Elliptical galaxy

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The giant elliptical galaxy ESO 325-4

An elliptical galaxy is a type of galaxy with an approximately ellipsoidal shape and a smooth, nearly featureless image. They are one of the three main classes of galaxy described by Edwin Hubble in his Hubble sequence and 1936 work The Realm of the Nebulae,[1] along with spiral and lenticular galaxies. Elliptical (E) galaxies are, together with lenticular galaxies (S0) with their large-scale disks, and ES galaxies[2][3][4] with their intermediate scale disks, a subset of the "early-type" galaxy population.

Most elliptical galaxies are composed of older, low-mass stars, with a sparse interstellar medium, and they tend to be surrounded by large numbers of globular clusters. Star formation activity in elliptical galaxies is typically minimal; they may, however, undergo brief periods of star formation when merging with other galaxies.[5] Elliptical galaxies are believed to make up approximately 10–15% of galaxies in the Virgo Supercluster, and they are not the dominant type of galaxy in the universe overall.[6] They are preferentially found close to the centers of galaxy clusters.[7]

Elliptical galaxies range in size from dwarf ellipticals with tens of millions of stars, to supergiants of over one hundred trillion stars that dominate their galaxy clusters. Originally, Edwin Hubble hypothesized that elliptical galaxies evolved into spiral galaxies, which was later discovered to be false,[8] although the accretion of gas and smaller galaxies may build a disk around a pre-existing ellipsoidal structure.[9][10] Stars found inside of elliptical galaxies are on average much older than stars found in spiral galaxies.[8]

Examples

General characteristics

Elliptical galaxy IC 2006[13]

Elliptical galaxies are characterized by several properties that make them distinct from other classes of galaxy. They are spherical or ovoid masses of stars, starved of star-making gases. Furthermore, there is very little

old stellar populations, giving them red colors. Large elliptical galaxies typically have an extensive system of globular clusters. They generally have two distinct populations of globular clusters: one that is redder and metal-rich, and another that is bluer and metal-poor.[14]

The galaxy located in the image is 4C 73.08, a giant elliptical galaxy.[15]

The dynamical properties of elliptical galaxies and the

Sersic's law, and a range of scaling relations between the elliptical galaxies' structural parameters unify the population.[16]

Every massive elliptical galaxy contains a supermassive black hole at its center. Observations of 46 elliptical galaxies, 20 classical bulges, and 22 pseudobulges show that each contain a black hole at the center.[17] The mass of the black hole is tightly correlated with the mass of the galaxy,[18] evidenced through correlations such as the M–sigma relation which relates the velocity dispersion of the surrounding stars to the mass of the black hole at the center.

Elliptical galaxies are preferentially found in

galaxy clusters and in compact groups of galaxies
.

Unlike flat spiral galaxies with organization and structure, elliptical galaxies are more three-dimensional, without much structure, and their stars are in somewhat random orbits around the center.

Sizes and shapes

Hercules A, a supergiant elliptical galaxy and also a radio galaxy. The radio lobes shown here in pink are over a million light-years across.

The

gravitational lensing
.

The Hubble classification of elliptical galaxies contains an integer that describes how elongated the galaxy image is. The classification is determined by the ratio of the major (a) to the minor (b) axes of the galaxy's isophotes:

Thus for a spherical galaxy with a equal to b, the number is 0, and the Hubble type is E0. While the limit in the literature is about E7, it has been known since 1966[2] that the E4 to E7 galaxies are misclassified lenticular galaxies with disks inclined at different angles to our line of sight. This has been confirmed through spectral observations revealing the rotation of their stellar disks.[21][22] Hubble recognized that his shape classification depends both on the intrinsic shape of the galaxy, as well as the angle with which the galaxy is observed. Hence, some galaxies with Hubble type E0 are actually elongated.

It is sometimes said that there are two physical types of ellipticals: the giant ellipticals with slightly "boxy"-shaped isophotes, whose shapes result from random motion which is greater in some directions than in others (anisotropic random motion); and the "disky" normal and

dwarf ellipticals, which contain disks.[23][24]
This is, however, an abuse of the nomenclature, as there are two types of early-type galaxy, those with disks and those without. Given the existence of ES galaxies with intermediate-scale disks, it is reasonable to expect that there is a continuity from E to ES, and onto the S0 galaxies with their large-scale stellar disks that dominate the light at large radii.

