Astronomy:Abell 1942 BCG

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Abell 1942 Brightest Cluster Galaxy
Abell 1942 BCG, as seen by DESI Legacy Surveys
Observation data (J2000.0 epoch)
ConstellationVirgo
Right ascension 14h 38m 21.87s[1]
Declination+03° 40′ 13.21″ [1]
Redshift0.224679[1]
Helio radial velocity67,357 km/s[1]
Distance2.731 Gly (832.3 Mpc)
Group or clusterAbell 1942
Apparent magnitude (V)0.118
Apparent magnitude (B)0.156
Characteristics
TypeBrCLG, AGN[1]
Size~938,500 ly (287.74 kpc) (estimated)[1]
Apparent size (V)0.30' x 0.23'
Notable featuresBrightest cluster galaxy, radio galaxy
Other designations
PKS 1435+038, 2MASX J14382188+0340138, LEDA 1256558, PMN J1438+0340, MRC 1435+038, NVSS J143822+034016, 2CXO J143821.8+034012[1]

Abell 1942 BCG (short for Abell 1942 Brightest Cluster Galaxy), also known as PGC 1256558, is a massive elliptical galaxy of type-cD residing as the brightest cluster galaxy of the Abell 1942 galaxy cluster, located in the constellation Virgo. With a redshift of 0.224, the galaxy is located nearly 2.7 billion light-years away from Earth.[1]

Characteristics

Abell 1942 BCG is one of the largest galaxies with a diameter of 939,200 light-years across. A luminous red galaxy observed by Sloan Digital Sky Survey, the total stellar mass of the galaxy is estimated to be ~3 × 1011 Msolar.[2] It is also classfied as an active wide-angled tailed radio galaxy.[3][4][5] With an astrophysical jet speed within of the range (0.3-0.7)c[6] and a peaked spectrum source of between 1.4 GHz and 325 MHz,[7] Abell 1942 BCG is found to be radio-luminous with values below 1022 WHz−1 at 1.4 GHz.[8]

Moreover, Abell 1942 BCG contains an extended radio source[9][10] listed by researchers in the 408-MHz Molonglo Reference Catalogue[11] and also Parkes Catalogue of radio sources.[12] Its luminosity function is estimated to be frequencies of 400 and 2700 MHz.[13]

Abell 1942 BCG is aligned along its major axis towards its parent cluster.[14][15] It has a large galactic halo displaying a light profile with surface brightness ranging from 27.5 mag arcsec-2 at 100 kpc to ~32 mag arcsec-2 at 700 kpc as observed through r-bands.[16] Such of these light profiles in massive galaxies like Abell 1942 BCG tend to reach up to several hundreds of kilometers.[17] Because Abell 1942 BCG has special properties, researchers theorized it might have been formed through the process of galactic cannibalism as the galaxy merges with its surrounding satellite galaxies thus increasing its luminosity.[18][19] As merger process continues, the mass of Abell 1942 BCG is build-up while at the same time, the number of satellite galaxies reduces.[20]

The star formation in Abell 1942 BCG, is estimated to contribute less mass friction and a stellar age of 200 Myr. Because the galaxy host's cluster has X-ray properties and the young star population, this strongly hints the star formation of Abell 1942 BCG is fueled by gas cooling out of the intracluster medium.[21] As observed by Galaxy Evolution Explorer (GALEX), Spitzer Space Telescope, and Two Micron All Sky Survey (2MASS), researchers found the galaxy displays ultraviolet (38%) and mid-infrared emission (43%) from 8 to 160 μm, above as expected.[22]

Abell 1942

The galaxy cluster where Abell 1942 BCG is residing, is found be a rich cluster.[23][24] As observed by researchers, they found it has a mean redshift value of z = 0.22513 \pm 0.0008 and also a velocity dispersion sigma of = 908^{+147}_{-139} km/s. Through the analysis, they found the cluster is relaxed with no signs of remarkable features and a fair distribution of the X-ray emission traces.[25]

They also found Abell 1942 has two possible optical substructures, seen at ~5 arcmin from the center towards the Northwest and the Southwest direction. However, they are not confirmed by the velocity field. The clumps are however, kinematically bound to the main structure of Abell 1942. Upon looking at the velocity dispersion through usage of the T_X-sigma scaling relation, they found the temperature is in good agreement with measured galaxies velocities.

