS PSC sources (Beichman, C. A. et al., eds. 1988, Infrared Astronomical Satellite (IRAS) Catalogs and Atlases: The Point Source Catalog, NASA RP–1190, Washington, DC). It makes use of the IR colours, DSS images, and the First Byurakan Spectral Survey (Markarian, B. E. et al. 1989, Commun. Special Astrophys. Obs., 62, 5).All IRAS sources in the region +61° < δ < 90° at high galactic latitudes (|b| >15°) in an area of 1487 deg2 have been revealed up to the limit of the IRAS survey. The BIG sample (Mickaelian, A. M. 2000, Afz, 43, 425 and references therein) consists of 1500 galaxies, including 870 that were previously known. A redshift survey for brighter objects is being carried out with the SAO (Russia) 6 m, Byurakan Observatory 2.6 m, and Observatoire de Haute Provence 1.93 m telescopes. Redshifts in the range of 0.009–0.173 have been measured. For fainter objects, including 30 empty fields corresponding to sources with IR colors typical of galaxies, deep imaging is being carried out to reveal faint objects and study their morphologies. These objects are candidate ULIRGs. Many are multiple galaxies and small groups. About half of the galaxies are radio sources, and a number are also X-ray sources. The IR luminosity may be due to normal star formation or triggered by interaction or active galactic nuclei (AGNs). The AGNs and interacting/merging systems among the nearest BIG objects are the most interesting cases: they provide understanding of the properties of activity, starburst, and interaction phenomena and their interrelation, thus allowing a study of the physics and evolution of galaxies in the Local Universe.
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Mickaelian, Areg M. "Galaxy Evolution Traced by Multiple Galaxies from the BIG Sample." Proceedings of the International Astronomical Union 2, S235 (August 2006): 225. http://dx.doi.org/10.1017/s1743921306006314.
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AbstractOptical identifications of all IRAS PSC sources at high galactic latitudes by means of the First Byurakan Survey (FBS) in the area with +61° < δ < +90° at galactic latitudes |b|>15° have been carried out with a total surface of 1487 deg2. 1577 sources have been optically identified, 1178 sources corresponding to galaxies. The BIG sample (Byurakan-IRAS Galaxies) was constructed of 1178 newly identified galaxies and 789 other IRAS galaxies in the same area, known before, altogether 1967 galaxies. Studies of the BIG objects include: spectroscopic follow-up for the brighter (<18m) objects; discovery and study of new AGN; discovery and study of new ULIRGs; deep imagery of the most interesting objects and the “empty fields”; 2D spectroscopy of interacting/merging systems; search for obscured IRAS galaxies (with the Spitzer Space Telescope), etc. The BIG objects are a rich source for new AGN, high-luminosity IR galaxies (hence, starburst activity), and interacting/merging systems. All these phenomena are crucial for understanding the galaxy evolution and their interrelation, as well as the triggering of the powerful IR radiation. In frame of the redshift survey of these galaxies, spectroscopic observations have been carried out for the BIG objects (including the pairs and multiples) by means of the Byurakan Astrophysical Observatory (BAO, Armenia) 2.6m, Special Astrophysical Observatory (SAO, Russia) 6m, and Observatoire de Haute Provence (OHP, France) 1.93m telescopes. It is shown that, without an exception, all double/multiple BIG systems are physical pairs or groups, and they are mostly interacting and/or merging systems. From the high IR luminosities derived from the observations, one can conclude that perhaps the ULIRG/HLIRG phenomenon is connected with galaxy interactions/merging. We find an evolution in luminosity function of these objects with respect to their redshift distribution.Existence of AGN among the multiple BIG objects provides a chance for study of the galaxy evolution in sense of interrelationship between the three phenomena: starburst, interactions/merging, and nuclear activity. We have shown (Mickaelian et al. 2001) that the maximum IR luminosity of a single spiral galaxy may not be larger than 1012 Solar luminosities. Hence, all high-L IRAS galaxies are interacting pairs/multiples or mergers. But what is the relation of the active nucleus to the starburst (i.e. IR) activity?
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Barger, Amy. "High-Redshift Galaxies." Symposium - International Astronomical Union 216 (2005): 309–24. http://dx.doi.org/10.1017/s0074180900196743.
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Mapping the history of star formation requires combining observations at many wavelengths. The most dramatic episodes of star formation occurred in high-redshift (z > 1) galaxies obscured by dust. These galaxies can be seen at submillimeter wavelengths. While these episodes clearly constitute much of the star formation in the universe, we still do not know the redshift distribution. Although progess has been made in determining the nature of the brightest members of the submillimeter population, these galaxies comprise only a tiny fraction of the submillimeter extragalactic background light. Optical star formation, by contrast, is well mapped but hard to interpret because of the problems of extinction. At recent times there is still substantial star formation, but it primarily takes place in small galaxies. This cosmic downsizing is paralleled by similar evolution in the properties of AGNs.
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Giovanelli, Riccardo, and Martha P. Haynes. "Redshift Surveys of Galaxies." Annual Review of Astronomy and Astrophysics 29, no. 1 (September 1991): 499–541. http://dx.doi.org/10.1146/annurev.aa.29.090191.002435.
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McCarthy, Patrick J. "High Redshift Radio Galaxies." Annual Review of Astronomy and Astrophysics 31, no. 1 (September 1993): 639–88. http://dx.doi.org/10.1146/annurev.aa.31.090193.003231.
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Salvaterra, Ruben, Andrea Ferrara, and Pratika Dayal. "Simulating high-redshift galaxies." Monthly Notices of the Royal Astronomical Society 414, no. 2 (May 25, 2011): 847–59. http://dx.doi.org/10.1111/j.1365-2966.2010.18155.x.
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Pelló, Roser, Daniel Schaerer, Johan Richard, Jean-Franc Le Borgne, Jean-Paul Kneib, Angela Hempel, Eiichi Egami, et al. "High-redshift lensed galaxies." Proceedings of the International Astronomical Union 2, no. 14 (August 2006): 250. http://dx.doi.org/10.1017/s1743921307010320.
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Miley, George. "High-Redshift Radio Galaxies." Highlights of Astronomy 10 (1995): 543–46. http://dx.doi.org/10.1017/s1539299600011990.
