WN B1127.5+4927

WN B1127.5+4927
SDSS image of WN B1127.5+4927
Observation data (J2000.0 epoch)
ConstellationUrsa Major
Right ascension11h 30m 18.32s[1]
Declination+49° 11′ 16.08″[1]
Redshift0.260465[1]
Heliocentric radial velocity78,085 ± 18 km/s[1]
Distance3,766.3 ± 263.6 Mly (1,154.74 ± 80.83 Mpc)[1]
Group or clusterWHL J113018.3+491116
magnitude (K)14.90[1]
Characteristics
TypeBrClG[1]
Size~291,000 ly (89.1 kpc) (estimated)[1]
Other designations
2MASS J11301832+4911163, [LHC2018] J172.57632+49.18780, LEDA 2335893, NYU-VAGC 0795797, RGZ J113018.3+491116, SDSS J113018.32+491116.0, WHL J113018.3+491116 BCG, [YHW2016] J172.57631+49.18781[1]

WN B1127.5+4927 also known as RGZ J113018.3+491116 and NYU-VAGC 0795797, is a radio galaxy located in the constellation of Ursa Major. The redshift of the galaxy is (z) 0.260[1] and it was first discovered as a background astronomical radio source by astronomers in January 1989.[2]

Description

WN B1127.5+4927 is a red luminous galaxy residing as the brightest cluster galaxy of the WHL J113018.3+491116 galaxy cluster with 29 confirmed galaxy member candidates. The R-band magnitude of the galaxy has been estimated to be 17.46 magnitude while the absolute magnitude is -23.20.[3][4][5] Its stellar velocity dispersion is calculated to be 284 kilometers per seconds and has an effective radius of 13.8 kiloparsecs. The total physical size of the galaxy is 222 kiloparsecs.[6] The R-band luminosity is 6.90 × 1010 Lʘ while the Z-band luminosity is 8.47 × 1010 Lʘ.[7]

The central nucleus is found to be active and is categorized as a bend Fanaroff-Riley Class Type II radio galaxy hosting a FRII-like radio source. The total flux density measured by NRAO VLA Sky Survey (NVSS) has been estimated to be 15.90 mJy at 1.4 GHz frequencies.[8] The angular size of the source is 39 arcseconds whereas the linear size is 157.2 kiloparsecs. The total radio luminosity at 1.4 GHz is 25.04 W Hz-1.[9]

A study published in 2012, has found a pair of resolved radio lobes. The projected length of the first lobe is found to be 81.1 kiloparsecs while the second lobe has a projected length of 118.1 kiloparsecs. The angular separation of the lobes are estimated to be 12.7 and 18.4 arcseconds respectively.[7] The galaxy also contains a presence of a double radio source with an unresolved radio core. The eastern and western lobes have linear sizes of 100 × 52 and 80 × 72 kiloparsecs respectively in total.[10] Evidence also found the source is bend with a measured bending angle of 0.0° while the excess bending angle is -7.3°.[11]

References

  1. 1 2 3 4 5 6 7 8 9 10 "NED Search results for WN B1127.5+4927". NASA/IPAC Extragalactic Database. Retrieved 2026-07-12.
  2. ↑ Vallee, J. P.; Roger, R. S. (January 1989). "Radio surveys and source counts at 408 MHz and 1420 MHz towards the Abell 1314 cluster of galaxies". Astronomy and Astrophysics, Suppl. Ser. 77: 31–38.
  3. ↑ Barber, Tom; Meiksin, Avery; Murphy, Tara (2007-05-11). "Properties of luminous red galaxies in the Sloan Digital Sky Survey". Monthly Notices of the Royal Astronomical Society. 377 (2): 787–805. arXiv:astro-ph/0611053. Bibcode:2007MNRAS.377..787B. doi:10.1111/j.1365-2966.2007.11650.x. ISSN 0035-8711.
  4. ↑ Wen, Z. L.; Han, J. L.; Liu, F. S. (2012-03-30). "A Catalog of 132,684 Clusters of Galaxies Identified from Sloan Digital Sky Survey III". The Astrophysical Journal Supplement Series. 199 (2): 34. arXiv:1202.6424. Bibcode:2012ApJS..199...34W. doi:10.1088/0067-0049/199/2/34. ISSN 0067-0049.
  5. ↑ Yuan, Z. S.; Han, J. L.; Wen, Z. L. (2016-05-12). "Radio luminosity function of brightest cluster galaxies". Monthly Notices of the Royal Astronomical Society. 460 (4): 3669–3678. arXiv:1605.03387. doi:10.1093/mnras/stw1125. ISSN 0035-8711.
  6. ↑ Lin, Yen-Ting; Shen, Yue; Strauss, Michael A.; Richards, Gordon T.; Lunnan, Ragnhild (2010-10-19). "ON THE POPULATIONS OF RADIO GALAXIES WITH EXTENDED MORPHOLOGY ATz< 0.3". The Astrophysical Journal. 723 (2): 1119–1138. arXiv:1006.5452. Bibcode:2010ApJ...723.1119L. doi:10.1088/0004-637x/723/2/1119. ISSN 0004-637X.
  7. 1 2 Antognini, Joe; Bird, Jonathan; Martini, Paul (2012-08-21). "THE LIFETIME AND POWERS OF FR IIs IN GALAXY CLUSTERS". The Astrophysical Journal. 756 (2): 116. arXiv:1204.3896. Bibcode:2012ApJ...756..116A. doi:10.1088/0004-637x/756/2/116. ISSN 0004-637X.
  8. ↑ Ma, Zhixian; Xu, Haiguang; Zhu, Jie; Hu, Dan; Li, Weitian; Shan, Chenxi; Zhu, Zhenghao; Gu, Liyi; Li, Jinjin; Liu, Chengze; Wu, Xiangping (2019-02-01). "A Machine Learning Based Morphological Classification of 14,245 Radio AGNs Selected from the Best–Heckman Sample". The Astrophysical Journal Supplement Series. 240 (2): 34. arXiv:1812.07190. Bibcode:2019ApJS..240...34M. doi:10.3847/1538-4365/aaf9a2. ISSN 0067-0049.
  9. ↑ Kozieł-Wierzbowska, Dorota; Stasińska, Grażyna (2011-08-01). "FRII radio galaxies in the SDSS: Observational facts". Monthly Notices of the Royal Astronomical Society. 415 (2): 1013–1026. arXiv:1101.3223. doi:10.1111/j.1365-2966.2011.18346.x.
  10. ↑ Parma, P.; Murgia, M.; Ruiter, H. R. de; Fanti, R.; Mack, K.-H.; Govoni, F. (2007-08-01). "In search of dying radio sources in the local universe" (PDF). Astronomy & Astrophysics. 470 (3): 875–888. arXiv:0705.3209. Bibcode:2007A&A...470..875P. doi:10.1051/0004-6361:20077592. ISSN 0004-6361.
  11. ↑ Garon, Avery F.; Rudnick, Lawrence; Wong, O. Ivy; Jones, Tom W.; Kim, Jin-Ah; Andernach, Heinz; Shabala, Stanislav S.; Kapińska, Anna D.; Norris, Ray P.; de Gasperin, Francesco; Tate, Jean; Tang, Hongming (2019-02-28). "Radio Galaxy Zoo: The Distortion of Radio Galaxies by Galaxy Clusters". The Astronomical Journal. 157 (3): 126. arXiv:1901.05480. Bibcode:2019AJ....157..126G. doi:10.3847/1538-3881/aaff62. ISSN 0004-6256.
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