Dwarf spheroidal galaxies appear to be a distinct class: their properties are more similar to those of irregulars and late spiral-type galaxies.

At the large end of the elliptical spectrum, there is further division, beyond Hubble's classification. Beyond gE giant ellipticals, lies

D-galaxies and cD-galaxies
. These are similar to their smaller brethren, but more diffuse, with large haloes that may as much belong to the galaxy cluster within which they reside than the centrally-located giant galaxy.

NGC 3597 is the product of a collision between two galaxies. It is evolving into a giant elliptical galaxy.

Star formation

In recent years, evidence has shown that a reasonable proportion (~25%) of early-type (E, ES and S0) galaxies have residual gas reservoirs[25] and low-level star formation.[26]

Herschel Space Observatory researchers have speculated that the central black holes in elliptical galaxies keep the gas from cooling enough for star formation.[27]

See also

References

  1. OCLC 611263346. {{cite book}}: ISBN / Date incompatibility (help) Alt URL
    (pp. 124–151)
  2. ^ a b Liller, M.H. (1966), The Distribution of Intensity in Elliptical Galaxies of the Virgo Cluster. II
  3. ^ Nieto, J.-L. et al. (1988), More isotropic oblate rotators in elliptical galaxies
  4. ^ Graham, A.W. et al. (2016), Disky Elliptical Galaxies and the Allegedly Over-massive Black Hole in the Compact “ES“ Galaxy NGC 1271 (see their Fig.7).
  5. doi:10.1051/0004-6361/201936337
    .
  6. doi:10.1093/mnras/278.4.1025
    .
  7. doi:10.1086/157753
    .
  8. ^ a b John, D. (2006). Astronomy: The definitive guide to the universe. Bath, UK: Parragon Publishing., p. 224-225
  9. ^ Dekel, A., et al. (2009), Cold streams in early massive hot haloes as the main mode of galaxy formation
  10. ^ Stewart, Kyle R., et al. (2013), Angular Momentum Acquisition in Galaxy Halos
  11. S2CID 146068771
    .
  12. ^ Jeffrey, K. (10 April 2019). "These are the first pictures of a black hole — And that's a big, even supermassive, deal". Time. Retrieved 10 April 2019.
  13. ^ "Elliptical galaxy IC 2006". www.spacetelescope.org. ESA/Hubble. Retrieved 21 April 2015.
  14. S2CID 248853311
    .
  15. ^ [email protected]. "Galactic fireflies". www.esahubble.org. Retrieved 12 September 2024.
  16. ^ Graham, A.W. (2013), Elliptical and Disk Galaxy Structure and Modern Scaling Laws
  17. S2CID 118172025
    .
  18. ^ Graham, A.W. (2016), Galaxy Bulges and Their Massive Black Holes: A Review
  19. ^ Fraknoi, Andrew; Morrison, David; Wolf, Sidney C. (13 January 2017). Open Stax Astronomy. Retrieved 2 February 2017.
  20. ^ "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 8 May 2023.
  21. ^ Graham, A.W. et al. (1998), Extended stellar kinematics of elliptical galaxies in the Fornax cluster
  22. ^ Emsellem, E. (2011), The ATLAS3D project – III. A census of the stellar angular momentum within the effective radius of early-type galaxies: unveiling the distribution of fast and slow rotators
  23. ^ Pedraz, S. et al. (2002), Evidence of fast rotation in dwarf elliptical galaxies
  24. ^ Toloba, E. et al. (2015), Stellar Kinematics and Structural Properties of Virgo Cluster Dwarf Early-type Galaxies from the SMAKCED Project. III. Angular Momentum and Constraints on Formation Scenarios
  25. S2CID 119267988
    .
  26. S2CID 54764264
    .
  27. ^ "Red And Dead Galaxies Have Beating Black Hole 'Hearts', Preventing Star Formation | HNGN - Headlines & Global News". 27 February 2014. Retrieved 8 May 2023.

Further reading

  • Mo, Houjun; van den Bosch, Frank; White, Simon (June 2010), Galaxy Formation and Evolution (1 ed.),
    ISBN 978-0521857932
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