Astronomy:Abell 478

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Abell 478
Abell 478 seen by Legacy Surveys
Abell 478 seen by Legacy Surveys
Observation data (Epoch J2000)
Constellation(s)Taurus
Right ascension 04h 13m 20.7s[1]
Declination+10° 28′ 35″[1]
Richness class2[2]
Redshift0.0881 (26 412 km/s)[1]
Distance
(co-moving)		367 Mpc (1,197 Mly) h−10.705
ICM temperature7.94 keV[3]
Binding mass7.68×1014[3] M☉
X-ray flux(7.9 ± 1.1)×10−11 erg s−1 cm−2 (0.1–2.4 keV)
Other designations
ZwCl 0410.8+1023; MCXC J0413.4+1028; SWIFT J0413.5+1027; XSS J04127+1029; RX J0413.4+1027; RXGCC 165
See also: Galaxy group, Galaxy cluster, List of galaxy groups and clusters

Abell 478 is an X-ray luminous galaxy cluster listed in the Abell catalogue. Abell 478 has a reasonably long exposure for 42.4 ksec by Chandra X-ray Observatory.[4] A dusty quasar found in the background of Abell 478 that is detected by 15 m James Clerk Maxwell Telescope.[5] The center of Abell 478 has a temperature of 2.46 keV, the outer regions has a temperature of 4.14 keV, indicating a cool flow core.[6] Abell 478 has been deeply studied by X-ray observatories and satellites like EXOSAT, Einstein Observatory, ROSAT, Very Long Baseline Array, Chandra X-ray Observatory, XMM-Newton and Advanced Satellite for Cosmology and Astrophysics (ASCA)[7], due to Abell 478 is considered one of the largest cooling flow cores, and there is two X-ray cavities detected.

Properties

A study shows that Abell 478 is considered a dynamically relaxed galaxy cluster. Chandra X-ray Observatory found two X-ray cavities within central 15 MPC of Abell 478. These two cavities mainly caused by the past activities of the central supermassive black hole (SMBH). The current radio lobes are much smaller than the X-ray cavities, and the current radio strength is at least 10 times smaller than the minimum strength needed to create the X-ray cavities, indicating the central supermassive black hole of Abell 478 is significantly more active in the past.[4]

Abell 478 is found to have one of the largest cooling flows ever observed, with cooling rate of ~1000 solar masses a year. A Marginal Carbon Monoxide (CO) Detection has been conducted, found that Abell 478 has an amount of Neutral Hydrogen (4.5 ± 2.2 × 10⁹ M☉), but not significant. Abell 478 has a X-ray morphology of near circular, has an ellipticity of 0.2. This supports the idea that Abell 478 is dynamically relaxed.[4] A study of Dark matter have found that Abell 478 has cuspy dark matter profile with inner profile of n = 1, in agreement of the Cold Dark-Matter Model (CDM).[8]

It is found that there is extra gas around the galaxy cluster that is absorbing the X-ray Gas, which is found that Abell 478 has an excess X-ray absorption (N_H) of ~4–5 × 10²¹ cm⁻². However, an analysis suggests that the excess gas that is absorbing the X-ray Gas is Galactic Origin, rather than Extragalactic origin.[7] Another X-ray study found that the fact that Abell 478 is near circular is rejected, as Abell 478 is found to be significantly elliptical, from an analysis using the high resolution X-ray image from ROSAT.[9] X-ray observations of Abell 478 found that Abell 478 is consistent with a hot, smooth, and dilute intracluster medium, centered on the central cD galaxy (PGC 14685).[10]

Four hotspots are detected in the Intracluster Medium (ICM), with temperatures twice hotter than its surrounding gas. The excess energy detected in these hotspots is approximately 10 times the energy needed to create X-ray Cavities, suggesting that they are created by strong shocks of jets from the central Active Galactic Nuclei (AGN). The dark matter profile of Abell 478 is characterized of soft core, with a logarithmic slope of 0.35 ± 0.22. This is significantly flatter than the NFW profile (slope 1.0), but is consistent with other clusters containing a central dominating galaxy (cD galaxy), revealing that it is likely the cD galaxy of Abell 478 has modified the dark matter distribution.[11] It is found that the jets and X-ray cavities in Abell 478 is not perfectly aligned, suggesting that the AGN activity has changed the direction overtime.[12] This misalignment (ΔΨ) of 37.7° and 34.8° is not unique, and this pattern is seen in many other galaxy clusters such as Abell 2390 and Abell 496.[13]

See also

  • Abell 478's BCG
    Abell 478's BCG
  • Abell 478
    Abell 478
  • Abell 478 galaxy cluster seen by Legacy Surveys
    Abell 478 galaxy cluster seen by Legacy Surveys
  • Abell 478 seen by 2MASS
    Abell 478 seen by 2MASS
  • Hot gas emitted by 16 Supermassive black holes in Abell 478 that is detected by Abell 478
    Hot gas emitted by 16 Supermassive black holes in Abell 478 that is detected by Abell 478
  • Abell 478 seen by Pan-STARRS
    Abell 478 seen by Pan-STARRS
  • Hot gas seen in Abell 478 by Herschel Space Telescope
    Hot gas seen in Abell 478 by Herschel Space Telescope

