NGC 3109

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NGC 3109
NGC 3109 GALEX WikiSky.jpg
NGC 3109 by GALEX (ultraviolet)
Observation data (J2000 epoch)
Constellation Hydra
Right ascension 10h 03m 06.9s [1]
Declination −26° 09′ 34″ [1]
Redshift 403 ± 1 km/s [1]
Distance 1.333 ± 0.19  Mpc (4.348 ± 0.6197  Mly) [2] [3]
Apparent magnitude  (V)10.4 [1]
Characteristics
Type SB(s)m [1]
Size41,748  ly × 8,773.6 ly
(12.80  kpc × 2.69 kpc)
( diameter; ESO D25.5 B-band isophote) [4] [lower-alpha 1]
3,946  ly × 3,946 ly
(1.21  kpc × 1.21 kpc)
( diameter; 2MASS K-band total isophote) [4] [lower-alpha 1]
Apparent size  (V)19.1′ × 3.7′ [1]
Other designations
UGCA 194, PGC, 29128, [1] h 3221, GC 2003 [5]

NGC 3109 is a small barred Magellanic type spiral or irregular galaxy around 4.35 Mly away in the direction of the constellation of Hydra. NGC 3109 is believed to be tidally interacting with the dwarf elliptical galaxy Antlia Dwarf. [6] It was discovered by John Herschel on March 24, 1835 while he was in what is now South Africa. [5]

Contents

Size and morphology

NGC 3109 is classified as a Magellanic type irregular galaxy, [7] but it may in fact be a small spiral galaxy. Based on the D25.5 isophote at the B-band with an angular diameter of 1,980 arcseconds, it has an isophotal diameter approximately 12.80 kiloparsecs (41,700 light-years ) across, slightly larger than the Large Magellanic Cloud but smaller than the Triangulum Galaxy. [1] If it is a spiral galaxy, it would be the smallest in the Local Group. [8] NGC 3109 has a mass of about 2.3×109 times the mass of the Sun (M☉), of which 20% is in the form of neutral hydrogen. [9] It is oriented edge-on from our point of view, and may contain a disk and a halo. [8] The disk appears to be composed of stars of all ages, whereas the halo contains only very old and metal-poor stars. [10] NGC 3109 does not appear to possess a galactic nucleus. [9]

From measurements of the neutral atomic hydrogen in the galaxy, it has been found that the disk of NGC 3109 is warped. The warp has the same radial velocity as gas in the Antlia Dwarf galaxy, indicating that the two galaxies had a close encounter approximately one billion years ago. [11]

Composition

Based on spectroscopy of blue supergiants in NGC 3109, it is known that the galaxy has a low metallicity, similar to that to the Small Magellanic Cloud. [12] It is one of the most metal-poor star-forming galaxies in the Local group. [13] NGC 3109 seems to contain an unusually large number of planetary nebulae for its luminosity. [14] It also contains a substantial amount of dark matter. [15]

Location

NGC 3109 is located about 1.33 megaparsecs (4.3 Mly) away, in the constellation Hydra. This puts it at the very outskirts of the Local Group. [12] Its membership of the Local Group has been questioned, because it seems to be receding faster than estimates of the Local Group's escape velocity. [16] It is distant enough from the largest members of the Local Group that it has not been tidally influenced by them. [13]

Notes

  1. 1 2 The quoted diameters in this infobox was based on NED's provided scale of 0.0065 kpc/arcsec multiplied with the given angular diameters.

Related Research Articles

<span class="mw-page-title-main">Local Group</span> Group of galaxies that includes the Milky Way

The Local Group is the galaxy group that includes the Milky Way. It has a total diameter of roughly 3 megaparsecs (10 million light-years; 9×1019 kilometres), and a total mass of the order of 2×1012 solar masses (4×1042 kg). 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 (3×10^6 ly; 2×1019 km) and are moving toward one another with a velocity of 123 km/s. The group itself is a part of the larger Virgo Supercluster, which may be a part of the Laniakea Supercluster. The exact number of galaxies in the Local Group is unknown as some are occluded by the Milky Way; however, at least 80 members are known, most of which are dwarf galaxies.

