Galaxy morphology /

Galaxy morphology is a long-standing subfield of astronomy, moving from visual qualifications to quantitative morphometrics. This book covers the descriptions developed by astronomers to describe the appearance of galaxies, primarily in optical, ultraviolet and near-infrared wavelengths.

Detalles Bibliográficos
Clasificación:Libro Electrónico
Autor principal: Holwerda, B. W. (Autor)
Formato: Electrónico eBook
Idioma:Inglés
Publicado: Bristol [England] (Temple Circus, Temple Way, Bristol BS1 6HG, UK) : IOP Publishing, [2021]
Colección:IOP (Series). Release 22.
AAS-IOP astronomy. 2022 collection.
Temas:
Galaxies.
Galaxies > Classification.
Galaxies & stars.
AAS: Galaxies and Cosmology.
Acceso en línea:Texto completo
Tabla de Contenidos:
  • 1. Introduction
  • 1.1. Earlier classifications
  • 1.2. Hubble's tuning fork
  • 1.3. The 90% rule
  • 1.4. Assignments
  • 1.5. Further reading
  • 2. Galaxy scale
  • 2.1. Introduction
  • 2.2. de Vaucouleurs profile
  • 2.3. Exponential profile
  • 2.4. Sérsic profile
  • 2.5. Two-component galaxies
  • 2.6. Vertical profiles
  • 2.7. Sérsic profile with wavelength
  • 2.8. Software packages
  • 2.9. New Sérsic fitters
  • 2.10. Sérsic classifying of galaxies
  • 2.11. Assignments
  • 2.12. Further reading
  • 3. Galaxy sizes
  • 3.1. Photometric radii
  • 3.2. Effective radius
  • 3.3. Isomass radius (R1)
  • 3.4. Relating galaxy scales
  • 3.5. Assignments
  • 3.6. Further reading
  • 4. Sub-galaxy scale elements
  • 4.1. Bulges
  • 4.2. Bulge formation
  • 4.3. Spiral arms
  • 4.4. Bars
  • 4.5. Lenses
  • 4.6. Rings
  • 4.7. Lopsidedness
  • 4.8. Power spectra
  • 4.9. Stellar clusters
  • 4.10. Dust lanes
  • 4.11. Assignments
  • 4.12. Further reading
  • 5. Visual classifications
  • 5.1. Personal example
  • 5.2. Special features
  • 5.3. Radio zoo
  • 5.4. Clump scout
  • 5.5. Machine-aided crowds
  • 5.6. Assignments
  • 5.7. Further reading
  • 6. Galaxy morphometrics
  • 6.1. Cas
  • 6.2. Gini and M20
  • 6.3. Gini second order moment
  • 6.4. Patchiness
  • 6.5. MID statistics
  • 6.6. Implementation
  • 6.7. Uncertainties
  • 6.8. Caveats
  • 6.9. Orthogonalizing
  • 6.10. Morphometric uses
  • 6.11. Assignment
  • 6.12. Further reading
  • 7. Low surface brightness
  • 7.1. Observing LSB
  • 7.2. LSB from star counts
  • 7.3. The stellar halo
  • 7.4. Thick disks
  • 7.5. Disk breaks
  • 7.6. Disk warps
  • 7.7. XUV disks
  • 7.8. LSB dwarfs
  • 7.9. Assignments
  • 7.10. Further reading
  • 8. Kinematics and morphology
  • 8.1. Evolution : random to rotation to random
  • 8.2. Rotating disks
  • 8.3. Vertical stability
  • 8.4. Bars
  • 8.5. Bar kinematics
  • 8.6. Rings : resonances
  • 8.7. Spiral arms
  • 8.8. Tidal features
  • 8.9. Ellipticals versus disks
  • 8.10. Angular momentum
  • 8.11. Assignments
  • 8.12. Further reading
  • 9. Wavelength dependence
  • 9.1. Radio galaxies
  • 9.2. HI maps
  • 9.3. Sub-mm and mid-infrared
  • 9.4. Ultraviolet
  • 9.5. X-Ray
  • 9.6. Sérsic Profile
  • 9.7. Morphometrics
  • 9.8. Assignments
  • 10. Morphology Evolution
  • 10.1. Observed dependencies
  • 10.2. Morphology evolution
  • 10.3. Morphology evolution
  • 10.4. Mergers
  • 10.5. Galaxies in the universe
  • 10.6. Simulated galaxies
  • 10.7. Modern simulations
  • 10.8. Morpho-kinematics
  • 10.9. Assignments
  • 10.10. Further reading
  • 11. Future outlook
  • 11.1. Future observatories
  • 11.2. Spectro-morphometric
  • 11.3. Machine learning
  • 11.4. Outlook.

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