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Abell 646 BCG

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Abell 646 BCG
SDSS image of Abell 646 BCG
Observation data (J2000.0 epoch)
ConstellationLynx
Right ascension08h 22m 09.54s[1]
Declination+47° 05′ 52.79″[1]
Redshift0.127081[1]
Heliocentric radial velocity38,098 ± 4 km/s[1]
Distance1,833.7 ± 128.4 Mly (562.23 ± 39.36 Mpc)[1]
Group or clusterAbell 646
magnitude (J)14.10[1]
magnitude (H)13.51[1]
Characteristics
TypeBrClG Sy1.5[1]
Size~454,000 ly (139.3 kpc) (estimated)[1]
Other designations
2MASX J08220955+4705529, Abell 0646:[REK2022] BCG, ABELL 0646:KYDISC 00007, LEDA 2292300, IVS B0818+47A, NVSS J082209+470552, MaxBCG J125.53981+47.09802 BCG, SDSS J082209.54+470553.1[1]

Abell 646 BCG (short for Abell 646 Brightest Cluster Galaxy) is an elliptical galaxy residing as the brightest cluster galaxy (BCG) of the X-ray galaxy cluster, Abell 646[2] in the constellation of Lynx. The redshift of the galaxy is (z) 0.127[1] and it was first discovered by astronomers in July 1999, who found the optical spectrum of the galaxy has presence of emission lines.[2] This galaxy also contains an active galactic nucleus (AGN).[3][4]

Description

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Abell 646 BCG is classified as a Seyfert galaxy. The total hydrogen-alpha luminosity is estimated to be 0.33 × 1042 erg s-1 and the hydrogen-alpha broad component has a full width at half maximum (FWHM) measurement of 1,889.2 kilometers per second. The central supermassive black hole mass is estimated to be 6.83 Mʘ or 1.87 × 109 Mʘ based on a study of dynamical masses for BCGs published in June 2020.[3][5] It is also a radio galaxy containing a compact radio source with a radio power of 24.37 W Hz-1 at 1.4 GHz frequencies.[6]

The total infrared luminosity of the BCG is estimated to be 1.49 × 1044 erg s-1 and it displays signs of infrared radio emission with flux densities of 1.78 and 1.27 mJy based on detections by the Spitzer Space Telescope at 3.6 and 4.5 micrometer respectively.[7] The BCG also shows an intermediate stellar population of blue stars, with the inner populations being aged 3,680 ± 510 million years and the outer populations being 5,780 ± 2,150 million years.[8] A study published in 2018 found the BCG has kinematic properties. The central velocity dispersion is 313 ± 5 kilometers per second and the rotation is estimated to be 028 ± 0.09 Vmax.[9]

There is also evidence that the BCG contains carbon oxide (CO) line emission having lines that have widths of 221 ± 97 kilometers per second and velocity shifts of 125 ± 97 kilometers per second. The molecular gas mass is estimated to be less than 1.3 × 1010 Mʘ, while the total dust mass is also less than 1.3 × 107 Mʘ.[10] The molecular line luminosity is calculated at 1.6 ± 0.6 × 1040 erg s-1.[11] The BCG has cold molecular gas with an estimated hydrogen mass (H2) of 7.9 ± 0.2 x 109 Mʘ.[12]

References

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  1. 1 2 3 4 5 6 7 8 9 10 11 "NED Search results for Abell 646 BCG (LEDA 2292300)". NASA/IPAC Extragalactic Database. Retrieved 2026-05-15.
  2. 1 2 Crawford, C. S.; Allen, S. W.; Ebeling, H.; Edge, A. C.; Fabian, A. C. (1999-07-11). "The ROSAT Brightest Cluster Sample -- III. Optical spectra of the central cluster galaxies". Monthly Notices of the Royal Astronomical Society. 306 (4): 857–896. arXiv:astro-ph/9903057. Bibcode:1999MNRAS.306..857C. doi:10.1046/j.1365-8711.1999.02583.x. ISSN 0035-8711.
  3. 1 2 Wang, J.; Wei, J. Y. (2010-07-27). "UNDERSTANDING AGN-HOST CONNECTION IN PARTIALLY OBSCURED ACTIVE GALACTIC NUCLEI. III. PROPERTIES OFROSAT-SELECTED SDSS ACTIVE GALACTIC NUCLEI". The Astrophysical Journal. 719 (2): 1157–1167. arXiv:1006.5494. Bibcode:2010ApJ...719.1157W. doi:10.1088/0004-637x/719/2/1157. ISSN 0004-637X.
  4. ↑ Xu, Da-Wei; Wei, Jian-Yan; Hu, Jing-Yao (February 2001). "Optical Identifications of X-ray Selected AGNs". Chinese Journal of Astronomy and Astrophysics. 1 (1): 46–49. Bibcode:2001ChJAA...1...46X. doi:10.1088/1009-9271/1/1/46. ISSN 1009-9271.
  5. ↑ Loubser, S I; Babul, A; Hoekstra, H; Bahé, Y M; O’Sullivan, E; Donahue, M (2020-06-12). "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.
  6. ↑ Maccagni, Filippo M.; Morganti, Raffaella; Oosterloo, Tom A.; Geréb, Katinka; Maddox, Natasha (August 2017). "Kinematics and physical conditions of HI in nearby radio sources. The last survey of the old Westerbork Synthesis Radio Telescope". Astronomy & Astrophysics. 604: A43. arXiv:1705.00492. Bibcode:2017A&A...604A..43M. doi:10.1051/0004-6361/201730563. ISSN 0004-6361.
  7. ↑ Quillen, Alice C.; Zufelt, Nicholas; Park, Jaehong; O’Dea, Christopher P.; Baum, Stefi A.; Privon, George; Noel-Storr, Jacob; Edge, Alastair; Russell, Helen; Fabian, Andy; Donahue, Megan; Bregman, Joel N.; McNamara, Brian R.; Sarazin, Craig L. (May 2008). "An Infrared Survey of Brightest Cluster Galaxies. I." The Astrophysical Journal Supplement Series. 176 (1): 39–58. arXiv:0711.1118. Bibcode:2008ApJS..176...39Q. doi:10.1086/525560. ISSN 0067-0049.
  8. ↑ 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.
  9. ↑ 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" (PDF). Monthly Notices of the Royal Astronomical Society. 477 (1): 335–358. doi:10.1093/mnras/sty498. ISSN 0035-8711.
  10. ↑ Edge, A.C. (December 2001). "The detection of molecular gas in the central galaxies of cooling flow clusters". Monthly Notices of the Royal Astronomical Society. 328 (3): 762–782. arXiv:astro-ph/0106225. Bibcode:2001MNRAS.328..762E. doi:10.1046/j.1365-8711.2001.04802.x. ISSN 0035-8711.
  11. ↑ Edge, A. C.; Wilman, R. J.; Johnstone, R. M.; Crawford, C. S.; Fabian, A. C.; Allen, S. W. (November 2002). "A survey of molecular hydrogen in the central galaxies of cooling flows". Monthly Notices of the Royal Astronomical Society. 337 (1): 49–62. arXiv:astro-ph/0206379. Bibcode:2002MNRAS.337...49E. doi:10.1046/j.1365-8711.2002.05790.x. ISSN 0035-8711.
  12. ↑ Salomé, P.; Combes, F. (December 2003). "Cold molecular gas in cooling flow clusters of galaxies". Astronomy & Astrophysics. 412 (3): 657–667. arXiv:astro-ph/0309304. Bibcode:2003A&A...412..657S. doi:10.1051/0004-6361:20031438. ISSN 0004-6361.
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