4C 39.32

Last updated
4C 39.32
Image of 4C 39.32.png
SDSS image of 4C 39.32
Observation data (J2000.0 epoch)
Constellation Leo Minor
Right ascension 10h 28m 44.27s [1]
Declination +38° 44′ 36.89″ [1]
Redshift 0.362162 [1]
Heliocentric radial velocity 108,574 km/s [1]
Distance 5.231 Gly (1603.87 Mpc) [1]
Apparent magnitude  (B)18.4
Characteristics
Type Radio galaxy LEG? [1]
Size~305,500  ly (93.68  kpc) (estimated) [1]
Other designations
2MASS J10284427+3844369, 6C 1025+39, 87GB 102547.9+390008, B2 1025+390B, LEDA 2820609, IVS B1025+389, PS 150, RX J1028.7+3844 [1]

4C 39.32 also known as B2 1025+29B, is an elliptical galaxy [2] with an active galactic nucleus (AGN) located in the constellation of Leo Minor. The redshift of the galaxy is (z) 0.36 [1] and it was first discovered as extragalactic radio source by astronomers in October 1982. [3] It has also been classified as a compact steep spectrum (CSS) source. [4]

Contents

Description

4C 39.32 has been categorized as a radio galaxy of low excitation. [5] The source of this galaxy is found to be both compact and also complex with a flat radio spectrum at high frequencies when observed with Very Large Array (VLA). [6] Its central bright radio core is found well resolved, dominating the entire source spectrum. There is presence of radio emission found as having an amorphous appearance and is extended. A hotspot is suggested to be located in the southern component. [4] An extended structure is shown surrounding the main source components based on multi-frequency imaging observations made with VLA. [7] The total radio luminosity of the source at 1.4 GHz, is found to be 0.27 x 1027 W Hz −1. [8]

A study has found 4C 39.32 contains a radio jet with the jet trail located in the northwest direction that is found to coincide with an ultraviolet knot feature, located by around five kiloparsecs from the core region. This alignment hints that the stellar populations in the knot directly in the jet's direction are caused by shock-trigged star formations. [2] The estimated young stellar population the galaxy is suggested to be between 0.06 and 0.1 years old, while the old stellar population is around less than 5 million years old. [8] [2] The host galaxy is described to have a flat bulge structure with an effective radius of 3.5 kiloparsecs and an elliptical component on the outer side. The nuclear point source of the galaxy has been depicted as relatively fainter compared to the bulge. [2] The supermassive black hole lying in the center of the galaxy has been estimated to be around 9.15 ± 1.37 Mʘ. The neon emission lines in its spectrum has been found to have a flux of 0.05 ± 0.05 x 10−15 erg s−1. [9]

References

  1. 1 2 3 4 5 6 7 8 9 "NED Search results for 4C 39.32". NASA/IPAC Extragalactic Database. Retrieved 2026-02-07.
  2. 1 2 3 4 Duggal, C.; O’Dea, C. P.; Baum, S. A.; Labiano, A.; Tadhunter, C.; Worrall, D. M.; Morganti, R.; Tremblay, G. R.; Dicken, D. (2024-04-01). "Optical- and UV-continuum Morphologies of Compact Radio Source Hosts". The Astrophysical Journal. 965 (1): 17. arXiv: 2309.00110 . Bibcode:2024ApJ...965...17D. doi: 10.3847/1538-4357/ad2513 . ISSN   0004-637X.
  3. ↑ Allington-Smith, J. R.; Perryman, M. a. C.; Longair, M. S.; Gunn, J. E.; Westphal, J. A. (October 1982). "A complete sample of extragalactic radio sources at 1 Jy at 408 MHz. II. The optical observations". Monthly Notices of the Royal Astronomical Society. 201: 331–344. Bibcode:1982MNRAS.201..331A. doi: 10.1093/mnras/201.2.331 . ISSN   0035-8711.
  4. 1 2 Rossetti, A.; Fanti, C.; Fanti, R.; Dallacasa, D.; Stanghellini, C. (2006-04-01). "The B3-VLA CSS sample - VI. VLA images at 2 cm" (PDF). Astronomy & Astrophysics. 449 (1): 49–60. arXiv: 0806.1824 . Bibcode:2006A&A...449...49R. doi:10.1051/0004-6361:20053945. ISSN   0004-6361.
  5. ↑ Allington-Smith, J. R.; Spinrad, H.; Djorgovski, S.; Liebert, J. (1988-10-01). "Further redshifts of 1-Jy radio sources". Monthly Notices of the Royal Astronomical Society. 234 (4): 1091–1103. doi: 10.1093/mnras/234.4.1091 . ISSN   0035-8711.
  6. ↑ Naundorf, C. E.; Alexander, P.; Riley, J. M.; Eales, S. A. (1992-10-01). "A sample of 6C sources selected at the peak of the source counts - IV. Further radio observations". Monthly Notices of the Royal Astronomical Society. 258 (3): 647–656. doi: 10.1093/mnras/258.3.647 . ISSN   0035-8711.
  7. ↑ Fanti, C.; Pozzi, F.; Dallacasa, D.; Fanti, R.; Gregorini, L.; Stanghellini, C.; Vigotti, M. (2001-04-01). "Multi-frequency VLA observations of a new sample of CSS/GPS radio sources" (PDF). Astronomy & Astrophysics. 369 (2): 380–420. Bibcode:2001A&A...369..380F. doi:10.1051/0004-6361:20010051. ISSN   0004-6361.
  8. 1 2 Fanti, C.; Fanti, R.; Zanichelli, A.; Dallacasa, D.; Stanghellini, C. (April 2011). "The B3-VLA CSS sample. VIII. New optical identifications from the Sloan Digital Sky Survey The ultraviolet-optical spectral energy distribution of the young radio sources". Astronomy and Astrophysics. 528: A110. arXiv: 1102.1619 . Bibcode:2011A&A...528A.110F. doi:10.1051/0004-6361/201015379. ISSN   0004-6361.
  9. ↑ Marques, Bárbara L. Miranda; Rodríguez-Ardila, Alberto; Fonseca-Faria, Marcos A.; Panda, Swayamtrupta (2024-11-18). "Powerful outflows of compact radio galaxies". The Astrophysical Journal. 978 (1): 16. arXiv: 2411.03130 . Bibcode:2025ApJ...978...16M. doi: 10.3847/1538-4357/ad8f40 .
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