NGC 5846

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NGC 5846
NGC5850 Galaxy from the Mount Lemmon SkyCenter Schulman Telescope courtesy Adam Block.jpg
NGC 5846 (right) and NGC 5850 (left) by the Schulman Telescope at Mount Lemmon SkyCenter
Observation data (J2000 epoch)
Constellation Virgo
Right ascension 15h 06m 29.3s [1]
Declination +01° 36′ 20″ [1]
Redshift 0.005711 ± 0.000017 [1]
Heliocentric radial velocity 1,712 ± 5 km/s [1]
Distance 93 ± 32 Mly (28.5 ± 9.8 Mpc) [1]
Apparent magnitude  (V)10.1 [2]
Characteristics
Type E0-1 [1]
Apparent size  (V)4′.1 × 3′.8
Notable featuresStrong X-ray source
Other designations
UGC 9706, CGCG 020-061, MCG +00-38-025, PGC 53932 [1]

NGC 5846 is an elliptical galaxy located in the constellation Virgo. It is located at a distance of circa 90 million light years from Earth, which, given its apparent dimensions, means that NGC 5846 is about 110,000 light years across. It was discovered by William Herschel on February 24, 1786. [3] It lies near 110 Virginis and is part of the Herschel 400 Catalogue. [4] It is a member of the NGC 5846 Group of galaxies, itself one of the Virgo III Groups strung out to the east of the Virgo Supercluster of galaxies. [5]

Contents

Characteristics

NGC 5846 is a giant elliptical galaxy with a round shape. It has a low luminosity active galactic nucleus, whose categorisation is ambiguous, having features that are observed both in LINER and HII regions. [6] The source of nuclear activity in galaxies is suggested to be a supermassive black hole that accretes material. NGC 5846 harbors a supermassive black hole with estimated mass (1.1±0.1)×109  M☉ based on the central velocity dispersion. [7] [8]

NGC 5846 harbors a large number of globular clusters; over 1,200 have been detected in images by Hubble Space Telescope. [9] The specific frequency is similar to other elliptical galaxies in groups. As has been observed in other large elliptical galaxies, the metallicity has bimodial distribution, with metallicities roughly of [Fe/H]=-1.2 and -0.2. [10] Their typical effective radii are in the range of 3 - 5 pc, with the largest clusters located in the central regions. Seven of the globular clusters have X-ray counterparts, which are among the most luminous X-ray sources in NGC 5846. These clusters are mostly in the central region and they are optically luminous, compact and belong to the red subpopulation. [11]

Chandra image of NGC 5846 with superimposed contours of Ha+[N ii] emission. White crosses mark the detected CO cloud positions. Chandra image of NGC 5846 with Ha+Nii contours.jpg
Chandra image of NGC 5846 with superimposed contours of Hα+[N ii] emission. White crosses mark the detected CO cloud positions.

The galaxy has complex X-ray morphology [13] that is considered to be the result of AGN outflows. Two inner bubbles in the hot gas, at a distance of 600 pc from the center and filled with radio emission, are clear indications of recent AGN feedback. A weak radio source, elongated in the NE–SW direction, connects the inner cavities. X-ray-bright rims surround the inner X-ray bubbles. [7] Many X-ray knots are visible, suggesting cooling sites. The scenario indicated by the Chandra observation is that of an AGN outflow, compressing and cooling the gas [14] in the central ~2 kpc (20" at the distance of NGC 5846). [12]

Hα observations [13] [15] [16] reveal the presence of warm ionized gas in the inner 2 kpc of NGC 5846. Spectra of this gas indicate irregular motion, with a typical velocity of 150–200 km s−1. The warm gas traces the X-ray-bright features, again suggesting a multiphase AGN outflow. [12] Using the Spitzer IRS [17] mid-infrared lines were detected (e.g., [Ne ii] 12.81 μm, [Ne iii] 15.55 μm) but no trace of polycyclic aromatic hydrocarbon (PAH) emission. Several sources are identified in the radio at 2.3, 5, and 15 GHz using VLBA data; these sources are aligned in the south–north direction. [18]

Recent Herschel PACS observations have detected the presence of [C ii]-emitting gas that extends to a radius of ~2 kpc and is centrally peaked. The [C ii] emission is almost exactly cospatial with the H-alpha +[N II] emission, and the total fluxes in [C ii] and H-alpha +[N II] have a ratio of 2.5, a very similar flux ratio value observed in other group-centered ellipticals. [16] Furthermore, the velocities inferred from the [C ii] line are consistent with those measured for the Hα line. [15] All of this evidence suggests that the [C ii] line is emitted by the warm gas, and it is not necessarily tracing the molecular phase. [12]

