J114403.9+440022.0

J114403.9+440022.0
SDSS image of J114403.9+440022.0
Observation data (J2000.0 epoch)
ConstellationUrsa Major
Right ascension11h 44m 03.88s[1]
Declination+44° 00′ 21.97″[1]
Redshift0.299049[1]
Heliocentric radial velocity89,653 ± 19 km/s[1]
Distance4,323.9 ± 302.7 Mly (1,325.72 ± 92.80 Mpc)[1]
Group or clusterWHL J114403.9+440022
magnitude (K)13.82[1]
Characteristics
TypeBrClG[1]
Size~333,000 ly (102.2 kpc) (estimated)[1]
Other designations
2MASX J11440384+4400214, NYU-VAGC 1120250, NVSS J114404+440019, OGC 0266, SDSSCGB 11250.01, RGZ J114403.8+440021, WHL J114403.9+440022 BCG, [YHW2016] J176.01616+44.00609,[1] LEDA 3545497

J114403.9+440022.0 also known as OGC 266, J114403+440021 and RGZ J114403.8+440021 is a radio galaxy located in the constellation of Ursa Major. The redshift of the galaxy is (z) 0.299.[1]

Description

J114403.9+440022.0 is an elliptical galaxy[2] residing as the brightest cluster galaxy of the WHL J114403.9+440022 galaxy cluster with 14 confirmed galaxy member candidates. The R-band magnitude of the galaxy is estimated to be 17.22 while the absolute magnitude of the galaxy is -23.70.[3][4] The galaxy is also designated as 7C B114125.4+441658 in the Seventh Cambridge Survey with its central supermassive black hole mass estimated as 9.09 M☉. There are detections of both hydrogen-alpha and doubly ionized oxygen emission lines with line luminosities estimated as 0.000 and 7.111 L☉.[5] The g–r color value is 1.68 magnitude.[6]

The nucleus is found to be active and it has been categorized as a Fanaroff-Riley Class Type II radio galaxy with a bent-tail FR II-like radio source with the total radio flux density being estimated to be 49.60 mJy at 1.4 GHz frequencies by NRAO VLA Sky Survey (NVSS) and has radio luminosity of 14.1 × 1024 W Hz−1.[4][7] Both of the radio lobes are found to be resolved with a projected length of 125.3 and 145.4 kiloparsecs respectively. The lobes also have an angular separation of 16.7 and 19.4 arcseconds.[7] There is a presence of a radio core but no detections of hotspot features. The total angular size is found to be 55 arcseconds while the linear size is 244.54 kiloparsecs.[8]

A study published in 2025, has found it is a wide-angle-tail radio galaxy. There are presence of radio jets with the opening angle estimated to be 145.6° while the curvature radius is 65.8 arcseconds in total. The jet power has been calculated to be 44.65 erg s−1.[6][9] An angular size of the source has been measured to be 63 arcseconds whereas the largest linear size is 289.0 kiloparsecs. The spectral index is estimated as 0.78α.[6] Evidence also found the source is indeed bend with its bending angle calculated to be 11.0°.[10]

References

  1. 1 2 3 4 5 6 7 8 9 10 "NED Search results for J114403.9+440022.0". NASA/IPAC Extragalactic Database. Retrieved 2026-06-27.
  2. ↑ Ogle, Patrick M.; Lanz, Lauranne; Appleton, Philip N.; Helou, George; Mazzarella, Joseph (2019-07-15). "A Catalog of the Most Optically Luminous Galaxies at z < 0.3: Super Spirals, Super Lenticulars, Super Post-mergers, and Giant Ellipticals". The Astrophysical Journal Supplement Series. 243 (1): 14. arXiv:1904.02806. Bibcode:2019ApJS..243...14O. doi:10.3847/1538-4365/ab21c3. ISSN 1538-4365.
  3. ↑ 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.
  4. 1 2 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.
  5. ↑ Sikora, Marek; Stasińska, Grażyna; Kozieł-Wierzbowska, Dorota; Madejski, Greg M.; Asari, Natalia V. (2013-02-15). "Constraining Jet Production Scenarios by Studies of Narrow-Line Radio Galaxies". The Astrophysical Journal. 765 (1): 62. arXiv:1210.2571. Bibcode:2013ApJ...765...62S. doi:10.1088/0004-637x/765/1/62. ISSN 0004-637X.
  6. 1 2 3 Lao, Baoqiang; Andernach, Heinz; Yang, Xiaolong; Zhang, Xiang; Zhao, Rushuang; Zhao, Zhen; Yu, Yun; Sun, Xiaohui; Qin, Sheng-Li (2025-01-16). "Identification of 4876 Bent-tail Radio Galaxies in the FIRST Survey Using Deep Learning Combined with Visual Inspection". The Astrophysical Journal Supplement Series. 276 (2): 46. arXiv:2501.09883. Bibcode:2025ApJS..276...46L. doi:10.3847/1538-4365/ad9c6d. ISSN 0067-0049.
  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. ↑ 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.
  9. ↑ Rusinek, Katarzyna; Sikora, Marek; Kozieł-Wierzbowska, Dorota; Godfrey, Leith (2016-12-23). "On the efficiency of jet production in FR II radio galaxies and quasars". Monthly Notices of the Royal Astronomical Society. 466 (2): 2294–2301. arXiv:1612.07392. doi:10.1093/mnras/stw3330. ISSN 0035-8711.
  10. ↑ 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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