Literatura científica selecionada sobre o tema "Primeval galaxies"

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Artigos de revistas sobre o assunto "Primeval galaxies"

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Miley, George. "Primeval galaxies". Physics World 2, n.º 10 (outubro de 1989): 35–38. http://dx.doi.org/10.1088/2058-7058/2/10/22.

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Cowen, Ron. "Found: Primeval Galaxies". Science News 149, n.º 8 (24 de fevereiro de 1996): 120. http://dx.doi.org/10.2307/3979806.

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OZERNOY, LEONID M. "Primeval and "Rejuvenated" Galaxies." Annals of the New York Academy of Sciences 571, n.º 1 Texas Symposi (dezembro de 1989): 219–27. http://dx.doi.org/10.1111/j.1749-6632.1989.tb50509.x.

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Collins, C. A. "Searches for primeval galaxies". Contemporary Physics 40, n.º 1 (janeiro de 1999): 1–10. http://dx.doi.org/10.1080/001075199181675.

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Wada, Keiichi, e Asao Habe. "Primeval starburst and bulge formation". Symposium - International Astronomical Union 153 (1993): 397–98. http://dx.doi.org/10.1017/s0074180900123769.

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Pritchet, C. J. "The search for primeval galaxies". Publications of the Astronomical Society of the Pacific 106 (outubro de 1994): 1052. http://dx.doi.org/10.1086/133479.

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Mori, Masao, e Masayuki Umemura. "Galactic winds from primeval galaxies". Astrophysics and Space Science 311, n.º 1-3 (8 de junho de 2007): 111–15. http://dx.doi.org/10.1007/s10509-007-9533-5.

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Baron, E., e Simon D. M. White. "The appearance of primeval galaxies". Astrophysical Journal 322 (novembro de 1987): 585. http://dx.doi.org/10.1086/165754.

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Collins, C. A., e R. D. Joseph. "An infrared search for primeval galaxies". Monthly Notices of the Royal Astronomical Society 235, n.º 1 (1 de novembro de 1988): 209–20. http://dx.doi.org/10.1093/mnras/235.1.209.

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Derobertis, M. M., e Marshall L. McCall. "A Continuum Search for Primeval Galaxies". Astronomical Journal 109 (maio de 1995): 1947. http://dx.doi.org/10.1086/117420.

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Teses / dissertações sobre o assunto "Primeval galaxies"

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Thompson, David Djorgovski S. G. "Surveys for primeval galaxies /". Diss., Pasadena, Calif. : California Institute of Technology, 1995. http://resolver.caltech.edu/CaltechETD:etd-10242007-142316.

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Lecroq, Marie. "Modelling primeval galaxies in the JWST era". Electronic Thesis or Diss., Sorbonne université, 2024. http://www.theses.fr/2024SORUS154.

