Astronomy:MACS J1447.4+0827 BCG

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MACS J1447.4+0826 BCG
SDSS image of MACS J1447.4+0827 BCG
Observation data (J2000.0 epoch)
ConstellationBoötes
Right ascension 14h 47m 26.00s[1]
Declination+08° 28′ 25.09″[1]
Redshift0.375463[1]
Helio radial velocity112,561 ± 3 km/s[1]
Distance5,415.8 ± 379.1 Mly (1,660.48 ± 116.23 Mpc)[1]
Characteristics
TypeBrCIG[1]
Size~569,000 ly (174.6 kpc) (estimated)[1]
Other designations
2MASX J14472597+0828253, NVSS J144726+082825, MACS J1447.4+0827 BCG, SDSS J144726.02+082825.1[1] LEDA 3833752

MACS J1447.4+0827 BCG (short for MACS J1447.4+0827 Brightest Cluster Galaxy), is a massive elliptical galaxy residing as the brightest cluster galaxy of the X-ray luminous galaxy cluster, MACS J1447.4+0827 which is also known as RX J1447.4+0827.[2][3][4] The redshift of the galaxy is estimated to be (z) 0.37[1] and it contains an active galactic nucleus (AGN) based on evidence of a central point-like region that is coincident with its position.[3]

Description

MACS J1447.4+0827 BCG is classified as a central galaxy. When observed with the Hubble Space Telescope (HST), it is contains filament structures depicted as optically bright with an extent of around 25 kiloparsecs in total. Two of the filament structures are shown positioned from west to south and west to north respectively.[3]

The nucleus of the galaxy is active and it has been classified as a radio galaxy with the presence of strong emission lines in its optical spectrum.[5][6] Radio imaging made by the Very Large Array (VLA), showed there is a compact radio component that coincides with an X-ray source and the presence of radio emission that is extending outwards by 160 kiloparsecs. There is also evidence of two X-ray cavities located both north and south from the BCG, with a cavity power of 6 × 1044 erg s-1.These cavities have an elliptical morphology and an extent of 32 kiloparsecs in.[3] Two collimated radio jets emerge outwards with a measured radius of 20 kiloparsecs. A diffused component extends from the inner jet regions. This component is estimated to have a spectral index of -1.2 ± 1.0 and has a total radio power of 3.0 ± 0.3 × 1024 W Hz-1.[7] A study also found the jets are also aligned together with the cavities.[4] The mass of the central supermassive black hole of the BCG is estimated to be in the range of 9 to 10 × 109 Mʘ.[3]

