Astronomy:Abell 2009 BCG

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Abell 2009 BCG
SDSS image of Abell 2009 BCG
Observation data (J2000.0 epoch)
ConstellationBoötes
Right ascension 15h 00m 19.52s[1]
Declination+21° 22′ 09.87″[1]
Redshift0.151928[1]
Helio radial velocity45,547 ± 22 km/s[1]
Distance2,213.6 ± 155.0 Mly (678.70 ± 47.51 Mpc)[1]
Group or clusterAbell 2009
Characteristics
TypeBrCIG[1]
Size~591,000 ly (181.3 kpc) (estimated)[1]
Other designations
2MASX J15001950+2122108, Abell 2009:[CAC2009] BCM, LEDA 140447, OGC 0698, MaxBCG J225.08133+21.36941 BCG, RX J1500.3+2122:[BEV98] 010[1]

Abell 2009 BCG (short for Abell 2009 Brightest Cluster Galaxy) is a massive elliptical galaxy residing as the brightest cluster galaxy (BCG) of the galaxy cluster, Abell 2009.[2] The redshift of the galaxy is (z) 0.151[1] and it was first discovered by astronomers in July 1999, who observed emission lines in its optical spectrum.[3]

Description

Abell 2009 BCG is the dominant galaxy of Abell 2009.[3] The central nucleus of the BCG is found to be active and it has been classified as a Fanaroff-Riley Class Type I radio galaxy based on radio imaging made with the Very Large Array (VLA) at 1.5 GHz frequencies. It has a resolved radio core and a pair of butterfly-shaped radio lobes 17 kiloparsecs in length. Both of the lobes are orientated from the northwest direction towards the southeast direction.[2]

The total radio flux density of the BCG is estimated to be 23 ± 1.0 mJy with radio power being calculated as 1.45 ± 0.06 × 1024 W Hz-1.[2] The radio core flux density at 10 GHz frequencies is 3.3 ± 1.4 mJy, with the steep index spectrum being 1.81 ± 0.05.[4] The emission is associated with another radio galaxy in the cluster, located 50 arcseconds away from the BCG.[2]

The BCG has an elliptical appearance according to Hubble Space Telescope (HST) imaging data.[5] The supermassive black hole lying in the center of the BCG is estimated to be 9.74 ± 0.08 Mʘ based on a calculation of the fundamental plane relation with the total stellar mass of 12.17 ± 0.04 Mʘ.[6] The infrared luminosity of the BCG has been calculated as less than 1.0 × 1044 erg s-1, making it somehow less luminous compared to others.[7] A study published in 2024, has found the BCG is offset from the X-ray center by about 7 kiloparsecs.[8]

