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4C +41.26

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4C +41.26
4C +41.26 captured by SDSS
Observation data (J2000.0 epoch)
ConstellationCanes Venatici
Right ascension13h 35m 20.09s[1]
Declination+41° 00′ 04.34″[1]
Redshift0.228300[1]
Heliocentric radial velocity68,443 ± 9 km/s[1]
Distance3,301.9 ± 231.1 Mly (1,012.37 ± 70.87 Mpc)[1]
Group or clusterAbell 1763
Magnitude (K)12.96[1]
Characteristics
TypeBrClG
Size~861,000 ly (264.1 kpc) (estimated)[1]
Other designations
B3 1333+412, LEDA 2174167, TXS 1333+412, RX J1335.2+410, OGC 0110, 7C 1333+4115, 2MASX J13352009+4100041, ATATS J133519.5+410002, NVSS J133519+410004[1]

4C +41.26 known as B3 1333+412, is a massive elliptical galaxy of type E[2] located in the constellation of Canes Venatici. Its redshift is 0.228324, estimating the galaxy to be located 3.3 billion light years away from Earth.[1] It is the brightest cluster galaxy of Abell 1763 (ACO 1763).[3][4][5]

Characteristics

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4C +41.26 is a wide-angle tail (WAT) radio galaxy hosted by a central dominant galaxy residing in the central region of Abell 1763.[6][7] The galaxy is known to contain a double-lobed source with the radio power estimated to be 1026 W Hz-1.[8] The radio lobes are found resolved with the northern radio lobe notably being less polarized when compared to the southern radio lobe.[9] There is a presence of a radio core with a total flux density of 3.23 ± 0.01 mJy although a study in 2015, has suggested the flux density is 72.83 mJy.[10][5]

A radio image made at high resolution, showed a presence of a radio jet located at the southern part, cutting though a plume feature before ending at the spot of a compact region.[9] This jet has a minimum pressure of around 1.8 × 10-11 dyn cm-2 and has a jet flux density of 5.07 mJy.[7][10]

The galaxy has a total ultraviolet star formation rate of 1.06 M☉ per year, while the total infrared star formation rate is suggested to be 7.68 M☉ per year. The stellar mass of the galaxy is 4.18 M☉.[11] The core of the galaxy is depicted to have a red appearance based on its inner color shape profile with its surface brightness profile parameter measured as 24.47+0.19-0.21 kiloparsecs.[12] There are no detections of any hydrogen-alpha emission.[13] A study in 2018, has found there is a presence of a supermassive black hole in the center with a mass of 10.12 ± 0.05 M☉ based on its K-band galactic bulge luminosity.[14] The peculiar velocity of the galaxy is 650 kilometers per seconds.[8]

