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The stellar structure of irregular galaxies. Face-on galaxies
Astronomy Reports, 2005Stellar photometry of nearby irregular galaxies of the Local Group is used to identify and study the young and old stellar populations of these galaxies. An analysis of the spatial distributions of stars of different ages in face-on galaxies shows that the young stellar populations in irregular galaxies are concentrated toward the center, and form ...
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The Spiral Structure of Galaxies
1995About two-thirds of all galaxies are spiral galaxies, and a large number of them, more than two-thirds, have a regular spiral structure with two arms that can be followed continuously from the centre of the galaxy (the central bulge) to the extremities of the disc.
Françoise Combes +3 more
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The Structure of Radio Galaxies
Annual Review of Astronomy and Astrophysics, 1966Discrete radio sources were discovered in large numbers in the late 1940's, but for several years it was an open question whether they were extragalactic objects or members of our Galaxy. The discovery, by Baade & Minkowski (1), of the optical counterpart of Cygnus A made it clear that the majority of the "radio stars" were in fact radio galaxies ...
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The Structure of Elliptical Galaxies
1988Recent imaging investigations highlight the structural diversity of elliptical galaxies. The distribution of light within the cores and envelopes shows a wide range in central and average system stellar densities at any galaxy luminosity. These variations appear to offer new information on galaxy formation mechanisms.
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The structure of elliptical galaxies and galaxy clusters
1995Thesis (Ph. D.)--Massachusetts Institute of Technology, Dept. of Physics, 1995. ; Includes bibliographical references. ; by David Augustin Buote. ; Ph.D.
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Highly accurate protein structure prediction with AlphaFold
Nature, 2021John Michael Jumper +2 more
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STRUCTURE AND EVOLUTION OF CLUSTER GALAXIES
Thinking, Observing and Mining the Universe, 2004Busarello G +5 more
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The Structure of Galaxy Clusters
1992I discuss both equilibrium and nonequilibrium methods for determining the masses of galaxy clusters, and point out the difficulties encountered when applying these methods to real optical and X—ray data. The best data sets now give quite precise determinations of the mass in the inner regions of relaxed clusters. The observed ratio of baryonic to total
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2005
Tracing the spiral structure of our Galaxy requires to identify and position the star-forming complexes. Each complex can be seen as a parental molecular cloud with associated ionised hydrogen, young stars and young clusters. The analysis of the ionised gas at Halpha wavelength (diffuse emission as well as discrete HII regions) is essential to ...
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Tracing the spiral structure of our Galaxy requires to identify and position the star-forming complexes. Each complex can be seen as a parental molecular cloud with associated ionised hydrogen, young stars and young clusters. The analysis of the ionised gas at Halpha wavelength (diffuse emission as well as discrete HII regions) is essential to ...
openaire +1 more source