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Radio galaxies are unique cosmological probes. As with radio-loud quasars, the presence of luminous radio continuum and optical line emission enable radio galaxies to be observed and recognized at large distances, up to z = 4.2. However, unlike the situation for most quasars, their optical emission can be spatially resolved from the ground and studied in detail.Progress in detecting distant radio galaxies has been rapid in recent years due to the use of CCDs and the exploitation of new selection criteria. Now, more than 60 radio galaxies are known with z > 2. More than half of these have been found by our group by concentrating on radio sources with the steepest spectra, most of these in a “Key Programme” of the European Southern Observatory. Although several people contributed to this Key Programme, most of the work was done by Huub Röttgering, who presented his Ph.D thesis in January and Rob van Ojik, who succeededhim. Redshifts of 1.5 to 4 correspond to a time when the Universe was 10% -20% of its present age. This was a crucial period in history when galaxy formation must have been rampant. It corresponds to the AGN era, a two-billion year “delta function” in the population evolution of luminous quasars and radio galaxies, when their space-density rose to a value several hundred times larger than the present density before the species mysteriously and suddenly became almost extinct.
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Meisenheimer, K., H. Hippelein, and M. Neeser. "High Redshift Radio Galaxies." Symposium - International Astronomical Union 175 (1996): 571–76. http://dx.doi.org/10.1017/s0074180900081894.
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One hundred years after G. Marconi recorded radio waves over a distance of more than 1000 m, the most sensitive radio telescopes are able to detect the radio emission from light travel distances at least 1.4 × 1023 times greater. The electromagnetic waves from these distant objects are red shifted by Δλ/λ = z > 4. It is not the mere distance of high redshift objects which is fascinating, but rather the fact that one looks back into the early history of the universe by observing them: Objects at a redshift of 4 shined at a time when the universe had reached only about 1/5 of its present age.
Dissertations / Theses on the topic "Galaxies : à haute redshift"
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Pham, Tuan Anh. "Observations millimétriques-submillimétriques de galaxies lentillées gravitationellement à haut redshift." Toulouse 3, 2014. http://thesesups.ups-tlse.fr/2709/.
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Nous présentons une étude détaillée d'observations faites de la galaxie hôte d'un quasar lointain (z~2. 8), RX J0911. La détection de l'émission des molécules CO a été possible grâce au lentillage gravitationnel dû à la présence d'une galaxie plus proche sur la ligne de vue et à la qualité de l'interféromètre du Plateau de Bure. On a obtenu de très bonnes résolutions tant en fréquence, permettant une mesure précise de la largeur de raie, qu'en direction, permettant de résoudre la source aussi bien sur la raie que dans le continu, donc à la fois pour le gaz et pour la poussière. Nous avons discuté en détail le mécanisme de lentillage gravitationnel. Comme souvent lorsqu'il s'agit de grandissements importants, la source est proche de la caustique de la lentille, dans le cas précis elle la chevauche. Il en résulte une dépendance importante du grandissement sur la position précise des sources ponctuelles à l'intérieur de la galaxie, donc des grandissements différents pour le gaz, la poussière et le quasar. D'autre part, les images sont non seulement aggrandies mais aussi déformées. Les données illustrent les avantages offerts par le lentillage en termes de sensibilité en même temps que les complications de l'analyse qui en découlent, source d'incertitudes sur les mesures. La raie CO(7-6) sort clairement du continu, permettant des mesures fiables des luminositées associées au gaz et à la poussière. Des études détaillées des quatre images ont permis de résoudre la source tant sur la raie que dans le continu, avec des rayons de 106±15 et 39±18 mas respectivement. Dans le cas de la raie, la qualité des données a permis de mettre en évidence une excentricité à 3. 3 déviations standard et un gradient de vitesse à 4. 5 déviations standards. La largeur très étroite de la raie implique une masse dynamique basse et les évaluations faites des masses de gaz et de poussière sont elles aussi très au dessous de ce qu'on mesure généralement pour des quasars à fort décalage vers le rouge. La valeur élevée de l'efficacité de formation d'étoiles situe la galaxie dans la partie haute de la distribution des galaxies, qu'elles soient à haut ou bas z: une fraction importante du volume gazeux semble avoir été épuisée à la suite d'une période de formation d'étoiles intense, laissant la galaxie à la frontière des galaxies hôtes de quasar à haut et bas zThe thesis gives a detailed account of observations of the host galaxy of a distant quasar, RX J0911. Detailed observations of the CO emission have been made possible thanks to the gravitational lensing offered by the presence of a galaxy in the foreground and to the quality of the Plateau de Bure Interferometer. High resolutions have been obtained both in frequency, allowing for a precise measurement of the line width, and in space, allowing for resolving spatially the source both on the line and in the continuum, namely both in its dust and gas content. The mechanism of gravitational lensing has been discussed in detail. As is often the case with large magnifications, the source happens to be in the vicinity of the lens caustic, in fact to overlap it. A consequence is a strong dependence of the magnification on the precise position of point sources in the galaxy, resulting in significantly different magnifications for the gas, the dust and the central QSO. Moreover, the morphology of the observed images is distorted in addition to being amplified. The data illustrate the advantage offered by the strong lensing in terms of increased sensitivity as well as the complication that results, causing an additional source of uncertainties on the quantities that are accessible to measurement. The CO(7-6) line stands out clearly above continuum, allowing for reliable measurements of the gas and dust luminosities. Detailed studies of the four lensed images have made it possible to resolve the source in both the line and the continuum with rms radii of 106±15 and 39±18 mas respectively. In the line case, the quality of the data have provided evidence for an ellipticity of the source, 3. 3 standard deviations away from circular, and for a velocity gradient correlated with the source ellipticity, at the level of 4. 5 standard deviations. The very narrow CO(7-6) line implies a low dynamical mass and both gas and dust mass evaluations fall on the low side of the normal high-z quasar host population. The large star formation efficiency is on the high side of both low-z and high-z galaxies: much of the gas has been exhausted after an intense star formation period, leaving the galaxy at the border between high-z and low-z quasar hosts
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Zanella, Anita. "Structural properties of clumpy galaxies and spheroids at high redshift." Thesis, Sorbonne Paris Cité, 2016. http://www.theses.fr/2016USPCC314/document.
