UGC 10143

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UGC 10143
UGC10143HST.png
Hubble Space Telescope image of UGC 10143
Observation data (J2000 epoch)
Constellation Hercules
Right ascension 16h 02m 17.03s
Declination 15° 59' 59.94"
Redshift 0.03535
Heliocentric radial velocity 10410
Distance 537.2 million ly (164.71 million pc)
Group or cluster Abell 2147
Apparent magnitude  (B)14.9
Characteristics
Type cD
Mass 1.514 trillion  M☉
Size312,600 ly (95,830 pc)
Other designations
Z 108-73, Abell 2147 BCG, VV 159, Arp 324, LEDA 56784

UGC 10143 also known as Abell 2147 BCG, is a supergiant elliptical galaxy, luminous infrared galaxy, active galaxy, radio galaxy, and brightest cluster galaxy in the constellation of Hercules. [1] [2] The galaxy is 537 million light years (or 164,710,000 parsecs) away at a spectroscopic redshift of 0.03535. [1] [2] The galaxy has an apparent B magnitude of 14.9, and it can be observed both in the northern and southern hemispheres. [1] UGC 10143 is the brightest cluster galaxy of Abell 2147 [1] , which is a B-M class III galaxy cluster. The galaxy was discovered in 1959 by Boris Vorontsov-Velyaminov's catalogue of interacting galaxies. [3]

Contents

Characteristics

UGC 10143 is a large, massive supergiant elliptical galaxy in the galaxy cluster, Abell 2147. [1] The galaxy has a total diameter of 313,000 light years (or 95,830 parsecs), or roughly three times larger than the Milky Way. [2] The size was estimated using intermediate surface brightness (POSS1 103a-O) angular diameter of 2 arcmin, and a mean redshift-independent distance of 537 million light years away (or 164,710,000 parsecs). [2]

UGC 10143 is predicted to be extremely massive, having a dynamical stellar mass of 1.51 trillion M☉ (or 1012.18). [4] The galaxy is one of the most massive known in the universe, and is roughly seven times more massive than the stellar mass of the Milky Way. [4]

UGC 10143 is classified as a luminous infrared galaxy, due to the galaxy having an intrinsic K-band luminosity of 224 billion L☉ (or 1011.35). [5]

UGC 10143 has an estimated star-formation rate of 1.06 M☉, typical for low-star forming, and gas poor elliptical galaxies. [6]

The galactic center of UGC 10143 has a active galactic nucleus (also known as an AGN), which is a compact region at the center of a galaxy that is extremely luminous and energetic. [7] The active galactic nucleus is powered by an extremely massive, accreting ultramassive black hole (also referred as a UMBH) with a core-break radius derived mass of 26.3 billion M☉ (or 1010.42). [8] However, there are lower mass estimates for the central black hole of 891 million M☉, and 8.51 billion M☉, but these were calculated using velocity dispersion, and luminosity, which usually leads to underestimated masses.

UGC 10143 has a large population of over 35,000 globular clusters with their brightness, and metal contents measured, which was discovered using data from the Hubble Space Telescope in a survey of star clusters in brightest cluster galaxies. [9] The total mass of all of the 35,000 globular clusters is 5.13 billion M☉. [10]

UGC 10143 is interacting with two different galaxies designated Z 108-70, and Z 108-71. [3] These three galaxies were first noted to be interacting galaxies in 1959 in Boris Vorontsov-Velyaminov's catalogue of interacting galaxies. [3] These galaxies are also considered to be a chain of galaxies by Halton Arp in his atlas of peculiar galaxies. [11]

X-ray source

One x-ray source has been discovered in UGC 10143: 2CXO J160218.2+155912, which is classified as a ultraluminous x-ray source, and it was first found in 2022 in a survey of ULX candidates [12] The x-ray source has a total luminosity of 4 million L☉, equivalent to 1.535*1040 erg/s. [12]

Supernova

One supernova has been identified in UGC 10143: SN 2010ad was discovered at magnituide 16 on February 19, 2010 by the Lick Observatory. [13] It was classified as a weak hydrogen line Type II supernova (abbreviated as SNIIb), and is believed to be similar to other supernovae such as SN 1993J. [14] The progenitors of weak hydrogen line Type II supernovae are usually massive stars between 8 M☉ and 50 M☉, or interacting binary stars. (SN 2010ad may actually be hosted by the neighboring galaxy, Z 108-71 [15] ).

