Astronomy:MS 0440+0204 BCG

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MS 0440+0204 BCG
File:Image of MS 0440+0204 BCG.png
DESI Legacy Surveys image of MS 0440+0204 BCG
Observation data (J2000.0 epoch)
ConstellationTaurus
Right ascension 04h 43m 09.78s[1]
Declination+02° 10′ 19.83″[1]
Redshift0.198680[1]
Helio radial velocity59,563 ± 39 km/s[1]
Distance2,862.2 ± 200.4 Mly (877.56 ± 61.43 Mpc)[1]
Group or clusterMS 0440+0204
Characteristics
TypecD[1]
Size~716,000 ly (219.4 kpc) (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

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 × 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 × 1023 W Hz-1 and the radio flux density is 30.2 ± 0.07 mJy.[10]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 "NED Search results for MS 0440+0204 BCG (LEDA 1218292)". https://ned.ipac.caltech.edu/byname?objname=LEDA+1218292&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1. 
  2. ↑ 2.0 2.1 2.2 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" (in en). The Astrophysical Journal 416: 444. doi:10.1086/173249. ISSN 0004-637X. Bibcode: 1993ApJ...416..444L. https://ui.adsabs.harvard.edu/scan/manifest/1993ApJ...416..444L?art=true. 
  3. ↑ 3.0 3.1 3.2 Carrasco, E. R.; Verdugo, T.; Motta, V.; Foëx, G.; Ellingson, E.; Gomez, P. L.; Falco, E.; Limousin, M. (2021-09-01). "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. doi:10.3847/1538-4357/ac0c1b. ISSN 0004-637X. Bibcode: 2021ApJ...918...61C. 
  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" (in en). The Astrophysical Journal 497 (2): 573–586. doi:10.1086/305471. ISSN 0004-637X. Bibcode: 1998ApJ...497..573G. 
  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" (in en). The Astrophysical Journal Supplement Series 94: 583. doi:10.1086/192083. ISSN 0067-0049. Bibcode: 1994ApJS...94..583G. 
  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" (in en). Monthly Notices of the Royal Astronomical Society 389 (4): 1637–1654. doi:10.1111/j.1365-2966.2008.13699.x. ISSN 0035-8711. Bibcode: 2008MNRAS.389.1637B. 
  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" (in en). Monthly Notices of the Royal Astronomical Society 395 (1): 462–471. doi:10.1111/j.1365-2966.2009.14534.x. ISSN 0035-8711. Bibcode: 2009MNRAS.395..462P. https://articles.adsabs.harvard.edu/pdf/2009MNRAS.395..462P. 
  8. ↑ Lidman, C.; Suherli, J.; Muzzin, A.; Wilson, G.; Demarco, R.; Brough, S.; Rettura, A.; Cox, J. et al. (2012-11-01). "Evidence for significant growth in the stellar mass of brightest cluster galaxies over the past 10 billion years". Monthly Notices of the Royal Astronomical Society 427 (1): 550–568. doi:10.1111/j.1365-2966.2012.21984.x. ISSN 0035-8711. Bibcode: 2012MNRAS.427..550L. https://watermark02.silverchair.com/stw1184.pdf?token=AQECAHi208BE49Ooan9kkhW_Ercy7Dm3ZL_9Cf3qfKAc485ysgAAA1EwggNNBgkqhkiG9w0BBwagggM-MIIDOgIBADCCAzMGCSqGSIb3DQEHATAeBglghkgBZQMEAS4wEQQMiZfLe7D_TW60tAhwAgEQgIIDBDZCq-RS_Iy7ENmHiyUXYagR4_gUbWutqd4pyWpX72POZRQ-Bz0VFzpNZvJiL61yWL_7cGtYOFIul9bnTig9_URUHqjRnacxqfwzQzkoOxZ212Nb3YQ9wLstcOtUZ6-k5cFATI3IS-HbLVKr4-BQcSDnC36yMaJkeBsG7X4QMiC6PaBFJVJkcJW5_3qNA9V650RR5y7vTQ6Y2rwusAm4rpR09uX7P1sms6siGF16ghtp66OK4wB83Jt9ZYB7ZapCi-MBmfaExSxWdUcWfDcCsE4kgcryxT0_4DKDVZrGe51kj5RVEpVLYKzacKh4xSf389ib_UsJA05mms2X2uW3fzj4kfumtKWgjQtUiEeUdEPUauSCw6nBHJTmhyNulz1LUZLw8qS2tRL_YFko3LZZzMxMGjVOqSErVcMRZotzbg3loAz_DLX5gJTLDfH2R-QioLGMQnyXI-jb2WYINBYSL5lk5L3VbzReSPoYZUPI3W704IWwzfUWciYPqwlBs3C_NKiT-OmgzCtnPdGYtpwFVC0PD4PaCuCXcl40wE3ITKp2olpABfcZBTXRe3m-lwAJXhD5ODlBzPU6JzFluhIm2SP74Z65i9_5oUoxK-GolQLl1e2rFIHYHRgckoU44T0JEziFF0ecl6S5WSQuTWEsBn9NgQ6bbVSJkCICbNG0H-yH1mwomCYt7kkdrd-bTLm6rompfsnbnx0N00a-orbMvbSXs5Rdu9JCpxfBBlGved9kBhSZrSMNC8aRk3irQA2eYMw8QcSDdPWRTkbrzF7MazbKBNwlkvONfxJbrKxLgi7HWbjusZ3wVJoZVog1zyxEAiAQcOO22VdmWNQIRv9pCiBgf3LCrfkUN5pyafjz-hrQ25RGFxKKr8zPRBHkywqE5PxUPyFFTps6L_oOV_wuf1aBKGnYAZXsO4wAMd1Py-p6-wHaCVHSWrXp_u7ne3Q0zL9MgdD-Oh8LQAqpVaIys5NzHU4C0kzngAkU3KiTKcNYlJuI4icmgNcJODKJ0VxNtN2_A6w. 
  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" (in en). Monthly Notices of the Royal Astronomical Society 456 (2): 1565–1578. doi:10.1093/mnras/stv2784. ISSN 0035-8711. 
  10. ↑ Hart, Quyen N.; Stocke, John T.; Hallman, Eric J. (2009-10-15). "X-Ray Point Sources and Radio Galaxies in Clusters of Galaxies". The Astrophysical Journal 705 (1): 854–867. doi:10.1088/0004-637x/705/1/854. ISSN 0004-637X. Bibcode: 2009ApJ...705..854H. https://iopscience.iop.org/article/10.1088/0004-637X/705/1/854#apj317756t3fn1. 



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