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Le télescope spatial James Webb, lancé en décembre 2021, est considéré comme l'observatoire majeur de la décennie en cours. S'il doit explorer toutes les phases de l'histoire cosmique, l'un de ses principaux buts scientifiques est de dévoiler les premières étoiles et galaxies formées dans l'obscurité de l'Univers primitif, qui ont conduit à sa réionisation avant d'évoluer vers la population de galaxies observable aujourd'hui. Pour interpréter les données spectroscopiques recueillies par le JWST, il est nécessaire de développer des modèles qui contraignent efficacement la physique de l'émission des galaxies primitives. Cette démarche peut être guidée par l'observation de galaxies proches aux propriétés similaires à celles attendues pour les galaxies primitives, c'est-à-dire extrêmement pauvres en métaux et formant activement des étoiles. De telles galaxies dans l'Univers local présentent des champs de rayonnement étonnamment durs, se traduisant notamment par d'intenses raies d'émission à haute ionisation, qui ne peuvent être pleinement expliquées par aucun modèle existant. De récentes études pointent vers le rôle essentiel que pourraient jouer les étoiles binaires massives dans cette émission. Le but de cette thèse est d'abord d'ouvrir une nouvelle brèche dans la modélisation de l'émission des galaxies primitives, en explorant les signatures spectrales d'étoiles binaires massives. Pour cela, j'étudie l'émission nébulaire de populations d'étoiles jeunes générées grâce au nouveau modèle GALSEVN, qui combine le code de synthèse de population SEVN, qui inclut les interactions entre étoiles binaires, et le code d'évolution spectrale GALAXEV. Cette démarche confirme que les interactions entre les étoiles des systèmes binaires influencent fortement les propriétés d'émission des galaxies jeunes. Je montre en particulier que GALSEVN reproduit les rapports d'intensités HeII/Hb élevés communément observés dans les galaxies sous métalliques à formation stellaire active, difficiles à reproduire avec les modèles actuels. Je montre également comment la considération de sursauts de formation stellaire successifs peut améliorer l'accord avec les observations, tandis que les valeurs les plus extrêmes des caractéristiques spectrales de HeII peuvent être reproduites par des populations stellaires dominées par les étoiles massives. GALSEVN permet aussi de calculer de manière inédite l'émission des disques d'accrétion dans les binaires X et des chocs radiatifs issus des vents stellaires et des supernovae, en utilisant une approche auto-cohérente construite à partir des caractéristiques des populations stellaires. Ce travail montre que ces contributions n'affectent que peu les rapports tels que HeII/Hb, contrairement à ce qui a pu être prédit par d'autres modèles, qui semblent surestimer les luminosités X de galaxies proches par rapport à la fonction de luminosité moyenne observée pour les binaires X. GALSEVN peut également prédire l'émission de populations stellaires extrêmement sous-métalliques, représentatives des premières générations d'étoiles de notre Univers. L'étude de différents paramètres caractérisant l'émission de ces étoiles conforte l'idée que les premières étoiles ont pu jouer un rôle majeur dans la réionisation de l'Univers et la formation des structures observées aujourd'hui. L'ensemble des résultats présentés dans cette thèse permettent finalement d'établir une solide base pour l'investigation plus poussée des propriétés des galaxies primitives. En construisant une grille étendue de modèles aux propriétés stellaires et nébulaires variées, il est possible d'appliquer des méthodes statistiques pour interpréter les données collectées par le JWST et contraindre les propriétés physiques des galaxies observées. En conclusion, cette thèse a conduit au développement et à la publication de nouveaux modèles permettant une interprétation inédite des propriétés physiques de galaxies à l'émission dominée par leur jeune population stellaire
The James Webb Space Telescope, launched in December 2021, is heralded as the major observatory of the coming decade. While it will explore all phases of cosmic history, one of its main scientific goals is to reveal the first stars and galaxies formed in the darkness of the early Universe, which led to its reionisation before evolving into the population of galaxies observable today. To interpret the spectroscopic data collected by JWST, it is necessary to develop models which can effectively constrain the physics of primeval-galaxy emission. This approach can be guided by observations of nearby galaxies with properties similar to those expected of primeval galaxies, i.e. extremely metal-poor and actively star-forming. Such galaxies in the local Universe exhibit surprisingly hard radiation fields, resulting notably in intense high-ionization emission lines, which cannot be fully explained by any existing model. Recent studies point to the essential role that massive binary stars could play in this emission.The aim of this thesis is to open up a new gap in the modelling of the emission from primeval galaxies, by exploring the spectral signatures of massive binary stars. To this end, I study the nebular emission of populations of young stars generated using the new GALSEVN model, combining the population synthesis code SEVN, which includes interactions between stars in binary systems, with the spectral evolution code GALAXEV. This approach confirms that interactions between stars in binary systems strongly influence the emission properties of young galaxies. In particular, I show that GALSEVN is able to account for the high HeII/Hb intensity ratios commonly observed in metal-poor galaxies with active stellar formation, which are difficult to reproduce with current models. I also demonstrate how successive bursts of star formation can improve agreement with observations, while the most extreme HeII spectral features can be reproduced by stellar populations dominated by massive stars. GALSEVN also makes it possible to evaluate the emission from accretion discs of X-ray binaries and radiative shocks from stellar winds and supernovae in an innovative way, using a self-consistent approach built from the characteristics of the modelled stellar populations. This work shows that these contributions likely have little effect on ratios such as HeII/Hb, contrary to predictions from other models, which appear to overestimate the X-ray luminosities of nearby galaxies relative to the observed mean luminosity function of X-ray binaries. GALSEVN can also predict the emission of extremely metal-poor stellar populations, representative of the first generations of stars in our Universe. A study of different parameters characterising the emission of these stars supports the view that the first stars may have played a major role in the reionization of the Universe and the subsequent formation of the structures observed today. Overall, the results presented in this thesis provide a solid basis for further investigation of the properties of early galaxies. By building a grid of models spanning a wide range of stellar and nebular properties, it is possible to apply statistical methods to interpret data collected by JWST in terms of constraints on the physical properties of the observed galaxies. In conclusion, this thesis has led to the development and publication of new models enabling a novel interpretation of the physical properties of galaxies whose emission is dominated by young stellar populations
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Caruana, Joseph. "Spectroscopic analysis of primeval galaxy candidates". Thesis, University of Oxford, 2013. http://ora.ox.ac.uk/objects/uuid:1c354597-28a3-4d7f-9b52-9e809655318b.