According to researchers conducting a photometric redshift analysis, they suggest the weak lensing signal observed at the south part of the cluster, is contributed to dark matter concentration by background sources, that are possibly distributed as a single filamentary structure.[26][27] Thus, they could use limiting magnitude of H = 22, for detection of such clusters with appropriate mass that have comparable redshifts with the mean redshift of background sources.[28]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 "NED Search results for Abell 1942 BCG". https://ned.ipac.caltech.edu/byname?objname=Leda+1256558&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1. 
  2. ↑ Barber, Tom; Meiksin, Avery; Murphy, Tara (2007-05-01). "Properties of luminous red galaxies in the Sloan Digital Sky Survey". Monthly Notices of the Royal Astronomical Society 377 (2): 787–805. doi:10.1111/j.1365-2966.2007.11650.x. ISSN 0035-8711. Bibcode: 2007MNRAS.377..787B. 
  3. ↑ Owen, Frazer N.; Ledlow, Michael J.; Keel, William C. (1996-01-01). "Optical Spectroscopy of Radio Galaxies in Abell Clusters II. BL Lacs and FR I Unification". The Astronomical Journal 111: 53. doi:10.1086/117759. ISSN 0004-6256. Bibcode: 1996AJ....111...53O. https://ui.adsabs.harvard.edu/abs/1996AJ....111...53O. 
  4. ↑ Lin, Yen-Ting; Shen, Yue; Strauss, Michael A.; Richards, Gordon T.; Lunnan, Ragnhild (2010-11-01). "On the Populations of Radio Galaxies with Extended Morphology at z < 0.3". The Astrophysical Journal 723 (2): 1119–1138. doi:10.1088/0004-637X/723/2/1119. ISSN 0004-637X. Bibcode: 2010ApJ...723.1119L. https://ui.adsabs.harvard.edu/abs/2010ApJ...723.1119L. 
  5. ↑ Owen, Frazer N.; Ledlow, Michael J.; Keel, William C. (1995-01-01). "Optical Spectroscopy of Radio Galaxies in abell Clusters. I. Redshifts and Emission-Line Properties". The Astronomical Journal 109: 14. doi:10.1086/117252. ISSN 0004-6256. Bibcode: 1995AJ....109...14O. https://ui.adsabs.harvard.edu/abs/1995AJ....109...14O. 
  6. ↑ Jetha, Nazirah N.; Hardcastle, Martin J.; Sakelliou, Irini (2006-05-01). "Jet speeds in wide-angle tailed radio galaxies". Monthly Notices of the Royal Astronomical Society 368 (2): 609–618. doi:10.1111/j.1365-2966.2006.10155.x. ISSN 0035-8711. Bibcode: 2006MNRAS.368..609J. 
  7. ↑ Stein, Y.; Vollmer, B.; Boch, T.; Landais, G.; Vannier, P.; Brouty, M.; Allen, M. G.; Derriere, S. et al. (2021-11-01). "The SPECFIND V3.0 catalog of radio continuum cross-identifications and spectra: Reaching lower frequencies". Astronomy and Astrophysics 655: A17. doi:10.1051/0004-6361/202039659. ISSN 0004-6361. Bibcode: 2021A&A...655A..17S. https://ui.adsabs.harvard.edu/abs/2021A&A...655A..17S. 
  8. ↑ Best, P. N.; Kauffmann, G.; Heckman, T. M.; Ivezić, Ž. (2005-09-01). "A sample of radio-loud active galactic nuclei in the Sloan Digital Sky Survey". Monthly Notices of the Royal Astronomical Society 362 (1): 9–24. doi:10.1111/j.1365-2966.2005.09283.x. ISSN 0035-8711. Bibcode: 2005MNRAS.362....9B. 
