SDSS J102040.84+315510.0

SDSS J102040.84+315510.0
The radio galaxy SDSS J102040.84+315510.0
Observation data (J2000.0 epoch)
ConstellationLeo Minor
Right ascension10h 20m 40.83s[1]
Declination+31° 55′ 10.21″[1]
Redshift0.285579[1]
Heliocentric radial velocity85,614 ± 14 km/s[1]
Distance4,132.0 ± 289.2 Mly (1,266.89 ± 88.68 Mpc)[1]
Group or clusterWHL J102040.8+315510
magnitude (J)15.40[1]
Characteristics
TypeBrClG[1]
Size~456,000 ly (139.9 kpc) (estimated)[1]
Other designations
2MASX J10204086+3155104, 7C 1017+3210 NED02, LEDA 1971163, RGZ J102040.8+315509, RGZ J102040.8+315510, NVSS J102040+315512, WHL J102040.8+315510 BCG, [YHW2016] J155.17015+31.91944[1]

SDSS J102040.84+315510.0 also known as J102040.8+315510.0, RGZ J102040.8+315509 and WISEA J102040.83+315510.2, is a radio galaxy located in the constellation of Leo Minor. The redshift of the galaxy has been estimated to be (z) 0.285.[1]

Description

SDSS J102040.84+315510.0 is a red luminous galaxy[2] residing as the brightest cluster galaxy (BCG) of the galaxy cluster, WHL J102040.8+315510, with at least 18 confirmed galaxy member candidates. The total r-band magnitude of the galaxy has been estimated as 17.65 while its absolute magnitude is -23.15.[3][4] The g–r color value is 1.58 magnitude.[5]

It is an elliptical galaxy.[6] The nucleus is active and it has been categorized as a Fanaroff-Riley Class Type II radio galaxy with the total flux density calculated by the NRAO VLA Sky Survey (NVSS) at 1.4 GHz frequencies being 60.90 mJy.[7][4] The calculated radio luminosity is 17.0 × 1024 W Hz-1.[8]

The radio lobes are resolved, with the first lobe having a length of 140.4 kiloparsecs while the other lobe has a length of 175.3 kiloparsecs. The angular separation of the lobes are estimated to be 18.9 and 23.5 arcseconds respectively.[8] The 1.4 GHz flux densities of the lobes at 3σ cuts obtained by the Faint Images of the Radio Sky at Twenty-Centimeters (FIRST), are found to be 17.3 mJy and 19.9 mJy.[7]

It is a bent wide-angle tail (WAT) radio galaxy, with the opening angle of the radio jet estimated to be 156.6° and the jet curvature is 125.9°. The largest linear size of the source is 325.0 kiloparsecs in total.[5] The source is also bent with its bending angle being 2.8° while the excessive bending angle is -6.0°.[9]

References

  1. 1 2 3 4 5 6 7 8 9 10 "NED Search results for SDSS J102040.84+315510.0". NASA/IPAC Extragalactic Database. Retrieved 2026-06-09.
  2. ↑ Lopes, P. A. A. (September 2007). "Empirical photometric redshifts of luminous red galaxies and clusters in the Sloan Digital Sky Survey". Monthly Notices of the Royal Astronomical Society. 380 (4): 1608–1620. arXiv:0706.1580. Bibcode:2007MNRAS.380.1608L. doi:10.1111/j.1365-2966.2007.12203.x. ISSN 0035-8711.
  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. 1 2 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.
  6. ↑ 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.
  7. 1 2 Rodman, P E; Turner, R J; Shabala, S S; Banfield, J K; Wong, O I; Andernach, H; Garon, A F; Kapińska, A D; Norris, R P; Rudnick, L (2018-11-13). "Radio Galaxy Zoo: observational evidence for environment as the cause of radio source asymmetry". Monthly Notices of the Royal Astronomical Society. 482 (4): 5625–5641. arXiv:1811.03726. doi:10.1093/mnras/sty3070. ISSN 0035-8711.
  8. 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.
  9. ↑ 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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