NGC 5846 has another indication that the cold gas is being disturbed by an AGN outburst. It has, in fact, an excess of cold (T ~ 30 K) dust approximately cospatial with the ionized and molecular gas. With a 70 μm luminosity of 3.5 × 1041 erg s−1, [19] NGC 5846 shares the same dust properties as several giant ellipticals (e.g., NGC 4636 and NGC 5044 [20] ), which are best explained with the ejection of dusty gas from their centers by AGN activity that occurred ~107 yr ago. [12]

Three CO clouds have been detected in NGC 5846. Clouds 1 and 3 are resolved in at least one direction by ALMA 12 m array observations and extend to 1"2 and 2"9, respectively, and are about 5"5 and 8"4 away (0.6 and 1.0 kpc) from the galaxy center, respectively. Cloud 3 is aligned almost exactly along a dust filament, while cloud 1 also coincides with small dust extinction structures. The elongation and potential bimodality of the surface brightness of cloud 3 of NGC 5846 could indicate that it might be composed of two nearby (in projection) clouds. Cloud 2 lies further away from the centre and is thought to originate from cooling in the wakes beneath buoyant X-ray cavities where compressions stimulate significant large-scale, coherent radiative cooling. [12]

Nearby galaxies

NGC 5846 forms a non-interacting pair with NGC 5846A, which lies 0.7 arcminutes from NGC 5846. [21] Its proximity to NGC 5846 and high surface brightness suggests it has been tidally stripped. [22] The barred spiral galaxy NGC 5850 lies at a projected distance of 10 arcminutes from NGC 5846 and may form an interacting pair with NGC 5846 based on its disturbed morphology. It is suggested that the two galaxies had a high speed encounter approximately 200 million years ago. [23]

NGC 5846 has a companion named NGC 5846-UDG1, an example of an ultra diffuse galaxy. Ultra-diffuse galaxies have higher proportions of globular clusters than other galaxies, but NGC 5846 is one of the most extreme, with about 13% of its luminosity coming from globular clusters. [24]

NGC 5846 is the foremost galaxy of the large galaxy group known as the NGC 5846 group. Other members of the group include NGC 5813, NGC 5831, NGC 5845, and NGC 5854. [25] The group has two subgroups, one centered around the elliptical NGC 5813 and the other around NGC 5846, lying at a projected separation of 600 kpc. [22] The group is part of the Virgo III Groups, a very obvious chain of galaxy groups on the left side of the Virgo cluster, stretching across 40 million light years of space. [26]

Related Research Articles

An active galactic nucleus (AGN) is a compact region at the center of a galaxy that emits a significant amount of energy across the electromagnetic spectrum, with characteristics indicating that this luminosity is not produced by the stars. Such excess, non-stellar emissions have been observed in the radio, microwave, infrared, optical, ultra-violet, X-ray and gamma ray wavebands. A galaxy hosting an AGN is called an active galaxy. The non-stellar radiation from an AGN is theorized to result from the accretion of matter by a supermassive black hole at the center of its host galaxy.

<span class="mw-page-title-main">Virgo Cluster</span> Galaxy cluster in the constellation Virgo

The Virgo Cluster is a large cluster of galaxies whose center is 53.8 ± 0.3 Mly away in the constellation Virgo. Comprising approximately 1,300 member galaxies, the cluster forms the heart of the larger Virgo Supercluster, of which the Local Group is a member. The Local Group actually experiences the mass of the Virgo Supercluster as the Virgocentric flow. It is estimated that the Virgo Cluster's mass is 1.2×1015M☉ out to 8 degrees of the cluster's center or a radius of about 2.2 Mpc.

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

The Sombrero Galaxy is a peculiar galaxy of unclear classification in the constellation borders of Virgo and Corvus, being about 9.55 megaparsecs from the Milky Way galaxy. It is a member of the Virgo II Groups, a series of galaxies and galaxy clusters strung out from the southern edge of the Virgo Supercluster. It has an isophotal diameter of approximately 29.09 to 32.32 kiloparsecs, making it slightly bigger in size than the Milky Way.

