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Articoli di riviste sul tema "Structure and evolution of the Galaxy"

Autore: Grafiati

Pubblicato: 8 giugno 2024

Ultima modifica: 31 luglio 2025

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1

White, Simon. "The influence of halo evolution on galaxy structure." Proceedings of the International Astronomical Union 10, H16 (2012): 371. http://dx.doi.org/10.1017/s1743921314011430.

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AbstractIf Einstein-Newton gravity holds on galactic and larger scales, then current observations demonstrate that the stars and interstellar gas of a typical bright galaxy account for only a few percent of its total nonlinear mass. Dark matter makes up the rest and cannot be faint stars or any other baryonic form because it was already present and decoupled from the radiation plasma at z = 1000, long before any nonlinear object formed. The weak gravito-sonic waves so precisely measured by CMB observations are detected again at z = 4 as order unity fluctuations in intergalactic matter. These s

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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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Maartens, Roy, José Fonseca, Stefano Camera, Sheean Jolicoeur, Jan-Albert Viljoen, and Chris Clarkson. "Magnification and evolution biases in large-scale structure surveys." Journal of Cosmology and Astroparticle Physics 2021, no. 12 (2021): 009. http://dx.doi.org/10.1088/1475-7516/2021/12/009.

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Abstract Measurements of galaxy clustering in upcoming surveys such as those planned for the Euclid and Roman satellites, and the SKA Observatory, will be sensitive to distortions from lensing magnification and Doppler effects, beyond the standard redshift-space distortions. The amplitude of these contributions depends sensitively on magnification bias and evolution bias in the galaxy number density. Magnification bias quantifies the change in the observed number of galaxies gained or lost by lensing magnification, while evolution bias quantifies the physical change in the galaxy number densit

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4

Robin, A. C., C. Reylé, and D. Marshall. "Modelling the Galaxy from survey data." Proceedings of the International Astronomical Union 3, S248 (2007): 443–49. http://dx.doi.org/10.1017/s1743921308019789.

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AbstractRecent optical and near-infrared surveys have considerably improved our knowledge of galactic structure and galactic evolution. Two ways can be used to infer this knowledge from datasets: either inversing the data to get parameters describing the Galaxy, or using a synthetic approaches to test scenarios of formation and theoretical models for star and galaxy formation and evolution, both approaches being complementary. Using the synthetic approach the Besancon Galaxy model allows to test scenarios for the structure and evolution of the Galaxy by comparing simulations with the survey da

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5

Nagai, Daisuke, Monique Arnaud, Sarthak Dasadia, Michael McDonald, Ikuyuki Mitsuishi, and Andrea Morandi. "Cluster Physics & Evolution." Proceedings of the International Astronomical Union 11, A29B (2015): 70–78. http://dx.doi.org/10.1017/s1743921316004543.

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AbstractRecent advances in X-ray and microwave observations have provided unprecedented insights into the structure and evolution of the hot X-ray emitting plasma from their cores to the virialization region in outskirts of galaxy clusters. Recent Sunyaev-Zel'dovich (SZ) surveys (ACT, Planck, SPT) have provided new cluster catalogs, significantly expanding coverage of the mass-redshift plane, whileChandraandXMM-NewtonX-ray follow-up programs have improved our understanding of cluster physics and evolution as well as the surveys themselves. However, the current cluster-based cosmological constr

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6

Conselice, Christopher J. "The Evolution of Galaxy Structure Over Cosmic Time." Annual Review of Astronomy and Astrophysics 52, no. 1 (2014): 291–337. http://dx.doi.org/10.1146/annurev-astro-081913-040037.

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7

Gilmore, Gerard, and Rosemary F. G. Wyse. "Structure and Evolution of the Milky Way Galaxy." International Astronomical Union Colloquium 111 (1989): 83–102. http://dx.doi.org/10.1017/s0252921100011465.

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AbstractThe combination of chemical abundance, kinematic, and age data for stars near the sun provides important information about the early evolution of the Galaxy. We review available data, with some new analysis, to show that the sum of all available information strongly suggests that the extreme population II subdwarf system formed during a period of rapid collapse of the proto-Galaxy. This subdwarf system now forms a flattened, pressure-supported distribution, with axial ratio ∼2:1. The thick disk formed subsequent to the subdwarf system. At least the metal-poor tail of the thick disk is

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8

Gilmore, Gerard, and Rodrigo Ibata. "Large Scale Galactic Structure." International Astronomical Union Colloquium 148 (1995): 258–66. http://dx.doi.org/10.1017/s0252921100022004.