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Cette thèse explore la question ouverte des mécanismes selon lesquels les galaxies lointaines évoluent au cours du temps. Elle se concentre sur l’étude des galaxies irrégulières et sur la cause de l’évolution en taille des galaxies passives et compactes. Bien que des régions de formation stellaire très lumineuses (clumps) soient observées dans les galaxies irrégulières depuis longtemps, leur nature et évolution sont encore débattues. Les instabilités gravitationnelles des disques ont été proposées comme la cause principale pour la formation in-situ des clumps, même si certains d’entre eux pourraient avoir une origine ex-situ. De plus, il n’est pas encore clair s’ils peuvent vivre longtemps ou si les vents stellaires les détruisent rapidement. À partir de l’étude détaillée d’un clump très jeune que nous avons découvert dans le disque d’une galaxie à redshift z~2 et de l’analyse d’un échantillon statistique, j’ai conclu que les clumps peuvent se former in-situ et qu’ils vivent typiquement 500 Myr. Ce résultat conforte les simulations numériques qui indiquent que les clumps ont un rôle important pour la croissance de leur noyau. Cela pourrait stabiliser le disque et y avoir un lien avec la formation des galaxies compactes et passives qui ont été decouvertes à haut redshift. Elles ont des tailles significativement plus petites, à masse égale, que celles de leurs homologues locales. Cette découverte a déclenché un débat concernant les possibles mécanismes qui peuvent augmenter leur taille sans altérer leur masse. J’ai analysé un échantillon de 32 galaxies et j’ai conclu que des multiples fusions mineures pourraient être les responsables principaux de leur evolution temporelleThis thesis explores the still unanswered question of how distant galaxies evolve through cosmic time: on one side it focuses on star-forming clumpy galaxies, on the other it investigates the size evolution of passive compact ones. Despite star forming clumps have been observed in high-redshift irregular galaxies since a while, their nature and fate are still highly debated. Violent gravitational disk instability in gas-rich, turbulent galaxies has been proposed as the main cause for in-situ clumps formation, although a fraction of them might have an ex-situ origin. Furthermore, clumps contribution to galaxy evolution is highly debated: it is not clear yet if they are long-lived or if stellar feedback rapidly disrupts them. From both the in-depth study of an extremely young clump that we discovered in the disk of a galaxy at redshift z ~ 2, and the analysis of a full statistical sample, I concluded that at least some clumps form in-situ due to violent disk instability and that they typically live ~ 500 Myr. This supports numerical simulations indicating that clumps are longlived and could play an important role in bulge growth. This might stabilize the disk, quench star formation and have therefore a link with the formation of the compact and passive galaxies that have been observed at high redshift. They have significant smaller sizes, at fixed stellar mass, than local counterparts. This discovery has ignited an important debate concerning the possible mechanisms that could inflate the galaxy sizes without altering much their mass. I analyzed a sample of 32 galaxies and I concluded that multiple minor mergers could be the main drivers of their observed time evolution
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Salmi, Fadia. "Comprendre les modes de formation d’étoiles dans l’univers lointain." Thesis, Paris 11, 2012. http://www.theses.fr/2012PA112173/document.
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L'objectif de mon travail de thèse a consisté à tenter de comprendre quels sont les mécanismes principaux à l'origine de la formation d'étoiles dans les galaxies au cours des derniers dix milliards d'années. Alors qu'il avait été proposé dans le passé que le rôle des fusions de galaxies était dominant pour expliquer l'allumage de la formation d'étoiles dans les galaxies lointaines formant leurs étoiles à de très grands taux, des études plus récentes ont au contraire mis en évidence des lois d'échelles reliant le taux de formation d'étoiles des galaxies à leur masse stellaire ou masse de gaz. La faible dispersion de ces lois semblait être en contradiction avec l'idée d'épisodes stochastiques violents de formation stellaire liés à des interactions, mais plutôt en accord avec une nouvelle vision de l'histoire des galaxies où celles-ci sont nourries de manière continue en gaz intergalactique.Nous nous sommes particulièrement intéressés à l'une de ces lois d'échelles, la relation entre le taux de formation d'étoiles (SFR) et la masse stellaire des galaxies, appelées communément la séquence principale des galaxies à formation d'étoiles. Nous avons étudié cette séquence principale, SFR-M*, en fonction de la morphologie et d'autres paramètres physiques comme le rayon, la couleur, la clumpiness. Le but étant de comprendre l'origine de la dispersion de cette relation en lien avec les processus physiques responsables de cette séquence afin d'identifier le mode principal de formation d'étoile gouvernant cette séquence. Ce travail a nécessité une approche multi-longueurs d'ondes ainsi que l'utilisation de simulations de profils de galaxies pour distinguer les différents types morphologiques de galaxies impliqués dans la séquence principaleThe goal of my PhD study consists at attempt to understand what are the main processes at the origin of the star formation in the galaxies over the last 10 billions years. While it was proposed in the past that merging of galaxies has a dominant role to explain the triggering of the star formation in the distant galaxies having high star formation rates, in the opposite, more recent studies revealed scaling laws linking the star formation rate in the galaxies to their stellar mass or their gas mass. The small dispersion of these laws seems to be in contradiction with the idea of powerful stochastic events due to interactions, but rather in agreement with the new vision of galaxy history where the latter are continuously fed by intergalactic gas. We were especially interested in one of this scaling law, the relation between the star formation (SFR) and the stellar mass (M*) of galaxies, commonly called the main sequence of star forming galaxies. We studied this main sequence, SFR-M*, in function of the morphology and other physical parameters like the radius, the colour, the clumpiness. The goal was to understand the origin of the sequence’s dispersion related to the physical processes underlying this sequence in order to identify the main mode of star formation controlling this sequence. This work needed a multi-wavelength approach as well as the use of galaxies profile simulation to distinguish between the different galaxy morphological types implied in the main sequence
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Bieri, Rebekka. "The Role of AGN Feedback in Galaxy Formation." Thesis, Paris 6, 2016. http://www.theses.fr/2016PA066292/document.
