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) | |
| Constellation | Boötes |
| Right ascension | 14h 57m 15.08s[1] |
| Declination | +22° 20′ 34.29″[1] |
| Redshift | 0.257620[1] |
| Heliocentric radial velocity | 77,233 km/s ± 0[1] |
| Distance | 3.736 Gly (1145.56 Mpc)[1] |
| Group or cluster | MS 1455.0+2232 |
| magnitude (J) | 14.71[1] |
| Characteristics | |
| Type | BrClG |
| 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]
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 × 1010 M☉ and also undergoing molecular gas outflows at the rate of around 1,227 M☉ 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 M☉ 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 2 3 4 5 6 7 8 "NED Search results for MS 1455.0+2232 BCG". NASA/IPAC Extragalactic Database. Retrieved 2026-02-14.
- ↑ 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". The Astrophysical Journal. 422: L5. doi:10.1086/187198. ISSN 0004-637X. Archived from the original on 2024-09-04.
- ↑ Cooray, Asantha R.; Grego, Laura; Holzapfel, William L.; Joy, Marshall; Carlstrom, John E. (April 1998). "Radio Sources in Galaxy Clusters at 28.5 GHz". The Astronomical Journal. 115 (4): 1388–1399. arXiv:astro-ph/9711218. Bibcode:1998AJ....115.1388C. doi:10.1086/300310. ISSN 0004-6256.
- 1 2 J, Riseley, C; K, Rajpurohit; F, Loi; A, Botteon; R, Timmerman; N, Biava; A, Bonafede; E, Bonnassieux; G, Brunetti; T, Enßlin; G, Di Gennaro; A, Ignesti; T, Shimwell; C, Stuardi; T, Vernstrom (2022-04-12). "A MeerKAT-meets-LOFAR study of MS 1455.0 + 2232: a 590 kiloparsec 'mini'-halo in a sloshing cool-core cluster". Monthly Notices of the Royal Astronomical Society. 512 (3). doi:10.1093/mnra (inactive 14 February 2026). ISSN 0035-8711. Archived from the original on 2024-06-23.
{{cite journal}}: CS1 maint: DOI inactive as of February 2026 (link) CS1 maint: multiple names: authors list (link) - ↑ 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" (PDF). Monthly Notices of the Royal Astronomical Society. 283 (1): 263–281. doi:10.1093/mnras/283.1.263. ISSN 0035-8711.
- ↑ 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. arXiv:astro-ph/9712104. Bibcode:1998MNRAS.297..128C. doi:10.1046/j.1365-8711.1998.01482.x. ISSN 0035-8711.
- ↑ 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.
- ↑ 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, arXiv:0802.2712, Bibcode:2008MNRAS.389.1637B, doi:10.1111/j.1365-2966.2008.13699.x
- ↑ Smith, Graham P.; Khosroshahi, Habib G.; Dariush, A.; Sanderson, A. J. R.; Ponman, T. J.; Stott, J. P.; Haines, C. P.; Egami, E.; Stark, D. P. (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. arXiv:1007.2196. Bibcode:2010MNRAS.409..169S. doi:10.1111/j.1365-2966.2010.17311.x. ISSN 0035-8711.
- ↑ Cassano, R.; Gitti, M.; Brunetti, G. (2008-08-01). "A morphological comparison between giant radio halos and radio mini-halos in galaxy clusters" (PDF). Astronomy & Astrophysics. 486 (3): L31–L34. arXiv:0806.1817. Bibcode:2008A&A...486L..31C. doi:10.1051/0004-6361:200810179. ISSN 0004-6361.
- ↑ 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". Astronomy & Astrophysics. 484 (2): 327–340. arXiv:0803.4084. doi:10.1051/0004-6361:200809622. ISSN 0004-6361.
- ↑ 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". Monthly Notices of the Royal Astronomical Society. 456 (2): 1565–1578. arXiv:1511.07884. doi:10.1093/mnras/stv2784. ISSN 0035-8711.
{{cite journal}}: CS1 maint: multiple names: authors list (link)
External links
- MS 1455.0+2232 BCG on WikiSky: DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images
- MS 1455.0+2232 BCG on SIMBAD
