TXS 1040+243

TXS 1040+243
SDSS image of TXS 1040+243
Observation data (J2000.0 epoch)
ConstellationLeo Minor
Right ascension10h 43m 43.32s[1]
Declination+24° 04′ 47.44″[1]
Redshift0.366680[1]
Heliocentric radial velocity109,928 ± 21 km/s[1]
Distance5,303.3 ± 371.2 Mly (1,626.00 ± 113.82 Mpc)[1]
Group or clusterWHL J104343.3+240447
magnitude (K)14.90[1]
Characteristics
TypeBrClG[1]
Size~870,900 ly (267.03 kpc) (estimated)[1]
Other designations
2MASX J10434332+2404470, 7C 1040+2420, NVSS J104343+240447, RX J1043.7+2404, TN J1043+2404, VLSS J1043.7+2404, B2 1040+24B, SDSS J104343.28+240446.7, WHL J104343.3+240447 BCG[1], LEDA 3759627

TXS 1040+243 also known as TN J1043+4304, is a radio galaxy located in the constellation of Leo Minor. The redshift of the galaxy is (z) 0.366[1] and it was first discovered as an astronomical radio source by astronomers with the Bologna Northern Cross Telescope in September 1972, where it was designated as B2 1040+24B.[2]

Description

TXS 1040+243 is an elliptical galaxy of Type E.[3] It is also a red luminous galaxy residing as the brightest cluster galaxy of the WHL J104343.3+240447 galaxy cluster with 32 confirmed galaxy member candidates. The R-band magnitude of the galaxy is found to be 17.30 magnitude, while its absolute magnitude is -23.80.[4][5][6]

The galaxy contains an active galactic nucleus (AGN) and is categorized as a compact radio galaxy containing a non-bent type source, with its total radio flux density calculated by the NRAO VLA Sky Survey (NVSS) estimated in units of 49.80 mJy at 1.4 GHz frequencies.[6] The radio spectrum of the source is categorized as being ultra steep with the radio spectra index of -1.59 ± 0.07α at low frequencies, with the radio structure orientated at the position angle of 90°.[7]

A study would find it is compact double made up of two unresolved components, with a major axis of 3.2 arcseconds. These components are estimated to have angular sizes of 3.2 and 1.3 arcseconds in total, with flux densities of 44.4 ± 1.4 mJy at 1365 MHz and 2.5 ± 0.59 mJy at 4860 MHz respectively.[8][9] Evidence suggested the source has an elongated morphology that is mainly depicted by a single elliptical profile component, with evidence of a radio core detected by Faint Images of the Radio Sky at Twenty-Centimeters (FIRST). The core flux density is estimated to be 49.85 mJy while the total radio power is calculated to be 23.49 × 1024 WHz-1.[3][10]

References

  1. 1 2 3 4 5 6 7 8 9 10 "NED Search results for TXS 1040+243". NASA/IPAC Extragalactic Database. Retrieved 2026-06-20.
  2. ↑ Colla, G.; Fanti, C.; Fanti, R.; Ficarra, A. (September 1972). "The B2 Catalogue of radio sources - second part". Astronomy and Astrophysics Supplement. 7: 1. Bibcode:1972A&AS....7....1C.
  3. 1 2 Kozieł-Wierzbowska, Dorota; Goyal, Arti; Żywucka, Natalia (2020-03-23). "Radio Sources Associated with Optical Galaxies and Having Unresolved or Extended Morphologies (ROGUE). I. A Catalog of SDSS Galaxies with FIRST Core Identifications". The Astrophysical Journal Supplement Series. 247 (2): 53. arXiv:1912.09959. Bibcode:2020ApJS..247...53K. doi:10.3847/1538-4365/ab63d3. ISSN 0067-0049.
  4. ↑ 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.
  5. ↑ 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.
  6. 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.
  7. ↑ Breuck, C. De; Breugel, W. van; Röttgering, H. J. A.; Miley, G. (2000-04-01). "A sample of 669 ultra steep spectrum radio sources to find high redshift radio galaxies" (PDF). Astronomy and Astrophysics Supplement Series. 143 (2): 303–333. arXiv:astro-ph/0002297. Bibcode:2000A&AS..143..303D. doi:10.1051/aas:2000181. ISSN 0365-0138.
  8. ↑ Kaplan, D. L.; Cordes, J. M.; Condon, J. J.; Djorgovski, S. G. (February 2000). "Compact Radio Sources with the Steepest Spectra". The Astrophysical Journal. 529 (2): 859–865. Bibcode:2000ApJ...529..859K. doi:10.1086/308307. ISSN 0004-637X.
  9. ↑ Kaplan, D. L.; Cordes, J. M.; Condon, J. J. (January 2000). "Radio Morphologies and Spectra of Compact Radio Sources with the Steepest Spectra". The Astrophysical Journal Supplement Series. 126 (1): 37–62. Bibcode:2000ApJS..126...37K. doi:10.1086/313294. ISSN 0067-0049.
  10. ↑ 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.
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