Bibliografias temáticas / Galaxie : structure

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Literatura científica selecionada sobre o tema "Galaxie : structure"

Autor: Grafiati
Publicado: 21 de dezembro de 2024

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Artigos de revistas sobre o assunto "Galaxie : structure"

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Fan, Yi-Liu. "Theoretical Analysis of Moving Galaxies in the Large Scale Structure of SpaceTime." Space Science Journal 1, no. 2 (2024): 01–08. http://dx.doi.org/10.33140/ssj.01.02.05.

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In this paper we will make further theoretical analysis for the validity of the accelerating universe based on General Relativity and three new problems of the standard model of the universe are presented from different perspectives. The first part, analyzed the explosion mechanism of the cosmic initial singularity and put forward a different view from the rest. It’s virtually impossible to start with a giant explosion, the big bang by now cosmologists had refined the idea. The second part devised a new model of the twin paradox. It’s one in which people have been consider to include both spec
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Masters, Karen L. "Galaxy Zoo 3D: Identifying Bars, Spirals and Foreground Stars in MaNGA Galaxy Data." Proceedings of the International Astronomical Union 17, S373 (2021): 39–41. http://dx.doi.org/10.1017/s1743921322004306.

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AbstractGalaxies, particularly disc galaxies, show a wide variety of internal structures (e.g. spirals, bars, and bulges). Mapping Nearby Galaxies at Apache Point Observatory (MaNGA, part of the fourth incarnation of the Sloan Digital Sky Surveys), obtained spatially resolved spectral maps for 10,010 nearby galaxies. Many results from MaNGA have collapsed this structure into azimuthally averaged radial gradients, or symmetric 2D shapes, but there is significantly more information about the effect internal structures have on the evolution of galaxies available if we can identify different inter
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Ge, Xue, Yi-Zhou Gu, Cheng-Long Lei, and Xing-Han Zhang. "The connections among morphology, environment, and star formation with Galaxy Zoo Hubble." Monthly Notices of the Royal Astronomical Society 536, no. 1 (2024): 905–12. https://doi.org/10.1093/mnras/stae2569.

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ABSTRACT Morphology is an important implication for studying the formation and evolution of galaxies. Previous studies have investigated the effects of spiral arms on star formation activities, but it is not clear how clumpy structure affects this process. In this work, we combine Galaxy Zoo Hubble project and 3D-HST/Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey programs to study the influence of morphological structure on star formation processes and the relationship between morphology and the environment at $0 \lt z \lt 1.0$. We find that galaxies with spiral arms and clumpy struc
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Shaver, PA. "Radio Surveys and Large Scale Structure." Australian Journal of Physics 44, no. 6 (1991): 759. http://dx.doi.org/10.1071/ph910759.

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An analysis of the Molonglo Reference Catalogue indicates that significant departures from isotropy are present in the sky distribution of strong extragalactic radio sources. This has been shown to be due to local large scale structure, specifically a concentration to the supergalactic plane, which also influences the slope of the source counts. A study of the three-dimensional distribution of local radio galaxies shows that they are more strongly concentrated to the supergalactic plane than are optically�selected galaxies, and that the supergalactic concentration is more extensive than hither
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Nasution, Budiman, Ruben Cornelius Siagian, Winsyahputra Ritonga, Lulut Alfaris, Aldi Cahya Muhammad, and Arip Nurahman. "A Monte Carlo Density Distribution Model Study to Analyze Galaxy Structure, Mass Distribution, and Dark Matter Phenomena." Indonesian Review of Physics 6, no. 1 (2023): 24–44. http://dx.doi.org/10.12928/irip.v6i1.8240.

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This research uses the Monte Carlo density distribution model to study the structure and mass distribution of galaxies and the dark matter phenomenon. Through computer simulations, the research developed a mathematical model with parameters such as rho0, rc, beta, and others, to describe the structure and mass distribution of galaxies. The results show that the model can reproduce various galaxy structures, including groups, clusters and filaments, and influence the behavior and characteristics of individual galaxies. This research provides a deeper understanding of dark matter and its impact
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Erwin, Peter. "The coexistence of classical bulges and disky pseudobulges in early-type disk galaxies." Proceedings of the International Astronomical Union 3, S245 (2007): 113–16. http://dx.doi.org/10.1017/s1743921308017419.