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L’objectif de ma thèse porte sur les interactions entre les noyaux actifs de galaxies et le milieu interstellaire des galaxies. En particulier, je mets l’accent sur les deux mécanismes possibles responsables de la production des vents par les trous noirs : les jets et les vents produits par le rayonnement de ces trous noirs. Les simulations hydrodynamiques de haute résolution des galaxies comprenant la rétroac- tion d’un jet ont montré que l’activité des noyaux actifs peut conduire à une pression exces- sive sur les régions denses de formation stellaire dans les galaxies, et donc à augmenter la formation d’étoiles, conduisant à un effet positif de rétroaction. Je montre que ces noyaux actifs induits par pression régulée et formation d’étoiles peuvent aussi être une explica- tion possible des taux de formation stellaire élevés observés dans l’Univers à haut décalage spectral. De plus, j’ai également étudié en détails comment le rayonnement émis à partir d’un disque d’accrétion autour du trou noir agit efficacement avec le milieu interstellaire et entraîne un fort vent galactique, en simulant la propagation des photons à partir des équations hydrodynamiques du rayonnement. Les simulations montrent que la grande luminosité d’un quasar est en effet capable de conduire des vents à grande échelle et à grande vitesse. Le rayonnement infrarouge est nécessaire pour transérer efficacement le gaz par multi-diffusion sur la poussière dans les nuages denses. Le nombre typique de multi-diffusion diminue rapidement quand le nuage central de gaz central se dilate et se rompt, ce qui permet au rayonnement de s’échapper à travers les canaux à faible densitéSupermassive black holes (SMBHs) are known to reside in the centres of most large galaxies. The masses of these SMBHs are known to correlate with large-scale properties of the host galaxy suggesting that the growth of the BHs and large-scale structures are tightly linked. A natural explanation for the observed correlation is to invoke a self-regulated mechanism involving feedback from Active Galactic Nuclei (AGN). The focus of this thesis is on the interactions between AGN outflows and the ISM and how the feedback impacts the host galaxy. In particular, it focuses on the two possible mechanism of outflows, namely, outflows related to AGN jets and outflows produced by AGN radiation. High resolution, galaxy scale hydrodynamical simulations of jet-driven feedback have shown that AGN activity can over-pressurise dense star-formation regions of galaxies and thus enhance star formation, leading to a positive feedback effect. I propose, that such AGN-induced pressure-regulated star formation may also be a possible explanation of the high star formation rates recently found in the high-redshift Universe. In order to study in more detail the effects of over-pressurisation of the galaxy, I have performed a large set of isolated disc simulations with varying gas-richness in the galaxy. I found that even moderate levels of over-pressurisation of the galaxy boosts the global star formation rate by an order of magnitude. Additionally, stable discs turn unstable which leads to significant fragmentation of the gas content of the galaxy, similar to what is observed in high-redshift galaxies. The observed increase in the star formation rate of the galaxy is in line with theoretical predictions. I have also studied in detail how radiation emitted from a thin accretion disc surrounding the BH effectively couples to the surrounding ISM and drives a large scale wind. Quasar activity is typically triggered by extreme episodes of gas accretion onto the SMBH, in particular in high-redshift galaxies. The photons emitted by a quasar eventually couple to the gas and drive large scale winds. In most hydrodynamical simulations, quasar feedback is approximated as a local thermal energy deposit within a few resolution elements, where the efficiency of the coupling between radiation of the gas is represented by a single parameter tuned to match global observations. In reality, this parameter conceals various physical processes that are not yet fully un- derstood as they rely on a number of assumptions about, for instance, the absorption of photons, mean free paths, optical depths, and shielding. To study the coupling between the photons and the gas I simulated the photon propagation using radiation-hydrodynamical equations (RHD), which describe the emission, absorption and propagation of photons with the gas and dust. Such an approach is critical for a better understanding of the coupling between the radiation and gas and how hydrodynamical sub-grid models can be improved in light of these results
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Villa, Vélez Jorge Andrés. "Spectrophotometric analysis around cosmic noon : emission-lines, dust attenuation, and star formation." Thesis, Aix-Marseille, 2021. http://www.theses.fr/2021AIXM0440.
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Les galaxies sont les éléments constitutifs de l'Univers. La compréhension de leur rôle dans le cosmos se fait grâce à l’étude de la lumière qu’elles émettent d'un point de vue multi-longueur d'onde car les processus physiques en leur sein sont responsables du rayonnement que nous observons. Dans ce travail, un échantillon de galaxies dans le champ COSMOS avec une photométrie de l'ultraviolet à l'infrarouge lointain et des flux Ha, Hb, [OIII]5007 est étudié à l'aide du logiciel CIGALE. La photométrie est ajustée avec les flux Ha pour obtenir des estimations robustes de la masse stellaire, du taux de formation d'étoiles (SFR) et de l'atténuation dans les raies d'émission. Grâce à la correction par la poussière nous avons proposé une correction de la relation liant le SFR et la luminosité de [OIII]5007. La dispersion de cette relation est étudiée en fonction des propriétés du milieu interstellaire comme le paramètre d'ionisation et la métallicité du gaz en ajustant la photométrie et les flux Ha, Hb, [OIII]5007. Les modèles d'émission nébulaire dans CIGALE sont mis à jour pour reproduire l'émission nébulaire de ces galaxies à z~1.6. Ces modèles sont également utilisés pour créer des catalogues de spectres fictifs pour la collaboration MOONS. Un sous-échantillon de galaxies dans le champ COSMOS est ajusté en couvrant la photométrie de l'ultraviolet à l'infrarouge moyen. Des spectres fictifs sont créés, incluant soit le continuum stellaire soit le continuum stellaire et l'émission nébulaire. L'utilité de l'inclusion des informations spectroscopiques en plus de la photométrie dans l'ajustement SED est présenté dans ce travail en préparation des futurs relevés spectroscopiquesGalaxies are the building blocks of the Universe. Understanding their role in the cosmos translates into studying their emitted light from a multi-wavelength perspective as a large variety of physical processes inside them are responsible for the radiation we observe. In this work, a sample of galaxies in the COSMOS field with ultraviolet to far-infrared photometry and Ha, Hb, [OIII]5007 fluxes is studied using spectral energy distribution (SED) fitting software CIGALE. The photometry is firstly fitted along with the Ha fluxes to derive robust estimations of the stellar mass, star formation rate (SFR), and attenuation in the emission lines. A dust-corrected relation between SFR and [OIII]5007 luminosity is proposed. The dispersion in this relation is studied under the light of the interstellar medium (ISM) properties as the ionization parameter and gas-phase metallicity fitting the photometry and the Ha, Hb, [OIII]5007 fluxes. The nebular emission models inside CIGALE are updated to reproduce the nebular emission of these galaxies at z~1.6. These models are also used to create mock spectra catalogs for the Multi-Object Optical and Near-infrared Spectrograph (MOONS) collaboration. A sub-sample of galaxies in the COSMOS field is fitted covering ultraviolet to mid-infrared photometry. Mock spectra are created including either stellar continuum-only or stellar continuum and nebular emission. The power of including spectroscopic information along with the photometry in the SED fitting process is presented in this work in preparation for future large spectroscopic surveys that will open a new era in galactic and extragalactic astronomy
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Roos, Orianne. "Modelling feedback processes, star formation and outflows in high-redshift galaxies." Thesis, Sorbonne Paris Cité, 2016. http://www.theses.fr/2016USPCC148/document.