<span class="mw-page-title-main">M81 Group</span> Galaxy group in Ursa Major and Camelopardalis

The M81 Group is a galaxy group in the constellations Ursa Major and Camelopardalis that includes the galaxies Messier 81 and Messier 82, as well as several other galaxies with high apparent brightnesses. The approximate center of the group is located at a distance of 3.6 Mpc, making it one of the nearest groups to the Local Group. The group is estimated to have a total mass of ×1012M☉. The M81 Group, the Local Group, and other nearby groups all lie within the Virgo Supercluster.

<span class="mw-page-title-main">Triangulum Galaxy</span> Spiral galaxy in the constellation Triangulum

The Triangulum Galaxy is a spiral galaxy 2.73 million light-years (ly) from Earth in the constellation Triangulum. It is catalogued as Messier 33 or NGC (New General Catalogue) 598. With the D25 isophotal diameter of 18.74 kiloparsecs (61,100 light-years), the Triangulum Galaxy is the third-largest member of the Local Group of galaxies, behind the Andromeda Galaxy and the Milky Way.

<span class="mw-page-title-main">NGC 404</span> Galaxy in the constellation Andromeda

NGC 404 is a field galaxy located about 10 million light years away in the constellation Andromeda. It was discovered by William Herschel in 1784, and is visible through small telescopes. NGC 404 lies just beyond the Local Group and does not appear gravitationally bound to it. It is located within 7 arc-minutes of second magnitude star Mirach, making it a difficult target to observe or photograph and granting it the nickname "Mirach's Ghost".

<span class="mw-page-title-main">Messier 94</span> Galaxy in the constellation Canes Venatici

Messier 94 is a spiral galaxy in the mid-northern constellation Canes Venatici. It was discovered by Pierre Méchain in 1781, and catalogued by Charles Messier two days later. Although some references describe M94 as a barred spiral galaxy, the "bar" structure appears to be more oval-shaped. The galaxy has two ring structures.

<span class="mw-page-title-main">Sculptor Galaxy</span> Intermediate spiral galaxy in the constellation Sculptor

The Sculptor Galaxy is an intermediate spiral galaxy in the constellation Sculptor. The Sculptor Galaxy is a starburst galaxy, which means that it is currently undergoing a period of intense star formation.

<span class="mw-page-title-main">NGC 1569</span> Galaxy in the constellation Camelopardalis

NGC 1569 is a dwarf irregular galaxy in Camelopardalis. The galaxy is relatively nearby and consequently, the Hubble Space Telescope can easily resolve the stars within the galaxy. The distance to the galaxy was previously believed to be only 2.4 Mpc. However, in 2008 scientists studying images from Hubble calculated the galaxy's distance at nearly 11 million light-years away, about 4 million light-years farther than previously thought, meaning it is a member of the IC 342 group of galaxies.

<span class="mw-page-title-main">Ursa Minor Dwarf</span> Dwarf spheroidal galaxy

The Ursa Minor Dwarf is a dwarf spheroidal galaxy, discovered by A.G. Wilson of the Lowell Observatory, in the United States, during the Palomar Sky Survey in 1955. It appears in the Ursa Minor constellation, and is a satellite galaxy of the Milky Way. The galaxy consists mainly of older stars and seems to house little to no ongoing star formation. Its centre is around 225,000 light years distant from Earth.

<span class="mw-page-title-main">NGC 6822</span> Galaxy in the constellation Sagittarius

NGC 6822 is a barred irregular galaxy approximately 1.6 million light-years away in the constellation Sagittarius. Part of the Local Group of galaxies, it was discovered by E. E. Barnard in 1884, with a six-inch refractor telescope. It is the closest non-satellite galaxy to the Milky Way, but lies just outside its virial radius. It is similar in structure and composition to the Small Magellanic Cloud. It is about 7,000 light-years in diameter.

<span class="mw-page-title-main">Satellite galaxy</span> Galaxy that orbits a larger galaxy due to gravitational attraction

A satellite galaxy is a smaller companion galaxy that travels on bound orbits within the gravitational potential of a more massive and luminous host galaxy. Satellite galaxies and their constituents are bound to their host galaxy, in the same way that planets within our own solar system are gravitationally bound to the Sun. While most satellite galaxies are dwarf galaxies, satellite galaxies of large galaxy clusters can be much more massive. The Milky Way is orbited by about fifty satellite galaxies, the largest of which is the Large Magellanic Cloud.