<span class="mw-page-title-main">Messier 84</span> Galaxy in the constellation Virgo

Messier 84 or M84, also known as NGC 4374, is a giant elliptical or lenticular galaxy in the constellation Virgo. Charles Messier discovered the object in 1781 in a systematic search for "nebulous objects" in the night sky. It is the 84th object in the Messier Catalogue and in the heavily populated core of the Virgo Cluster of galaxies, part of the local supercluster.

<span class="mw-page-title-main">Messier 89</span> Elliptical galaxy in the constellation Virgo

Messier 89 is an elliptical galaxy in the constellation Virgo. It was discovered by Charles Messier on March 18, 1781. M89 is a member of the Virgo Cluster of galaxies.

<span class="mw-page-title-main">NGC 3227</span> Galaxy in the constellation Leo

NGC 3227 is an intermediate spiral galaxy that is interacting with the dwarf elliptical galaxy NGC 3226. The two galaxies are one of several examples of a spiral with a dwarf elliptical companion that are listed in the Atlas of Peculiar Galaxies. Both galaxies may be found in the constellation Leo. It is a member of the NGC 3227 Group of galaxies, which is a member of the Leo II Groups, a series of galaxies and galaxy clusters strung out from the right edge of the Virgo Supercluster.

<span class="mw-page-title-main">NGC 3226</span> Dwarf elliptical galaxy in the constellation Leo

NGC 3226 is a dwarf elliptical galaxy that is interacting with the spiral galaxy NGC 3227. The two galaxies are one of several examples of a spiral with a dwarf elliptical companion that are listed in the Atlas of Peculiar Galaxies. Both galaxies may be found in the constellation Leo. It is a member of the NGC 3227 Group of galaxies, which is a member of the Leo II Groups, a series of galaxies and galaxy clusters strung out from the right edge of the Virgo Supercluster.

<span class="mw-page-title-main">Dorado Group</span> Galaxy cluster in the constellation Dorado

The Dorado Group is a loose concentration of galaxies containing both spirals and ellipticals. It is generally considered a 'galaxy group' but may approach the size of a 'galaxy cluster'. It lies primarily in the southern constellation Dorado and is one of the richest galaxy groups of the Southern Hemisphere. Gérard de Vaucouleurs was the first to identify it in 1975 as a large complex nebulae II in the Dorado region, designating it as G16.

<span class="mw-page-title-main">NGC 1404</span> Elliptical galaxy in the Fornax Cluster

NGC 1404 is an elliptical galaxy in the Southern constellation Eridanus. It was discovered on November 28, 1837, by the astronomer John Herschel. Based on the tip of the red-giant branch distance indicator, it lies at a distance of approximately 60 million light-years from the Milky Way. It is one of the brightest members of the Fornax Cluster.

<span class="mw-page-title-main">NGC 4478</span> Galaxy in the constellation of Virgo

NGC 4478 is an elliptical galaxy located about 50 million light-years away in the constellation Virgo. NGC 4478 was discovered by astronomer William Herschel on April 12, 1784. NGC 4478 is a member of the Virgo Cluster.

<span class="mw-page-title-main">Coma I</span> Galaxy cluster in constellation Coma Berenices

The Coma I Group is a group of galaxies located about 14.5 Mpc (47.3 Mly) away in the constellation Coma Berenices. The brightest member of the group is NGC 4725. The Coma I Group is rich in spiral galaxies while containing few elliptical and lenticular galaxies. Coma I lies in the foreground of the more distant Coma and Leo clusters and is located within the Virgo Supercluster.

<span class="mw-page-title-main">NGC 708</span> Galaxy in the constellation Andromeda

NGC 708 is an elliptical galaxy located 240 million light-years away in the constellation Andromeda and was discovered by astronomer William Herschel on September 21, 1786. It is classified as a cD galaxy and is the brightest member of Abell 262. NGC 708 is a weak FR I radio galaxy and is also classified as a type 2 Seyfert galaxy.

<span class="mw-page-title-main">NGC 720</span> Galaxy in the constellation Cetus

NGC 720 is an elliptical galaxy located in the constellation Cetus. It is located at a distance of circa 80 million light years from Earth, which, given its apparent dimensions, means that NGC 720 is about 110,000 light years across. It was discovered by William Herschel on October 3, 1785. The galaxy is included in the Herschel 400 Catalogue. It lies about three and a half degrees south and slightly east from zeta Ceti.