  9. ↑ Palimaka, J. J.; Bridle, A. H.; Fomalont, E. B. (1980-08-01). "Extended radio sources and elliptical galaxies. V. Optical positions for 40 identified sources.". The Astronomical Journal 85: 995–1002. doi:10.1086/112762. ISSN 0004-6256. Bibcode: 1980AJ.....85..995P. https://ui.adsabs.harvard.edu/abs/1980AJ.....85..995P. 
  10. ↑ Wills, B. J. (1976-12-01). "Optical identifications of radio sources using accurate radio and optical positions. II.". The Astronomical Journal 81: 1031–1052. doi:10.1086/111985. ISSN 0004-6256. Bibcode: 1976AJ.....81.1031W. https://ui.adsabs.harvard.edu/abs/1976AJ.....81.1031W. 
  11. ↑ Robertson, J. G.; Roach, G. J. (1990-12-01). "Molonglo radio sources in the directions of southern Abell clusters.". Monthly Notices of the Royal Astronomical Society 247: 387–399. ISSN 0035-8711. Bibcode: 1990MNRAS.247..387R. https://ui.adsabs.harvard.edu/abs/1990MNRAS.247..387R. 
  12. ↑ Day, G. A.; Shimmins, A. J.; Ekers, R. D.; Cole, D. J. (1966-02-01). "The Parkes catalogue of radio sources, declination zone 0° to +20°". Australian Journal of Physics 19: 35. doi:10.1071/PH660035. ISSN 0004-9506. Bibcode: 1966AuJPh..19...35D. https://ui.adsabs.harvard.edu/abs/1966AuJPh..19...35D. 
  13. ↑ Merkelijn, J. K. (1971-11-01). "A Determination of the Luminosity Function of Radiogalaxies at 400 and 2700 MHz". Astronomy and Astrophysics 15: 11. ISSN 0004-6361. Bibcode: 1971A&A....15...11M. https://ui.adsabs.harvard.edu/abs/1971A&A....15...11M. 
  14. ↑ Hao, Jiangang; Kubo, Jeffrey M.; Feldmann, Robert; Annis, James; Johnston, David E.; Lin, Huan; McKay, Timothy A. (2011-10-01). "Intrinsic Alignment of Cluster Galaxies: The Redshift Evolution". The Astrophysical Journal 740 (1): 39. doi:10.1088/0004-637X/740/1/39. ISSN 0004-637X. Bibcode: 2011ApJ...740...39H. https://ui.adsabs.harvard.edu/abs/2011ApJ...740...39H. 
  15. ↑ Lambas, Diego G.; Groth, Edward J.; Peebles, P. J. E. (1988-04-01). "Alignments of Brightest Cluster Galaxies with Large-Scale Structures". The Astronomical Journal 95: 996. doi:10.1086/114695. ISSN 0004-6256. Bibcode: 1988AJ.....95..996L. https://ui.adsabs.harvard.edu/abs/1988AJ.....95..996L. 
  16. ↑ Zibetti, Stefano; White, Simon D. M.; Schneider, Donald P.; Brinkmann, Jon (2005-04-01). "Intergalactic stars in z~ 0.25 galaxy clusters: systematic properties from stacking of Sloan Digital Sky Survey imaging data". Monthly Notices of the Royal Astronomical Society 358 (3): 949–967. doi:10.1111/j.1365-2966.2005.08817.x. ISSN 0035-8711. Bibcode: 2005MNRAS.358..949Z. 
  17. ↑ Huang, Song; Leauthaud, Alexie; Greene, Jenny E.; Bundy, Kevin; Lin, Yen-Ting; Tanaka, Masayuki; Miyazaki, Satoshi; Komiyama, Yutaka (2018-04-01). "Individual stellar haloes of massive galaxies measured to 100 kpc at 0.3 < z < 0.5 using Hyper Suprime-Cam". Monthly Notices of the Royal Astronomical Society 475 (3): 3348–3368. doi:10.1093/mnras/stx3200. ISSN 0035-8711. Bibcode: 2018MNRAS.475.3348H. 
  18. ↑ Ostriker, J. P.; Tremaine, S. D. (1975-12-01). "Another evolutionary correction to the luminosity of giant galaxies.". The Astrophysical Journal 202: L113–L117. doi:10.1086/181992. ISSN 0004-637X. Bibcode: 1975ApJ...202L.113O. https://ui.adsabs.harvard.edu/abs/1975ApJ...202L.113O. 