The total star formation rate of the BCG is found be 60-80 Mʘ per year. There is also evidence of a molecular gas reservoir region, elongated from east to west direction, with the total molecular gas mass estimated as 9 × 1010 Mʘ. A study showed detections of carbon oxide (CO) emitting components located in the center, and both the subregions located in the eastern and western directions. One of the components is shown to have a high velocity dispersion of 200 kilometers per seconds.[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 MACS J1447.4+0827 BCG". https://ned.ipac.caltech.edu/byname?objname=+SDSS+J144726.02+082825.1&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1. 
  2. ↑ Hlavacek-Larrondo, J.; Fabian, A. C.; Edge, A. C.; Ebeling, H.; Sanders, J. S.; Hogan, M. T.; Taylor, G. B. (2012-02-06). "Extreme AGN feedback in the MAssive Cluster Survey: a detailed study of X-ray cavities atz>0.3". Monthly Notices of the Royal Astronomical Society 421 (2): 1360–1384. doi:10.1111/j.1365-2966.2011.20405.x. ISSN 0035-8711. Bibcode: 2012MNRAS.421.1360H. 
  3. ↑ 3.0 3.1 3.2 3.3 3.4 Prasow-Émond, M.; Hlavacek-Larrondo, J.; Rhea, C. L.; Latulippe, M.; Gendron-Marsolais, M.-L.; Richard-Laferrière, A.; Sanders, J. S.; Edge, A. C. et al. (2020-08-07). "A Multiwavelength Study of the Cool Core Cluster MACS J1447.4+0827". The Astronomical Journal 160 (3): 103. doi:10.3847/1538-3881/ab9ff3. ISSN 0004-6256. Bibcode: 2020AJ....160..103P. 
  4. ↑ 4.0 4.1 Ubertosi, Francesco; Schellenberger, Gerrit; O’Sullivan, Ewan; Vrtilek, Jan; Giacintucci, Simona; David, Laurence P.; Forman, William; Gitti, Myriam et al. (2024-01-01). "Jet Reorientation in Central Galaxies of Clusters and Groups: Insights from VLBA and Chandra Data". The Astrophysical Journal 961 (1): 134. doi:10.3847/1538-4357/ad11d8. ISSN 0004-637X. Bibcode: 2024ApJ...961..134U. 
  5. ↑ Best, P. N.; Heckman, T. M. (2012-04-01). "On the fundamental dichotomy in the local radio-AGN population: accretion, evolution, and host galaxy properties". Monthly Notices of the Royal Astronomical Society 421 (2): 1569–1582. doi:10.1111/j.1365-2966.2012.20414.x. Bibcode: 2012MNRAS.421.1569B. 
  6. ↑ Green, T. S.; Edge, A. C.; Stott, J. P.; Ebeling, H.; Burgett, W. S.; Chambers, K. C.; Draper, P. W.; Metcalfe, N. et al. (2016-06-07). "A multiwavelength 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. https://watermark02.silverchair.com/stw1338.pdf?token=AQECAHi208BE49Ooan9kkhW_Ercy7Dm3ZL_9Cf3qfKAc485ysgAAA1AwggNMBgkqhkiG9w0BBwagggM9MIIDOQIBADCCAzIGCSqGSIb3DQEHATAeBglghkgBZQMEAS4wEQQMlvQCrq68fQEsZr86AgEQgIIDA_jer9e4lMwbgXgYDIB4TEnjwx1KmHplsGkJV4czcsnH-dLVvaEujyPGJuyagRnkNBRPE5Kn-hmyxdRHNKPlSJAbJpUfdP9nVPh7nNspzU8UtrDPLX0cChQ8Hx6dgAoxBqXxWTdDcnnKAExVXE5meXDZfylEXAQr1eYnfqoIt11Ye8-j10IKJl-SghHzGSdMhKTVMAWrVS6OQhewkhmzbjS7Kqr4VG2ynRhF5cWSy-WwLG8egJhbkq22Qu9B2X35tk9LlqrF2le7xg714k6XOVAc-lqUNpIFJxDA6X0PMqwBbDHaqBGH8JVSEzq9QXwRiK5LiCWbHAvaCG75Czo6j4UwLRNXeaYczlgV0qTNjkoHsYGmwpEqEUZhfX_MAFyl9fHVP3_9YuQstGb9E6RNkbGVMXuuQZb6iRtCHxjtLT6Z4y7ZLADXsmD6Fbh70t3jykDvzZyjGCVbnEU656MXpVmU_nJ4EW8FJ9nHIM838X4FRmeCvNSFuW4m2-7qq3nDqkOJ1tO-D_HWMRm11Q1dyKFybNPXVk5SJia7KJCjB7FvjqBKvSrZFEqP7HTD6QYD8U_FWGOVr5ZJkr_XAI2XZeUqLfRyMYXA7AemNbjIg5mEi82mg7LdLdpw4ZxkGFTAeWrooNyW9uIdWtIIctSIYOI8_lhPB2pJ1gNMkN7zGyoIP_njnHYCPdI7sYgeVwOF7PxlSfqMqDy4H6nFYWAhbUZBygYlanFKl-ZRiXk7pspC9XXvIPPmIVC08zk_IFm3sp_fbz5RaLPq5mzmNkEEuAYMl0o5pc8xFt2Ttl1jShCs1AktfSDDLjpF_-j9HPWcb5fDl-SpycYAnV1yrc9JNuEbt8BtV1f0JHjIfdBz1pmSOfBQ5IwFYnbdl8oiqg4mX-_kZGqAKmYHBq_VCJqDoJKQuEzO5Tf-d5EVDPxv3p7EGbo_08mhsrTyeqrfp3nCcNKTEy441kElXhh-HGt4duHk4zTJ3QRuxwq5NNnzmprU5adPq5j2qik6sfk-DY0R_ifbPw. 
  7. ↑ Richard-Laferrière, A.; Hlavacek-Larrondo, J.; Nemmen, R. S.; Rhea, C. L.; Taylor, G. B.; Prasow-Émond, M.; Gendron-Marsolais, M.; Latulippe, M. et al. (2020-10-23). "On the relation between mini-halos and AGN feedback in clusters of galaxies". Monthly Notices of the Royal Astronomical Society 499 (2): 2934–2958. doi:10.1093/mnras/staa2877. ISSN 0035-8711. https://academic.oup.com/mnras/article/499/2/2934/5917087?guestAccessKey=#209340151. 
  8. ↑ Castignani, G.; Combes, F.; Salomé, P.; Edge, A.; Jablonka, P. (August 2025). "Molecular gas in cool-core brightest cluster galaxies at z ≃ 0.4". Astronomy & Astrophysics 700: A197. doi:10.1051/0004-6361/202453289. ISSN 0004-6361. Bibcode: 2025A&A...700A.197C. https://www.aanda.org/articles/aa/full_html/2025/08/aa53289-24/aa53289-24.html. 



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