<span class="mw-page-title-main">NGC 4665</span> Galaxy in the constellation of Virgo

NGC 4665, also catalogued as NGC 4624 and NGC 4664, is a barred lenticular or spiral galaxy located in the constellation Virgo. It is a member of the Virgo II Groups, a series of galaxies and galaxy clusters strung out from the southern edge of the Virgo Supercluster. It is located at a distance of circa 60 million light years from Earth, which, given its apparent dimensions, means that NGC 4665 is about 75,000 light years across. NGC 4665 lies 2 and 3/4 degrees east-south east of Delta Virginis and 50 arcminutes southwest of 35 Virginis. It can be viewed through a moderately sized telescope with 23x magnification, forming a pair with an 11th magnitude star 1.5 arcminutes southwest. It is part of the Herschel 400 Catalogue.

<span class="mw-page-title-main">NGC 4636</span> Galaxy in the constellation Virgo

NGC 4636 is an elliptical galaxy located in the constellation Virgo. It is a member of the NGC 4753 Group of galaxies, which is a member of the Virgo II Groups, a series of galaxies and galaxy clusters strung out from the southern edge of the Virgo Supercluster. It is located at a distance of about 55 million light years from Earth, which, given its apparent dimensions, means that NGC 4636 is about 105,000 light years across.

<span class="mw-page-title-main">IC 1459</span> Elliptical galaxy in the constellation of Grus

IC 1459 is an elliptical galaxy located in the constellation Grus. It is located at a distance of circa 85 million light-years from Earth, which, given its apparent dimensions, means that IC 1459 is about 130,000 light-years across. It was discovered by Edward Emerson Barnard in 1892.

<span class="mw-page-title-main">NGC 4278</span> Galaxy in the constellation Coma Berenices

NGC 4278 is an elliptical galaxy located in the constellation Coma Berenices. It is located at a distance of circa 55 million light years from Earth, which, given its apparent dimensions, means that NGC 4278 is about 65,000 light years across. It was discovered by William Herschel on March 13, 1785. NGC 4278 is part of the Herschel 400 Catalogue and can be found about one and 3/4 of a degree northwest of Gamma Comae Berenices even with a small telescope.

<span class="mw-page-title-main">NGC 4302</span> Galaxy in the constellation Coma Berenices

NGC 4302 is an edge-on spiral galaxy located about 55 million light-years away in the constellation Coma Berenices. It was discovered by astronomer William Herschel on April 8, 1784 and is a member of the Virgo Cluster.

<span class="mw-page-title-main">NGC 4318</span> Galaxy in the constellation Virgo

NGC 4318 is a small lenticular galaxy located about 72 million light-years away in the constellation Virgo. It was discovered by astronomer John Herschel on January 18, 1828. NGC 4318 is a member of the Virgo W′ group, a group of galaxies in the background of the Virgo Cluster that is centered on the giant elliptical galaxy NGC 4365.

<span class="mw-page-title-main">NGC 4325</span> Galaxy

NGC 4325 is an elliptical galaxy located about 330 million light-years away in the constellation Virgo. It was discovered by astronomer Heinrich d'Arrest on April 15, 1865, who described it as "vF, vS, iR, nf of 2". Despite being listed in the Virgo Cluster catalog as VCC 616, it is not a member of the Virgo Cluster but instead a background galaxy.