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This thesis presents spectroscopic observations of z ≥ 7 galaxy candidates in the Hubble Ultra Deep Field, which were selected with HST WFC3 imaging, using the Lyman-Break technique. Four z-band (z ≈ 7) dropout galaxies were targeted with Gemini/GNIRS, one z-band dropout galaxy and three Y -band (z ≈ 8 − 9) dropout galaxies with VLT/XSHOOTER, and 22 z-band dropouts with VLT/FORS2, where 15 of the latter are strong candidates. No evidence of Lyman-α emission is found, and the upper limits on the Lyman-α flux and the broad-band magnitudes are used to constrain the rest-frame equivalent widths for this line emission. Amongst the targeted objects, observations were made of HUDF.YD3, a relatively bright Y -band dropout galaxy likely to be at z ≈ 8 − 9 on the basis of its colours in the HST ACS and WFC3 images. Lehnert et al. (2010) observed this galaxy using the VLT/SINFONI integral field spectrograph and claim that it exhibits Lyman-α emission at z = 8.55. In observations of this object described in this thesis, which were made with VLT/XSHOOTER and Subaru/MOIRCS, this line was not reproduced despite the expected signal in the combined MOIRCS & XSHOOTER data being 5σ. Hence it appears unlikely that the reported Lyman-α line emission at z > 8 is real. Accounting for incomplete spectral coverage, in total (across all spectro- graphs) 9.63 z-band dropouts and 1.15 Y -band dropouts are surveyed to a Lyman-α rest-frame Equivalent Width better than 75 ̊A. A model where the fraction of high rest-frame equivalent width emitters follows the trend seen at z = 3−6.5 is inconsistent with these non-detections at z = 7−9 at a confidence level of ∼ 91%, which may indicate that a significant neutral HI fraction (χHI) in the intergalactic medium suppresses the Lyman-α line at z > 7. In particular, the lack of detection of Lyman-α emission in this spectroscopy is compared with results at lower redshift by Stark et al. (2010), who derive a mapping between Lyman-α fractions and χHI based on radiative transfer simulations by McQuinn et al. (2007). These results suggest a lower limit of χHI ~ 0.5.
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Lipman, Keith. "Chemical abundances of primeval galaxies from QSO absorption lines". Thesis, University of Cambridge, 1995. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.363292.

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Vidal, García Alba. "Modeling and interpretation of the ultraviolet spectral energy distributions of primeval galaxies". Thesis, Paris 6, 2016. http://www.theses.fr/2016PA066667/document.

