Galaxy morphological classification

Tuning-fork-style diagram of the Hubble sequence

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.

Hubble sequence

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):

The Hubble sequence throughout the universe's history.[3]

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).

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. Lenticular galaxies are placed between the ellipticals and the spirals, at the point where the two prongs meet the “handle”.

To this day, the Hubble sequence is the most commonly used system for classifying galaxies, both in professional astronomical research and in amateur astronomy.

De Vaucouleurs system

Hubble - de Vaucouleurs Galaxy Morphology Diagram
NGC 6782: a spiral galaxy (type SB(r)0/a) with three rings of different radii, as well as a bar.
NGC 7793: a spiral galaxy of type SA(s)d.
The Large Magellanic Cloud: a type SBm galaxy.

The de Vaucouleurs system for classifying galaxies is a widely used extension to the Hubble sequence, first described by Gérard de Vaucouleurs in 1959.[4] 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.[5]

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:

  • Bars. Galaxies are divided on the basis of the presence or absence of a nuclear bar. De Vaucouleurs introduced the notation SA to denote spiral galaxies without bars, complementing Hubble’s use of SB for barred spirals. He also allowed for an intermediate class, denoted SAB, containing weakly barred spirals.[6] Lenticular galaxies are also classified as unbarred (SA0) or barred (SB0), with the notation S0 reserved for those galaxies for which it is impossible to tell if a bar is present or not (usually because they are edge-on to the line-of-sight).
  • Rings. Galaxies are divided into those possessing ring-like structures (denoted ‘(r)’) and those without rings (denoted ‘(s)’). So-called ‘transition’ galaxies are given the symbol (rs).[6]
  • Spiral arms. As in Hubble’s original scheme, spiral galaxies are assigned to a class based primarily on the tightness of their spiral arms. The de Vaucouleurs scheme extends the arms of Hubble’s tuning fork to include several additional spiral classes:
    • Sd (SBd) - diffuse, broken arms made up of individual stellar clusters and nebulae; very faint central bulge
    • Sm (SBm) - irregular in appearance; no bulge component
    • Im - highly irregular galaxy
    Most galaxies in these three classes were classified as Irr I in Hubble’s original scheme. In addition, the Sd class contains some galaxies from Hubble’s Sc class. Galaxies in the classes Sm and Im are termed the “Magellanic” spirals and irregulars, respectively, after the Magellanic Clouds. The Large Magellanic Cloud is of type SBm, while the Small Magellanic Cloud is an irregular (Im).

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.[7]

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). 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).

Numerical Hubble stage
Hubble stage T −6 −5 −4 −3 −2 −1 0 1 2 3 4 5 6 7 8 9 10 11
de Vaucouleurs class[7] cE E E+ S0− S00 S0+ S0/a Sa Sab Sb Sbc Sc Scd Sd Sdm Sm Im
approximate Hubble class[8] E S0 S0/a Sa Sa-b Sb Sb-c Sc Sc-Irr Irr I

The use of numerical stages allows for more quantitative studies of galaxy morphology.

Yerkes (or Morgan) scheme

Created by American astronomer William Wilson Morgan. Together with Philip Keenan, Morgan 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.

Spectral Type Explanation
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 Shape Explanation
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.

See also

References

  1. ↑ Hubble, E. P. (1926). "Extra-galactic nebulae". Contributions from the Mount Wilson Observatory / Carnegie Institution of Washington. 324: 1–49. Bibcode:1926CMWCI.324....1H.
  2. ↑ Hubble, E. P. (1936). The Realm of the Nebulae. New Haven: Yale University Press. LCCN 36018182.
  3. ↑ "Hubble explores the origins of modern galaxies". ESA/Hubble Press Release. Retrieved 20 August 2013.
  4. ↑ De Vaucouleurs, G. (1959). "Classification and Morphology of External Galaxies". Handbuch der Physik. 53: 275. Bibcode:1959HDP....53..275D.
  5. ↑ Binney, J.; Merrifield, M. (1998). Galactic Astronomy. Princeton: Princeton University Press. ISBN 978-0-691-02565-0.
  6. 1 2 de Vaucouleurs, Gérard (April 1963). "Revised Classification of 1500 Bright Galaxies". Astrophysical Journal Supplement. 8: 31. Bibcode:1963ApJS....8...31D. doi:10.1086/190084.
  7. 1 2 De Vaucouleurs, G. (1994). "Global Physical Parameters of Galaxies" (PostScript). Retrieved 2008-01-02.
  8. ↑ Binney, J.; Merrifield, M. (1998). Galactic Astronomy. Princeton: Princeton University Press. ISBN 978-0-691-02565-0.
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