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AbstractClose examination of “pseudobulges” in several early-type disk galaxies indicates that they are actually composite structures consisting of both a flattened, kinematically cool disklike structure (“disky pseudobulge”) and a rounder, kinematically hot spheroidal structure (“classical bulge”). This indicates that pseudobulges, thought to form from internal secular evolution, and classical bulges, thought to form from rapid mergers, are not exclusive phenomena: some galaxies can have both.
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Yee, H. K. C., M. J. Sawicki, R. G. Carlberg, et al. "The CNOC2 Field Galaxy Redshipt Survey." Highlights of Astronomy 11, no. 1 (1998): 460–63. http://dx.doi.org/10.1017/s153929960002178x.

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Fundamental to our understanding of the universe is the evolution of structures, from galaxies to clusters of galaxies to large-scale sheets and filaments of galaxies and voids. The investigation of the evolution of large-scale structure not only provides us with the key test of theories of structure formation, but also allows us to measure fundamental cosmological parameters. The CNOC2 (Canadian Network for Observational Cosmology) Field Galaxy Redshift Survey is the first large redshift survey of faint galaxies carried out with the explicit goal of investigating the evolution of large scale
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Gao, Tiao. "State-of-art Simulations and Observations for Star Formation." Highlights in Science, Engineering and Technology 72 (December 15, 2023): 66–70. http://dx.doi.org/10.54097/fmnb7351.

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In recent year, the formation and formation of galaxies is a hot spot in astrophysics which has been widely investigated and discussed. On the basis of the theory of formation and formation of large-scale structures in modern cosmology, this study intends to systematically investigate and analyze the physical characteristics of galaxies in different stages, such as morphological structure, star family structure, gas accretion, stellar formation, black hole growth, chemical elements, stellar and gas movements, and their physical relationships with large-scale structures. According to the analys
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Fraser-McKelvie, A., L. Cortese, J. van de Sande, et al. "A SAMI and MaNGA view on the stellar kinematics of galaxies on the star-forming main sequence." Monthly Notices of the Royal Astronomical Society 503, no. 4 (2021): 4992–5005. http://dx.doi.org/10.1093/mnras/stab573.

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ABSTRACT Galaxy internal structure growth has long been accused of inhibiting star formation in disc galaxies. We investigate the potential physical connection between the growth of dispersion-supported stellar structures (e.g. classical bulges) and the position of galaxies on the star-forming main sequence at z ∼ 0. Combining the might of the SAMI and MaNGA galaxy surveys, we measure the λRe spin parameter for 3289 galaxies over $9.5 \lt \log M_{\star } [\rm {M}_{\odot }] \lt 12$. At all stellar masses, galaxies at the locus of the main sequence possess λRe values indicative of intrinsically
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HAQUE-COPILAH, S., and A. ACHONG. "THE FILAMENTARY NATURE OF PISCES-PERSEUS." International Journal of Modern Physics D 12, no. 03 (2003): 527–39. http://dx.doi.org/10.1142/s0218271803003141.

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Minimal Spanning Tree (MST) statistics and associated reducing procedures have been used to establish the level of filamentary structure, if any in Pisces-Perseus, a sample containing 4501 galaxies. The procedure has been applied to subsets of galaxies with 247 galaxies that we call the Most Conspicuous sample which contain the larger intrinsic linear diameters and the brighter galaxies, and to the Least Conspicuous samples with 253 galaxies containing the smaller intrinsic linear diameter and the fainter members as well as the entire sample. The results show that there are longer filaments in
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Teses / dissertações sobre o assunto "Galaxie : structure"

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Nieuwmunster, Niels. "Les systèmes les plus denses de l'Univers : le disque nucléaire." Electronic Thesis or Diss., Université Côte d'Azur, 2024. http://www.theses.fr/2024COAZ5041.

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Comprendre la formation et l'évolution des galaxies, et en particulier de leurs centres galactiques, est l'une des questions les plus intrigantes de l'astrophysique moderne. De nombreuses galaxies spirales comme la Voie lactée présentent en leur centre un disque nucléaire (NSD). Celui de la Voie lactée est, avec l'amas central et le trou noir super massif central, l'une des principales composantes internes et l'un des meilleurs laboratoires locaux disponibles pour étudier l'évolution des galaxies. En raison de la forte extinction, de l'importante densité d'étoiles et de la superposition de mul
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Machado, murtinheiras martins Andre. "Statistical analysis of large scale surveys for constraining the Galaxy evolution." Thesis, Besançon, 2014. http://www.theses.fr/2014BESA2026/document.