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AbstractModern models of Galaxy formation make fairly specific predictions which are amenable to detailed tests with galactic kinematic and chemical abundance data. For example, popular Cold Dark Matter models ‘predict’ growth of the Galaxy about a central core, which should contain the oldest stars. Later accretion of material forms the outer halo and the disks, while continuing accretion will continue to affect the kinematic structure of both the outer halo and the thin disk. This picture, which contains aspects of both the monolithic (‘ELS’) and the multifragment (‘Searle-Zinn’) pictures of

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9

Mazzei, P., A. Marino, R. Rampazzo, H. Plana, M. Rosado, and L. Arias. "Galaxy evolution in groups." Astronomy & Astrophysics 610 (February 2018): A8. http://dx.doi.org/10.1051/0004-6361/201731182.

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Context. Local Group (LG) analogs (LGAs) are galaxy associations dominated by a few bright spirals reminiscent of the LG. The NGC 3447/NGC 3447A system is a member of the LGG 225 group, a nearby LGA. This system is considered a physical pair composed of an intermediate-luminosity late-type spiral, NGC 3447 itself, and an irregular companion, NGC 3447A, linked by a faint, short filament of matter. A ring-like structure in the NGC 3447 outskirts has been emphasised by Galaxy Evolution Explorer (GALEX) observations. Aims. This work aims to contribute to the study of galaxy evolution in low-densit

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10

Keenan, Olivia C., Jonathan I. Davies, Rhys Taylor, and Robert F. Minchin. "The Structure of Halo Gas around M33." Proceedings of the International Astronomical Union 11, S321 (2016): 244–47. http://dx.doi.org/10.1017/s1743921316011455.

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AbstractUnderstanding the distribution of gas in and around galaxies is vital for our interpretation of galaxy formation and evolution. As part of the Arecibo Galaxy Environment Survey (AGES) we have observed the neutral hydrogen (HI) gas in and around the nearby Local Group galaxy M33 to a greater depth than previous observations. As part of this project we investigated the absence of optically detected dwarf galaxies in its neighbourhood, which is contrary to predictions of galaxy formation models. We observed 22 discrete clouds, 11 of which were previously undetected and none of which have

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11

Vesperini, Enrico. "Evolution of Globular Cluster Systems in Elliptical Galaxies." Symposium - International Astronomical Union 207 (2002): 664–72. http://dx.doi.org/10.1017/s0074180900224509.

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We study the evolution of the main properties of globular cluster systems in elliptical galaxies. In particular, we focus our attention on the evolution of the mass function of globular cluster systems (GCMF), on the fraction of surviving clusters and on the ratio of the final to initial total mass in clusters and we explore the dependence of these properties on the structure of the host galaxy and on the initial GCMF. We show that the observed universality of the GCMF parameters in galaxies with different structures can be reconciled with the effects of evolutionary processes and with the sig

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12

Linke, Laila, Patrick Simon, Peter Schneider, et al. "KiDS+VIKING+GAMA: Testing semi-analytic models of galaxy evolution with galaxy–galaxy–galaxy lensing." Astronomy & Astrophysics 640 (August 2020): A59. http://dx.doi.org/10.1051/0004-6361/202038355.

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Context. Several semi-analytic models (SAMs) try to explain how galaxies form, evolve, and interact inside the dark matter large-scale structure. These SAMs can be tested by comparing their predictions for galaxy–galaxy–galaxy lensing (G3L), which is weak gravitational lensing around galaxy pairs, with observations. Aims. We evaluate the SAMs by Henriques et al. (2015, MNRAS, 451, 2663, hereafter H15) and by Lagos et al. (2012, MNRAS, 426, 2142, hereafter L12), which were implemented in the Millennium Run, by comparing their predictions for G3L to observations at smaller scales than previous s

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13

Walton, Nicholas A., Janet E. Drew, Eduardo A. Gonzalez-Solares, Robert Greimel, Ella C. Hopewell, and Mike J. Irwin. "Mapping Galactic spiral arm structure: the IPHAS survey and Virtual Observatory access." Proceedings of the International Astronomical Union 2, no. 14 (2006): 595. http://dx.doi.org/10.1017/s1743921307011933.