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Dans l’Univers, on observe des galaxies lointaines ne formant plus d’étoiles, mais les astrophysiciens n’ont pas encore identifié avec certitude les phénomènes physiques à l’origine de leur “mort”. Pour apporter des éléments de réponse, je me suis penchée sur l’étude de phénomènes qui pourraient y jouer un rôle : les processus de rétroaction des étoiles et des trous noirs supermassifs actifs, la formation stellaire, et les vents galactiques. Le Chapitre 1 présente toutes les notions nécessaires à la compréhension du problème : les caractéristiques des galaxies typiques de l’Univers proche et lointain ; les vents galactiques ; la mort des galaxies; les trous noirs supermassifs actifs (noyaux actifs de galaxies, AGN) et les étoiles ; et leur rétroaction. Dans le Chapitre 2, je présente les techniques numériques utilisées : le code de simulations astrophysiques RAMSES et le code de transfert radiatif Cloudy, que j’ai utilisé pour développer une méthode de calcul de l’état d’ionisation d’une galaxie, détaillée au Chapitre 3. Le Chapitre 4 étudie le couplage entre les trous noirs actifs et les étoiles, avec le projet POGO, Origines Physiques des Vents Galactiques. Durant cette thèse, j’ai montré que les trous noirs actifs n’étaient pas en mesure de tuer subitement leur hôte, même en prenant en compte la rétroaction des étoiles, et que leur couplage peut réduire ou renforcer les vents dans les galaxies en fonction de leur masse. Le Chapitre 5 fait un état de l’art du domaine avant et pendant mon doctorat, reprend les conclusions de cette thèse et donne quelques perspectives, notamment en ce qui concerne le rôle additionnel des rayons cosmiques dans la mort des galaxiesIn the Universe, we observe galaxies forming no, or almost no, stars anymore, but astrophysicists do not know yet what physical mechanisms cause their “death”. To give clues to solve the problem, I studied feedback processes from stars and active supermassive black holes, star formation and galactic outflows. Chapter 1 presents all the notions to understand the problem: the characteristics of typical galaxies in the local and distant Universe, galactic outflows, galaxy death, active supermassive black holes, stars, and their feedback processes. In Chapter 2, I describe the numerical techniques I used: the simulation code RAMSES, and the radiative transfer code Cloudy, which I used to develop a computation method to get the ionization state of an entire galaxy. This method is presented in Chapter 3. Chapter 4 studies the coupling between the feedback processes of active supermassive black holes and stars, with the POGO project, Physical Origins of Galactic Outflows. During this thesis, I showed that typical active supermassive black hole cannot suddenly kill their host, even when stellar feedback processes are accounted for, and that their coupling either reduces or enhances the mass outflow rate depending on the mass of the host. In Chapter 5, I give a state-of-the-art about active supermassive black holes before and during my thesis, sum up the conclusions of the work, and give perspectives to enlarge the scope of the study, especially regarding the additional role of cosmic rays in the death of galaxies
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Yang, Chentao. "Physical conditions of the interstellar medium in high-redshift submillimetre bright galaxies." Thesis, Université Paris-Saclay (ComUE), 2017. http://www.theses.fr/2017SACLS361/document.
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La découverte d'une population de galaxies submillimétrique (SMG) obscurcies par la poussière à grand décalage spectral, à l'aide de caméras submm, a révolutionné notre connaissance de l'évolution des galaxies et de la formation stellaire dans les conditions physiques extrêmes. Elles sont les flambées de formation stellaire les plus intenses dans l'Univers, approchant la limite d'Eddington et sont considérées comme les progéniteurs des galaxies actuelles les plus massives. Les modèles théoriques d'évolution de galaxies ont été remis en question par la découverte d'un grand nombre de SMGs à grand décalage spectral. Quelques unes sont fortement lentillées gravitationnelement par une galaxie. Les grands relevés extragalactiges récemment effectués en ont découvert plusieurs centaines, ouvrant de nouvelles opportunités pour observer le milieu interstellaire dans ces objets exceptionnels.Nous avons donc sélectionné un échantillon de SMG fortement lentillées à l'aide des densités de flux submm du relevé Herschel-ATLAS. À l'aide des télescopes de l'IRAM, nous avons construit un échantillon de 16 SMG détectés par la raie de l'eau. Nous avons trouvé une corrélation linéaire forte entre les luminosité d'H2O et infrarouge totale. Cela indique le rôle important du pompage IR lointain dans l'excitation des raies de l'eau. En utilisant un modèle de pompage IR lointain, nous avons obtenus les propriétés physiques du gaz et de la poussière. Nous avons montré que l'eau trace un gaz chaud et dense qui peut être étroitement lié à la formation des étoiles. Plusieurs raies d'H2O+ ont également été détectées dans trois SMG, montrant une corrélation étroite entre les luminosités des raies de H₂ O/H₂ O+ des ULIRG locales aux SMG. Le rapport de flux H2O+/H2O suggère que les rayons cosmiques provenant des activités fortes de formation stellaire sont probablement à l'origine de la chimie de l'oxygène.Nous avons observé de multiples transitions de CO dans chacune de nos SMG. Nous avons mis en évidence un effet significatif de lentillage différentiel qui peut entraîner une sous-estimation de la largeur de raie d'un facteur ~2. A l'aide d'une modélisation de type LVG et en utilisant une approche bayésienne, nous avons estimé la densité et la température du gaz, ainsi que sa densité de colonne. Nous