References

  1. 1 2 3 4 5 6 7 "NASA/IPAC Extragalactic Database". Results for NGC 5846. Retrieved 2016-01-18.
  2. ↑ "Revised NGC Data for NGC 5846". spider.seds.org. Retrieved 25 November 2018.
  3. ↑ Seligman, Courtney. "NGC 5846 (= PGC 42734)". Celestial Atlas. Retrieved 19 November 2018.
  4. ↑ O'Meara, Steve (2007). Herschel 400 Observing Guide. Cambridge University Press. p. 205. ISBN   9780521858939.
  5. ↑ "The Virgo III Groups". Atlas of the Universe. Retrieved 2010-11-27.
  6. ↑ Ho, Luis C.; Filippenko, Alexei V.; Sargent, Wallace L. W.; Peng, Chien Y. (October 1997). "A Search for "Dwarf" Seyfert Nuclei. IV. Nuclei with Broad Hα Emission". The Astrophysical Journal Supplement Series. 112 (2): 391–414. arXiv: astro-ph/9704099 . Bibcode:1997ApJS..112..391H. doi:10.1086/313042. S2CID   15256980.
  7. 1 2 Machacek, Marie E.; Jerius, Diab; Kraft, Ralph; Forman, William R.; Jones, Christine; Randall, Scott; Giacintucci, Simona; Sun, Ming (10 December 2011). "Deep Chandra Observations of Edges and Bubbles in the NGC 5846 Galaxy Group". The Astrophysical Journal. 743 (1): 15. arXiv: 1108.5229 . Bibcode:2011ApJ...743...15M. doi:10.1088/0004-637X/743/1/15. S2CID   119239475.
  8. ↑ Hu, Jian (June 2008). "The black hole mass–stellar velocity dispersion correlation: bulges versus pseudo-bulges". Monthly Notices of the Royal Astronomical Society. 386 (4): 2242–2252. arXiv: 0801.1481 . Bibcode:2008MNRAS.386.2242H. doi: 10.1111/j.1365-2966.2008.13195.x . S2CID   10910326.
  9. ↑ Forbes, Duncan A.; Brodie, Jean P.; Huchra, John (December 1996). "Globular Cluster Luminosity Functions and the Hubble Constant from WFPC2 Imaging: The Dominant Group Elliptical NGC 5846". The Astronomical Journal. 112: 2448. arXiv: astro-ph/9611141 . Bibcode:1996AJ....112.2448F. doi:10.1086/118194. S2CID   14646588.
  10. ↑ Forbes, Duncan A.; Brodie, Jean P.; Huchra, John (March 1997). "Hubble Space Telescope Imaging of the Globular Cluster System Around NGC 5846". The Astronomical Journal. 113: 887. arXiv: astro-ph/9612172 . Bibcode:1997AJ....113..887F. doi:10.1086/118308. S2CID   119028977.
  11. ↑ Chies-Santos, A. L.; Pastoriza, M. G.; Santiago, B. X.; Forbes, D. A. (4 August 2006). "The globular cluster system of NGC 5846 revisited: colours, sizes and X-ray counterparts". Astronomy & Astrophysics. 455 (2): 453–459. arXiv: astro-ph/0604499 . Bibcode:2006A&A...455..453C. doi:10.1051/0004-6361:20054212. S2CID   14591501.
  12. 1 2 3 4 5 6 Temi, Pasquale; Amblard, Alexandre; Gitti, Myriam; Brighenti, Fabrizio; Gaspari, Massimo; Mathews, William G.; David, Laurence (27 April 2018). "ALMA Observations of Molecular Clouds in Three Group-centered Elliptical Galaxies: NGC 5846, NGC 4636, and NGC 5044". The Astrophysical Journal. 858 (1): 17. arXiv: 1711.10630 . Bibcode:2018ApJ...858...17T. doi: 10.3847/1538-4357/aab9b0 . S2CID   54062372. CC-BY icon.svg This article contains quotations from this source, which is available under the Creative Commons Attribution 3.0 Unported (CC BY 3.0) license.
  13. 1 2 Trinchieri, G.; Goudfrooij, P. (15 May 2002). "The peculiar small-scale X-ray morphology of NGC 5846 observed with Chandra". Astronomy & Astrophysics. 386 (2): 472–486. arXiv: astro-ph/0202416 . Bibcode:2002A&A...386..472T. doi:10.1051/0004-6361:20020311. S2CID   14880250.
  14. ↑ Brighenti, Fabrizio; Mathews, William G.; Temi, Pasquale (1 April 2015). "Hot Gaseous Atmospheres in Galaxy Groups and Clusters Are Both Heated and Cooled by X-Ray Cavities". The Astrophysical Journal. 802 (2): 118. arXiv: 1501.07647 . Bibcode:2015ApJ...802..118B. doi:10.1088/0004-637X/802/2/118. S2CID   119183888.
