Astronomy:MS 1455.0+2232 BCG

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MS 1455.0+2232 BCG
SDSS image of MS 1455.0+2232 BCG
Observation data (J2000.0 epoch)
ConstellationBoötes
Right ascension 14h 57m 15.08s[1]
Declination+22° 20′ 34.29″[1]
Redshift0.257620[1]
Helio radial velocity77,233 km/s ± 0[1]
Distance3.736 Gly (1145.56 Mpc)[1]
Group or clusterMS 1455.0+2232
Characteristics
TypeBrClG
Size~618,000 ly (189.4 kpc) (estimated)[1]
Other designations
RX J1457.3+2220, LEDA 1668167, NVSS J145715+222036, SDSS J145715.10+222034.4, 2MASX J14571507+2220341

MS 1455.0+2232 BCG (short for MS 1455.0+2232 Brightest Cluster Galaxy), is a massive type-cD galaxy[2] located in the constellation of Boötes. The redshift of the galaxy is (z) 0.257[1] and it was first discovered as an astronomical radio source by astronomers in April 1998.[3] It is the brightest cluster galaxy of the galaxy cluster MS 1455.0+2232.[4]

Description

MS 1455.0+2232 BCG is classified as a central cluster galaxy (CCG) of MS 1455.0+2232. Its optical spectrum is found to display emission lines that are categorized as both strong and narrow with a full width at half maximum of 500 kilometers per seconds. It also contains a blue continuum that is found to be enhanced.[5] The K-band magnitude of the BCG is estimated to be around 13.91.[6] It is also found to contain detections of molecular gas with an estimated mass of 6.1 ± 2.4 x 1010 Mʘ and also undergoing molecular gas outflows at the rate of around 1,227 Mʘ per year.[7] The central core of the BCG is described to have a blue appearance. Its total star formation rate is around 36 ± 4 Mʘ per year based on an ultraviolet excess technique.[8] The appearance of the galaxy is categorized as boxy.[9]

The nucleus of MS 1455.0+2232 BCG is found to be active and it has been classified as a radio galaxy.[10] There is a compact radio source associated with it and described as point-like. When observed, the source is found to contain a central compact component that is surrounded by a halo that is depicted as extended.[11] The radio core of the BCG remains unresolved although the source is further separated into several components; mainly a western component that is misaligned slightly with the galaxy and another component that has an eastern extension. The total flux density of the compact component is estimated as 11.93 ± 1.24 mJy.[4]

Young blue stellar populations have also been detected in the BCG, indicating a recent history of moderate star formations. Two stellar components are found located in the inner region with the mean ages estimated as 3440 ± 680 million years.[12]

