Astronomy:Abell 697 BCG

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Abell 697 BCG
SDSS image of Abell 697 BCG
Observation data (J2000.0 epoch)
ConstellationLynx
Right ascension 08h 42m 57.57s[1]
Declination+36° 21′ 59.70″[1]
Redshift0.282280[1]
Helio radial velocity84,625 ± 12 km/s[1]
Distance4,069.8 ± 284.9 Mly (1,247.82 ± 87.35 Mpc)[1]
Group or clusterAbell 697
Characteristics
TypeBrClG[1]
Size~647,400 ly (198.49 kpc) (estimated)[1]
Other designations
2MASX J08425763+3622000, Abell 0697:[BHB2008] BCG, GMBCG J130.73982+36.36646 BCG, [HWH2012] 05, LEDA 2079433, OGC 0043, SDSS J084257.55+362159.2, WHL J084257.6+362159 BCG[1]

Abell 697 BCG (short for Abell 697 Brightest Cluster Galaxy) also known as OGC 43, is a massive elliptical galaxy of Type-cD located in the constellation of Lynx. The redshift of the galaxy is (z) 0.282[1] and it is the brightest cluster galaxy of the galaxy cluster, Abell 697.[2][3]

Description

Abell 697 BCG is an elliptical galaxy dominating the center of the cluster. It displays a galactic halo, with its profile having a v band magnitude of 18.1. The halo has a roughly elliptical shape, but it becomes slightly asymmetric at a larger radius, with the halo's extension being visible up to 40 arcseconds towards the southeast. The BCG's isophotes on the inner sides are orientated in the position angle of 163°. There is a secondary nucleus in the northwest direction, with evidence of an extended low surface brightness feature from its center. It is suggested the halo of the BCG formed though several galaxy mergers.[4] The r-band luminosity of the BCG, calculated from the Sloan Digital Sky Survey (SDSS), is magnitude 15.1.[5]

The total infrared star formation of the BCG is estimated to be 13.33 Mʘ per year, with the total stellar mass is 13.70 × 1010 Mʘ.[6]

The core of the BCG has a red appearance based on its inner color profile, and the BCG is offset from the X-ray emission peak of the cluster by 20.3 kiloparsecs.[7] The radio core of the BCG has a flux density less than 0.21 mJy in total, while the optical spectrum of the BCG lacks emission lines.[8] The total radio power has been estimated to have a spectral density flux of 23.30 W Hz-1 at 1.4 GHz frequencies.[9] It also belongs to a fossil galaxy group.[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 697 BCG (LEDA 2079433)". https://ned.ipac.caltech.edu/byname?objname=LEDA+2079433&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1. 
  2. ↑ Cibirka, Nathália; Acebron, Ana; Zitrin, Adi; Coe, Dan; Agulli, Irene; Andrade-Santos, Felipe; Bradač, Maruša; Frye, Brenda et al. (2018-08-20). "RELICS: Strong Lensing Analysis of the Galaxy Clusters Abell S295, Abell 697, MACS J0025.4-1222, and MACS J0159.8-0849". The Astrophysical Journal 863 (2): 145. doi:10.3847/1538-4357/aad2d3. ISSN 0004-637X. Bibcode: 2018ApJ...863..145C. 
  3. ↑ Rawle, T. D.; Edge, A. C.; Egami, E.; Rex, M.; Smith, G. P.; Altieri, B.; Fiedler, A.; Haines, C. P. et al. (2012-02-10). "THE RELATION BETWEEN COOL CLUSTER CORES AND HERSCHEL- DETECTED STAR FORMATION IN BRIGHTEST CLUSTER GALAXIES". The Astrophysical Journal 747 (1): 29. doi:10.1088/0004-637x/747/1/29. ISSN 0004-637X. Bibcode: 2012ApJ...747...29R. https://iopscience.iop.org/article/10.1088/0004-637X/747/1/29/pdf. 
  4. ↑ Metzger, Mark R.; Ma, Chung-Pei (December 2000). "Lensed Arcs and Inner Structure of Abell 697". The Astronomical Journal 120 (6): 2879–2883. doi:10.1086/316843. ISSN 0004-6256. Bibcode: 2000AJ....120.2879M. https://iopscience.iop.org/article/10.1086/316843/fulltext/. 
  5. ↑ Ogle, Patrick M.; Lanz, Lauranne; Appleton, Philip N.; Helou, George; Mazzarella, Joseph (2019-07-15). "A Catalog of the Most Optically Luminous Galaxies at z < 0.3: Super Spirals, Super Lenticulars, Super Post-mergers, and Giant Ellipticals". The Astrophysical Journal Supplement Series 243 (1): 14. doi:10.3847/1538-4365/ab21c3. ISSN 1538-4365. Bibcode: 2019ApJS..243...14O. 
  6. ↑ 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. doi:10.1088/0067-0049/199/1/23. ISSN 0067-0049. Bibcode: 2012ApJS..199...23H. https://iopscience.iop.org/article/10.1088/0067-0049/199/1/23. 
  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. Bibcode: 2008MNRAS.389.1637B. 
  8. ↑ Hogan, M. T.; Edge, A. C.; Hlavacek-Larrondo, J.; Grainge, K. J. B.; Hamer, S. L.; Mahony, E. K.; Russell, H. R.; Fabian, A. C. et al. (2015-07-10). "A comprehensive study of the radio properties of brightest cluster galaxies" (in en). Monthly Notices of the Royal Astronomical Society 453 (2): 1201–1222. doi:10.1093/mnras/stv1517. 
  9. ↑ Kale, Ruta; Venturi, Tiziana; Cassano, Rossella; Giacintucci, Simona; Bardelli, Sandro; Dallacasa, Daniele; Zucca, Elena (2015-06-18). "Brightest cluster galaxies in the extended GMRT radio halo cluster sample" (in en). Astronomy & Astrophysics 581: A23. doi:10.1051/0004-6361/201526341. 
  10. ↑ Hess, Kelley M.; Wilcots, Eric M.; Hartwick, Victoria L. (2012-07-06). "FRESH ACTIVITY IN OLD SYSTEMS: RADIO AGNs IN FOSSIL GROUPS OF GALAXIES". The Astronomical Journal 144 (2): 48. doi:10.1088/0004-6256/144/2/48. ISSN 0004-6256. Bibcode: 2012AJ....144...48H. https://doi.org/10.1088/0004-6256/144/2/48. 



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