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Je combine de nouveaux modèles de production de radiations stellaires et de transport radiatif à travers le milieu interstellaire (MI). Cela permet de caractériser les étoiles ainsi que le MI neutre et ionisé dans des galaxies formant des étoiles (GFE), via des raies ultraviolettes dans leur spectre. J'évalue la fiabilité des modèles stellaires en ajustant dans l'ultraviolet les indices d'absorption mesurés dans les spectres stellaires de 10 amas d'étoiles dans le Grand Nuage de Magellan. Je montre que négliger l'échantillonnage stochastique de la fonction de masse initiale stellaire de ces amas jeunes et peu massifs a une faible influence dans l'estimation d'âge et de métallicité, mais peut entraîner une surestimation significative des estimations de leur masse. Ensuite, je développe une approche basée sur une description épurée des principales caractéristiques du MI, afin de calculer de manière auto-cohérente l'influence combinée de l'émission et de l'absorption de ce milieu dans le spectre ultraviolet des GFE. Ce modèle tient compte du transport radiatif aussi bien à travers les couches intérieures ionisées, qu'à travers les couches extérieures neutres des nuages de formation d'étoiles ainsi que le milieu diffus entre ces nuages. J'utilise cette approche pour étudier la signature enchevêtrée des étoiles, du milieu neutre et du milieu ionisé dans les spectres ultraviolets des GFE. J'obtiens que la plupart des indices stellaires dans l'ultraviolet sont susceptibles de présenter une contamination par le MI qui augmente avec la métallicité. Enfin, j'identifie des raies d'émission et d'absorption interstellaires pouvant discriminer efficacement les différentes phases du MI
I combine state-of-the-art models for the production of stellar radiation and its transfer through the interstellar medium (ISM) to investigate ultraviolet-line diagnostics of stars, the ionized and the neutral ISM in star-forming galaxies. I start by assessing the reliability of the stellar population synthesis modelling by fitting absorption-line indices in the ISM-free ultraviolet spectra of 10 Large-Magellanic-Cloud clusters. In doing so, I find that neglecting stochastic sampling of the stellar initial mass function in these young low-mass clusters affects negligibly ultraviolet-based age and metallicity estimates but can lead to significant overestimates of stellar mass. Then, I develop a simple approach, based on an idealized description of the main features of the ISM, to compute in a physically consistent way the combined influence of nebular emission and interstellar absorption on ultraviolet spectra of star-forming galaxies. My model accounts for the transfer of radiation through the ionized interiors and outer neutral envelopes of short-lived stellar birth clouds, as well as for radiative transfer through a diffuse intercloud medium. I use this approach to explore the entangled signatures of stars, the ionized and the neutral ISM in ultraviolet spectra of star-forming galaxies. I find that, aside from a few notable exceptions, most standard ultraviolet indices defined in the spectra of ISM-free stellar populations are prone to significant contamination by the ISM, which increases with metallicity. I also identify several nebular-emission and interstellar-absorption features, which stand out as particularly clean tracers of the different phases of the ISM
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Gutkin, Julia. "Constraints on the physical properties and chemical evolution of star-forming gas in primeval galaxies". Thesis, Paris 6, 2016. http://www.theses.fr/2016PA066255/document.

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Je présente un nouveau modèle d'émission nébulaire de galaxies à formation d'étoiles, que j'ai développé en combinant un modèle récent de synthèse de populations stellaires avec un code classique de photoionisation. Je détaille les principales caractéristiques de ce nouveau modèle, comme le traitement sophistiqué des abondances individuelles et des déplétions sur les grains de poussière qui permet d'explorer de façon appropriée les signatures des rapports non solaires d'abondances de métaux, et donc les propriétés des galaxies chimiquement jeunes à l'époque de la réionisation. Je présente la grille exhaustive publique de modèles de photoionisation que j'ai créée, explorant de larges éventails de paramètres stellaires et interstellaires. Je décris la capacité des modèles à reproduire simultanément les caractéristiques observationnelles de galaxies à formation d'étoiles dans plusieurs diagrammes de rapports de raies ultraviolettes et optiques, et j'explore l'influence des différents paramètres ajustables des modèles sur les prédictions de rapports de luminosités de raies. Je décris également comment la combinaison de ces modèles avec des modèles de régions d'émission de raies étroites autour de noyaux actifs de galaxies, effectués avec le même code de photoionisation, permet de définir de nouveaux diagnostics de rapports de raies d'émission ultraviolettes et optiques pour distinguer la formation stellaire et l'activité nucléaire dans les galaxies. Enfin, je montre comment le nouveau modèle présenté dans cette thèse a déjà été utilisé pour interpréter avec succès les raies d'émission ultraviolettes et optiques de galaxies naines lentillées à des décalages spectraux entre 2-7
I present a new model of nebular emission from star-forming galaxies, which I have developed by combining updated stellar population synthesis models with a standard photoionization code. I detail the main features of this new model, such as the recent advances in the theories of stellar interiors and atmospheres it incorporates to interpret the ionizing radiation from star-forming galaxies, and the careful treatment of individual abundances and depletion onto dust grains, which allows one to properly explore the signatures of non-solar metal abundance ratios, and then the properties of chemically young galaxies out to the reionization epoch. I present the public comprehensive grid of photoionization models I have computed, including full ranges of stellar and interstellar parameters. I describe the ability of the models to account simultaneously for observational trends followed by star-forming galaxies in several ultraviolet and optical diagnostic line-ratio diagrams, and I explore the influence of the various adjustable model parameters on predicted line-luminosity ratios. I also describe how the combination of this model with calculations of narrow-line emitting regions from active galactic nuclei computed using the same photoionization code allows one to define new ultraviolet and optical emission-line diagnostics to discriminate between star formation and nuclear activity in galaxies. Finally, I show how the new model presented in this thesis has already been used successfully to interpret the rest-frame ultraviolet and optical line emission of different types of high-redshift star-forming galaxies, mainly lensed dwarf star-forming galaxies at redshift between 2-7
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Thompson, David. "Surveys for primeval galaxies". Thesis, 1995. https://thesis.library.caltech.edu/4239/1/Thompson_dj_1995.pdf.