See also

References

  1. 1 2 3 4 5 "SIMBAD Results for UGC 10143". SIMBAD. Retrieved 2025-12-30.
  2. 1 2 3 4 "NED Results for UGC 10143". NASA/IPAC Extragalactic Database. Retrieved 2025-12-30.
  3. 1 2 3 Vorontsov-Velyaminov, B. A. (1959). "Atlas i Katalog Vzaimodejstvuûših Galakatik I." Atlas and Catalog of Interacting Galaxies. Bibcode:1959VV....C......0V . Retrieved 2025-12-31.
  4. 1 2 Mamon, Gary (2020). "The frequency of very young galaxies in the local Universe - II. The view from SDSS spectra". Monthly Notices of the Royal Astronomical Society. 492 (2): 1791. arXiv: 1912.06522 . Bibcode:2020MNRAS.492.1791M. doi: 10.1093/mnras/stz3556 .
  5. ↑ Tully, Brent (2015). "Galaxy Groups: A 2MASS Catalog". The Astronomical Journal. 149 (5): 171. arXiv: 1503.03134 . Bibcode:2015AJ....149..171T. doi:10.1088/0004-6256/149/5/171 . Retrieved 2025-12-31.
  6. ↑ Kovlakas, K. (2020). "A census of ultraluminous X-ray sources in the local Universe". Monthly Notices of the Royal Astronomical Society. 498 (4): 4790. arXiv: 2008.10572 . Bibcode:2020MNRAS.498.4790K. doi: 10.1093/mnras/staa2481 .
  7. ↑ Lin, Yen-Ting (2018). "An Analysis Framework for Understanding the Origin of Nuclear Activity in Low-power Radio Galaxies". The Astronomical Journal. 155 (5): 188. arXiv: 1803.02482 . Bibcode:2018AJ....155..188L. doi: 10.3847/1538-3881/aab5b4 .
  8. ↑ Dullo, Bililign (2019). "The Most Massive Galaxies with Large Depleted Cores: Structural Parameter Relations and Black Hole Masses". The Astrophysical Journal. 886 (2): 80. arXiv: 1910.10240 . Bibcode:2019ApJ...886...80D. doi: 10.3847/1538-4357/ab4d4f .
  9. ↑ "Hubble Captures Giant Elliptical in the Head of the Serpent". NASA/ESA. 13 May 2022. Retrieved 2025-12-31.
  10. ↑ Harris, William (2013). "A Catalog of Globular Cluster Systems: What Determines the Size of a Galaxy's Globular Cluster Population?". The Astrophysical Journal. 772 (2): 82. arXiv: 1306.2247 . Bibcode:2013ApJ...772...82H. doi:10.1088/0004-637X/772/2/82 . Retrieved 2025-12-31.
  11. ↑ Arp, Halton (1966). "Atlas of Peculiar Galaxies". The Astrophysical Journal Supplement Series. 14: 1. Bibcode:1966ApJS...14....1A. doi:10.1086/190147 . Retrieved 2025-12-30.
  12. 1 2 Walton, D. J. (2022). "A multimission catalogue of ultraluminous X-ray source candidates". Monthly Notices of the Royal Astronomical Society. 509 (2): 1587. arXiv: 2110.07625 . Bibcode:2022MNRAS.509.1587W. doi: 10.1093/mnras/stab3001 .
  13. ↑ "SN 2010ad". Transient Name Server. IAU . Retrieved 1 January 2026.
  14. ↑ Silverman, J. M. (2010). "Supernova 2010ad in UGC 10143". Central Bureau Electronic Telegrams (2177): 2. Bibcode:2010CBET.2177....2S . Retrieved 2025-12-31.
  15. ↑ "SIMBAD Results for SN 2010ad". SIMBAD. Retrieved 2026-01-02.
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