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There is now considerable interest in how stellar streams in the Milky Way can be used to probe how the earlier merger history of our galaxy, which in turn can be related to hierarchical models of galaxy evolution.

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Javadi, Atefeh, and Jacco Th van Loon. "AGB population as probes of galaxy structure and evolution." Proceedings of the International Astronomical Union 14, S343 (2018): 283–90. http://dx.doi.org/10.1017/s1743921318006671.

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AbstractThe evolution of galaxies is driven by the birth and death of stars. AGB stars are at the end points of their evolution and therefore their luminosities directly reflect their birth mass; this enables us to reconstruct the star formation history. These cool stars also produce dust grains that play an important role in the temperature regulation of the interstellar medium (ISM), chemistry, and the formation of planets. These stars can be resolved in all of the nearby galaxies. Therefore, the Local Group of galaxies offers us a superb near-field cosmology site. Here we can reconstruct th

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15

Xu, Zeyue. "Galaxy formation and evolution." Theoretical and Natural Science 11, no. 1 (2023): 59–64. http://dx.doi.org/10.54254/2753-8818/11/20230381.

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Galaxies as the most important structures in the universe and Galaxy formation is a sequential redistribution process.The basic picture of galaxy formation was first proposed by White and Rees.The physical processes involved in galaxy formation are very numerous and complex. We know very little about most of these processes. Therefore, we can only describe them with a few empirical formulas. In this article the popular simulation techniques for galaxy formation are discussed in detail, based on the most recently observed cosmic star formation history. This study will focus mostly on the goals

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16

West, Michael J., Roberto De Propris, Maret Einasto, Z. L. Wen, and J. L. Han. "Evolution of Cluster Alignments as Evidence of Large-scale Structure Formation in the Universe." Astrophysical Journal Letters 987, no. 2 (2025): L24. https://doi.org/10.3847/2041-8213/ade66d.

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Abstract The Universe’s large-scale structure forms a vast, interconnected network of filaments, sheets, and voids known as the cosmic web. For decades, astronomers have observed that the orientations of neighboring galaxy clusters within these elongated structures are often aligned over separations of tens of Mpc. Using the largest available catalog of galaxy clusters, we show for the first time that cluster orientations are correlated over even larger scales—up to 200–300 comoving Mpc—and such alignments are seen to redshifts of at least z ≃ 1. Comparison with numerical simulations suggests

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17

Gerhard, Ortwin. "Perspectives on Galactic Structure." Proceedings of the International Astronomical Union 13, S336 (2017): 147. http://dx.doi.org/10.1017/s1743921317010286.

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The Milky Way is currently the subject of great observational effort. This includes both ESA's unique Gaia mission, as well as a multitude of ground-based surveys. Several of these are already returning data of unprecedented depth and quality for large numbers of Milky Way stars. These new data are likely to lead to a quantum step in our understanding of Milky Way structure and evolution. Because the new data will allow us to study our Galaxy at much greater resolution than possible in other galaxies, we also expect to greatly improve our understanding of disk galaxy formation in general.

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18

Feast, M. W. "Mira Variables, Stellar Evolution and Galactic Structure." International Astronomical Union Colloquium 111 (1989): 205–13. http://dx.doi.org/10.1017/s0252921100011532.

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The Mira variables make important contributions to four of the main problems under discussion at this meeting, (1) stellar pulsation, (2) stellar evolution, (3) the morphology and history of the Galaxy, (4) the comparative study of different galaxies. The Miras also show how these rather different fields of study overlap, so that it is no longer possible to deal with any one field in isolation.

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Tolasa, Diriba Gonfa. "Exploring the Formation, Dynamics, and Structure of Galaxy Clusters: A Comprehensive Analysis." Acceleron Aerospace Journal 4, no. 1 (2025): 831–46. https://doi.org/10.61359/11.2106-2503.

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This study explores the formation, structure, and dynamics of galaxy groups and clusters, highlighting their significance in the cosmic web. Galaxy clusters are massive, self-gravitating systems that display complex interactions influenced by dark matter and the intracluster medium (ICM). Recent advancements in X-ray and optical observations have significantly improved our understanding of the morphology and kinematics of these clusters, shedding light on the processes governing their evolution. The research employs the virial theorem to determine mass distributions and examines gravitational

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Lucatelli, Geferson, Fabricio Ferrari, Arianna Cortesi, et al. "Curvature of galaxy brightness profiles." Proceedings of the International Astronomical Union 15, S359 (2020): 444–45. http://dx.doi.org/10.1017/s1743921320002318.