<span class="mw-page-title-main">NGC 7793</span> Galaxy in the constellation Sculptor

NGC 7793 is a flocculent spiral galaxy in the southern constellation of Sculptor. It was discovered in 1826 by Scottish astronomer James Dunlop. The galaxy is located at a distance of 12.2 million light years and is receding with a heliocentric radial velocity of 227 km/s. NGC 7793 is one of the five brightest galaxies within the Sculptor Group.

<span class="mw-page-title-main">NGC 4945</span> Galaxy in the constellation Centaurus

NGC 4945 (also known as Caldwell 83) is a barred spiral galaxy in the constellation Centaurus, visible near the star Xi Centauri. The galaxy was discovered by James Dunlop in 1826 and is thought to be similar to the Milky Way Galaxy, although X-ray observations show that NGC 4945 has an unusual energetic Seyfert 2 nucleus that might house a supermassive black hole. Around the nucleus of the galaxy, there is a dense disk of dust and gas, along with many dense star clusters. This object has an estimated mass of 1.4+1.4
−0.7×1011 M☉.

<span class="mw-page-title-main">NGC 2976</span> Galaxy in the constellation Ursa Major

NGC 2976 is a peculiar dwarf galaxy in the northern circumpolar constellation of Ursa Major. It was discovered by German-born astronomer William Herschel on November 8, 1801, and catalogued as H I.285. J. L. E. Dreyer described it as, "bright, very large, much extended 152°, star involved". It is a member of the M81 Group and lies 1° 20′ to the southwest of Messier 81. The projected separation of this galaxy from the M81 Group is 190 kpc.

<span class="mw-page-title-main">Dwarf spiral galaxy</span> Dwarf counterparts of spiral galaxies

A dwarf spiral galaxy is the dwarf version of a spiral galaxy. Dwarf galaxies are characterized as having low luminosities, small diameters, low surface brightnesses, and low hydrogen masses. The galaxies may be considered a subclass of low-surface-brightness galaxies.

<span class="mw-page-title-main">Sextans B</span> Dwarf irregular galaxy in the constellation Sextans

Sextans B is an irregular galaxy that may be part of the Local Group, or lie just beyond it. Sextans B is 4.44 million light-years away from Earth and thus is one of the most distant members of the Local Group, if it is indeed a member. It forms a pair with its neighbouring galaxy Sextans A. It is a type Ir IV–V galaxy according to the galaxy morphological classification scheme. Sextans B may also be gravitationally associated with the galaxies NGC 3109 and the Antlia Dwarf.

<span class="mw-page-title-main">Antlia Dwarf</span> Galaxy in the constellation Antlia

The Antlia Dwarf is a dwarf spheroidal/irregular galaxy. It lies about 1.3 Mpc from Earth in the constellation Antlia. It is the fourth and faintest member of the nearby Antlia-Sextans Group of galaxies. The galaxy contains stars of all ages, contains significant amounts of gas, and has experienced recent star formation. The Antlia Dwarf is believed to be tidally interacting with the small barred spiral galaxy NGC 3109.

<span class="mw-page-title-main">NGC 247</span> Galaxy in the constellation Cetus

NGC 247 is an intermediate spiral galaxy about 11.1 Mly away in the constellation Cetus. This distance was confirmed in late February 2011. Previous measurements showed that the galaxy was about 12.2 Mly away, but this was proved to be wrong. NGC 247 is a member of the Sculptor Group, and is 70 000 light years in diameter.

<span class="mw-page-title-main">NGC 4236</span> Galaxy in the constellation Draco

NGC 4236 is a barred spiral galaxy located in the constellation Draco.

<span class="mw-page-title-main">NGC 4449</span> Galaxy in the constellation Canes Venatici

NGC 4449, also known as Caldwell 21, is an irregular Magellanic type galaxy in the constellation Canes Venatici, being located about 13 million light-years away. It is part of the M94 Group or Canes Venatici I Group that is relatively close to the Local Group hosting our Milky Way galaxy.

