Local Group

The Local Group is the galaxy group that includes the Milky Way, where Earth is located. It consists of two collections of galaxies in a "dumbbell" shape; the Milky Way and its satellites form one lobe, and the Andromeda Galaxy and its satellites constitute the other. The two collections are separated by about 800 kiloparsecs (20,000,000,000,000,000,000 km) and are moving toward one another with a velocity of 123 km/s.^[8] The center of the group is located at about 450 kiloparsecs away from the Milky Way, placing it slightly closer to the Andromeda Galaxy by roughly 300 kiloparsecs, in which the latter may be more massive than the former in terms of mass.^[1]

The Local Group has a total mass of the order of 2e12 solar mass,^[9] and also a total diameter of 5.11 megaparsecs (160,000,000,000,000,000,000 kilometres) based on density matching and the potential surface of its parent structure, Local Sheet.^[3] It is itself a part of the Local Volume and the larger Virgo Supercluster, which is a part of the even greater Laniakea Supercluster along with the Pisces–Cetus Supercluster Complex. The exact number of galaxies in the Local Group is unknown, as the Milky Way obscures some; however, a current total of 134 members is known within 1 megaparsec from the center, most of which are dwarf galaxies.^[1] The Local Group was thought to have been more spread in the early universe with 7 megaparsecs (220,000,000,000,000,000,000 kilometres) by 700 million years after the Big Bang.^[10]

The two largest members, the Andromeda and the Milky Way galaxies, are both spiral galaxies with masses of about solar masses each. Each has its own system of satellite galaxies:

• The Andromeda Galaxy's satellite system consists of Messier 32 (M32), Messier 110 (M110), NGC 147, NGC 185, Andromeda I (And I), And II, And III, And V, And VI (also known as the Pegasus Dwarf Spheroidal Galaxy, or Pegasus dSph), And VII (a.k.a. the Cassiopeia Dwarf Galaxy), And VIII, And IX, And X, And XI, And XIX, And XXI and And XXII, plus several additional ultra-faint dwarf spheroidal galaxies.^[11]
• The Milky Way's satellite system comprises the Sagittarius Dwarf Galaxy, Large Magellanic Cloud, Small Magellanic Cloud, Canis Major Dwarf Galaxy (disputed, considered by some not a galaxy), Ursa Minor Dwarf Galaxy, Draco Dwarf Galaxy, Carina Dwarf Galaxy, Sextans Dwarf Galaxy, Sculptor Dwarf Galaxy, Fornax Dwarf Galaxy, Leo I (a dwarf galaxy), Leo II (a dwarf galaxy), Ursa Major I Dwarf Galaxy and Ursa Major II Dwarf Galaxy, plus several additional ultra-faint dwarf spheroidal galaxies.^[12]

The Triangulum Galaxy (M33) is the third-largest member of the Local Group, with a mass of approximately 5e10 solar mass, and is the third spiral galaxy.^[13] It is unclear whether the Triangulum Galaxy is a companion of the Andromeda Galaxy; the two galaxies are 750,000 light years apart,^[14] and experienced a close passage 2–4 billion years ago which triggered star formation across Andromeda's disk. The Pisces Dwarf Galaxy is equidistant from the Andromeda Galaxy and the Triangulum Galaxy, so it may be a satellite of either.^[15]

The other members of the group are likely gravitationally secluded from these large subgroups: IC 10, IC 1613, Phoenix Dwarf Galaxy, Leo A, Tucana Dwarf Galaxy, Cetus Dwarf Galaxy, Pegasus Dwarf Irregular Galaxy, Wolf–Lundmark–Melotte, Aquarius Dwarf Galaxy, and Sagittarius Dwarf Irregular Galaxy.^[16]

The membership of NGC 3109, with its companions Sextans A and the Antlia Dwarf Galaxy as well as Sextans B, Leo P, Antlia B and possibly Leo A, is uncertain due to extreme distances from the center of the Local Group.^[8] The Antlia-Sextans Group is unlikely to be gravitationally bound to the Local Group due to probably lying outside the Local Group's zero-velocity surface—which would make it a true galaxy group of its own rather than a subgroup within the Local Group.^[17] This possible independence may, however, disappear as the Milky Way continues coalescing with Andromeda due to the increased mass, and density thereof, plausibly widening the radius of the zero-velocity surface of the Local Group.

History

The term "The Local Group" was introduced by Edwin Hubble in Chapter VI of his 1936 book The Realm of the Nebulae.^[18] There, he described it as "a typical small group of nebulae which is isolated in the general field" and delineated, by decreasing luminosity, its members to be M31, Milky Way, M33, Large Magellanic Cloud, Small Magellanic Cloud, M32, NGC 205, NGC 6822, NGC 185, IC 1613 and NGC 147. He also identified IC 10 as a possible part of the Local Group.

Component galaxies

List

Structure

Streams

• Magellanic Stream, a stream of gas being stripped off the Magellanic Clouds due to their interaction with the Milky Way
• Monoceros Ring, a ring of stars around the Milky Way that is proposed to consist of a stellar stream torn from the Canis Major Dwarf Galaxy
• Virgo Stream, a stream formed from a dwarf galaxy.
• Helmi Stream

Future

The galaxies of the Local Group are likely to merge together under their own mutual gravitational attractions over a timescale of tens of billions of years into a single elliptical galaxy, with the coalescence of Andromeda and the Milky Way being the predominant event in this process.^[48] There is debate over whether ellipticity might be the immediate structure of the combined galaxy right after the collision or whether ellipticity might only emerge after a theoretical intermediate period of retaining a spiraling structure directly following the collision. Some even theorize a permanent superspiral or a transition toward a more lenticular galaxy, rather than a more elliptical or spiraled distribution, as the future of the Local Group's galactic merger.

Location

See also

• Galaxy cluster
• IC 342/Maffei Group, possibly the group of galaxies nearest to the Local Group
• List of galaxy groups and clusters
• Virgocentric flow

References

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Further reading

• Redd, Nola Taylor (18 December 2017). "Astronomers track dwarf galaxies to better understand the Milky Way's make-up and evolution". Proceedings of the National Academy of Sciences. 115 (51): 12836–12838. doi:10.1073/pnas.1817136115. PMC 6304947. PMID 30568025. S2CID 58645004

External links

• "The Local Group". www.messier.seds.org. Retrieved 12 March 2020.
• "Local Group Galaxies Survey". www2.lowell.edu. Retrieved 12 March 2020.
• van den Bergh, Sidney (2000). "Updated Information on the Local Group". The Publications of the Astronomical Society of the Pacific. 112 (770): 529–536. arXiv:astro-ph/0001040. Bibcode:2000PASP..112..529V. doi:10.1086/316548. S2CID 1805423
• Pritchet, Christopher J. & Van Den Bergh, Sidney (1999). "The Luminosity Distribution of Local Group Galaxies". The Astronomical Journal. 118 (2): 883–888. arXiv:astro-ph/9904250. Bibcode:1999AJ....118..883P. doi:10.1086/300977
• Teerikorpi, P. & Chernin, A. D. (2010). "The Hubble diagram for a system within dark energy: The location of the zero-gravity radius and the global Hubble rate". Astronomy and Astrophysics. 516: A93. arXiv:1006.0066. Bibcode:2010A&A...516A..93T. doi:10.1051/0004-6361/201014346