Galaxy morphological classification explained

Galaxy morphological classification is a system used by astronomers to divide galaxies into groups based on their visual appearance. There are several schemes in use by which galaxies can be classified according to their morphologies, the most famous being the Hubble sequence, devised by Edwin Hubble and later expanded by Gérard de Vaucouleurs and Allan Sandage. However, galaxy classification and morphology are now largely done using computational methods and physical morphology.

Hubble sequence

See main article: Hubble sequence.

The Hubble sequence is a morphological classification scheme for galaxies invented by Edwin Hubble in 1926.[1] [2] It is often known colloquially as the “Hubble tuning-fork” because of the shape in which it is traditionally represented. Hubble's scheme divides galaxies into three broad classes based on their visual appearance (originally on photographic plates):[3]

E=10 x \left(1-

b
a

\right)

These broad classes can be extended to enable finer distinctions of appearance and to encompass other types of galaxies, such as irregular galaxies, which have no obvious regular structure (either disk-like or ellipsoidal).[3]

The Hubble sequence is often represented in the form of a two-pronged fork, with the ellipticals on the left (with the degree of ellipticity increasing from left to right) and the barred and unbarred spirals forming the two parallel prongs of the fork on the right. Lenticular galaxies are placed between the ellipticals and the spirals, at the point where the two prongs meet the “handle”.[7]

To this day, the Hubble sequence is the most commonly used system for classifying galaxies, both in professional astronomical research and in amateur astronomy.[8] Nonetheless, in June 2019, citizen scientists through Galaxy Zoo reported that the usual Hubble classification, particularly concerning spiral galaxies, may not be supported, and may need updating.[9] [10]

De Vaucouleurs system

The de Vaucouleurs system for classifying galaxies is a widely used extension to the Hubble sequence, first described by Gérard de Vaucouleurs in 1959.[11] De Vaucouleurs argued that Hubble's two-dimensional classification of spiral galaxies—based on the tightness of the spiral arms and the presence or absence of a bar—did not adequately describe the full range of observed galaxy morphologies. In particular, he argued that rings and lenses are important structural components of spiral galaxies.[12]

The de Vaucouleurs system retains Hubble's basic division of galaxies into ellipticals, lenticulars, spirals and irregulars. To complement Hubble's scheme, de Vaucouleurs introduced a more elaborate classification system for spiral galaxies, based on three morphological characteristics:[13]

The different elements of the classification scheme are combined — in the order in which they are listed — to give the complete classification of a galaxy. For example, a weakly barred spiral galaxy with loosely wound arms and a ring is denoted SAB(r)c.

Visually, the de Vaucouleurs system can be represented as a three-dimensional version of Hubble's tuning fork, with stage (spiralness) on the x-axis, family (barredness) on the y-axis, and variety (ringedness) on the z-axis.[14]

Numerical Hubble stage

De Vaucouleurs also assigned numerical values to each class of galaxy in his scheme. Values of the numerical Hubble stage T run from −6 to +10, with negative numbers corresponding to early-type galaxies (ellipticals and lenticulars) and positive numbers to late types (spirals and irregulars).[15] Thus, as a rough rule, lower values of T correspond to a larger fraction of the stellar mass contained in a spheroid/bulge relative to the disk. The approximate mapping between the spheroid-to-total stellar mass ratio (MB/MT) and the Hubble stage is MB/MT=(10−T)2/256 based on local galaxies.[16]

Elliptical galaxies are divided into three 'stages': compact ellipticals (cE), normal ellipticals (E) and late types (E+). Lenticulars are similarly subdivided into early (S), intermediate (S0) and late (S+) types. Irregular galaxies can be of type magellanic irregulars (T = 10) or 'compact' (T = 11).

−6
−5−4−3−2−101234567891011
de Vaucouleurs classcEEE+S0S00S0+S0/aSaSabSbSbcScScdSdSdmSmIm
approximate Hubble class[17] ES0S0/aSaSa-bSbSb-cScSc-IrrIrr I
The use of numerical stages allows for more quantitative studies of galaxy morphology.

