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MS 0440+0204 BCG

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Type-cD galaxy in the constellation Taurus
MS 0440+0204 BCG
DESI Legacy Surveys image of MS 0440+0204 BCG
Observation data (J2000.0 epoch)
Constellation Taurus
Right ascension 04h 43m 09.78s[1]
Declination +02°10′19.83′′[1]
Redshift 0.198680[1]
Heliocentric radial velocity 59,563 ± 39 km/s [1]
Distance 2,862.2±200.4Mly (877.56±61.43Mpc)[1]
Group or cluster MS 0440+0204
magnitude(J)13.23[1]
Characteristics
Type cD[1]
Size~716,000ly (219.4kpc) (estimated)[1]
Other designations
2MASX J04430994+0210190, LEDA 1218292, MS 0440+0204:[BHB2008] BCG, NVSS J044309+021013, RX J0443.1+0210, VLSS J0443.1+0210[1]

MS 0440+0204 BCG is a massive elliptical galaxy of type-cD located in the constellation of Taurus. The redshift of the galaxy is (z) 0.198[1] and it was first discovered by astronomers in October 1993. This galaxy contains multiple nuclei and is the brightest cluster galaxy (BCG) located in the center of the MS 0440+0204 galaxy cluster.[2] [3]

Description

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MS 0440+204 BCG is categorized as a type-cD galaxy.[4] It has a compact appearance[5] and is made up of six close galaxies or components merging together to form a single giant elliptical galaxy.[2] [3] The velocity difference of the two known components is estimated to be 2,600 kilometers per second. A low surface brightness halo with a diameter of 157 kiloparsecs envelops the components.[3] The core of the BCG has a red appearance with a total near ultraviolet magnitude of 21.84 ± 0.44.[6] [7] The total mass of the BCG is estimated to be 0.53 ×ばつ 1012 Mʘ.[8]

There is an intermediate red stellar population in the BCG, but no presence of a young stellar component. The stars in the inner regions have an estimated age of 4,370 ± 160 million years old, while the stars in the outer regions are around 15,400 ± 6280 million years.[9]

A study published in 1993, has found the presence of 15 gravitational lensing arc features surrounding the BCG based on charged-coupled device (CCD) imaging. The largest known arc has a length of 10 arcseconds, however it is unresolved, while the other arc features trace out a 90 kiloparsec radius. There are also detections of hydrogen-alpha emission, suggesting cooling flow may be present in the BCG.[2] In 2009, the BCG was found to contain a radio source, classifying it as a radio galaxy. The radio power is estimated to be 34.2 ± 0.1 ×ばつ 1023 W Hz-1 and the radio flux density is 30.2 ± 0.07 mJy.[10]

References

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  1. 1 2 3 4 5 6 7 8 9 10 "NED Search results for MS 0440+0204 BCG (LEDA 1218292)". NASA/IPAC Extragalactic Database. Retrieved 2026年05月08日.
  2. 1 2 3 Luppino, G. A.; Gioia, I. M.; Annis, J.; Le Fevre, O.; Hammer, F. (October 1993). "The Complex, Gravitationally Lensed Arc System in the X-Ray--selected Cluster of Galaxies MS 0440+0204". The Astrophysical Journal. 416: 444. Bibcode:1993ApJ...416..444L. doi:10.1086/173249. ISSN 0004-637X.
  3. 1 2 3 Carrasco, E. R.; Verdugo, T.; Motta, V.; Foëx, G.; Ellingson, E.; Gomez, P. L.; Falco, E.; Limousin, M. (2021年09月01日). "Dissecting the strong lensing galaxy cluster MS 0440+0204 II. New optical spectroscopic observations in a wider area and cluster dynamical state". The Astrophysical Journal. 918 (2): 61. arXiv:2106.15583 . Bibcode:2021ApJ...918...61C. doi:10.3847/1538-4357/ac0c1b . ISSN 0004-637X.
  4. ↑ Gioia, I. M.; Shaya, E. J.; Le Fèvre, O.; Falco, E. E.; Luppino, G. A.; Hammer, F. (April 1998). "The Lensing Cluster MS 0440+0204 Seen by HST, ROSAT, and ASCA. I. Cluster Properties". The Astrophysical Journal. 497 (2): 573–586. arXiv:astro-ph/9712004 . Bibcode:1998ApJ...497..573G. doi:10.1086/305471. ISSN 0004-637X.
  5. ↑ Gioia, I. M.; Luppino, G. A. (October 1994). "The EMSS Catalog of X-Ray--selected Clusters of Galaxies. I. an Atlas of CCD Images of 41 Distant Clusters". The Astrophysical Journal Supplement Series. 94: 583. arXiv:astro-ph/9405069 . Bibcode:1994ApJS...94..583G. doi:10.1086/192083. ISSN 0067-0049.
  6. ↑ Bildfell, Chris; Hoekstra, Henk; Babul, Arif; Mahdavi, Andisheh (October 2008). "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. arXiv:0802.2712 . Bibcode:2008MNRAS.389.1637B. doi:10.1111/j.1365-2966.2008.13699.x . ISSN 0035-8711.
  7. ↑ Pipino, A.; Kaviraj, S.; Bildfell, C.; Babul, A.; Hoekstra, H.; Silk, J. (May 2009). "Evidence for recent star formation in BCGs: a correspondence between blue cores and UV excess". Monthly Notices of the Royal Astronomical Society. 395 (1): 462–471. arXiv:0807.2760 . Bibcode:2009MNRAS.395..462P. doi:10.1111/j.1365-2966.2009.14534.x . ISSN 0035-8711.
  8. ↑ Lidman, C.; Suherli, J.; Muzzin, A.; Wilson, G.; Demarco, R.; Brough, S.; Rettura, A.; Cox, J.; DeGroot, A.; Yee, H. K. C.; Gilbank, D.; Hoekstra, H.; Balogh, M.; Ellingson, E.; Hicks, A. (2012年11月01日). "Evidence for significant growth in the stellar mass of brightest cluster galaxies over the past 10 billion years" (PDF). Monthly Notices of the Royal Astronomical Society. 427 (1): 550–568. arXiv:1208.5143 . Bibcode:2012MNRAS.427..550L. doi:10.1111/j.1365-2966.2012.21984.x . ISSN 0035-8711.
  9. ↑ Loubser, S. I.; Babul, A.; Hoekstra, H.; Mahdavi, A.; Donahue, M.; Bildfell, C.; Voit, G. M. (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.
  10. ↑ Hart, Quyen N.; Stocke, John T.; Hallman, Eric J. (2009年10月15日). "X-Ray Point Sources and Radio Galaxies in Clusters of Galaxies". The Astrophysical Journal. 705 (1): 854–867. arXiv:0908.3158 . Bibcode:2009ApJ...705..854H. doi:10.1088/0004-637x/705/1/854. ISSN 0004-637X.
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