Description

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 "NED Search results for MS 1455.0+2232 BCG". https://ned.ipac.caltech.edu/byname?objname=2MASX+J14571507+2220341&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1. 
  2. ↑ Le Fevre, O.; Hammer, F.; Angonin, M. C.; Gioia, I. M.; Luppino, G. A. (February 1994). "Imaging of 16 distant EMSS clusters with Z greater than or equal to 0.2 and L(subx,44) greater than or equal to 4: New arcs and first consequences" (in en). The Astrophysical Journal 422: L5. doi:10.1086/187198. ISSN 0004-637X. https://articles.adsabs.harvard.edu/pdf/1994ApJ...422L...5L. 
  3. ↑ Cooray, Asantha R.; Grego, Laura; Holzapfel, William L.; Joy, Marshall; Carlstrom, John E. (April 1998). "Radio Sources in Galaxy Clusters at 28.5 GHz" (in en). The Astronomical Journal 115 (4): 1388–1399. doi:10.1086/300310. ISSN 0004-6256. Bibcode: 1998AJ....115.1388C. 
  4. ↑ 4.0 4.1 J, Riseley, C; K, Rajpurohit; F, Loi; A, Botteon; R, Timmerman; N, Biava; A, Bonafede; E, Bonnassieux et al. (2022-04-12). "A MeerKAT-meets-LOFAR study of MS 1455.0 + 2232: a 590 kiloparsec 'mini'-halo in a sloshing cool-core cluster" (in en). Monthly Notices of the Royal Astronomical Society 512 (3). doi:10.1093/mnra. ISSN 0035-8711. https://academic.oup.com/mnras/article/512/3/4210/6547010. 
  5. ↑ Allen, S. W.; Fabian, A. C.; Edge, A. C.; Bautz, M. W.; Furuzawa, A.; Tawara, Y. (1996-10-21). "ASCA and ROSAT observations of distant, massive cooling flows". Monthly Notices of the Royal Astronomical Society 283 (1): 263–281. doi:10.1093/mnras/283.1.263. ISSN 0035-8711. https://watermark02.silverchair.com/283-1-263.pdf?token=AQECAHi208BE49Ooan9kkhW_Ercy7Dm3ZL_9Cf3qfKAc485ysgAAA1gwggNUBgkqhkiG9w0BBwagggNFMIIDQQIBADCCAzoGCSqGSIb3DQEHATAeBglghkgBZQMEAS4wEQQMbLQOF_EhyesFPZCrAgEQgIIDC5Zr05DMAd_9YKkqLiFiSnwgnEiePD2hnVnqLKnnK6BcN8G1pVUagTXnJZ8PYrtNZiGZeFvdmV_4VhjDE5-nHb_JveaYw3NGooqsYjYzrfF-L5F0nOxnEHXJ6ZxXIycGiV_0P_KLmw-Dcmc6CdlJEyi2DkwSHh0blH0aEtUf9NKn8Gm_0ZIqFlu4q0zCQ5Bs1NPQFJ8cpxVUWtcBAY4e6xBxyK13olbz2cDEaXfQKL--zkWogT-tSkAOCLIPSVujl2tsjxO9KT2klVoayTSh-CYaXZM0MvU8JJPxWUmVgcdJ-lcdMhDLwMmFFsVBFIKc6OlgZMR8MzlC9dLSSoMhimJ5lISFSpbkS2RzUJTMpUZdsfPDId46yEC0oLJuID2Of411zDqR4cjAqF4Lz-oHsy6VVxS-_eA7O-VL6XwXsG-4S44vL1xW-drcq9cmXmZp0Ghtg9g7MyShcZjTPj7LcTWTAzb9XJDkCMnCA305Fidb7GBmk8CLd5mLRAHL7CLQ1Wd1XQLqQx20YKYSykE-5YQWjm9TILxOkG5lWoapSXSyF-RPBom6D3z9elvXppokJ1EZsO55DOHxfRjbRhZG_RLxm-HZVHuqyd7yAxu9UKOFRP7GVRqzB3Ze1Vd4DjPEX2rurJegSv52UM-IrIZR8lm3WmKCbjtUxdcnJvChSk8-G1Ta4FFukfW9NToYuUMEY1Ff99C-DpYYdm5unrh2yjYw16O-bHaomwZEN_7IyqdtmS5FHiW8y4EzJdBCU-903_qjQ9wgvn22hbPqqXLit0QyJfaQEsFAl6auZvPRCliF_oyTZMkbXMPp9nVT-qiXHermYPyoz74hL2xG0LuW0tkKT4T4_KENlpW4KRq10djCdizX3tVo_YUpop0fYAaRsS5zhbHLP_wjCB3ohu3FAPBunyNvFmWV2xuYUP6bRxM8pUjCSDsDuK6KlnY8FTpPy5lLNl-d1Yr6c-LfpxNGrGa2L-PRMwSsvRDAfMuhLiJ13K51s_yepbM_7GW9u28jWK9xtiib8TO81eSN. 
  6. ↑ Collins, C. A.; Mann, R. G. (June 1998). "The K-band Hubble diagram for brightest cluster galaxies in X-ray clusters". Monthly Notices of the Royal Astronomical Society 297 (1): 128–142. doi:10.1046/j.1365-8711.1998.01482.x. ISSN 0035-8711. Bibcode: 1998MNRAS.297..128C. 
  7. ↑ Edge, A.C. (December 2001). "The detection of molecular gas in the central galaxies of cooling flow clusters" (in en). Monthly Notices of the Royal Astronomical Society 328 (3): 762–782. doi:10.1046/j.1365-8711.2001.04802.x. ISSN 0035-8711. Bibcode: 2001MNRAS.328..762E. 
  8. ↑ Bildfell, C.; Hoekstra, H.; Babul, A.; Mahdavi, A. (2008-07-08), "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, doi:10.1111/j.1365-2966.2008.13699.x, Bibcode: 2008MNRAS.389.1637B 
  9. ↑ 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" (in en). Monthly Notices of the Royal Astronomical Society 409 (1): 169–183. doi:10.1111/j.1365-2966.2010.17311.x. ISSN 0035-8711. Bibcode: 2010MNRAS.409..169S. 
  10. ↑ Cassano, R.; Gitti, M.; Brunetti, G. (2008-08-01). "A morphological comparison between giant radio halos and radio mini-halos in galaxy clusters" (in en). Astronomy & Astrophysics 486 (3): L31–L34. doi:10.1051/0004-6361:200810179. ISSN 0004-6361. Bibcode: 2008A&A...486L..31C. https://www.aanda.org/articles/aa/pdf/2008/30/aa10179-08.pdf. 
  11. ↑ Venturi, T.; Giacintucci, S.; Dallacasa, D.; Cassano, R.; Brunetti, G.; Bardelli, S.; Setti, G. (2008-04-16). "GMRT radio halo survey in galaxy clusters atz= 0.2–0.4" (in en). Astronomy & Astrophysics 484 (2): 327–340. doi:10.1051/0004-6361:200809622. ISSN 0004-6361. 
  12. ↑ I., Loubser, S.; A., Babul; H., Hoekstra; A., Mahdavi; M., Donahue; C., Bildfell; M., Voit, G. (February 2016). "The regulation of star formation in cool-core clusters: imprints on the stellar populations of brightest cluster galaxies" (in en). Monthly Notices of the Royal Astronomical Society 456 (2): 1565–1578. doi:10.1093/mnras/stv2784. ISSN 0035-8711. 



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