Astronomy:Abell 521 BCG

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Abell 521 BCG
DESI Legacy Surveys image of Abell 521 BCG
Observation data (J2000.0 epoch)
ConstellationEridanus
Right ascension 04h 54m 06.92s[1]
Declination−10° 13′ 24.57″[1]
Redshift0.248085[1]
Helio radial velocity74,374 ± 47 km/s[1]
Distance3,562.8 ± 249.4 Mly (1,092.36 ± 76.47 Mpc)[1]
Group or clusterAbell 521
Characteristics
TypeEarly-Type[1]
Size~560,000 ly (171.6 kpc) (estimated)[1]
Other designations
2MASX J04540687−1013247, ABELL 0521:[BHB2008] BCG, LEDA 980855, ABELL 0521:[FMC2003] 065, GMRT J0454-1013b[1]

Abell 521 BCG (Short for Abell 521 Brightest Cluster Galaxy) is a massive elliptical galaxy residing as the brightest cluster galaxy (BCG) of a young rich merging Bautz-Morgan Class type III galaxy cluster called Abell 521.[2][3] The redshift of the galaxy is (z) 0.248[1] and it is located in the constellation of Eridanus.

Description

Abell 521 BCG is an early-type galaxy containing an unresolved radio source with a radio flux density of 0.47 mJy at 610 MHz frequencies and a radio power of 22.92 W Hz−1.[4] It has presence of multiple nuclei that is made up of a secondary nucleus and three others depicted as small and faint inside the inner regions. One of the nuclei is shown having a measured peculiar motion of -413 ± 57 kilometer per seconds, with further evidence of it having distorted isophote, indicating an interaction. The multiple nuclei are suggested to be remains of galaxies that have merged with the BCG though galactic cannibalism.[5]

There are also bright extended knot features that is superposed on an arc-like structure of the BCG. Three of these knots are gravitationally bounded to the BCG and have a measured mass of 7.97 × 1010 Mʘ. The arc-like structure is measured to have a curvature of approximately 7.5 arcseconds and is centered nearly on the BCG's position. The total length of the BCG is found to be extend more than 20 × 30 arcseconds with the total surface brightness between 22 and 27 arcsec−2 based on a de Vaucouleurs profile.[5] The total stellar mass of the BCG has been estimated as 0.55 × 1012 Mʘ.[6]

The core of the BCG is found to have a red appearance based on the inner color profile shape. The BCG is also found to have an offset peak of 32.8 kiloparsecs from the cluster and also located in the X-ray northern group region.[7][8] Four blob features are also found inside the arc-like structure within 24 kiloparsecs of the BCG's center.[8] The BCG has absence of both hydrogen-alpha emission and optical emission lines.[9][10]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 "NED Search results for Abell 521 BCG". https://ned.ipac.caltech.edu/byname?objname=2MASX+J04540687-1013247&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1. 
  2. ↑ Ferrari, C.; Arnaud, M.; Ettori, S.; Maurogordato, S.; Rho, J. (2006-02-01). "Chandra observation of the multiple merger cluster Abell 521" (in en). Astronomy & Astrophysics 446 (2): 417–428. doi:10.1051/0004-6361:20053946. ISSN 0004-6361. https://www.aanda.org/articles/aa/pdf/2006/05/aa3946-05.pdf. 
  3. ↑ Arnaud, M.; Maurogordato, S.; Slezak, E.; Rho, J. (March 2000). "A521: A cluster forming at the crossing of two filaments?". Astronomy and Astrophysics 355: 461–478. https://articles.adsabs.harvard.edu/pdf/2000A%26A...355..461A. 
  4. ↑ Giacintucci, S.; Venturi, T.; Bardelli, S.; Brunetti, G.; Cassano, R.; Dallacasa, D. (April 2006). "The cluster relic source in A 521". New Astronomy 11 (6): 437–451. doi:10.1016/j.newast.2005.11.001. ISSN 1384-1076. https://arxiv.org/pdf/astro-ph/0510433. 
  5. ↑ 5.0 5.1 Maurogordato, S.; Proust, D.; Beers, T. C.; Arnaud, M. (March 2000). "Abell 521: dynamical analysis of a young cluster". Astronomy and Astrophysics 355: 848–862. https://articles.adsabs.harvard.edu/pdf/2000A%26A...355..848M. 
  6. ↑ Lidman, C.; Suherli, J.; Muzzin, A.; Wilson, G.; Demarco, R.; Brough, S.; Rettura, A.; Cox, J. et al. (2012-11-01). "Evidence for significant growth in the stellar mass of brightest cluster galaxies over the past 10 billion years". Monthly Notices of the Royal Astronomical Society 427 (1): 550–568. doi:10.1111/j.1365-2966.2012.21984.x. ISSN 0035-8711. https://academic.oup.com/mnras/article/427/1/550/1032122. 
  7. ↑ Bildfell, Chris; Hoekstra, Henk; Babul, Arif; Mahdavi, Andisheh (2008-08-26). "Resurrecting the red from the dead: optical properties of BCGs in X-ray luminous clusters★". Monthly Notices of the Royal Astronomical Society 389 (4): 1637–1654. doi:10.1111/j.1365-2966.2008.13699.x. ISSN 0035-8711. https://doi.org/10.1111/j.1365-2966.2008.13699.x. 
  8. ↑ 8.0 8.1 Ferrari, C.; Maurogordato, S.; Cappi, A.; Benoist, C. (2003-03-01). "Multiple merging events in Abell 521" (in en). Astronomy & Astrophysics 399 (3): 813–828. doi:10.1051/0004-6361:20021741. ISSN 0004-6361. https://www.aanda.org/articles/aa/abs/2003/09/aa3005/aa3005.html. 
  9. ↑ Stott, J. P.; Edge, A. C.; Smith, G. P.; Swinbank, A. M.; Ebeling, H. (March 2008). "Near-infrared evolution of brightest cluster galaxies in the most X-ray luminous clusters since z = 1". Monthly Notices of the Royal Astronomical Society 384 (4): 1502–1510. doi:10.1111/j.1365-2966.2007.12807.x. ISSN 0035-8711. https://arxiv.org/pdf/0712.0496. 
  10. ↑ Green, T. S.; Edge, A. C.; Stott, J. P.; Ebeling, H.; Burgett, W. S.; Chambers, K. C.; Draper, P. W.; Metcalfe, N. et al. (2016-09-01). "A Multi-Wavelength Photometric Census of AGN and Star Formation Activity in the Brightest Cluster Galaxies of X-ray Selected Clusters". Monthly Notices of the Royal Astronomical Society 461 (1): 560–577. doi:10.1093/mnras/stw1338. ISSN 0035-8711. http://arxiv.org/abs/1606.01251. 



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