Concept

Disc galaxy

A disc galaxy (or disk galaxy) is a galaxy characterized by a galactic disc, a flattened circular volume of stars. These galaxies may or may not include a central non-disc-like region (a galactic bulge).

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https://en.wikipedia.org/wiki/Disc_galaxy

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Related courses (1)

PHYS-401: Astrophysics IV : stellar and galactic dynamics

The aim of this course is to acquire the basic knowledge on specific dynamical phenomena related to the origin, equilibrium, and evolution of star clusters, galaxies, and galaxy clusters. ...

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Potential Theory: Spherical Systems

Explores potential theory in spherical systems, including Nobel Prize-winning research on galactic centers.

Potential Theory: Axisymmetric Models for Disk Galaxies

Discusses potential theory and axisymmetric models for disk galaxies, focusing on mathematical tools and applications in astrophysics.

Galaxy Disk Models: Orbits and Potentials

Explores galaxy disk models, orbits, potentials, and circular velocity in disk galaxies.

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Official source

https://en.wikipedia.org/wiki/Disc_galaxy

About this result

Related courses (1)

PHYS-401: Astrophysics IV : stellar and galactic dynamics

The aim of this course is to acquire the basic knowledge on specific dynamical phenomena related to the origin, equilibrium, and evolution of star clusters, galaxies, and galaxy clusters. ...

Related lectures (11)

Potential Theory: Spherical Systems

Explores potential theory in spherical systems, including Nobel Prize-winning research on galactic centers.

Potential Theory: Axisymmetric Models for Disk Galaxies

Discusses potential theory and axisymmetric models for disk galaxies, focusing on mathematical tools and applications in astrophysics.

Galaxy Disk Models: Orbits and Potentials

Explores galaxy disk models, orbits, potentials, and circular velocity in disk galaxies.

Related publications (9)

Euclid Quick Data Release (Q1): XI. A first look at the fraction of bars in massive galaxies at z < 1★

Stellar bars are key structures in disc galaxies, driving angular momentum redistribution and influencing processes such as bulge growth and star formation. Quantifying the bar fraction as a function of redshift and stellar mass is therefore important for constraining the physical processes that drive disc formation and evolution across the history of the Universe. Leveraging the unprecedented resolution and survey area of the Euclid Q1 data release, combined with the Zoobot deep-learning model trained on c

2026

Euclid Quick Data Release (Q1): XXI. Active galactic nuclei identification using diffusion-based inpainting of Euclid VIS images

Light emission from galaxies exhibit diverse brightness profiles, influenced by factors such as galaxy type, structural features, and interactions with other galaxies. Elliptical galaxies feature more uniform light distributions, while spiral and irregular galaxies have complex, varied light profiles due to their structural heterogeneity and star-forming activity. In addition, galaxies with active galactic nuclei (AGN) feature intense, concentrated emission from gas accretion around supermassive black holes

2026

M 3D: Mosaicking M33 with MUSE datacubes I. Unveiling the diversity of H II regions in M33 with MUSE

We present new VLT/MUSE observations of a 3 × 8 arcmin2 mosaic along the southern major axis of the Local Group galaxy M33. These data provide an unprecedented view of the galaxy’s interstellar medium (ISM) and allow us to resolve ionised nebulae at a spatial scale of ≈5 pc. We identified and catalogued 131 H II regions, down to Hα luminosities of ≈5 × 1035 erg s−1, one order of magnitude fainter than previous surveys on nearby galaxies beyond the Local Group, and we compared these regions with the spatial

EDP Sciences2026

Related people (4)

Jean-Paul Richard Kneib

Expertise Cosmology, Gravitational Lensing, Redshift Survey, First Galaxies, Cluster of Galaxies, Fiber-positioner robotic system, Radio Astronomy, Space Sustainibility Current work

Former Principal investigator of the SDSS-IV eBOSS project. This is an international project assembling more than 150 participants located mainly in Europe, USA and China. This project will observe 1.5 million galaxy and quasars over 2014-2020 to accurately measure the expansion history of the Universe. * Member of the DESI co

Yves Revaz

Yves Revaz is a scientist at LASTRO/EPFL. After successful studies in physics at EPFL, he accomplished his PhD entitled: "Dynamics of external regions of spiral galaxies and constraints on the dark matter", at the Geneva Observatory in the galactic dynamics group of Prof. D. Pfenniger. He then moved to the Paris Observatory to work at the LERMA (Laboratory for Studies of Radiation and Matter in Astrophysics) under the supervision of Prof. F. Combes on the understanding of cooling flows in galaxy clusters. He joined LASTRO at EPFL in 2007, where, in collaboration with Pascale Jablonka, he developed a new TreePM/SPH chemo-dynamical code called GEAR, designed to study the chemical evolution of galaxies. His current main research focus on the evolution of dwarf spheroidal galaxies and their link with the cosmology. Yves Revaz is also the author of pNbody, a parallelized python toolbox designed to manipulate large N-body systems.

Robin Gopala Tress

Timothy Cohen

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Laboratory of Astrophysics

SCI SB PJ Group

ESC - Administration

Related concepts (5)

Milky Way

The Milky Way is the galaxy that includes the Solar System, with the name describing the galaxy's appearance from Earth: a hazy band of light seen in the night sky formed from stars that cannot be individually distinguished by the naked eye. The term Milky Way is a translation of the Latin via lactea, from the Greek γαλακτικὸς κύκλος (galaktikòs kýklos), meaning "milky circle". From Earth, the Milky Way appears as a band because its disk-shaped structure is viewed from within.

Hubble sequence

The Hubble sequence is a morphological classification scheme for galaxies published by Edwin Hubble in 1926. It is often colloquially known as the Hubble tuning-fork diagram because the shape in which it is traditionally represented resembles a tuning fork. It was invented by John Henry Reynolds and Sir James Jeans. The tuning fork scheme divided regular galaxies into three broad classes – ellipticals, lenticulars and spirals – based on their visual appearance (originally on photographic plates).

Galactic disc

A galactic disc (or galactic disk) is a component of disc galaxies, such as spiral galaxies, lenticular galaxies, and the Milky Way. Galactic discs consist of a stellar component (composed of most of the galaxy's stars) and a gaseous component (mostly composed of cool gas and dust). The stellar population of galactic discs tend to exhibit very little random motion with most of its stars undergoing nearly circular orbits about the galactic center.

Disc galaxy

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Euclid Quick Data Release (Q1): XI. A first look at the fraction of bars in massive galaxies at z < 1★

Euclid Quick Data Release (Q1): XXI. Active galactic nuclei identification using diffusion-based inpainting of Euclid VIS images

M 3D: Mosaicking M33 with MUSE datacubes I. Unveiling the diversity of H II regions in M33 with MUSE

Euclid Quick Data Release (Q1): XI. A first look at the fraction of bars in massive galaxies at z < 1★

Euclid Quick Data Release (Q1): XXI. Active galactic nuclei identification using diffusion-based inpainting of Euclid VIS images

M 3D: Mosaicking M33 with MUSE datacubes I. Unveiling the diversity of H II regions in M33 with MUSE

M 3D: Mosaicking M33 with MUSE datacubes I. Unveiling the diversity of H II regions in M33 with MUSE

M 3D: Mosaicking M33 with MUSE datacubes I. Unveiling the diversity of H II regions in M33 with MUSE