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AbstractGalaxy morphologies reflect the shapes of galaxies and their structural components, such as bulges, discs, bars, spiral arms, etc. The detailed knowledge of the morphology of a galaxy provides understanding of the physics behind its evolution, since the time of its formation, including interaction processes and influence of the environment. Thus, the more precisely we can describe a galaxy structure, the more we may understand about its formation and evolution. We present a method that measures curvature, using images, to describe galaxy structure and to infer the morphology of each co

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Komossa, S., J. G. Baker, and F. K. Liu. "Growth of Supermassive Black Holes, Galaxy Mergers and Supermassive Binary Black Holes." Proceedings of the International Astronomical Union 11, A29B (2015): 292–98. http://dx.doi.org/10.1017/s1743921316005378.

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AbstractThe study of galaxy mergers and supermassive binary black holes (SMBBHs) is central to our understanding of the galaxy and black hole assembly and (co-)evolution at the epoch of structure formation and throughout cosmic history. Galaxy mergers are the sites of major accretion episodes, they power quasars, grow supermassive black holes (SMBHs), and drive SMBH-host scaling relations. The coalescing SMBBHs at their centers are the loudest sources of gravitational waves (GWs) in the Universe, and the subsequent GW recoil has a variety of potential astrophysical implications which are still

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22

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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Gouin, C., N. Aghanim, V. Bonjean, and M. Douspis. "Probing the azimuthal environment of galaxies around clusters." Astronomy & Astrophysics 635 (March 2020): A195. http://dx.doi.org/10.1051/0004-6361/201937218.

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Galaxy clusters are connected at their peripheries to the large-scale structures by cosmic filaments that funnel accreting material. These filamentary structures are studied to investigate both environment-driven galaxy evolution and structure formation and evolution. In the present work, we probe in a statistical manner the azimuthal distribution of galaxies around clusters as a function of the cluster-centric distance, cluster richness, and star-forming or passive galaxy activity. We performed a harmonic decomposition in large photometric galaxy catalogue around 6400 SDSS clusters with masse

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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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Porqueres, Natàlia, Jens Jasche, Torsten A. Enßlin, and Guilhem Lavaux. "Imprints of the large-scale structure on AGN formation and evolution." Astronomy & Astrophysics 612 (April 2018): A31. http://dx.doi.org/10.1051/0004-6361/201732141.

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Black hole masses are found to correlate with several global properties of their host galaxies, suggesting that black holes and galaxies have an intertwined evolution and that active galactic nuclei (AGN) have a significant impact on galaxy evolution. Since the large-scale environment can also affect AGN, this work studies how their formation and properties depend on the environment. We have used a reconstructed three-dimensional high-resolution density field obtained from a Bayesian large-scale structure reconstruction method applied to the 2M++ galaxy sample. A web-type classification relyin

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Bartelmann, Matthias, Klaus Dolag, and Harald Lesch. "The Evolution of Magnetic Fields in Galaxy Clusters." Symposium - International Astronomical Union 208 (2003): 189–98. http://dx.doi.org/10.1017/s0074180900207146.

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Cosmological simulations of magnetic fields in galaxy clusters show that remarkable agreement between simulations and observations of Faraday rotation and radio haloes can be achieved assuming that seed fields of ∼ 10−9 G were present at redshifts ∼ 15−20. The structure of the seed field is irrelevant for the final intracluster field. On average, the field grows exponentially with decreasing cluster redshift, but merger events cause steep transient increases in the field strength. Typical field-reversal scales are of order 50h−1kpc. In most cases, the intracluster fields are dynamically unimpo

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Martig, Marie, Frédéric Bournaud, and Romain Teyssier. "Numerical simulations of galaxy evolution in cosmological context." Proceedings of the International Astronomical Union 4, S254 (2008): 429–34. http://dx.doi.org/10.1017/s1743921308027920.