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La formation et l'évolution du disque épais de la Voie Lactée restent controversées. Nous avons utilisé un modèle de synthèse de la population de la Galaxie, le Modèle de la Galaxie de Besançon (Robin et al., 2003), qui peut être utilisé pour l'interprétation des données, étudier la structure galactique et tester différents scénarios de formation et évolution Galactique. Nous avons examiné ces questions en étudiant la forme et la distribution de métallicité du disque mince et du disque épais en utilisant l'approche de synthèse de la population. Nous avons imposé sur des simulations les erreurs
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Siebert, Arnaud. "Structure et dynamique des disques de la Galaxie." Université Louis Pasteur (Strasbourg) (1971-2008), 2003. http://www.theses.fr/2003STR13036.

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Jesseit, Roland. "The orbital structure of galaxies and dark matter halos in N-body simulations." [S.l. : s.n.], 2004. http://deposit.ddb.de/cgi-bin/dokserv?idn=970059388.

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Pohlen, Michael. "The radial structure of galactic stellar disks surface photometric study on disk galaxies /." [S.l.] : [s.n.], 2001. http://deposit.ddb.de/cgi-bin/dokserv?idn=964128535.

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Conn, Anthony Rhys. "Structure of the M31 satellite system : bayesian distances from the tip of the red giant branch." Phd thesis, Université de Strasbourg, 2013. http://tel.archives-ouvertes.fr/tel-01012081.

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This study focuses on the spatial distribution of the M31 satellite system. A new Bayesian technique for determining object distances from the Tip of their Red Giant Branch is developed and used to obtain distance probability distributions for M31and 27 of its satellite galaxies. These distances are then used to calculate the satellite positions in three dimensions. Subsequent analysis of the resulting spatial distribution reveals striking inhomogeneity, with roughly half of the satellites confined to a curiously oriented thin disk. The distribution is also markedly asymmetric, with the majori
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Martin, Nicolas. "A la recherche de structures stellaires du disque galactique au halo de la galaxie d'Andromède." Université Louis Pasteur (Strasbourg) (1971-2008), 2006. https://publication-theses.unistra.fr/public/theses_doctorat/2006/MARTIN_Nicolas_2006.pdf.

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Cette thèse a pour but la recherche et l’étude des structures stellaires résultant de l’accrétion de galaxies naines par notre Voie Lactée ou la galaxie d’Andromède (M31). En effet, les théories actuelles sur la formation des halos de galaxies indiquent qu’ils pourraient se construire avec le temps par l’absorption successive de petites structures galactiques. Dans la théorie LCDM actuellement privilégiée, plusieurs centaines de ces fragments proto-galactiques sont nécessaires pour former le halo d’une grosse galaxie comme la Voie Lactée ou M31. Les importantes forces de marée misent en jeu dé
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GOZ, DAVID. "Numerical simulations of galaxies in cosmological volumes." Doctoral thesis, Università degli Studi di Trieste, 2016. http://hdl.handle.net/11368/2908076.

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Modelling galaxy formation in a cosmological context is challenging due to many physical processes and a wide range of scales involved. It is then convenient to address the problem by means of numerical techniques. Cosmological simulations are still orders of magnitude away from capturing directly the spatial scales where stars actually form. The treatment of the interstellar medium, with multiple gas phases co-existing at very different densities and temperatures, needs to be included in simulations in the form of sub-resolution effective models. In Murante et al. (2015), cosmological simulat
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Beuret, Maxime. "Formation stellaire dans la galaxie et interaction avec le milieu interstellaire." Thesis, Strasbourg, 2016. http://www.theses.fr/2016STRAE017/document.

