Astronomy:Abell 478 BCG

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Abell 478 BCG
Pan-STARRS image of Abell 478 BCG
Observation data (J2000.0 epoch)
ConstellationTaurus
Right ascension 04h 13m 25.30s[1]
Declination+10° 27′ 54.49″[1]
Redshift0.086003[1]
Helio radial velocity25,783 ± 100 km/s[1]
Distance1,239.4 ± 87.0 Mly (379.99 ± 26.68 Mpc)[1]
Group or clusterAbell 478
Characteristics
TypeBrCLG[1]
Size~560,000 ly (171.8 kpc) (estimated)[1]
Other designations
2MASX J04132526+1027551, Abell 478:[ZAC2011] BCG, PGC 14685, NVSS J041325+102754, 2XMM J041325.2+102752[1]

Abell 478 BCG (short for Abell 478 Brightest Cluster Galaxy) is a Type-cD galaxy[2] located in the constellation of Taurus. The redshift of the galaxy is (z) 0.086[1] and it was first discovered from a 20 centimeter Very Large Array (VLA) study of Abell clusters in July 1993 and such, is categorized as a radio galaxy.[3] It is the brightest cluster galaxy of the cool-core galaxy cluster Abell 478, shown dominating its center.[4]

Description

Abell 478 BCG is classified as a central dominant galaxy. The continuous star formation of the galaxy is estimated to be around 10 Mʘ per year and the supermassive black hole lying in the center of the galaxy is found to be growing with a change rate of 1.6+1.2-0.4 x 10-2 Mʘ per year. The total bulge mass has been estimated as 28 ± 1 × 1011 Mʘ.[5]

The nucleus of Abell 478 BCG is shown as active with a presence of central radio source, described as point-like.[4][2] The inner region of the core is found to contain four hotspot features with three located in the northern direction while the fourth is located in the southern direction. All the hotspots are estimated to be positioned between 30 and 60 kiloparsecs from each other.[4] A radio observation has found two radio lobes, described as weak with an extend of four kiloparsecs in diameter and also pointing towards the directions of southwest and northeast. There is also detection of X-ray emission being double peaked on both eastern and western sides of its nucleus. The total radio flux of the source at 1.4 GHz frequencies, is estimated to be 30 mJy, with around 35% of the flux being contributed by the lobes. Evidence also found the presence of X-ray cavities, with radio plasma sweeping out the gas from it.[2] The total cavity power is estimated to be 100.0+80.0-20.0 × 1042 erg-1.[6] The radio core is found to have a flat radio spectrum with the total luminosity of 39.85 ± 0.03 at 5 GHz.[7]

A study published in December 2001, has found detection of molecular gas in the galaxy. The total mass of the gas is estimated to be 4.5 ± 2.6 × 109 Mʘ and the mass outflow rate has been estimated to be 616 Mʘ per year. The dust mass has been found to be approximately 1.0 × 107 Mʘ.[8]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 "NED Search results for Abell 478 BCG (PGC 14685)". https://ned.ipac.caltech.edu/byname?objname=LEDA+14685&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1. 
  2. ↑ 2.0 2.1 2.2 Sun, M.; Jones, C.; Murray, S. S.; Allen, S. W.; Fabian, A. C.; Edge, A. C. (April 2003). "Chandra Observations of the Galaxy Cluster A478: The Interaction of Hot Gas and Radio Plasma in the Core, and an Improved Determination of the Compton y-Parameter" (in en). The Astrophysical Journal 587 (2): 619–624. doi:10.1086/368300. ISSN 0004-637X. Bibcode: 2003ApJ...587..619S. 
  3. ↑ Owen, Frazer N.; White, Richard A.; Ge, Jingping (July 1993). "A 20 Centimeter VLA Survey of Abell Clusters of Galaxies. III. Images and Optical Identifications" (in en). The Astrophysical Journal Supplement Series 87: 135. doi:10.1086/191800. ISSN 0067-0049. Bibcode: 1993ApJS...87..135O. https://articles.adsabs.harvard.edu/pdf/1993ApJS...87..135O. 
  4. ↑ 4.0 4.1 4.2 Sanderson, Alastair J. R.; Finoguenov, Alexis; Mohr, Joseph J. (September 2005). "Possible AGN Shock Heating in the Cool-Core Galaxy Cluster Abell 478" (in en). The Astrophysical Journal 630 (1): 191–205. doi:10.1086/431750. ISSN 0004-637X. Bibcode: 2005ApJ...630..191S. 
  5. ↑ Rafferty, D. A.; McNamara, B. R.; Nulsen, P. E. J.; Wise, M. W. (November 2006). "The Feedback-regulated Growth of Black Holes and Bulges through Gas Accretion and Starbursts in Cluster Central Dominant Galaxies" (in en). The Astrophysical Journal 652 (1): 216–231. doi:10.1086/507672. ISSN 0004-637X. Bibcode: 2006ApJ...652..216R. 
  6. ↑ Pulido, F. A.; McNamara, B. R.; Edge, A. C.; Hogan, M. T.; Vantyghem, A. N.; Russell, H. R.; Nulsen, P. E. J.; Babyk, I. et al. (2018-02-01). "The Origin of Molecular Clouds in Central Galaxies". The Astrophysical Journal 853 (2): 177. doi:10.3847/1538-4357/aaa54b. ISSN 0004-637X. Bibcode: 2018ApJ...853..177P. 
  7. ↑ Hlavacek-Larrondo, J.; Fabian, A. C.; Edge, A. C.; Hogan, M. T. (2012-07-21). "On the hunt for ultramassive black holes in brightest cluster galaxies". Monthly Notices of the Royal Astronomical Society 424 (1): 224–231. doi:10.1111/j.1365-2966.2012.21187.x. Bibcode: 2012MNRAS.424..224H. 
  8. ↑ 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. 



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