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NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document. We present the results from two complementary surveys for young and forming ellipticals or spheroids at high redshift, one based on a narrowband imaging technique using a Fabry-Perot interferometer, and the other a serendipitous long-slit spectroscopic survey. The Fabry-Perot survey is sensitive to Lya emission in four discrete redshift ranges: z = 2.80 - 2.98, 3.27 - 3.45, 4.42 - 460, and 4.75 - 4.89. The total area of the survey was 0.63 [...], surveyed to a 1[...] limiting line flux of [...] 8.5 x [...] erg [...]. An area of 0.05 [...] was surveyed to a fainter flux limit of [...] 1.5 x [...] erg [...]. A total comoving volume of 110,000 [...] was surveyed to a [...] limiting restframe emission line luminosity of [...] 2.0 x [...] erg [...] (a Friedman cosmology with [...] = 75 km [...] Mpc[...] and [...] = 0.2 is assumed throughout this thesis). The long-slit survey is sensitive to [...] in the range of 3.1 [...] 5.2, with lesser areas surveyed across the entire optical passband. A total of 421 independent spectroscopic frames were searched, covering an area of 0.0042 [...] (14.97 arcmin[...]). 65 emission-line candidates were identified, including 30 galaxies with [...] and 2 quasars. An additional 20 objects were assigned tentative redshifts, all with [...], and have properties consistent with the galaxies seen in the deep field redshift surveys. The remaining objects are candidate [...] galaxies at high red-shift, with isolated, unidentified emission lines and little or no continuum. They require further spectroscopy to check on their nature. A total comoving volume of 102,600 [...] was surveyed to a [...] limiting restframe emission line luminosity of [...] erg [...]. In neither case was an obvious population of primeval galaxies revealed, despite the combined surveys covering a volume of space sufficient to include [...] 200 galaxies with [...] (using the local space density of massive galaxies, and assuming no density evolution). These galaxies could have been detected if they were unobscured by dust and were actively forming stars at a rate of 100 [...]. A number of candidates remain to be followed up with spectroscopic observations, and may yet prove to be the elusive PGs. The lack of detection of a population of [...]-luminous objects could be due to dust quenching of the [...] line, a higher redshift of formation than surveyed, short lifetime in the [...]-bright phase, or even masking of the star-formation emission-line signature by an active nucleus. A study on the feasibility of conducting primeval galaxy surveys in the near infrared, based on emission-lines of [0 II], [0 III], and the Balmer lines, and the results of a preliminary survey based on these techniques, are also presented. It is shown that the new large-format infrared arrays will reach the necessary sensitivities over large enough areas to make such surveys practical.
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Livros sobre o assunto "Primeval galaxies"

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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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Rossi, Luis Sebastián. Kittler en la galaxia Turing. Teseo, 2021. http://dx.doi.org/10.55778/ts877233124.