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Comment les étoiles se forment elles ?. Cette vaste question fait appel à des connaissances dans plusieurs domaines dont deux majeurs, la Formation Stellaire et le Milieu Interstellaire. C’est dans ce cadre générale que s’inscrit ma thèse. Notre galaxie est un vaste laboratoire d’études de cette formation et je me suis donc intéressé aux premières étapes de la formation des étoiles, allant du nuage moléculaire à la proto-étoile. J’ai principalement utilisé des données provenant du télescope Herschel qui nous fournit des images et des données dans l’infrarouge lointain et le domaine sub-milimét
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Terral, Philippe. "Structure du champ magnétique interstellaire dans le disque et le halo de notre galaxie." Thesis, Toulouse 3, 2016. http://www.theses.fr/2016TOU30234/document.

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La caractérisation du champ magnétique interstellaire de notre Galaxie représente un enjeu majeur de l'astrophysique. Une meilleure connaissance de ses propriétés, en particulier de sa structure, constituerait en effet un atout important pour de nombreux domaines de recherche allant de l'étude des rayons cosmiques à la dynamique de la Galaxie en passant par l'évolution du milieu interstellaire et la formation stellaire. Des observations radio récentes ont permis de mettre en évidence des caractéristiques communes dans la structure magnétique de galaxies proches semblables à la Voie Lactée. Lor
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Livros sobre o assunto "Galaxie : structure"

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De Zeeuw, Tim, ed. Structure and Dynamics of Elliptical Galaxies. Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-3971-4.

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Mulder, Pieter Samuel. Structure and kinematics of two nearby disc galaxies. Rijksuniversiteit te Groningen], 1995.

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Jong, Roelof Sybe de, 1965-, ed. Island universes: Structure and evolution of disk galaxies. Springer, 2007.

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1916-, Lin C. C., ed. Spiral structure in galaxies: A density wave theory. MIT Press, 1996.

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Méchéri, Hervé-Frédéric. La galaxie jeunesse: Mémoguide des structures publiques de jeunesse. Institut national de la jeunesse et de l'éducation populaire, 2004.

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Purucker, G. de. Galaxies and solar systems: Their genesis, structure, and destiny. Point Loma Publications, 1987.

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Kamphuis, Peter. The structure and kinematics of halos in disk galaxies. s. n., 2008.

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S, Mulchaey John, Dressler Alan Michael, and Oemler Augustus 1945-, eds. Clusters of galaxies: Probes of cosmological structure and galaxy evolution. Cambridge University Press, 2004.

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Jägers, Willem Joseph. The polarization of radio galaxies: Its structure at low frequencies. Sterrewacht Leiden, 1986.

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Keith, Jahoda, McCammon Dan, and United States. National Aeronautics and Space Administration., eds. The structure of galactic HI in directions of low total column density. National Aeronautics and Space Administration?, 1985.

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Capítulos de livros sobre o assunto "Galaxie : structure"

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Abrams, Bernard, and Michael Stecker. "Galaxies and Galaxy Groups." In Structures in Space. Springer London, 2000. http://dx.doi.org/10.1007/978-1-4471-0441-4_5.

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Peeples, Molly S., and Paul Martini. "Barstrength and Circumnuclear Dust Structure." In Mapping the Galaxy and Nearby Galaxies. Springer New York, 2008. http://dx.doi.org/10.1007/978-0-387-72768-4_106.

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Chiba, Masashi, Hirohito Hayashi, and Motoko Yamada. "Structure and Dynamics of the Old Galactic Components." In Mapping the Galaxy and Nearby Galaxies. Springer New York, 2008. http://dx.doi.org/10.1007/978-0-387-72768-4_8.

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Nishiyama, Shogo, Tetsuya Nagata, and Koji Sugitani. "Structure of the Galactic Bulge and Near Infrared Interstellar Extinction Law." In Mapping the Galaxy and Nearby Galaxies. Springer New York, 2008. http://dx.doi.org/10.1007/978-0-387-72768-4_101.

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Marshall, Douglas J., A. C. Robin, C. Reylé, et al. "Revealing the Three Dimensional Structure of the ISM in the Galaxy." In Mapping the Galaxy and Nearby Galaxies. Springer New York, 2008. http://dx.doi.org/10.1007/978-0-387-72768-4_85.

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Van Der Kruit, P. C. "Structure of Galaxies." In Astrophysics and Space Science Library. Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-0794-5_32.

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Carretero, Conrado, Ignacio Trujillo, and Santiago Patiri. "The Effect of Cosmological Large–scale Structure on the Orientation of Galaxies." In Mapping the Galaxy and Nearby Galaxies. Springer New York, 2008. http://dx.doi.org/10.1007/978-0-387-72768-4_49.