avons ensuite mis en évidence une corrélation entre la pression thermique du gaz et l'efficacité de la formation stellaire. Nous avons également étudié les propriétés globales du gaz moléculaire et sa relation avec la formation d'étoiles ainsi que le rapport masse de gaz sur poussière et le temps d'épuisement du gaz. La détections de raies de carbone atomique dans ces SMG a étendu la corrélation linéaire locale entre luminosité des raies de CO/CI. Enfin, nous avons comparé les largeurs de raie de CO/H₂ O et constaté qu'elles étaient en bon accord. Cela suggère que les régions émettrices soient co-spatiale.Afin de comprendre les propriétés des émissions moléculaires dans ces sources, et plus généralement, leur structure et leur propriétés dynamiques, il est crucial d'acquérir des images à haute résolution angulaire. Nous avons donc observé deux sources avec ALMA/NOEMA en configuration étendue. Ces données nous permettent de reconstituer la morphologie intrinsèque de la source. Les émissions de poussière froide ont une plus petite taille en comparaison avec le gaz CO/H2 O, tandis que les deux derniers sont de taille similaire. En ajustant le modèle dynamique aux données CO, nous avons montré que ces galaxies peuvent être modélisée avec un disque en rotation, duquel nous avons pu déduire leurs masses dynamiques projetées et leurs rayons effectifs.Avec le futur NOEMA/ALMA, nous pourrons étendre ce genre d'observations à un plus grand nombre de SMG fortement amplifiées et même à des SMG non lentillées, afin d'étudier divers traceurs du gaz moléculaire et de comprendre les conditions physiques du milieux interstellaire et leur relation avec la formation des étoilesThe discovery of a population of high-redshift dust-obscured submillimeter galaxies (SMGs) from ground-based submm cameras has revolutionised our understanding of galaxy evolution and star formation in extreme conditions. They are the strongest starbursts in the Universe approaching the Eddington limit and are believed to be the progenitors of the most massive galaxies today. However, theoretical models of galaxy evolution have even been challenged by a large number of detections of high-redshift high-redshift SMGs. A very few among them are gravitationally lensed by an intervening galaxy. Recent wide-area extragalactic surveys have discovered hundreds of such strongly lensed SMGs, opening new exciting opportunities for observing the interstellar medium in these exceptional objects.We have thus carefully selected a sample of strongly gravitational lensed SMGs based on the submm flux limit from the Herschel-ATLAS sample. Using IRAM telescopes, we have built a rich H₂ O-line-detected sample of 16 SMGs. We found a close-to-linear tight correlation between the H2O line and total infrared luminosity. This indicates the importance of far-IR pumping to the excitation of the H2O lines. Using a far-IR pumping model, we have derived the physical properties of the H2O gas and the dust. We showed that H2O lines trace a warm dense gas that may be closely related to the active star formation. Along with the H2O lines, several H2O+ lines have also been detected in three of our SMGs. We also find a tight correlation between the luminosity of the lines of H2O and H2O+ from local ULIRGs to high-redshift SMGs. The flux ratio between H2O+ and H2O suggests that cosmic rays from strong star forming activities are possibly driving the related oxygen chemistry.Another important common molecular gas tracer is the CO line. We have observed multiple transitions of the CO lines in each of our SMGs with IRAM30m telescope. By analysing the CO line profile, we discovered a significant differential lensing effect that might cause underestimation of the linewidth by a factor of ~2. Using LVG modelling and fitting the multi-J CO fluxes via a Bayesian approach, we derived gas densities and temperature, and CO column density per unit velocity gradient. We then found a correlation between the gas thermal pressure and the star formation efficiency. We have also studied the global properties of the molecular gas and its relationship with star formation. We have derived the gas to dust mass ratio and the gas depletion time, they show no difference compared with other SMGs. With the detections of atomic carbon lines in our SMGs, we extended the local linear correlation between the CO and CI line luminosity. Finally, we compared the linewidths of the CO and H2O emission line, which agree very well with each other. This suggests that the emitting regions of these two molecules are likely to be co-spatially located.In order to understand the properties of molecular emission in high-redshift SMGs, and more generally, the structure and the dynamical properties of these galaxies, it is crucial to acquire high-resolution images. We thus observed two of our brightest source with ALMA and NOEMA interferometers using their high spatial resolution configuration. These images have allowed us to reconstruct the intrinsic morphology of the sources. We compared the CO, H2O and dust emission. The cold dust emission has a smaller size compared with the CO and H2O gas, while the latter two are similar in size. By fitting the dynamical model to the CO data of the source, we have shown that the source can be modelled with a rotating disk. We derived the projected dynamical mass and the effective radius of those sources.With the future NOEMA and ALMA, we will be able to extend such kind of observations to a larger sample lensed SMGs and even to unlensed SMGs, to study various gas tracers, and to understand the physical conditions of the ISM and their relation to the star formation
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Fensch, Jérémy. "Star and stellar cluster formation in gas-dominated galaxies." Thesis, Sorbonne Paris Cité, 2017. http://www.theses.fr/2017USPCC207/document.