  15. 1 2 Caon, Nicola; Macchetto, Duccio; Pastoriza, Miriani (March 2000). "A Survey of the Interstellar Medium in Early-Type Galaxies. III. Stellar and Gas Kinematics". The Astrophysical Journal Supplement Series. 127 (1): 39–58. Bibcode:2000ApJS..127...39C. doi:10.1086/313315. hdl: 10183/109051 . S2CID   53492991.
  16. 1 2 Werner, N.; Oonk, J. B. R.; Sun, M.; Nulsen, P. E. J.; Allen, S. W.; Canning, R. E. A.; Simionescu, A.; Hoffer, A.; Connor, T.; Donahue, M.; Edge, A. C.; Fabian, A. C.; von der Linden, A.; Reynolds, C. S.; Ruszkowski, M. (11 April 2014). "The origin of cold gas in giant elliptical galaxies and its role in fuelling radio-mode AGN feedback". Monthly Notices of the Royal Astronomical Society. 439 (3): 2291–2306. arXiv: 1310.5450 . Bibcode:2014MNRAS.439.2291W. doi: 10.1093/mnras/stu006 . S2CID   53953986.
  17. ↑ Rampazzo, R.; Panuzzo, P.; Vega, O.; Marino, A.; Bressan, A.; Clemens, M. S. (11 June 2013). "A Spitzer–IRS spectroscopic atlas of early-type galaxies in the Revised Shapley–Ames Catalog". Monthly Notices of the Royal Astronomical Society. 432 (1): 374–403. arXiv: 1303.4584 . Bibcode:2013MNRAS.432..374R. doi: 10.1093/mnras/stt475 . S2CID   119266149.
  18. ↑ Filho, M. E.; Fraternali, F.; Markoff, S.; Nagar, N. M.; Barthel, P. D.; Ho, L. C.; Yuan, F. (9 April 2004). "Further clues to the nature of composite LINER/H II galaxies". Astronomy & Astrophysics. 418 (2): 429–443. arXiv: astro-ph/0401593 . Bibcode:2004A&A...418..429F. doi:10.1051/0004-6361:20034486. S2CID   21486526.
  19. ↑ Mathews, William G.; Temi, Pasquale; Brighenti, Fabrizio; Amblard, Alexandre (11 April 2013). "Variations of Mid- and Far-Infrared Luminosities Among Early-Type Galaxies: Relation to Stellar Metallicity and Cold Dust". The Astrophysical Journal. 768 (1): 28. arXiv: 1303.3350 . Bibcode:2013ApJ...768...28M. doi:10.1088/0004-637X/768/1/28. S2CID   118646459.
  20. ↑ Temi, Pasquale; Brighenti, Fabrizio; Mathews, William G. (September 2007). "Spitzer Observations of Transient, Extended Dust in Two Elliptical Galaxies: New Evidence of Recent Feedback Energy Release in Galactic Cores". The Astrophysical Journal. 666 (1): 222–230. arXiv: 0705.3710 . Bibcode:2007ApJ...666..222T. doi:10.1086/520123. S2CID   14440363.
  21. ↑ Sandage, A., Bedke, J. (1994), The Carnegie Atlas of Galaxies. Volume I, Carnegie Institution of Washington
  22. 1 2 Mahdavi, Andisheh; Trentham, Neil; Tully, R. Brent (October 2005). "The NGC 5846 Group: Dynamics and the Luminosity Function to MR = -12". The Astronomical Journal. 130 (4): 1502–1515. arXiv: astro-ph/0506737 . Bibcode:2005AJ....130.1502M. doi:10.1086/444560. S2CID   119085469.
  23. ↑ Higdon, James L.; Buta, Ronald J.; Purcell, Guy B. (January 1998). "An Optical and H [CSC]i[/CSC] Study of NGC 5850: Victim of a High-Speed Encounter?". The Astronomical Journal. 115 (1): 80–104. doi: 10.1086/300193 .
  24. ↑ Danieli, Shany; Van Dokkum, Pieter; Trujillo-Gomez, Sebastian; Kruijssen, J. M. Diederik; Romanowsky, Aaron J.; Carlsten, Scott; Shen, Zili; Li, Jiaxuan; Abraham, Roberto; Brodie, Jean; Conroy, Charlie; Gannon, Jonah S.; Greco, Johnny (2022). "NGC 5846-UDG1: A Galaxy Formed Mostly by Star Formation in Massive, Extremely Dense Clumps of Gas". The Astrophysical Journal Letters. 927 (2): L28. arXiv: 2111.14851 . Bibcode:2022ApJ...927L..28D. doi: 10.3847/2041-8213/ac590a . S2CID   244729821.
  25. ↑ Makarov, Dmitry; Karachentsev, Igor (21 April 2011). "Galaxy groups and clouds in the local (z∼ 0.01) Universe". Monthly Notices of the Royal Astronomical Society. 412 (4): 2498–2520. arXiv: 1011.6277 . Bibcode:2011MNRAS.412.2498M. doi: 10.1111/j.1365-2966.2010.18071.x . S2CID   119194025.
  26. ↑ "The Virgo III Groups". www.atlasoftheuniverse.com. Retrieved 9 January 2019.
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