Wikipedia

Abell 1576 BCG

Abell 1576 BCG (short for Abell 1576 Brightest Cluster Galaxy) also known as PGC 2651193, is a supergiant elliptical galaxy and is the brightest cluster galaxy in Abell 1576, located in the constellation of Ursa Major. At a redshift of 0.300, the galaxy is about 3.8 billion light-years away from Earth.[1]

Abell 1576 Brightest Cluster Galaxy
Abell 1576 BCG, observed by SDSS
Observation data (J2000.0 epoch)
ConstellationUrsa Major
Right ascension12h 36m 58.73s
Declination+63d 11m 14.0s
Redshift0.300718
Heliocentric radial velocity90,153 km/s
Distance3.819 Gly (1170.9 Mpc)
Group or clusterAbell 1576
Apparent magnitude (V)0.039
Apparent magnitude (B)0.052
Surface brightness15.20
Characteristics
TypecD, db
Size1,077,000 ly
Other designations
PGC 2651193, WN B1234+6327, 2MASX J12365866+6311145, RX J1236.9+6311: [ZEH2003] 01

Characteristics

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Abell 1576 BCG is one of the largest galaxies to have a diameter exceeding one million light-years. A binary galaxy,[2] it is radio-loud compared to other galaxies with similar mass, with a stellar mass of ~5 × 1011Msolar, but has a rising magnitude value that is below 1011Msolar.[3]

Abell 1576 BCG is classified as a low-excitation radio galaxy with radio luminosity of 4 GHz between the ranges of 2 × 1023 and 3 × 1025 W Hz-1, showing a strong dependence on halo mass[4] and radio emission.[5] Located in the cool cluster within 0.035 r 500 of the peak of the X-ray emission,[6] the galaxy is known to exhibit enhanced ultraviolet (38%) and mid-infrared emission (43%) from 8 to 160 μm. Although having an old stellar population, this indicates Abell 1576 BCG has ongoing star formation activity[7] caused by high-density, X-ray-emitting intergalactic gas from its cluster core[8][9]

Abell 1576 BCG is also classified a cD galaxy containing an envelope of excess light profile described by the de Vaucouleurs surface brightness law, þ(r) ∞ r1/4, over a large range of radii,[10] associated with the cluster formation.[11] Compared to other elliptical galaxies inside galaxy clusters, Abell 1576 BCG has a lower relative peculiar velocity.[12]

Like all bright cluster galaxies, Abell 1576 BCG has a large stellar envelope.[13] This is thought to be formed through one or more galaxy mergers through galactic cannibalism.[14] As the galaxies collide with each other, the dynamical friction combined with tidal forces and orbital kinetic energy, is redistributed into random energy, allowing the galaxies to merge into an amorphous, triaxial system which resembles an elliptical galaxy like Abell 1576 BCG.[15][16] According to researchers, they found the central source of Abell 1576 BCG resolves into at least two components coincident with other optically detected galaxies, with the galaxy's jet-like extension feature extending toward the north-west.[17] This indicates the radio emission is of nuclear origin.[18]

Abell 1576

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The galaxy cluster where Abell 1576 BCG is residing, is known to be a rich cluster with a richness of R = 3 with a redshift of 0.302 (1' = 4.50 kpc)[17] observed by ROSAT.[19] It is considered massive (M500 > 5 × 1014 M⊙), with its mass profile shape ratio of M500 to M2500 and density masses contrasting 500 and 2500[20] as observed by Hubble SNAPshot surveys.[21]

The cluster is X-ray luminous with a luminosity value of LX [0.1-2.4 keV] > 5 x1044 erg s−1.[22][23] It also has an X-ray emitter with a flux above 1 x 10^13^ erg cm^-2^ s^-1^[24] and a declination of >−31 observed by the Extended GMRT Radio Halo Survey.[25] The cluster is also known to be relatively hot with temperatures reaching up 8.65 keV.[26]

According to researchers who found velocity dispersion estimated for 12 clusters in their gravitational lensing sample, they found a good agreement between the velocity dispersion estimates based on spectroscopy and on weak lensing. This was done through comparing the dynamical velocity dispersion estimate with the researchers' estimates of the velocity dispersions made from gravitational lensing via fitting a singular isothermal sphere profile to the observed tangential weak lensing distortion as a function of radius.[22]

Observations by Hubble Space Telescope, indicates the presence of jellyfish galaxies located at large distances from the cluster core of Abell 1576 (>400 kpc) due to ram-pressure stripping. This suggests they are triggered by the cluster mergers which is an interpretation supported by the disturbed dynamical state of many of the host clusters like Abell 1576.[27]