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Nous étudions la formation d’étoiles et d’amas d’étoiles dans les galaxies dominées par le gaz. Ce terme réfère en premier lieu aux galaxies de l’époque du pic de formation d’étoiles dans l’histoire de l’Univers, qui s’est déroulé vers z ~ 2, mais aussi à leurs analogues locaux, les galaxies naines de marées. En premier lieu, en utilisant des simulations numériques, nous montrons que les galaxies massives typiques de z=2, avec une fraction de gaz d’environ 50%, forment des structures gazeuses massives (10**7-8 masses solaires) et liées gravitationnellement, appelées grumeaux dans la suite. Ces grumeaux ne se forment dans des galaxies avec une fraction de gaz inférieure à 25%. Nous présentons ensuite une étude observationnelle d’un analogue local de grumeaux de galaxies à z=2, la galaxie naine de marée NGC 5291N. Une analyse des raies d’émission de cette galaxie montre la présence de chocs sur les pourtours de l’objet. La photométrie des amas d’étoiles de cette galaxie montre que les amas les plus jeunes (< 10 millions d’années) sont significativement moins massifs que les amas plus âgés. Ceci peut être le signe de fusions progressives d’amas et/ou d’une forte activité de formation stellaire dans ce système il y a environ 500 millions d’années.Dans un second lieu nous étudions comment la fraction de gaz influe sur la formation d’étoiles et d’amas stellaires dans des fusions de galaxies à z=2. En utilisant des simulations numériques nous montrons que ces fusions n’augmentent que relativement peu le taux de formation d’étoiles et d’amas stellaires comparativement aux fusions de galaxies locales, à faible fraction de gaz. Nous montrons que ceci est due à une saturation de plusieurs facteurs physiques, qui sont déjà présents naturellement dans les galaxies isolées à z=2 et sont donc comparativement peu accentués par les fusions. Il s’agit de la turbulence du gaz, des zones de champ de marée compressif et des flux de matières vers le noyau de la galaxie. Nous montrons aussi que les structures stellaires formées au sein des grumeaux de gaz sont préservées par la fusion : elles sont éjectées des disques et orbitent dans le halo de la galaxie résultante de la fusion, où elles peuvent devenir les progéniteurs de certains amas globulairesWe study the formation of stars and stellar clusters in gas-dominated galaxies. This term primarily refers to galaxies from the epoch of the peak of the cosmic star formation history, which occurred at z ~ 2, but also to their local analogues, the tidal dwarf galaxies.Firstly, using numerical simulations, we show that the massive galaxies at z = 2, which have a gas fraction of about 50%, form massive (10**7-8 solar masses) and gravitationally bound structures, which we call clumps thereafter. These clumps do not form in galaxies with a gas fraction below 25%. We then present an observational study of a local analogue of a z = 2 galactic clump, which is the tidal dwarf galaxy NGC 5291N. The analysis of emission lines show the presence of shocks on the outskirts of the object. Photometry of this galaxy’s stellar clusters show that the youngest clusters (< 10 million years) are significantly less massive than older clusters. This could be the sign of ongoing cluster mergers and/or of a strong star formation activity in this system about 500 million years ago).Secondly, we study how the gas fraction impacts the formation of stars and stellar clusters in galaxy mergers at z = 2. Using numerical simulations we show that these mergers only slightly increase the star and stellar cluster formation rate, compared to local galaxy mergers, which have a lower gas fraction. We show that this is due to the saturation of several physical quantities, which are already strong in isolated z=2 galaxies and are thus less enhanced by the merger. These factors are gas turbulence, compressive tides and nuclear gas inflows, We also show that the stellar structures formed in the gaseous clumps are preserved by the fusion: they are ejected from the disk and orbit in the halo of the remnant galaxy, where they may become the progenitors of some globular clusters
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Ribeiro, Bruno. "Morphology as a tracer of evolution in the early phases of galaxy assembly." Thesis, Aix-Marseille, 2016. http://www.theses.fr/2016AIXM4744/document.
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Les propriétés globales des galaxies montrent une forte évolution du taux de formation stellaire et de la densité de masse stellaire à l'époque de l'assemblage des galaxies précédent le pic de formation stellaire dans l'univers, produite par plusieurs processus physiques concurrents (fusion, accrétion, rétroaction, environnement, ...). Les propriétés morphologiques des galaxies ont aussi fortement évolué à la même époque. Dans cette thèse, j'étudie comment l'évolution des propriétés morphologique est reliée aux propriétés spectrophotométriques des galaxies depuis z ~ 6. Les données spectroscopiques obtenues au sein du VIMOS Ultra Deep Survey (VUDS), un nouveau sondage spectroscopique unique de ~ 10000 galaxies entre redshift z~2 et z~6 qui fournissent un excellent moyen de sonder l'évolution galactique à travers cette époque cosmique. A partir des mes résultats, je conclus que les différentes propriétés morphologiques de galaxies à formation stellaire aux redshifts 2The global properties of galaxies show a strong evolution of the star formation rate and stellar mass density at the epoch of galaxy assembly, driven by several competing physical processes (merging, accretion, feedback, environment,...). The morphological properties of galaxies are also strongly evolving over the same timescales. I investigate how the evolution of the morphological properties is connected to the spectrophotometric properties of galaxies since z~6. The spectroscopic data obtained within the VIMOS Ultra Deep Survey (VUDS), a new unique spectroscopic survey of ~10000 galaxies between redshifts z~2 and z~6 conducted at the ESO-VLT, combined with the available Hubble Space Telescope imaging surveys such as COSMOS or CANDELS provide a great way of probing galactic evolution across this cosmic epoch.From the results that I have obtained, I conclude that the different morphological properties of star-forming galaxies at 2
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Collet, Cédric. "Role of AGN feedback in galaxy evolution at high-redshift." Phd thesis, Université Paris Sud - Paris XI, 2014. http://tel.archives-ouvertes.fr/tel-01061155.
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There is growing evidence that supermassive black holes may play a crucial role for galaxy evolution, in particular during the formation of massive galaxies at high redshift (z ~ 2 - 3). Our work focuses on quantifying the effects of jets of radiogalaxies and of large bolometric luminosities of quasars on the interstellar gas in their host galaxies. To this end, we studied the kinematics of the ionized gas in 12 moderately powerful radio galaxies and 11 quasars (6 radio-loud and 5 radio-quiet) at high redshifts with rest-frame optical imaging spectroscopy obtained at the VLT with SINFONI. We searched for outflows and other signatures of feedback from the supermassive black holes in the centers of these galaxies to evaluate if the AGN may plausibly quench star formation. In our sample of moderately powerful radiogalaxies, we observe velocity dispersions nearly as large as those observed in the most powerful ones (with FWHM ~ 1000 km/s), but the quantity of ionized gas is decreased by one order of magnitude (Mion gas ~ 10^8 - 10^9 Msun) and velocity gradients tend to be less dramatic (Δv < 400 km/s), when they are observed. In our sample of quasars, we had to carefully subtract the broad spectral component of emission lines to have access to its narrow, and spatially extended, component. We detect truly extended emission line regions in 4/6 sources of our radio-loud subsample and in 1/5 source of our radio-quiet subsample. We estimate that masses of ionized gas in these sources are smaller than in our sample of high-redshift radiogalaxies (with Mion gas ~ 10^7 - 10^8 Msun) and kinematics tend to be more quiescent, akin to what is observed in local quasars. Finally, detailed observations of two outliers among our sample of high-redshift radiogalaxies revealed that one of them is closely surrounded by 14 companions galaxies, hence lying in an overdensity. We therefore interpret the presence and morphology of ionized gas around these galaxies as evidence for repeated cycles ouf AGN outbursts, akin to what can be observed in local clusters of galaxies, which are prime examples of AGN feedback in the nearby Universe.