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Yee, H. K. C. "Properties of Galaxies and Galaxy Clusters Associated with Quasars." In Large Scale Structures of the Universe. Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2995-1_129.

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Yen, David Chien-Chang. "Structure, Evolution and Instability of a Self-gravitating Disk Subject to a Rapidly Rotating Bar." In Mapping the Galaxy and Nearby Galaxies. Springer New York, 2008. http://dx.doi.org/10.1007/978-0-387-72768-4_122.

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Yoshida, Naoki. "Structure of Galactic Dark Halos and Observational Prospects for Identifying the Nature of Dark Matter." In Mapping the Galaxy and Nearby Galaxies. Springer New York, 2008. http://dx.doi.org/10.1007/978-0-387-72768-4_44.

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Trabalhos de conferências sobre o assunto "Galaxie : structure"

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Milošević, Stanislav. "KINEMATICAL SIGNATURE OF DWARF GALAXY TIDAL DISRUPTION." In XIV Serbian-Bulgarian Astronomical Conference. Astronomical Observatory, 2024. http://dx.doi.org/10.69646/14sbac23a.

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We can observe stellar structures in a halo of the Milky Way and M31 galaxy (host galaxy). Some of these structures are formed in merger events with dwarf satellite galaxies. With observed velocities in these structures, we can probe different N-body models of dwarf galaxies and run simulations of merger events. In some cases, we can detect the remnant of the dwarf, but sometimes it seems fully disrupted, or it is in the region of the disk, and it is impossible to detect with available resolution. In this work, we investigated the kinematical properties of faint stellar structures and differen
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Silchenko, O. K. "Galaxies as open systems." In 51-st All-Russian with international participation student scientific conference "Physics of Space". Ural University Press, 2024. http://dx.doi.org/10.15826/b978-5-7996-3848-1.06.

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The galaxy evolution implies permanent change of its main parameters: size, structure, chemical composition of stars, the total stellar mass... Many galaxies proceed their evolution very smoothly. What governs the evolution of galaxies? If does a single physical factor exist which determines all these characteristics? Currently astronomers think that it exists. It is a steady outer cold gas inflow, and its rate and geometry define completely the evolutionary state of a galaxy in every moment of its evolution. To find a source of this outer cold gas is a quite actual problem, unsolved yet.
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Zasov, A., A. Saburova, and O. Egorov. "Sites of star formation in tidal structures." In ASTRONOMY AT THE EPOCH OF MULTIMESSENGER STUDIES. Proceedings of the VAK-2021 conference, Aug 23–28, 2021. Crossref, 2022. http://dx.doi.org/10.51194/vak2021.2022.1.1.172.

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Regions of young stars and emission gas in tidal structures of interacting galaxies are studied on the basis of observationscarried out (jointly with SAO RAS) at BTA telescope. Estimates of the line-of-sight velocities of gas and stars, the oxygenabundance of gas, and the age of stellar population were obtained. On the example of three systems - Arp 305, Arp 194,NGC 90 – we demonstrate the variety of star formation conditions and properties of emission regions outside the stellardisks. In the first two systems, tidal dwarf galaxies were formed. In NGC 90 we found HII regions projecting onto the
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Pannikkote, Meghana, Vaidehi S. Paliya, and D. J. Saikia. "UNVEILING GAMMA-RAY-EMITTING FR0 RADIO GALAXIES." In VI Conference on Active Galactic Nuclei and ravitational Lensing. Astronomical Observatory Belgrade, Volgina 7, 11060 Belgrade 38, Serbia, 2024. http://dx.doi.org/10.69646/aob24025.

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Fanaroff-Riley type 0 (FR0) radio galaxies are the latest entry in the jetted active galactic nuclei family. They are characterized by their compact radio morphology and similarities to host galaxy properties of FR I sources. We have recently identified, for the first time, seven gamma-ray emitting FR0s by leveraging the high-resolution radio and optical spectroscopic datasets provided by the ongoing wide-field sky surveys, e.g., the Very Large Array Sky Survey. The subsequent analysis of the multi-wavelength observations reveals the gamma rays to be produced by misaligned jets similar to more
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Du, Lun, Zhicong Lu, Yun Wang, Guojie Song, Yiming Wang, and Wei Chen. "Galaxy Network Embedding: A Hierarchical Community Structure Preserving Approach." In Twenty-Seventh International Joint Conference on Artificial Intelligence {IJCAI-18}. International Joint Conferences on Artificial Intelligence Organization, 2018. http://dx.doi.org/10.24963/ijcai.2018/287.