References

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  1. ^ "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 2024-06-12.
  2. ^ Struble, Mitchell F. (1988-11-01). "Position-Angle Statistics of the Brightest Binary Galaxies in Abell Clusters". The Astronomical Journal. 96: 1534. Bibcode:1988AJ.....96.1534S. doi:10.1086/114904. ISSN 0004-6256.
  3. ^ Best, P. N.; von der Linden, A.; Kauffmann, G.; Heckman, T. M.; Kaiser, C. R. (2007-08-01). "On the prevalence of radio-loud active galactic nuclei in brightest cluster galaxies: implications for AGN heating of cooling flows". Monthly Notices of the Royal Astronomical Society. 379 (3): 894–908. arXiv:astro-ph/0611197. Bibcode:2007MNRAS.379..894B. doi:10.1111/j.1365-2966.2007.11937.x. ISSN 0035-8711.
  4. ^ Lin, Yen-Ting; Huang, Hung-Jin; Chen, Yen-Chi (2018-05-01). "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. ISSN 0004-6256.
  5. ^ Yuan, Z. S.; Han, J. L.; Wen, Z. L. (2016-08-01). "Radio luminosity function of brightest cluster galaxies". Monthly Notices of the Royal Astronomical Society. 460 (4): 3669–3678. arXiv:1605.03387. Bibcode:2016MNRAS.460.3669Y. doi:10.1093/mnras/stw1125. ISSN 0035-8711.
  6. ^ Haarsma, Deborah B.; Leisman, Luke; Donahue, Megan; Bruch, Seth; Böhringer, Hans; Croston, Judith H.; Pratt, Gabriel W.; Voit, G. Mark; Arnaud, Monique; Pierini, Daniele (2010-04-01). "Brightest Cluster Galaxies and Core Gas Density in REXCESS Clusters". The Astrophysical Journal. 713 (2): 1037–1047. arXiv:0911.2798. Bibcode:2010ApJ...713.1037H. doi:10.1088/0004-637X/713/2/1037. ISSN 0004-637X.
  7. ^ Liu, F. S.; Mao, Shude; Meng, X. M. (2012-06-01). "Star formation activities in early-type brightest cluster galaxies". Monthly Notices of the Royal Astronomical Society. 423 (1): 422–436. arXiv:1203.1840. Bibcode:2012MNRAS.423..422L. doi:10.1111/j.1365-2966.2012.20886.x. ISSN 0035-8711.
  8. ^ Hoffer, Aaron S.; Donahue, Megan; Hicks, Amalia; Barthelemy, R. S. (2012-03-01). "Infrared and Ultraviolet Star Formation in Brightest Cluster Galaxies in the ACCEPT Sample". The Astrophysical Journal Supplement Series. 199 (1): 23. arXiv:1201.3373. Bibcode:2012ApJS..199...23H. doi:10.1088/0067-0049/199/1/23. ISSN 0067-0049.
  9. ^ O'Dea, Christopher P.; Baum, Stefi A.; Privon, George; Noel-Storr, Jacob; Quillen, Alice C.; Zufelt, Nicholas; Park, Jaehong; Edge, Alastair; Russell, Helen; Fabian, Andrew C.; Donahue, Megan; Sarazin, Craig L.; McNamara, Brian; Bregman, Joel N.; Egami, Eiichi (2008-07-01). "An Infrared Survey of Brightest Cluster Galaxies. II. Why are Some Brightest Cluster Galaxies Forming Stars?". The Astrophysical Journal. 681 (2): 1035–1045. arXiv:0803.1772. Bibcode:2008ApJ...681.1035O. doi:10.1086/588212. ISSN 0004-637X.
  10. ^ Kormendy, John; Djorgovski, S. (1989-01-01). "Surface photometry and the structure of elliptical galaxies". Annual Review of Astronomy and Astrophysics. 27: 235–277. Bibcode:1989ARA&A..27..235K. doi:10.1146/annurev.aa.27.090189.001315. ISSN 0066-4146.
  11. ^ Dubinski, John (1998-07-20). "The Origin of the Brightest Cluster Galaxies". The Astrophysical Journal. 502 (1): 141–149. arXiv:astro-ph/9709102. Bibcode:1998ApJ...502..141D. doi:10.1086/305901. ISSN 0004-637X.
  12. ^ Coziol, R.; Andernach, H.; Caretta, C. A.; Alamo-Martínez, K. A.; Tago, E. (2009-06-01). "The Dynamical State of Brightest Cluster Galaxies and The Formation of Clusters". The Astronomical Journal. 137 (6): 4795–4809. arXiv:0903.2360. Bibcode:2009AJ....137.4795C. doi:10.1088/0004-6256/137/6/4795. ISSN 0004-6256.
  13. ^ Durret, F.; Tarricq, Y.; Márquez, I.; Ashkar, H.; Adami, C. (2019-02-01). "Link between brightest cluster galaxy properties and large scale extensions of 38 DAFT/FADA and CLASH clusters in the redshift range 0.2 < z < 0.9". Astronomy & Astrophysics. 622: A78. arXiv:1812.03672. Bibcode:2019A&A...622A..78D. doi:10.1051/0004-6361/201834374. ISSN 0004-6361.
