Abell 1650 BCG

Abell 1650 BCG
DESI Legacy Surveys image of Abell 1650 BCG.
Observation data (J2000.0 epoch)
ConstellationVirgo
Right ascension12h 58m 41.48s[1]
Declination−01° 45′ 41.27″[1]
Redshift0.084565[1]
Heliocentric radial velocity25,352 ± 16 km/s[1]
Distance1,215.7 ± 85.1 Mly (372.72 ± 26.09 Mpc)[1]
Group or clusterAbell 1650
magnitude (J)12.97[1]
magnitude (H)12.21[1]
Characteristics
TypecD;BrClG[1]
Size~626,000 ly (191.8 kpc) (estimated)[1]
Other designations
2dFRGS N256Z066, 2MASX J12584149−0145410, Abell 1650:[FDE2024] BCG, APMUKS(BJ) B125607.22−012932.1, LEDA 1110773, OGC 0336, WHL J125841.5−014541 BCG[1]

Abell 1650 BCG (Short for Abell 1650 Brightest Cluster Galaxy) is a massive elliptical galaxy of type-cD located in the constellation of Virgo. It has a redshift of (z) 0.084[1] and is the brightest cluster galaxy (BCG) of the Bautz-Morgan Type I-II galaxy cluster, Abell 1650, with an extrapolated magnitude of 10.31 ± 0.41 × 1011 L☉.[2][3]

Description

Abell 1650 BCG is classified as a type-cD galaxy dominating the center of Abell 1650.[4][5] The BCG is radio-quiet based on radio imaging by the Very Large Array (VLA)[6] with no sign of radio emission associated with it. A faint radio source has been detected through deep imaging at 1.4 GHz frequencies coinciding with the BCG's position with a total flux density of 0.44 ± 0.09 mJy and a radio power of 7.6 × 1021 W/Hz.[7] The optical center of the BCG is misaligned by 23 kiloparsecs towards the southeast direction along with the X-ray surface brightness peak. There is also evidence of X-ray emission around the BCG.[5]

The U–R color magnitude of the BCG is estimated to be -0.05 ± 0.11, while the U–I color magnitude is -0.02 ± 0.11.[8] A study published in November 2020, found the BCG has an intermediate stellar population with the inner population aged 6,640 ± 970 million years, while the outer population is aged 5,550 ± 370 million years. The core of the BCG has a red appearance.[9] The total stellar mass of the BCG is estimated to be 7.2 ± 1.4 × 1011 M☉. A supermassive black hole is at the center of the BCG ,with a mass of 7.58 × 109 M☉.[10]

The BCG also displays kinematic properties. It has a central velocity dispersion of 412 ± 18 kilometers per second, while the rotation is measured to be 0.10 ± 0.07 Vmax.[11]

References

  1. 1 2 3 4 5 6 7 8 9 10 11 "NED Search results for Abell 1650 BCG (LEDA 1110773)". NASA/IPAC Extragalactic Database. Retrieved 2026-05-16.
  2. ↑ Quintana, H.; Infante, L.; Fouque, P.; Carrasco, E. R.; Cuevas, H.; Hertling, G.; Nunez, I. (January 2000). "Photometry of the Central Regions in a Complete Sample of High Bautz-Morgan–Type Abell Clusters. I. Observations and Data Calibration". The Astrophysical Journal Supplement Series. 126 (1): 1–17. Bibcode:2000ApJS..126....1Q. doi:10.1086/313295. ISSN 0067-0049.
  3. ↑ Lin, Yen-Ting; Mohr, Joseph J. (2004-08-30). "K -band Properties of Galaxy Clusters and Groups: Brightest Cluster Galaxies and Intracluster Light". The Astrophysical Journal. 617 (2): 879–895. arXiv:astro-ph/0408557. Bibcode:2004ApJ...617..879L. doi:10.1086/425412.
  4. ↑ Gu, Liyi; Xu, Haiguang; Gu, Junhua; Wang, Yu; Zhang, Zhongli; Wang, Jingying; Qin, Zhenzhen; Cui, Haijuan; Wu, Xiang-Ping (2009-08-01). "A Chandra Study of Temperature Substructures in Intermediate-Redshift Galaxy Clusters". The Astrophysical Journal. 700 (2): 1161–1172. arXiv:0905.3933. Bibcode:2009ApJ...700.1161G. doi:10.1088/0004-637X/700/2/1161. ISSN 0004-637X.
  5. 1 2 Takahashi, Seiji; Yamashita, Koujun (December 2003). "XMM-Newton Observation of the Cluster of Galaxies Abell 1650". Publications of the Astronomical Society of Japan. 55 (6): 1105–1113. arXiv:astro-ph/0401178. doi:10.1093/pasj/55.6.1105. ISSN 0004-6264.
  6. ↑ Burns, Jack O. (January 1990). "The radio properties of cD galaxies in Abell clusters. I - an X-ray selected sample". The Astronomical Journal. 99: 14. Bibcode:1990AJ.....99...14B. doi:10.1086/115307. ISSN 0004-6256.
  7. ↑ Govoni, F.; Murgia, M.; Markevitch, M.; Feretti, L.; Giovannini, G.; Taylor, G. B.; Carretti, E. (2009-05-01). "A search for diffuse radio emission in the relaxed, cool-core galaxy clusters A1068, A1413, A1650, A1835, A2029, and Ophiuchus" (PDF). Astronomy & Astrophysics. 499 (2): 371–383. arXiv:0901.1941. Bibcode:2009A&A...499..371G. doi:10.1051/0004-6361/200811180. ISSN 0004-6361.
  8. ↑ Rafferty, D. A.; McNamara, B. R.; Nulsen, P. E. J. (2008-11-10). "The Regulation of Cooling and Star Formation in Luminous Galaxies by Active Galactic Nucleus Feedback and the Cooling-Time/Entropy Threshold for the Onset of Star Formation". The Astrophysical Journal. 687 (2): 899–918. arXiv:0802.1864. Bibcode:2008ApJ...687..899R. doi:10.1086/591240. ISSN 0004-637X.
  9. ↑ Loubser, S I; Hoekstra, H; Babul, A; Bahé, Y M; Donahue, M (2020-11-13). "Dynamical masses of brightest cluster galaxies – II. Constraints on the stellar IMF". Monthly Notices of the Royal Astronomical Society. 500 (3): 4153–4165. arXiv:2011.05350. doi:10.1093/mnras/staa3530. ISSN 0035-8711.
  10. ↑ Loubser, S. I.; Babul, A.; Hoekstra, H.; Bahé, Y. M.; O'Sullivan, E.; Donahue, M. (2020-08-01). "Dynamical masses of brightest cluster galaxies I: stellar velocity anisotropy and mass-to-light ratios". Monthly Notices of the Royal Astronomical Society. 496 (2): 1857–1880. arXiv:2006.05706. doi:10.1093/mnras/staa1682. ISSN 0035-8711.
  11. ↑ Loubser, S I; Hoekstra, H; Babul, A; O'Sullivan, E (2018-02-23). "Diversity in the stellar velocity dispersion profiles of a large sample of brightest cluster galaxies z ≤ 0.3". Monthly Notices of the Royal Astronomical Society. 477 (1): 335–358. arXiv:1802.07745. doi:10.1093/mnras/sty498. ISSN 0035-8711.
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