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AbstractLarge volume cosmological simulations succeed in reproducing the large-scale structure of the Universe. However, they lack resolution and may not take into account all relevant physical processes to test if the detail properties of galaxies can be explained by the CDM paradigm. On the other hand, galaxy-scale simulations could resolve this in a robust way but do not usually include a realistic cosmological context.To study galaxy evolution in cosmological context, we use a new method that consists in coupling cosmological simulations and galactic scale simulations. For this, we record

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Fujita, Yutaka, Keiichi Umetsu, Elena Rasia, et al. "The new fundamental plane dictating galaxy cluster evolution." Proceedings of the International Astronomical Union 15, S341 (2019): 271–72. http://dx.doi.org/10.1017/s1743921319001376.

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AbstractIn this study, we show that the characteristic radius rs, mass Ms, and the X-ray temperature, TX, of galaxy clusters form a thin plane in the space of (log rs, log Ms, log TX). This tight correlation indicates that the cluster structure including the temperature is affected by the formation time of individual clusters. Numerical simulations show that clusters move along the fundamental plane as they evolve. The plane and the cluster evolution within the plane can be explained by a similarity solution of structure formation. The angle of the plane shows that clusters have not achieved “

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Friedman-Shaw, Batia, Alex Krolewski, Matteo Foglieni, and Niayesh Afshordi. "Doppler bias: impact of peculiar velocities on color selection and the large scale structure of galaxy surveys." Journal of Cosmology and Astroparticle Physics 2025, no. 03 (2025): 059. https://doi.org/10.1088/1475-7516/2025/03/059.

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Abstract Lightcone selection effects on cosmic observables must be precisely accounted for in the next generation of surveys, including the Dark Energy Spectroscopic Instrument (DESI) survey. This will allow us to correctly model the data and extract subtle shifts from general-relativistic effects. We examine the effects of peculiar velocities on color selection in spectroscopic galaxy surveys, with a focus on their implications for the galaxy clustering dipole P 1(k). Using DESI Emission Line Galaxy (ELG) targets, we show that peculiar velocities can shift spectral emission features into or o

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Wenger, Trey V., Dana S. Balser, L. D. Anderson, and T. M. Bania. "Structure in the Milky Way." Proceedings of the International Astronomical Union 13, S334 (2017): 381–82. http://dx.doi.org/10.1017/s1743921317007578.

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AbstractThe morphological and chemical structure of the Milky Way today is an important constraint on models of the formation and evolution of the Galaxy. We use H ii regions, the sites of recent massive star formation, to probe both the Galactic spiral structure and the Galactic metallicity structure. H ii regions are the brightest objects in the Galaxy at radio wavelengths and are detected across the entire Galactic disk. We derive the distances to H ii regions using parallax measurements or by deriving kinematic distances. Here we summarize ongoing work to assess the accuracy of kinematic d

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Linke, Laila, Patrick Simon, Peter Schneider, and Stefan Hilbert. "Measuring galaxy-galaxy-galaxy-lensing with higher precision and accuracy." Astronomy & Astrophysics 634 (January 29, 2020): A13. http://dx.doi.org/10.1051/0004-6361/201936693.

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Context. Galaxy-galaxy-galaxy lensing (G3L) is a powerful tool for constraining the three-point correlation between the galaxy and matter distribution and thereby models of galaxy evolution. Aims. We propose three improvements to current measurements of G3L: (i) a weighting of lens galaxies according to their redshift difference, (ii) adaptive binning of the three-point correlation function, and (iii) accounting for the effect of lens magnification by the cosmic large-scale structure. Improvement (i) is designed to improve the precision of the G3L measurement, whereas improvements (ii) and (ii

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Quillen, Alice C., and Ivan Minchev. "Non-equilibrium Dynamical Processes in the Galaxy." Proceedings of the International Astronomical Union 5, H15 (2009): 178–79. http://dx.doi.org/10.1017/s1743921310008604.

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AbstractDynamical models have often necessarily assumed that the Galaxy is nearly steady state or dynamically relaxed. However observed structure in the stellar metallicity, spatial and velocity distributions imply that heating, mixing and radial migration has taken place. Better comprehension of non-equilibrium processes will allow us to not only better understand the current structure of the galaxy but its past evolution.

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Sjouwerman, Loránt O., Ylva M. Pihlström, Michael C. Stroh, et al. "BAaDE: The Bulge Asymmetries and Dynamical Evolution survey." Proceedings of the International Astronomical Union 14, S353 (2019): 45–46. http://dx.doi.org/10.1017/s1743921319008147.