  19. ↑ Hausman, M. A.; Ostriker, J. P. (1978-09-01). "Galactic cannibalism. III. The morphological evolution of galaxies and clusters.". The Astrophysical Journal 224: 320–336. doi:10.1086/156380. ISSN 0004-637X. Bibcode: 1978ApJ...224..320H. https://ui.adsabs.harvard.edu/abs/1978ApJ...224..320H. 
  20. ↑ Pobre, Savannah; Dalal, Roohi; Strauss, Michael A.; Lin, Yen-Ting (2023-02-09). "Are Brightest Cluster Galaxies Special?". Research Notes of the AAS 7 (2): 19. doi:10.3847/2515-5172/acb9e1. ISSN 2515-5172. Bibcode: 2023RNAAS...7...19P. 
  21. ↑ Pipino, A.; Kaviraj, S.; Bildfell, C.; Babul, A.; Hoekstra, H.; Silk, J. (2009-05-01). "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. doi:10.1111/j.1365-2966.2009.14534.x. ISSN 0035-8711. Bibcode: 2009MNRAS.395..462P. 
  22. ↑ Hoffer, Aaron S.; Donahue, Megan; Hicks, Amalia; Barthelemy, R. S. (2012-03-01). "Infrared and Ultraviolet Star Formation in Brightest Cluster Galaxies in the ACCEPT Sample". The Astrophysical Journal Supplement Series 199 (1): 23. doi:10.1088/0067-0049/199/1/23. ISSN 0067-0049. Bibcode: 2012ApJS..199...23H. https://ui.adsabs.harvard.edu/abs/2012ApJS..199...23H. 
  23. ↑ Hao, Jiangang; McKay, Timothy A.; Koester, Benjamin P.; Rykoff, Eli S.; Rozo, Eduardo; Annis, James; Wechsler, Risa H.; Evrard, August et al. (2010-12-01). "A GMBCG Galaxy Cluster Catalog of 55,424 Rich Clusters from SDSS DR7". The Astrophysical Journal Supplement Series 191 (2): 254–274. doi:10.1088/0067-0049/191/2/254. ISSN 0067-0049. Bibcode: 2010ApJS..191..254H. https://ui.adsabs.harvard.edu/abs/2010ApJS..191..254H. 
  24. ↑ Bahcall, Neta A. (1999). "1999ApJ...525C.873B Page C873". The Astrophysical Journal 525C: 873. Bibcode: 1999ApJ...525C.873B. https://adsabs.harvard.edu/full/1999ApJ...525C.873B. Retrieved 2024-06-10. 
  25. ↑ Capelato, H. V.; Proust, D.; Neto, G. B. LIma; Santos, W. A.; Sodre Jr., L. (December 2008). "Enlightening the structure and dynamics of Abell 1942". Astronomy & Astrophysics 492 (2): 345–354. doi:10.1051/0004-6361:200810427. ISSN 0004-6361. Bibcode: 2008A&A...492..345C. 
  26. ↑ Capelato, H. V.; Proust, D.; Lima Neto, G. B.; Santos, W. A.; Sodré, L., Jr. (2008-12-01). "The structure and dynamics of Abell 1942". Astronomy and Astrophysics 492 (2): 345–354. doi:10.1051/0004-6361:200810427. ISSN 0004-6361. Bibcode: 2008A&A...492..345C. https://ui.adsabs.harvard.edu/abs/2008A&A...492..345C. 
  27. ↑ Erben, Th.; van Waerbeke, L.; Mellier, Y.; Schneider, P.; Cuillandre, J. -C.; Castander, F. J.; Dantel-Fort, M. (2000-03-01). "Mass-detection of a matter concentration projected near the cluster Abell 1942: Dark clump or high-redshift cluster?". Astronomy and Astrophysics 355: 23–36. ISSN 0004-6361. Bibcode: 2000A&A...355...23E. https://ui.adsabs.harvard.edu/abs/2000A&A...355...23E. 
  28. ↑ Gray, M. E.; Ellis, R. S.; Lewis, J. R.; McMahon, R. G.; Firth, A. E. (2001-07-11). "Infrared constraints on the dark mass concentration observed in the cluster Abell 1942". Monthly Notices of the Royal Astronomical Society 325 (1): 111–118. doi:10.1046/j.1365-8711.2001.04393.x. ISSN 0035-8711. Bibcode: 2001MNRAS.325..111G. 



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