  14. ^ De Lucia, Gabriella; Blaizot, Jérémy (2007-02-01). "The hierarchical formation of the brightest cluster galaxies". Monthly Notices of the Royal Astronomical Society. 375 (1): 2–14. arXiv:astro-ph/0606519. Bibcode:2007MNRAS.375....2D. doi:10.1111/j.1365-2966.2006.11287.x. ISSN 0035-8711.
  15. ^ Barnes, Joshua E. (1988-08-01). "Encounters of Disk/Halo Galaxies". The Astrophysical Journal. 331: 699. Bibcode:1988ApJ...331..699B. doi:10.1086/166593. ISSN 0004-637X.
  16. ^ Hernquist, Lars (1992-12-01). "Structure of Merger Remnants. I. Bulgeless Progenitors". The Astrophysical Journal. 400: 460. Bibcode:1992ApJ...400..460H. doi:10.1086/172009. ISSN 0004-637X.
  17. ^ a b Kale, R.; Venturi, T.; Giacintucci, S.; Dallacasa, D.; Cassano, R.; Brunetti, G.; Macario, G.; Athreya, R. (September 2013). "The Extended GMRT Radio Halo Survey". Astronomy & Astrophysics. 557: A99. arXiv:1306.3102. doi:10.1051/0004-6361/201321515. ISSN 0004-6361.
  18. ^ Kale, R.; Venturi, T.; Cassano, R.; Giacintucci, S.; Bardelli, S.; Dallacasa, D.; Zucca, E. (2015-08-26). "Brightest cluster galaxies in the extended GMRT radio halo cluster sample". Astronomy & Astrophysics. 581: A23. arXiv:1506.05612. doi:10.1051/0004-6361/201526341. ISSN 0004-6361.
  19. ^ David, Laurence P.; Forman, William; Jones, Christine (1999-07-01). "ROSAT PSPC Observations of the Richest (R>=2) ACO Clusters". The Astrophysical Journal. 519 (2): 533–548. arXiv:astro-ph/9902129. Bibcode:1999ApJ...519..533D. doi:10.1086/307388. ISSN 0004-637X.
  20. ^ Bartalucci, I.; Arnaud, M.; Pratt, G. W.; Démoclès, J.; Lovisari, L. (2019-08-01). "The Most Massive galaxy Clusters (M2C) across cosmic time: link between radial total mass distribution and dynamical state". Astronomy and Astrophysics. 628: A86. arXiv:1906.02339. Bibcode:2019A&A...628A..86B. doi:10.1051/0004-6361/201935984. ISSN 0004-6361.
  21. ^ Repp, A.; Ebeling, H. (2018-09-01). "Science from a glimpse: Hubble SNAPshot observations of massive galaxy clusters". Monthly Notices of the Royal Astronomical Society. 479 (1): 844–864. arXiv:1706.01263. Bibcode:2018MNRAS.479..844R. doi:10.1093/mnras/sty1489. ISSN 0035-8711.
  22. ^ a b Irgens, Ragnvald J.; Lilje, Per B.; Dahle, Haakon; Maddox, S. J. (November 2002). "Weak Gravitational Lensing by a Sample of X-Ray Luminous Clusters of Galaxies -- II. Comparison with Virial Masses". The Astrophysical Journal. 579 (1): 227–235. arXiv:astro-ph/0206234. Bibcode:2002ApJ...579..227I. doi:10.1086/342751. ISSN 0004-637X.
  23. ^ Briel, Ulrich G.; Henry, J. Patrick (1993). "1993A&A...278..379B Page 379". Astronomy and Astrophysics. 278: 379. Bibcode:1993A&A...278..379B. Retrieved 2024-06-12.
  24. ^ Briel, Ulrich G.; Henry, J. Patrick (1993-11-01). "X-ray emission from a complete sample of Abell clusters of galaxies". Astronomy and Astrophysics. 278: 379–390. Bibcode:1993A&A...278..379B. ISSN 0004-6361.
  25. ^ Venturi, T.; Giacintucci, S.; Dallacasa, D.; Cassano, R.; Brunetti, G.; Bardelli, S.; Setti, G. (2008-06-01). "GMRT radio halo survey in galaxy clusters at z = 0.2–0.4 - II. The eBCS clusters and analysis of the complete sample". Astronomy & Astrophysics. 484 (2): 327–340. arXiv:0803.4084. Bibcode:2008A&A...484..327V. doi:10.1051/0004-6361:200809622. ISSN 0004-6361.
  26. ^ Cavagnolo, Kenneth W.; Donahue, Megan; Voit, G. Mark; Sun, Ming (2009-05-01). "Intracluster Medium Entropy Profiles for a Chandra Archival Sample of Galaxy Clusters". The Astrophysical Journal Supplement Series. 182 (1): 12–32. arXiv:0902.1802. Bibcode:2009ApJS..182...12C. doi:10.1088/0067-0049/182/1/12. ISSN 0067-0049.
  27. ^ McPartland, Conor; Ebeling, Harald; Roediger, Elke; Blumenthal, Kelly (2016-01-01). "Jellyfish: the origin and distribution of extreme ram-pressure stripping events in massive galaxy clusters". Monthly Notices of the Royal Astronomical Society. 455 (3): 2994–3008. arXiv:1511.00033. Bibcode:2016MNRAS.455.2994M. doi:10.1093/mnras/stv2508. ISSN 0035-8711.
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