Galaxy morphology /

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"Version: 202112"--Title page verso.Includes bibliographical references.1. Introduction -- 1.1. Earlier classifications -- 1.2. Hubble's tuning fork -- 1.3. The 90% rule -- 1.4. Assignments -- 1.5. Further reading2. Galaxy scale -- 2.1. Introduction -- 2.2. de Vaucouleurs profile -- 2.3. Exponential profile -- 2.4. S?ersic profile -- 2.5. Two-component galaxies -- 2.6. Vertical profiles -- 2.7. S?ersic profile with wavelength -- 2.8. Software packages -- 2.9. New S?ersic fitters -- 2.10. S?ersic classifying of galaxies -- 2.11. Assignments -- 2.12. Further reading3. 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 reading4. 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 reading5. 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 reading6. 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 reading7. 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 reading8. 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 reading9. 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. S?ersic Profile -- 9.7. Morphometrics -- 9.8. Assignments10. 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 reading11. Future outlook -- 11.1. Future observatories -- 11.2. Spectro-morphometric -- 11.3. Machine learning -- 11.4. Outlook.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.Researchers and graduate students working in the field of galaxy imaging/large scale galaxy surveys.Also available in print.Mode of access: World Wide Web.System requirements: Adobe Acrobat Reader, EPUB reader, or Kindle reader.Benne Holwerda is an associate professor at the University of Louisville, and is a leading expert in astronomical source catalogues and object characterization. He has worked on several projects that involve galaxy morphology classification and characterization; the Spitzer Survey of Spiral Structure in Galaxies, the Galaxy and Mass Assembly survey and the GHOSTS survey which explore extremes of low surface brightness. He authored the application of galaxy morphometrics on HI images.Title from PDF title page (viewed on January 18, 2022).

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Series Title

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Call Number

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Publisher

: .,

Collation

1 online resource (various pagings) :illustrations (some color).

Language

English

ISBN/ISSN

9780750334990

Classification

523.1/12

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-

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-

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Subject(s)

Galaxies & stars.
Galaxies
AAS: Galaxies and Cosmology.
Galaxies.

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Statement of Responsibility

B.W. Holwerda.

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