References

  1. ↑ 1.0 1.1 1.2 "NED results for object ABELL 0478". NASA/IPAC Extragalactic Database (NED). http://ned.ipac.caltech.edu/cgi-bin/nph-objsearch?objname=Abell+478&extend=no. 
  2. ↑ Abell, George O.; Corwin, Harold G. Jr.; Olowin, Ronald P. (May 1989). "A catalog of rich clusters of galaxies". Astrophysical Journal Supplement Series 70 (May 1989): 1–138. doi:10.1086/191333. ISSN 0067-0049. Bibcode: 1989ApJS...70....1A. 
  3. ↑ 3.0 3.1 Table 4 from Vikhlinin, A.; Kravtsov, A.; Forman, W.; Jones, C.; Markevitch, M.; Murray, S. S.; Van Speybroeck, L. (April 2006). "Chandra Sample of Nearby Relaxed Galaxy Clusters: Mass, Gas Fraction, and Mass-Temperature Relation". The Astrophysical Journal (Chicago, Illinois, USA) 640 (2): 691–709. doi:10.1086/500288. Bibcode: 2006ApJ...640..691V. 
  4. ↑ 4.0 4.1 4.2 Sun, M.; Jones, C.; Murray, S. S.; Allen, S. W.; Fabian, A. C.; Edge, A. C. (2005). "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". The Astrophysical Journal 629 (2): 729–740. doi:10.1086/431731. Bibcode: 2005ApJ...629..729S. 
  5. ↑ Knudsen, K. K.; van der Werf, P. P.; Jaffe, W. (2003). "A submillimetre selected quasar in the field of Abell 478". Astronomy & Astrophysics 411: 343–350. doi:10.1051/0004-6361:20031291. Bibcode: 2003A&A...411..343K. https://www.aanda.org/articles/aa/pdf/2003/46/aah5046.pdf. 
  6. ↑ de Plaa, J.; Kaastra, J. S.; Tamura, T.; Pointecouteau, E.; Mendez, M.; Peterson, J. R. (2004). "X-ray spectroscopy on Abell 478 with XMM-Newton". Astronomy & Astrophysics 423: 49–56. doi:10.1051/0004-6361:20047170. Bibcode: 2004A&A...423...49D. https://www.aanda.org/articles/aa/pdf/2004/32/aa7170.pdf. 
  7. ↑ 7.0 7.1 Pointecouteau, E.; Arnaud, M.; Kaastra, J.; de Plaa, J. (2004). "XMM-Newton observation of the relaxed cluster A478: Gas and dark matter distribution from 0.01R200 to 0.5R200". Astronomy & Astrophysics 423: 33–47. doi:10.1051/0004-6361:20047171. Bibcode: 2004A&A...423...33P. https://www.aanda.org/articles/aa/pdf/2004/32/aa7171.pdf. 
  8. ↑ Mahdavi, Andisheh; Hoekstra, Henk; Babul, Arif; Sievers, Jonathan; Myers, Steven T.; Henry, J. Patrick (2007). "Joint Analysis of Cluster Observations. I. Mass Profile of Abell 478 from Combined X-Ray, Sunyaev-Zel'dovich, and Weak-Lensing Data". The Astrophysical Journal 664 (1): 162–180. doi:10.1086/517958. Bibcode: 2007ApJ...664..162M. https://iopscience.iop.org/article/10.1086/517958. 
  9. ↑ White, D. A.; Fabian, A. C.; Allen, S. W.; Edge, A. C.; Crawford, C. S.; Johnstone, R. M.; Stewart, G. C.; Voges, W. (1994). "A ROSAT HRI observation of the Abell 478 cluster of galaxies". Monthly Notices of the Royal Astronomical Society 269 (3): 589–606. doi:10.1093/mnras/269.3.589. Bibcode: 1994MNRAS.269..589W. 
  10. ↑ Schnopper, H. W.; Delvaille, J. P.; Epstein, A.; Iken, H. H.; Harris, D. E.; Strom, R. G.; Clark, G. W.; Jernigan, J. G. (1977). "X-Ray and Radio Observations of the Structure of Abell 478". The Astrophysical Journal 217: L67–L70. doi:10.1086/182536. Bibcode: 1977ApJ...217L..67S. 
  11. ↑ Sanderson, Alastair J. R.; Finoguenov, Alexis; Mohr, Joseph J. (2005). "Possible AGN Shock Heating in the Cool-Core Galaxy Cluster Abell 478". The Astrophysical Journal 630 (2): 749–760. doi:10.1086/432006. Bibcode: 2005ApJ...630..749S. 
  12. ↑ "Spotted: 'Death Star' Black Holes in Action". 2024-05-22. https://www.nasa.gov/image-article/spotted-death-star-black-holes-in-action/. 
  13. ↑ Ubertosi, Francesco; Schellenberger, Gerrit; O'Sullivan, Ewan; Vrtilek, Jan; Giacintucci, Simona; David, Laurence P.; Forman, William; Gitti, Myriam et al. (2024). "Jet reorientation in central galaxies of clusters and groups: insights from VLBA and Chandra data". The Astrophysical Journal 963 (1): 16. doi:10.3847/1538-4357/ad1510. Bibcode: 2024ApJ...963...16U. https://arxiv.org/abs/2312.02283. 



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