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AbstractThe Bulge Asymmetries and Dynamical Evolution (BAaDE) survey aims to use circumstellar SiO maser line-of-sight velocities as probes for the Galactic gravitational potential and dynamical structure. The SiO masers are detected at a high rate in specific color-selected MSX infrared sources. Furthermore, the SiO maser properties and line ratios, in combination with infrared spectral energy distributions and location in the Galaxy, will statistically yield detailed information on population and evolution of low- to intermediate-mass evolved stars in the Galaxy.

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Anosova, J., and G. F. Benedict. "Dynamical Explorations of Nuclear Structures in Barred Galaxies." Symposium - International Astronomical Union 186 (1999): 348. http://dx.doi.org/10.1017/s0074180900112951.

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NGC 4314 (Benedict et al. 1996) has a complex nuclear morphology with recent star formation confined to a nuclear ring. HST observations resolve the nuclear ring into multiple sites of new star formation and resolve the associated dust lanes into discrete clouds. We construct dynamical models of this galaxy in order to provide plausible identification of the dynamical processes that led to the formation of the observed structure. We assume that the center of this galaxy contains a very massive double black-hole, surrounded by relatively low-mass particles - the star clusters as well as gas and

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Petersen, Michael S., Martin D. Weinberg, and Neal Katz. "Using commensurabilities and orbit structure to understand barred galaxy evolution." Monthly Notices of the Royal Astronomical Society 500, no. 1 (2020): 838–58. http://dx.doi.org/10.1093/mnras/staa3202.

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ABSTRACT We interpret simulations of secularly evolving disc galaxies through orbit morphology. Using a new algorithm that measures the volume of orbits in real space using a tessellation, we rapidly isolate commensurate (resonant) orbits. We identify phase-space regions occupied by different orbital families. Compared to spectral methods, the tessellation algorithm can identify resonant orbits within a few dynamical periods, crucial for understanding an evolving galaxy model. The flexible methodology accepts arbitrary potentials, enabling detailed descriptions of the orbital families. We appl

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Foëx, Gaël, Veronica Motta, Marceau Limousin, Tomas Verdugo, and Fabio Gastaldello. "Studying structure formation and evolution with strong-lensing galaxy groups." Proceedings of the International Astronomical Union 11, S308 (2014): 211–12. http://dx.doi.org/10.1017/s1743921316009881.

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AbstractWe present the analysis of a sample of strong-lensing galaxy group candidates. Our main findings are: confirmation of group-scale systems, complex light distributions, presence of large-scale structures in their surroundings, and evidence of a strong-lensing bias in the mass-concentration relation. We also report the detection of the first 'Bullet group'.

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Dolag, K., M. Bartelmann, and H. Lesch. "Evolution and structure of magnetic fields in simulated galaxy clusters." Astronomy & Astrophysics 387, no. 2 (2002): 383–95. http://dx.doi.org/10.1051/0004-6361:20020241.

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38

Nishida, M. T., and K. Wakamatsu. "Bar Destruction Mechanism by External Interactions." International Astronomical Union Colloquium 157 (1996): 366–68. http://dx.doi.org/10.1017/s025292110005003x.

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Abstract (sommario):

AbstractTo investigate bar destruction by a vertical head-on galaxy encounter, the dynamical evolution after the instantaneous momentum change of the impulsive approximation of a vertical head-on galaxy encounter, and the instability of finite amplitude one-armed perturbations to barred structure, are investigated by 2-dimensional N-body simulations.Preliminary results show that off-center vertical head-on collisions induce bar destruction but collisions in which the colliding galaxy passes through the very center of the target galaxy do not induce bar destruction.

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39

Papaderos, P. "Photometric Structure and Star Formation in Blue Compact Dwarf Galaxies." Proceedings of the International Astronomical Union 2, S235 (2006): 327. http://dx.doi.org/10.1017/s1743921306006922.

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Abstract (sommario):

The star-formation history and chemodynamical evolution of Blue Compact Dwarf (BCD) galaxies are central issues in dwarf galaxy research. In spite of being old in their vast majority, BCDs resemble in many aspects unevolved low-mass galaxies in the early universe. They are gas-rich (Hi mass fraction of typically > 30%) and metal-deficient (7.1 $\la$ 12+log(O/H) $\la$ 8.3) extragalactic systems, undergoing intense star-forming (SF) activity within an underlying low-surface brightness (LSB) host galaxy.