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 2009 BCG (LEDA 140447)". https://ned.ipac.caltech.edu/byname?objname=LEDA+140447&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1. 
  2. ↑ 2.0 2.1 2.2 2.3 Fornasiero, I.; Ubertosi, F.; Gitti, M. (March 2025). "Investigating AGN feedback in Hα-luminous galaxy clusters: First Chandra X-ray analysis of Abell 2009". Astronomy & Astrophysics 695: A265. doi:10.1051/0004-6361/202453315. ISSN 0004-6361. 
  3. ↑ 3.0 3.1 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. doi:10.1046/j.1365-8711.1999.02583.x. ISSN 0035-8711. 
  4. ↑ 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. (2015-10-21). "A Comprehensive Study of the Radio Properties of Brightest Cluster Galaxies". Monthly Notices of the Royal Astronomical Society 453 (2): 1201–1222. doi:10.1093/mnras/stv1517. ISSN 0035-8711. 
  5. ↑ Smith, Graham P.; Khosroshahi, Habib G.; Dariush, A.; Sanderson, A. J. R.; Ponman, T. J.; Stott, J. P.; Haines, C. P.; Egami, E. et al. (2010-10-06). "LoCuSS: connecting the dominance and shape of brightest cluster galaxies with the assembly history of massive clusters". Monthly Notices of the Royal Astronomical Society 409 (1): 169–183. doi:10.1111/j.1365-2966.2010.17311.x. ISSN 0035-8711. 
  6. ↑ Phipps, Frederika; Bogdán, Ákos; Lovisari, Lorenzo; Kovács, Orsolya E.; Volonteri, Marta; Dubois, Yohan (2019-04-20). "Expanding the Sample: The Relationship between the Black Hole Mass of BCGs and the Total Mass of Galaxy Clusters". The Astrophysical Journal 875 (2): 141. doi:10.3847/1538-4357/ab107c. ISSN 0004-637X. 
  7. ↑ O’Dea, Christopher P.; Baum, Stefi A.; Privon, George; Noel-Storr, Jacob; Quillen, Alice C.; Zufelt, Nicholas; Park, Jaehong; Edge, Alastair et al. (May 2008). "An Infrared Survey of Brightest Cluster Galaxies. I.". The Astrophysical Journal 681 (2): 1035–1045. doi:10.1086/588212. ISSN 0004-637X. 
  8. ↑ Cross, D.; Thoron, G.; Jeltema, T. E.; Swart, A. (February 2024). "Examining the self-interaction of dark matter through central cluster galaxy offsets.". Monthly Notices of the Royal Astronomical Society 529 (1). doi:10.33232/001c.122309. ISSN 2565-6120. https://watermark02.silverchair.com/stae442.pdf?token=AQECAHi208BE49Ooan9kkhW_Ercy7Dm3ZL_9Cf3qfKAc485ysgAAA08wggNLBgkqhkiG9w0BBwagggM8MIIDOAIBADCCAzEGCSqGSIb3DQEHATAeBglghkgBZQMEAS4wEQQMJI_11ztfdzP2NbHgAgEQgIIDAsIsfYz20Hsv92KStglCIDOeXItrHBg70-Q2eubxN9hGZGfbEmFvU4FrseB1GnnG5lIWanR_mTZAg2wxdTVxm5fQv9_9V1Z-fEqe2zyRtlAqnN8lhESYwbs4Bsm16LA8GPO73SDbcAbKKlnb3a75cvZyKDKvkhuCuVa8gMliZfw3SQBFnVRxbNCuV4l-DjNYe0uHpy7hd4jq7d4joJYg5hQlV8ug_qCNFPhczV-sGWDBRTo5TT9EUtL1ElatYnO9z_dj_5LNrgiLS_KfMfd0vot5IVx3qy0ZQzsb_KgnDP3uNPrugZvJSG3pn9Ie1bdR5cNjtyVYJfX_s2ad4-f30yGeqZbf66FVHd90JnUwK5LH4yiGdh7dxNNJ-nzCy3w5T-lB3F_a0_GfuWt2Xpa_kXmnPIfGpmyhP5S8m8cbk1XmHQ03nQ5AF-_tE-xuIzfG9XfglDomwlEsSX-ac56VelHf4qd_SvcePjRwvFJArXePk3CgMIlGwKYkM1UEYayf1LFBlrDnl-Cp9tbbB3FnZb3nCdrgrDDWkca8YjxI_h_xhAcCGoA1qa2THSRhOszvFs9AmheuxHyz6Bu6btgIQNB7JUEWwyt-mw85CL7dV4Hn7igSHoo2f6Xu7aGx2Eehz3PDvsci9GYxqHzDb7FHnb-H8tSUdDR80VHs5l9a_HZpzG32xRx8Blq1qMkz1V6vdi42kHWrx7ggXxORF6857LfXO0WF2iUswPuehEml8pJm0-RFbGQW6zTGj85oM-j0pXXjBu5BRPvWCdcYmTF3jcjMGyvUFv-qadGtg-ieBaZJzGKvLmawACQU7oaB2zl74VV3qNqubRYVaErgWJUVtMYjn4Or5GYMG090tz9nuszq1W1hCVhJCBxY3dUGfXFHoKYjMfzY0Lj7b2HXe4LU1lVxs5rHameNz521JOg9StOGWXopAJij4DZK7Fb4VSzl2rnUUX0lLKjNfQ1TG_ZZmhucGtsKgRNiiHh--NJnTXSxmBrigjqDO7eZtYuE0TMjiWcD. 



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