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Network embedding is a method of learning a low-dimensional vector representation of network vertices under the condition of preserving different types of network properties. Previous studies mainly focus on preserving structural information of vertices at a particular scale, like neighbor information or community information, but cannot preserve the hierarchical community structure, which would enable the network to be easily analyzed at various scales. Inspired by the hierarchical structure of galaxies, we propose the Galaxy Network Embedding (GNE) model, which formulates an optimization pro
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Zasov, A., A. Khoperskov, N. Zaitseva, and S. Khrapov. "When dwarf galaxies turn to be spiral?" In ASTRONOMY AT THE EPOCH OF MULTIMESSENGER STUDIES. Proceedings of the VAK-2021 conference, Aug 23–28, 2021. Crossref, 2022. http://dx.doi.org/10.51194/vak2021.2022.1.1.173.

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Spiral structure is rarely observed in dwarf galaxies because the formation of spiral arms requires special conditions. Weanalyze the sample of about 40 dS-galaxies found among the bright late-type galaxies with M B > −18 m and photometricdiameter D 25 < 12 kpc. These galaxies do not differ statistically from non-dS galaxies apart from the lower average gas (HI)fraction. To check the conditions of formation of spiral structure we carried out a series of direct N-body/hydrodynamicsimulations of dynamic evolution of low-mass stellar/gaseous discs varying the initial parameters of galaxies.
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Sheth, Ravi K., Mario Novello, and Santiago Perez. "Large Scale Structure and Galaxies." In COSMOLOGY AND GRAVITATION: XIII Brazilian School on Cosmology and Gravitation (XIII BSCG). AIP, 2009. http://dx.doi.org/10.1063/1.3151838.

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BUSARELLO, G., F. LA BARBERA, P. MERLUZZI, C. HAINES, A. MERCURIO, and M. CAPACCIOLI. "STRUCTURE AND EVOLUTION OF CLUSTER GALAXIES." In Proceedings of the International Conference. WORLD SCIENTIFIC, 2004. http://dx.doi.org/10.1142/9789812702999_0007.

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Fang, Li Zhi. "ORIGIN, STRUCTURE AND EVOLUTION OF GALAXIES." In Proceedings of the Yellow Mountain Summer School. WORLD SCIENTIFIC, 1988. http://dx.doi.org/10.1142/9789814542005.

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10

Makarov, D., S. Savchenko, A. Mosenkov, et al. "Catalog of edge-on galaxies using the Pan-STARRS1 survey data." In ASTRONOMY AT THE EPOCH OF MULTIMESSENGER STUDIES. Proceedings of the VAK-2021 conference, Aug 23–28, 2021. Crossref, 2022. http://dx.doi.org/10.51194/vak2021.2022.1.1.151.

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Resumo:
We have created a catalog of edge-on galaxies based on the publicly available DR2 data from the Pan-STARRS survey.The intensive use of an artificial neural network has significantly improved the quality of candidate selection. The catalogprovides homogeneous information on astrometry, photometry, and non-parametric morphological statistics for 16551 edge-on galaxies. Our catalog is intended for studying the three-dimensional structure of galaxies with different morphologiesand the scaling relations for disks and bulges.
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Relatórios de organizações sobre o assunto "Galaxie : structure"

1

Piacentine, J. Detection of Galaxy Clusters with the XMM-Newton Large Scale Structure Survey. Office of Scientific and Technical Information (OSTI), 2004. http://dx.doi.org/10.2172/833122.

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2

Keller, Christopher J. Analysis of Pacific Enroute Structure in Support of C-5M Super Galaxy. Defense Technical Information Center, 2015. http://dx.doi.org/10.21236/ada619564.

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3

Andersson, K. Complex Structure of Galaxy Cluster Abell 1689: Evidence for a Merger from X-Ray Data? Office of Scientific and Technical Information (OSTI), 2004. http://dx.doi.org/10.2172/826743.

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