PKS 1932−46

PKS 1932−46
DESI Legacy Surveys image of PKS 1932−46
Observation data (J2000.0 epoch)
ConstellationTelescopium
Right ascension19h 35m 56.43s[1]
Declination−46° 20′ 40.50″[1]
Redshift0.230700[1]
Heliocentric radial velocity69,162 km/s[1]
Distance2.833 Gly
Apparent magnitude (V)19.9
Characteristics
TypeNLRG;BLRG Sy2[1]
Other designations
PKS B1932−464, LEDA 2830107, MRC 1932−464, SUMSS J193557−464038, Cul 1932−464, OCARS 1932−464, PAPER J294.05−46.38[1]

PKS 1932−46 is a broad-line[2] radio galaxy located in the constellation of Telescopium. The redshift of the galaxy is (z) 0.230[1] and it was first identified as an astronomical radio source in the Parkes Catalogue survey in 1970.[3]

Description

PKS 1932−46 has strong detections of emission lines towards the eastern direction from its nucleus.[4] The host galaxy is a large elliptical galaxy with a Fanaroff-Riley Class Type 2 radio morphology and has a total radio power of 5.5 x 1026 W Hz-1.[5][6][7] It has a mainly old stellar population around 12 billion years old, although a very young stellar population is suggested. A disturbed companion with a double nucleus is found north-east from the host galaxy, confirming they are gravitationally interacting. Further evidence of the interaction is two tidal tails extending in both directions from the galaxies.[7][8] The nucleus of PKS 1932−46 has irregular structures surrounding it, based on r-band imaging.[9]

The radio source of the galaxy has been classified as a double,[4] containing two asymmetrical radio lobes with bright hot spot features. Both lobes are located 54 and 35 kiloparsecs away from the nucleus. The lobe of the western side has strong polarization signs compared to the lobe on the eastern side. A small rotation measure is found on the western lobe with a range between -14 and 35 rad m-2.[10]

The galaxy has an extended emission line region (EELR). When observed, the region is found to be mainly complex. The center of the region close to the active galactic nucleus displays several velocity structures with detections of broad line widths reaching up to 1000 kilometer per seconds. However, the outer regions of the EELR lacks disturbed kinematics.[7] Further evidence also showed the EELR is also reaching the outer boundaries of the western lobe.[11] This EELR has also been suggested to be classified as star-forming halo feature likely triggered by tidal debris from the companion, with the gas showing an irregular morphology that is described as knotty and with a total extent of 160 kiloparsecs.[12]

References

  1. ^ a b c d e f g "NED Search results for PKS 1932-46". NASA/IPAC Extragalactic Database. Retrieved 2025-10-19.
  2. ^ Mingo, B.; Hardcastle, M. J.; Croston, J. H.; Dicken, D.; Evans, D. A.; Morganti, R.; Tadhunter, C. (2014-03-08). "An X-ray survey of the 2 Jy sample – I. Is there an accretion mode dichotomy in radio-loud AGN?". Monthly Notices of the Royal Astronomical Society. 440 (1): 269–297. arXiv:1402.1770. doi:10.1093/mnras/stu263.
  3. ^ Mullan, D. J. (September 1970). "Identification of Parkes Radio Sources on ADH plates". Irish Astronomical Journal. 9: 246. Bibcode:1970IrAJ....9..246M.
  4. ^ a b di Serego Alighieri, S.; J., Danziger, I.; R., Morganti; N., Tadhunter, C. (August 1994). "New identifications and redshifts for southern 2-Jy radio sources". Monthly Notices of the Royal Astronomical Society. 269 (4): 998. Bibcode:1994MNRAS.269..998D. doi:10.1093/mnras/269.4.998. Archived from the original on 2022-11-07. Retrieved 2025-10-19.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  5. ^ Holt, J.; Tadhunter, C. N.; González Delgado, R. M.; Inskip, K. J.; Rodriguez, J.; Emonts, B. H. C.; Morganti, R.; Wills, K. A. (October 2007). "The properties of the young stellar populations in powerful radio galaxies at low and intermediate redshifts". Monthly Notices of the Royal Astronomical Society. 381 (2): 611–639. arXiv:0708.2605. Bibcode:2007MNRAS.381..611H. doi:10.1111/j.1365-2966.2007.12140.x.
  6. ^ Tadhunter, C.; Dickson, R.; Morganti, R.; Robinson, T. G.; Wills, K.; Villar-Martin, M.; Hughes, M. (March 2002). "The origin of the UV excess in powerful radio galaxies: spectroscopy and polarimetry of a complete sample of intermediate-redshift radio galaxies". Monthly Notices of the Royal Astronomical Society. 330 (4): 977–996. arXiv:astro-ph/0201391. Bibcode:2002MNRAS.330..977T. doi:10.1046/j.1365-8711.2002.05153.x.
  7. ^ a b c Inskip, K. J.; Tadhunter, C. N.; Dicken, D.; Holt, J.; Villar-Martin, M.; Morganti, R. (2007-11-21). "PKS1932-46: a radio source in an interacting group?". Monthly Notices of the Royal Astronomical Society. 382 (1): 95–108. arXiv:0708.2848. Bibcode:2007MNRAS.382...95I. doi:10.1111/j.1365-2966.2007.12378.x.
  8. ^ Ramos Almeida, C.; Tadhunter, C. N.; Inskip, K. J.; Morganti, R.; Holt, J.; Dicken, D. (October 2010). "The optical morphologies of the 2 Jy sample of radio galaxies: evidence for galaxy interactions". Monthly Notices of the Royal Astronomical Society: no. arXiv:1008.2683. doi:10.1111/j.1365-2966.2010.17542.x.
  9. ^ Inskip, K. J.; Tadhunter, C. N.; Morganti, R.; Holt, J.; Ramos Almeida, C.; Dicken, D. (2010-07-15). "A near-IR study of the host galaxies of 2 Jy radio sources at 0.03 ≲z≲ 0.5 - I. The data★". Monthly Notices of the Royal Astronomical Society. 407 (3): 1739–1766. arXiv:1005.2195. doi:10.1111/j.1365-2966.2010.17002.x.
  10. ^ M., Villar-Martin; C., Tadhunter; R., Morganti; N., Clark; N., Killeen; D., Axon (April 1998). "PKS 1932-464: a jet-cloud interaction in a radio galaxy?". Astronomy and Astrophysics. 332: 479. arXiv:astro-ph/9801039. Bibcode:1998A&A...332..479V.
  11. ^ Inskip, K. J.; Villar-Martin, M.; Tadhunter, C.; Morganti, R.; Holt, J.; Dicken, D. (2007-04-25), "VIMOS spectroscopy of extended emission line regions", The Central Engine of Active Galactic Nuclei, 373: 546, arXiv:0704.3380, Bibcode:2007ASPC..373..546I
  12. ^ Villar-Martín, M.; Tadhunter, C.; Morganti, R.; Holt, J. (2005-05-01). "The giant star forming halo associated with the radio galaxy PKS 1932–46". Monthly Notices of the Royal Astronomical Society: Letters. 359 (1): L5 – L9. arXiv:astro-ph/0501414. Bibcode:2005MNRAS.359L...5V. doi:10.1111/j.1745-3933.2005.00022.x.
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