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<p>Este título recupera la obra del historiador y filósofo alemán Friedrich A. Kittler (1943-2011). Se trata de una indagación en las tesis de un pensamiento provocador formulado para transformar las Ciencias de la Comunicación y los estudios de los medios. El trabajo cuenta con tres ejes que abordan los núcleos materialistas del autor. La primera parte examina los <i>sistemas de registro</i> tanto desde su definición como desde los cambios tecnológicos e institucionales de 1800 y 1900. La segunda parte se aproxima a los problemas de las <i>historias de los medios técnicos</i> (acústicos, ópticos y escriturales) a la luz tanto de sus temporalidades como de las dimensiones marciales que tienen en su génesis. Por último, la tercera parte se aboca a las <i>técnicas culturales</i> explorando −desde vías arqueológicas, genealógicas y ontológicas− la computación ubicua como medio universal. Además, el título indaga aspectos biográficos e intelectuales que –uniendo amor, música, guerra y codificación− permiten presentar los nexos de Kittler con el pensamiento del siglo XX, mientras admiten problematizar las realidades de silicio y los algoritmos en nuestra época: <i>Turingzeit.</i></p>
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Capítulos de livros sobre o assunto "Primeval galaxies"

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Djorgovski, S., e D. J. Thompson. "Searches for Primeval Galaxies". In The Stellar Populations of Galaxies, 337–47. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2434-8_44.

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Mannucci, F., S. V. W. Beckwith e M. J. Mccaughrean. "An Infrared Search for Primeval Galaxies". In Infrared Astronomy with Arrays, 503–4. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-1070-9_149.

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McCall, Marshall L., e Michael M. Derobertis. "Searching the Continuum for Primeval Galaxies". In New Light on Galaxy Evolution, 417. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0229-9_129.

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Thommes, E., e K. Meisenheimer. "Number Density Predictions for Primeval Galaxies". In New Light on Galaxy Evolution, 454. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0229-9_165.

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Koo, David C. "Quests for Primeval Galaxies: A Review of Optical Surveys". In Spectral Evolution of Galaxies, 419–38. Dordrecht: Springer Netherlands, 1986. http://dx.doi.org/10.1007/978-94-009-4598-2_33.

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Heckman, Timothy M. "Primeval Galaxies, the IGM, and the QSO-protogalaxy Connection". In Astrophysics and Space Science Library, 155–58. Dordrecht: Springer Netherlands, 1993. http://dx.doi.org/10.1007/978-94-011-1882-8_11.

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Meisenheimer, K., S. Beckwith, R. Fockenbrock, J. Fried, H. Hippelein, U. Hopp, Ch Leinert, H. J. Röser, E. Thommes e C. Wolf. "The Calar Alto Deep Imaging Survey for Primeval Galaxies". In The Early Universe with the VLT, 165–72. Berlin, Heidelberg: Springer Berlin Heidelberg, 1997. http://dx.doi.org/10.1007/978-3-540-49709-7_19.

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Schaerer, Daniel. "Expected Properties of Primeval Galaxies and Confrontation with Observations". In Multiwavelength Cosmology, 219–22. Dordrecht: Springer Netherlands, 2004. http://dx.doi.org/10.1007/0-306-48570-2_46.

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Muradian, R. M. "The Primeval Hadron: Origin of Rotation and Magnetic Fields in the Universe". In Observational Evidence of Activity in Galaxies, 341–45. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-3851-9_51.

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Pritchet, C. J., e F. D. A. Hartwick. "New Limits on the Surface Density of Z = 5 Primeval Galaxies". In Astrophysics and Space Science Library, 213–16. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2919-7_26.

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Trabalhos de conferências sobre o assunto "Primeval galaxies"

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Schaerer, Daniel, e Anne Verhamme. "Modeling the Emission Line and Ionizing Properties of Primeval Galaxies". In FIRST STARS III: First Stars II Conference. American Institute of Physics, 2008. http://dx.doi.org/10.1063/1.2905542.

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