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40

Bobylev, V. V., and A. T. Bajkova. "Study of the structure and kinematics of the Galaxy based on data on classical Cepheids." Publications of the Pulkovo Observatory 228 (May 2023): 1–25. http://dx.doi.org/10.31725/0367-7966-2023-228-2.

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Abstract (sommario):

Classical Cepheids are important for studying the properties of the galactic disk, the spiral structure of the Galaxy, its rotation, evolution, etc. This article provides an overview of the main results of studying the structure and kinematics of the Galaxy, which were obtained by various scientific teams using classical Cepheids. The main attention is paid to the results of studying the Galaxy obtained by the authors of this work. The following issues are considered: a) the nature of the spatial distribution of Cepheids in the Galaxy, both near the equatorial plane of the Galaxy and in the ve

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41

Haud, U., M. Jôeveer, and J. Einasto. "A model of our Galaxy." Symposium - International Astronomical Union 106 (1985): 85–94. http://dx.doi.org/10.1017/s0074180900242113.

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Abstract (sommario):

The construction of models is the most effective tool for a synthesis of various observational data and for a quantitative study of physical and dynamical structure and evolution of stellar systems. Classical models of spiral galaxies were based on rotational velocities, which were identified with circular velocities. They were designed to represent the galactic attraction force in the radial direction.

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42

O'Hely, Eileen, Warrick J. Couch, Ian Smail, Alastair C. Edge, and Ann Zabludoff. "The Las Campanas/AAT Rich Cluster Survey." Publications of the Astronomical Society of Australia 15, no. 3 (1998): 273–79. http://dx.doi.org/10.1071/as98273.

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Abstract (sommario):

AbstractSome unsolved cosmological questions remain in relation to the formation of structure in the universe. One way of addressing such questions is to use rich galaxy clusters as tracers of the growth of large-scale structure. To date, studies of rich clusters of galaxies have concentrated on systems generally at either high redshift or in the local universe. The properties of clusters and their constituent galaxies at these extrema are becoming well understood. In particular, it is becoming clear that rich clusters have undergone considerable evolution both dynamically and in their galaxy

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43

Boulanger, François. "Structure and evolution of the Milky Way: the interstellar medium perspective." Proceedings of the International Astronomical Union 5, H15 (2009): 182–83. http://dx.doi.org/10.1017/s1743921310008628.

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Abstract (sommario):

AbstractThe Herschel and Planck satellites have started imaging the sky at far-IR to mm wavelengths with an unprecedented combination of sky and spectral coverage, angular resolution, and sensitivity, thus opening the last window of the electromagnetic spectrum on the Galaxy. Dedicated observing programs on Herschel and the Planck all-sky survey will provide the first complete view at cold dust across the Galaxy, opening new perspectives on the structure and dynamical evolution of the Milky Way relevant to Gaia. The analysis and modelling of these observations will contribute to our understand

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44

Murakami, I., and A. Babul. "Evolution of Dwarf Galaxies in High Pressure Environments." Symposium - International Astronomical Union 186 (1999): 483. http://dx.doi.org/10.1017/s0074180900113476.

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Abstract (sommario):

We use 2D hydrodynamical calculations to examine the effect of the external medium on evolution of supernova-driven outflows from dwarf galaxies. Babul & Rees (1992) have suggested a high external pressure may be able to prevent the outflows from escaping beyond the galaxy and that this material, as it cools and falls back into the galaxy, would serve as fuel for a second epoch of star formation. When thermal pressure is dominant, such evolution of the outflows is seen in our simulations and the gas falls back into the galaxy. Babul & Rees, however, did not take into account the possib

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45

Eskridge, P. B. "Dwarf Spheroidal Galaxies." Symposium - International Astronomical Union 161 (1994): 525–33. http://dx.doi.org/10.1017/s0074180900048026.