Books on the topic "Galaxies : à haute redshift"
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Appenzeller, Immo. High-Redshift Galaxies. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-540-75824-2.
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IAP Workshop (3rd 1987 Paris, France). High redshift and primeval galaxies. Gif sur Yvette, France: Editions Frontières, 1987.
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Kron, Richard G., and Alvio Renzini, eds. Towards Understanding Galaxies at Large Redshift. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2919-7.
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Arp, Halton C. Catalogue of discordant redshift associations. Montreal: Apeiron, 2003.
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High-redshift galaxies: Light from the early universe. Berlin: Springer, 2009.
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Ellis, Simon Charles. The evolution of high redshift clusters of galaxies. Birmingham: University of Birmingham, 2003.
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Bender, Ralf, and Alvio Renzini, eds. The Mass of Galaxies at Low and High Redshift. Berlin, Heidelberg: Springer Berlin Heidelberg, 2003. http://dx.doi.org/10.1007/b10204.
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Law-Green, John Duncan Bradburn. The distant DRAGNS survey: A radio imaging survey of radio galaxies at high redshift. Manchester: University of Manchester, 1996.
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I, Pérez-Fournon, ed. Galaxies at high redshift: XI Canary Islands Winter School of Astrophysics, Santa Cruz de Tenerife, Tenerife, Spain, November 15-26, 1999. Cambridge: Cambridge University Press, 2003.
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Canary Islands Winter School on Astrophysics (11th 1999 Santa Cruz de Tenerife, Canary Islands). Galaxies at high redshift: Proceedings of the XI Canary Islands Winter School of Astrophysics, Santa Cruz de Tenerife, Tenerife, Spain, November 15-26, 1999. Cambridge: Cambridge University Press, 2003.
Find full textBook chapters on the topic "Galaxies : à haute redshift"
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Bahcall, Neta A. "High-Redshift Galaxies." In Highlights of Astronomy, 669–708. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2828-5_17.
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Chincarini, Guido, and Paolo Saracco. "High Redshift Galaxies." In Generation of Cosmological Large-Scale Structure, 1–31. Dordrecht: Springer Netherlands, 1997. http://dx.doi.org/10.1007/978-94-009-0053-0_1.
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Appenzeller, Immo. "Introduction." In High-Redshift Galaxies, 3–10. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-540-75824-2_1.
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Appenzeller, Immo. "Implications." In High-Redshift Galaxies, 293–307. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-540-75824-2_10.
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Appenzeller, Immo. "Ongoing Work." In High-Redshift Galaxies, 311–18. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-540-75824-2_11.
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Appenzeller, Immo. "Future Facilities and their Opportunities." In High-Redshift Galaxies, 319–31. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-540-75824-2_12.
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Appenzeller, Immo. "The Nearby Universe." In High-Redshift Galaxies, 11–72. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-540-75824-2_2.
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Appenzeller, Immo. "The Past and the Future." In High-Redshift Galaxies, 73–117. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-540-75824-2_3.
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Appenzeller, Immo. "Basic Techniques and their Limitations." In High-Redshift Galaxies, 121–51. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-540-75824-2_4.
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Appenzeller, Immo. "Finding Very Distant Galaxies." In High-Redshift Galaxies, 153–73. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-540-75824-2_5.
Full textConference papers on the topic "Galaxies : à haute redshift"
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van Breugel, Willem J. "Highest redshift radio galaxies." In Astronomical Telescopes and Instrumentation, edited by Jacqueline Bergeron. SPIE, 2000. http://dx.doi.org/10.1117/12.390129.
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Fosbury, Robert A. E. "High redshift radio galaxies." In Astronomical Telescopes and Instrumentation, edited by Jacqueline Bergeron. SPIE, 2000. http://dx.doi.org/10.1117/12.390128.
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Woodgate, Bruce E., Paul J. Francis, and Anthony C. Danks. "High redshift galaxies already old?" In The ultraviolet universe at low and high redshift. AIP, 1997. http://dx.doi.org/10.1063/1.53801.
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Strazzullo, V., P. Rosati, C. Lidman, C. Mullis, R. Demarco, R. Gobat, M. Nonino, et al. "Cluster galaxies at redshift 1.4." In PROBING STELLAR POPULATIONS OUT TO THE DISTANT UNIVERSE: CEFALU 2008, Proceedings of the International Conference. AIP, 2009. http://dx.doi.org/10.1063/1.3141528.
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ALEXANDER, D. M. "WHAT POWERS HIGH-REDSHIFT SCUBA GALAXIES?" In Proceedings of the Guillermo Haro Conference 2003. WORLD SCIENTIFIC, 2004. http://dx.doi.org/10.1142/9789812702432_0033.
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Heckman, Timothy M. "Starburst galaxies: implications at high-redshift." In AFTER THE DARK AGES. ASCE, 1999. http://dx.doi.org/10.1063/1.58617.
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Merrifield, Michael R. "A low redshift perspective on galaxies." In INTERNATIONAL CONFERENCE ON CONDENSED MATTER AND APPLIED PHYSICS (ICC 2015): Proceeding of International Conference on Condensed Matter and Applied Physics. Author(s), 2016. http://dx.doi.org/10.1063/1.4948804.
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Calzetti, Daniela. "UV opacity in nearby galaxies and application to distant galaxies." In The ultraviolet universe at low and high redshift. AIP, 1997. http://dx.doi.org/10.1063/1.53764.
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Gordon, Karl D., Daniela Calzetti, and Adolf N. Witt. "Dust in starburst galaxies." In The ultraviolet universe at low and high redshift. AIP, 1997. http://dx.doi.org/10.1063/1.53805.
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Gardner, Jonathan P., Sara R. Heap, Eliot M. Malumuth, Robert S. Hill, and Eric P. Smith. "Morphological evolution of galaxies." In The ultraviolet universe at low and high redshift. AIP, 1997. http://dx.doi.org/10.1063/1.53808.
Full textReports on the topic "Galaxies : à haute redshift"
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Miley, G., C. Carilli, G. B. Taylor, C. de Breuck, and A. Cohen. High Redshift Radio Galaxies: Laboratories for Massive Galaxy and Cluster Formation in the Early Universe. Fort Belvoir, VA: Defense Technical Information Center, January 2010. http://dx.doi.org/10.21236/ada520904.
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