References

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  1. 1 2 3 4 5 6 7 8 9 "NED Search results for 4C +41.26". NASA/IPAC Extragalactic Database. Retrieved 2026-06-25.
  2. ↑ "HyperLeda -object description". atlas.obs-hp.fr. Retrieved 2024-05-26.
  3. ↑ Owen, Frazer N.; Ledlow, Michael J. (1997). "A 20 Centimeter VLA Survey of Abell Clusters of Galaxies. VII. Detailed Radio Images". The Astrophysical Journal Supplement Series. 108 (1): 41–98. Bibcode:1997ApJS..108...41O. doi:10.1086/312954. Retrieved 2024-05-26.
  4. ↑ Edwards, Louise O. V.; Fadda, Dario; Biviano, Andrea; Marleau, Francine R. (2010-02-01). "Spitzer Observations of Abell 1763. I. Infrared and Optical Photometry". The Astronomical Journal. 139 (2): 434–446. arXiv:1009.5752. Bibcode:2010AJ....139..434E. doi:10.1088/0004-6256/139/2/434. ISSN 0004-6256. Retrieved 2024-05-26.
  5. 1 2 Hogan, M. T.; Edge, A. C.; Hlavacek-Larrondo, J.; Grainge, K. J. B.; Hamer, S. L.; Mahony, E. K.; Russell, H. R.; Fabian, A. C.; McNamara, B. R.; Wilman, R. J. (2015-10-21). "A Comprehensive Study of the Radio Properties of Brightest Cluster Galaxies". Monthly Notices of the Royal Astronomical Society. 453 (2): 1201–1222. arXiv:1507.03019. doi:10.1093/mnras/stv1517. ISSN 0035-8711.
  6. ↑ Sakelliou, I.; Merrifield, M. R. (2000-01-21). "The origin of wide-angle tailed radio galaxies". Monthly Notices of the Royal Astronomical Society. 311 (3): 649–656. arXiv:astro-ph/9909511. Bibcode:2000MNRAS.311..649S. doi:10.1046/j.1365-8711.2000.03079.x. ISSN 0035-8711.
  7. 1 2 Edwards, Louise O. V.; Fadda, Dario; Frayer, David T.; Neto, Gastao B. Lima; Durret, Florence (2010-11-09). "SPITZER OBSERVATIONS OF A1763. II. CONSTRAINING THE NATURE OF ACTIVITY IN THE CLUSTER-FEEDING FILAMENT WITH VLA AND XMM-NEWTON DATA". The Astronomical Journal. 140 (6): 1891–1904. arXiv:1009.5753. Bibcode:2010AJ....140.1891E. doi:10.1088/0004-6256/140/6/1891. ISSN 0004-6256.
  8. 1 2 Douglass, E. M.; Blanton, E. L.; Randall, S. W.; Clarke, T. E.; Edwards, L. O. V.; Sabry, Z.; ZuHone, J. A. (2018-11-30). "The Megaparsec-scale Gas-sloshing Spiral in the Remnant Cool Core Cluster Abell 1763". The Astrophysical Journal. 868 (2): 121. arXiv:1812.02645. Bibcode:2018ApJ...868..121D. doi:10.3847/1538-4357/aae9e7. ISSN 0004-637X.
  9. 1 2 Hardcastle, M. J.; Sakelliou, I. (April 2004). "Jet termination in wide-angle tailed radio sources". Monthly Notices of the Royal Astronomical Society. 349 (2): 560–575. arXiv:astro-ph/0312245. Bibcode:2004MNRAS.349..560H. doi:10.1111/j.1365-2966.2004.07522.x.
  10. 1 2 Jetha, N. N.; Hardcastle, M. J.; Sakelliou, I. (2006-05-11). "Jet speeds in wide-angle tailed radio galaxies". Monthly Notices of the Royal Astronomical Society. 368 (2): 609–618. arXiv:astro-ph/0602162. Bibcode:2006MNRAS.368..609J. doi:10.1111/j.1365-2966.2006.10155.x. ISSN 0035-8711.
  11. ↑ 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. arXiv:1201.3373. Bibcode:2012ApJS..199...23H. doi:10.1088/0067-0049/199/1/23. ISSN 0067-0049.
  12. ↑ Bildfell, Chris; Hoekstra, Henk; Babul, Arif; Mahdavi, Andisheh (2008-08-26). "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.
  13. ↑ Stott, J. P.; Edge, A. C.; Smith, G. P.; Swinbank, A. M.; Ebeling, H. (March 2008). "Near-infrared evolution of brightest cluster galaxies in the most X-ray luminous clusters since z = 1". Monthly Notices of the Royal Astronomical Society. 384 (4): 1502–1510. arXiv:0712.0496. Bibcode:2008MNRAS.384.1502S. doi:10.1111/j.1365-2966.2007.12807.x. ISSN 0035-8711.
  14. ↑ Mezcua, M.; Hlavacek-Larrondo, J.; Lucey, J. R.; Hogan, M. T.; Edge, A. C.; McNamara, B. R. (2017-10-30). "The most massive black holes on the Fundamental Plane of black hole accretion". Monthly Notices of the Royal Astronomical Society. 474 (1): 1342–1360. arXiv:1710.10268. doi:10.1093/mnras/stx2812. ISSN 0035-8711.
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