<span class="mw-page-title-main">Antlia-Sextans Group</span> Galaxy group in the constellations of Hydra, Sextans, Antlia and Leo

The Antlia-Sextans Group is a small grouping of galaxies in the constellations Hydra, Sextans, Antlia and Leo. It is generally considered to be at the very edge of the Local Group and thus part of it. However, other researchers indicate it is an independent group, and thus the nearest group to the Local Group. It is, on average, approximately 4.3 million light-years away from the Milky Way.

References

  1. 1 2 3 4 5 6 7 8 "NASA/IPAC Extragalactic Database". Results for NGC 3109. Retrieved 2006-11-19.
  2. ↑ I. D. Karachentsev; V. E. Karachentseva; W. K. Hutchmeier; D. I. Makarov (2004). "A Catalog of Neighboring Galaxies". Astronomical Journal (abstract). 127 (4): 2031–2068. Bibcode:2004AJ....127.2031K. doi: 10.1086/382905 .
  3. ↑ Karachentsev, I. D.; Kashibadze, O. G. (2006). "Masses of the local group and of the M81 group estimated from distortions in the local velocity field". Astrophysics. 49 (1): 3–18. Bibcode:2006Ap.....49....3K. doi:10.1007/s10511-006-0002-6. S2CID   120973010.
  4. 1 2 "Detailed Information for Object NGC 3109". NASA/IPAC Extragalactic Database . Retrieved September 13, 2023.
  5. 1 2 Irregular Galaxy NGC 3109 Archived 2007-11-07 at the Wayback Machine
  6. ↑ Grebel, Gallagher, Harbeck, p.7
  7. ↑ Aparicio, Antonio; Artemio Herrero; F. Sánchez (1998). Stellar astrophysics for the local group: VIII Canary Islands Winter School. University of Cambridge. p. 286. ISBN   978-0-521-63255-3.
  8. 1 2 Sauvage, Marc; Grazyna Stasinska; Daniel Schaerer (2002). The evolution of galaxies: II—basic building blocks, Volume 2. Kluwer Academic Publishers. pp. 123, 124. ISBN   978-1-4020-0622-7.
  9. 1 2 van den bergh, Sidney (2000). The galaxies of the Local Group. University of Cambridge. p. 265. ISBN   978-0-521-65181-3.
  10. ↑ Hidalgo, Sebastian L.; et al. (2008). "The Disc-Halo Structure of NGC 3109". The Astronomical Journal . 136 (6): 2332–2342. Bibcode:2008AJ....136.2332H. doi: 10.1088/0004-6256/136/6/2332 .
  11. ↑ Barnes, D. G.; de Blok, W. J. G. (August 2001). "On the Neutral Gas Content and Environment of NGC 3109 and the Antlia Dwarf Galaxy". The Astronomical Journal . 122 (2): 825. arXiv: astro-ph/0107474 . Bibcode:2001AJ....122..825B. doi:10.1086/321170. S2CID   15734118.
  12. 1 2 Evans, Chris; et al. (2006). "The ARAUCARIA Project – First Observations of Blue Supergiants in NGC 3109" (PDF). The Messenger. 126: 5. Bibcode:2006Msngr.126....5E . Retrieved 2010-09-24.
  13. 1 2 Pena, M. "An interesting comparison between PNE and H II regions in NGC 3109 and NGC 6822" (PDF). Revista Mexicana de Astronomía y Astrofísica. 35: 74–75. Retrieved 2010-09-24.
  14. ↑ Richer, Michael G.; Marshall L. McCall (1992). "Planetary nebulae and H II regions in NGC 3109". The Astronomical Journal . 103: 54–59. Bibcode:1992AJ....103...54R. doi: 10.1086/116040 .
  15. ↑ Jobin, Marc; Carignan, Claude (1990). "The dark side of NGC 3109". The Astronomical Journal . 100 (3): 648–662. Bibcode:1990AJ....100..648J. doi: 10.1086/115548 .
  16. ↑ Plotner, Tammy (2009-05-18). "Turning the Tides – NGC 3109 by Ken Crawford". Universe Today . Retrieved 2010-09-24.

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