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Abstract (sommario):

Dwarf Spheroidal (dSph) galaxies are the faintest baryonic systems recognized as galaxies. Understanding the structure and stellar populations of these systems is critical for the modelling of their formation and evolution, and by extension, for understanding the general problem of galaxy formation and evolution. Further, as dSphs are the only available probes of the distant halo of the Galaxy, understanding their structure is a crucial step in the study of the gravitational potential of the halo and the mass of the Galaxy. I will not attempt to review fully all current topics of dSph research

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46

Kormendy, John. "Internal secular evolution in disk galaxies: the growth of pseudobulges." Proceedings of the International Astronomical Union 3, S245 (2007): 107–12. http://dx.doi.org/10.1017/s1743921308017407.

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Abstract (sommario):

AbstractObservational and theoretical evidence that internal, slow (“secular”) evolution reshapes galaxy disks is reviewed in Kormendy & Kennicutt (2004). This update has three aims. First, I emphasize that this evolution is very general – it is as fundamental to the evolution of galaxy disks as (e. g.) core collapse is to globular clusters, as the production of hot Jupiters is to the evolution of protoplanetary disks, and as evolution to red giants containing proto-white-dwarfs is to stellar evolution. One consequence for disk galaxies is the buildup of dense central components that get m

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47

Poezd, A., A. Shukurov, and D. D. Sokoloff. "Nonlinear Dynamo in a Disk Galaxy." Symposium - International Astronomical Union 157 (1993): 349–53. http://dx.doi.org/10.1017/s0074180900174406.

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Abstract (sommario):

A nonlinear thin-disk galactic dynamo model based on α-quenching is proposed. Assuming that the mean helicity depends on the magnetic field strength averaged across the disk, we derive a universal form of nonlinearity in the radial dynamo equation. We discuss the evolution of the regular magnetic field in the Milky Way and the Andromeda Nebula. It is argued that the reversals of the regular magnetic field in the Galaxy are a relic inherited from the structure of the seed field. We also briefly discuss the role of the turbulent diamagnetism and the effects of galactic evolution on the dynamo.

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48

Tolasa, Diriba. "The Interplay Between Supermassive Black Holes and Their Host Galaxies: A Multi-wavelength Approach." International Journal of Astrophysics and Space Science 13, no. 2 (2025): 36–48. https://doi.org/10.11648/j.ijass.20251302.12.

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Abstract (sommario):

The interplay between supermassive black holes (SMBHs) and their host galaxies is a critical area of research in extragalactic astronomy, shedding light on the fundamental processes that govern galaxy formation and evolution. This study employs a multi-wavelength approach to investigate the correlation between SMBHs and their host galaxies, utilizing data from radio, optical, infrared, and X-ray observations. Recent advancements in observational technologies have enabled deeper insights into the mechanisms at play in this complex relationship. We begin by examining the fundamental connection b

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49

Nasello, G., A. C. Robin, C. Reylé, and N. Lagarde. "Study of the thick disc of the Milky Way from a population synthesis model." Proceedings of the International Astronomical Union 13, S334 (2017): 347–48. http://dx.doi.org/10.1017/s1743921317006846.

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Abstract (sommario):

AbstractThe thick disc is a major component of the Milky Way but its epoch of formation and characteristics are still not yet well constrained. The Besançon Galaxy Model (BGM, Robin et al. 2003) is a population synthesis model based on a scenario of formation and evolution of the Galaxy, a star formation history, and a set of stellar evolution models. Thanks to Lagarde et al. (2017), new evolutionary tracks have been introduced into the Besancon Galaxy Model (STAREVOL, Lagarde et al. 2012) to provide global asteroseismic and surface chemical properties along the evolutionary stages. This updat

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50

Doi, Akihiro, Motoki Kino, Nozomu Kawakatu, and Kazuhiro Hada. "The radio-loud narrow-line Seyfert 1 galaxy 1H 0323+342 in a galaxy merger." Monthly Notices of the Royal Astronomical Society 496, no. 2 (2020): 1757–65. http://dx.doi.org/10.1093/mnras/staa1525.

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Abstract (sommario):

ABSTRACT The supermassive black holes (SMBHs) of narrow-line Seyfert 1 galaxies (NLS1s) are at the lower end of the mass function of active galactic nuclei (AGNs) and reside preferentially in late-type host galaxies with pseudobulges, which are thought to be formed by internal secular evolution. On the other hand, the population of radio-loud NLS1s presents a challenge for the relativistic jet paradigm, which states that powerful radio jets are associated exclusively with very high mass SMBHs in elliptical hosts, which are built up through galaxy mergers. We investigated distorted radio struct

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