Local (astronomy)

In astronomy, Local is a term applied to an astronomical object or structure when it is close to an Earth observer, relative to its size. If the scale is large enough to make Earth's distance from the Sun immaterial, the relative closeness of the phenomenon to the star system of the Sun is considered instead.[1]

History

Hendrik C. van de Hulst in 1965 used the following table to describe local objects and structures on varying scales, and the local universe at given times:[1]

Object log size (cm) Beginning of scientific investigations (year A.C.)
Lecture room 3.0
Alpbach 5.5
Tirol 7.3
Austria 7.8
Europe 8.6 0
Earth 9.1 1500
Solar System 13.2 = 1 AU 1700
Local spiral arm 21.5 = 1000 parsecs 1850-1900
The galaxy 23.0 = 30 kpc
Local clusters of galaxies 24.5 = 3M-lightyears 1930
The universe 28.0 = 10G-lightyears

Updated terms

In the 21st century, the term "local" commonly applies to a list of astronomical groups on successively larger scales. Many of the entries correspond to the latter portion of van de Hulst's list, beyond the roughly two-light-year diameter of the Solar System. Some entries are based on a more detailed understanding of astronomical structures:[2]

  • The Local Interstellar Cloud containing the Solar System, roughly 30 light years across
  • The Local Bubble of gas in turn containing the Local Interstellar Cloud, 300-800 light years across
  • The Local Arm, a.k.a. the Orion-Cygnus Arm (of the Milky Way galaxy), 3,500 light years wide, and approximately 10,000 long
  • The Local Galaxy, the Milky Way, a lens or disc about 1,000 light years thick and 100,000 in diameter
  • The Local Group, the group of galaxies, roughly 53 in number, that contains the Milky Way, 10 million light-years across
  • The Extended Local Group, the Local Group, plus the Maffei (pronounced "mah-FYE-ee") and the Sculptor Group of galaxies.
  • The Local Supercluster or Virgo Supercluster, 110 million light-years across, contains the Virgo Cluster and the Extended Local Group.
  • The Local Filament, the Extended Local Group, plus the superstructures of galaxies known as the Coma-Supercluster and the Sculptor Wall, hundreds of millions of light years across.
    • The Local Filament is one boundary for the Local Void, 196 million light-years across, which forms a central frame of reference for numerous other superclusters, both inside and outside of the Local Filament.

A few years after scientific investigations of local clusters of galaxies began (1930), Edwin Hubble stated that knowledge of "galactic systems" such as the local group, a term Hubble had coined,[3] is sufficient for understanding the structure of all unobserved parts of the universe: "Thus, for purposes of speculation, we may apply the principal of uniformity, and suppose that any other equal portion of the universe, selected at random, is much the same as the observable region. We may assume that the realm of the nebulæ[a] is the universe and that the observable region is a fair sample.": p. 34 [3] This understanding of locality at the scale of galaxies was a restatement of the Cosmological Principle.

Hubble placed the scale at which the universe becomes homogeneous (same in any random location) and isotropic (same in any direction) at the limits of what telescopes of his day could see. Modern physical cosmology agrees with Hubble's statement but, since the advent of better telescopes, has differed on the size of the scale, placing it closer to around 100 Mpc (roughly 300 million light-years),[5] which is roughly at the scale of the local filament, the largest astronomical term to which has been commonly attached the word "local."

Note

  1. ^ The term nebulæ was understood in Hubble's time to mean galaxies, although the word 'galaxy' was often used to refer solely to the Milky Way.[4] The usage current at that time was analogous to the way our sun is referred to as the Sun, and other 'suns' are referred to as stars.

References

  1. ^ a b H.C. van de Hulst (1965). "Introduction to Astrophysics". In J.G. Emming (ed.). Electromagnetic Radiation in Space. Dordrecht, Holland: D. Reidel Publishing Company. pp. 1–2. Retrieved 27 December 2025.
  2. ^ Michel Marie Deza; Elena Deza (2014). "Distances in Earth Science and Astronomy". Encyclopedia of Distances, Third Edition. Springer-Verlag. pp. 559–560. ISBN 978-3-662-44342-2.
  3. ^ a b Edwin Hubble (1936). The Realm of the Nebulæ (PDF). Oxford University Press. pp. 124–151. Retrieved 3 January 2026.
  4. ^ Helge Kragh. (2024). "Nebulae or galaxies? The history of a change in astronomical terminology". Journal for the History of Astronomy. 55 (3): 287. doi:10.1177/00218286241238732.
  5. ^ Ivan Debono; George Smoot (2016-09-28). "General Relativity and Cosmology: Unsolved Questions and Future Directions". Universe. 2 (4): 17. arXiv:1609.09781. Bibcode:2016Univ....2...23D. doi:10.3390/universe2040023. ISSN 2218-1997.

See also

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