Yerkes (or Morgan) scheme

The Yerkes scheme was created by American astronomer William Wilson Morgan. Together with Philip Keenan, Morgan also developed the MK system for the classification of stars through their spectra. The Yerkes scheme uses the spectra of stars in the galaxy; the shape, real and apparent; and the degree of the central concentration to classify galaxies.[18]

Spectral TypeExplanation
a Prominent A stars
af Prominent A–F stars
f Prominent F stars
fg Prominent F–G stars
g Prominent G stars
gk Prominent G–K stars
k Prominent K stars
Galactic ShapeExplanation
B Barred spiral
D Rotational symmetry without pronounced spiral or elliptical structure
E Elliptical
Ep Elliptical with dust absorption
I Irregular
L Low surface brightness
N Small bright nucleus
S Spiral
Inclination Explanation
1 Galaxy is "face-on"
2
3
4
5
6
7 Galaxy is "edge-on"

Thus, for example, the Andromeda Galaxy is classified as kS5.[19]

References

  1. Hubble . E. P. . Edwin Hubble . 1926 . Extra-galactic nebulae . Contributions from the Mount Wilson Observatory / Carnegie Institution of Washington . 324 . 1–49. 1926CMWCI.324....1H .
  2. Book: Hubble, E. P. . Edwin Hubble . The Realm of the Nebulae . 1936 . . New Haven . 36018182.
  3. Web site: The Hubble tuning fork – classification of galaxies. www.spacetelescope.org. en. 2019-02-06.
  4. Book: Binney, James. Galactic Astronomy. Princeton University Press. 1998. 978-0-691-02565-0. Princeton.
  5. Web site: Elliptical Galaxy . COSMOS – The SAO Encyclopedia of Astronomy . 2020-09-19 .
  6. Web site: Lenticular Galaxies. cas.sdss.org. 2019-02-06.
  7. Web site: Galaxies. www.jb.man.ac.uk. 2019-02-06.
  8. Web site: THE HUBBLE SEQUENCE. Iafrate. G.. uni-heidelberg.de. 2019-02-06.
  9. News: Royal Astronomical Society . Citizen scientists re-tune Hubble's galaxy classification . 11 June 2019 . . 11 June 2019 . Royal Astronomical Society .
  10. Masters, Karen L.. et al. . Galaxy Zoo: unwinding the winding problem – observations of spiral bulge prominence and arm pitch angles suggest local spiral galaxies are winding . 30 April 2019 . . 487 . 2 . 1808–1820 . 10.1093/mnras/stz1153 . 1904.11436 . 2019MNRAS.487.1808M . 12 June 2019 . free .
  11. Book: De Vaucouleurs, G. . Classification and Morphology of External Galaxies . Gérard de Vaucouleurs. 1959 . Astrophysik IV: Sternsysteme / Astrophysics IV: Stellar Systems . Handbuch der Physik . Handbuch der Physik / Encyclopedia of Physics . 53 . 275–310. 10.1007/978-3-642-45932-0_7 . 1959HDP....53..275D . 978-3-642-45934-4 .
  12. Book: Binney, J. . James Binney . Merrifield, M. . Galactic Astronomy . 1998 . . Princeton . 978-0-691-02565-0.
  13. Web site: Galaxy – Types of galaxies. Encyclopedia Britannica. en. 2019-02-06.
  14. De Vaucouleurs . G. . Gérard de Vaucouleurs . 1994 . Global Physical Parameters of Galaxies . . Proceedings of "Quantifying Galaxy Morphology at High Redshift", A Workshop Held at the Space Telescope Science Institute, Baltimore MD, April 27-29 1994 . https://web.archive.org/web/20180817141814/http://www.stsci.edu/institute/conference/galaxy-morphology/devaucouleurs.ps . 2018-08-17 . 2008-01-02.
  15. Web site: Qualitative and Quantitative Classifications of Galaxies. ned.ipac.caltech.edu. 2019-02-06.
  16. Simulation of the Cosmic Evolution of Atomic and Molecular Hydrogen in Galaxies. The Astrophysical Journal. 698. 2. Equation (18). 0904.2221. 10.1088/0004-637X/698/2/1467. 2009. Obreschkow. D.. Croton. D.. De Lucia. G.. Khochfar. S.. Rawlings. S.. 2009ApJ...698.1467O. 204925243 .
  17. Book: Binney, J. . Merrifield, M. . Galactic Astronomy . 1998 . Princeton University Press . Princeton . 978-0-691-02565-0.
  18. Web site: The Yerkes Classification. ned.ipac.caltech.edu. 2019-02-06.
  19. Web site: galaxy classification. Darling. David. www.daviddarling.info. 2019-02-06.

External links