PKS 2250−41

PKS 2250−41
The radio galaxy PKS 2250−41.
Observation data (J2000.0 epoch)
ConstellationGrus
Right ascension22h 53m 03.11s[1]
Declination−40° 57′ 46.71″[1]
Redshift0.309000[1]
Heliocentric radial velocity92,636 km/s[1]
Distance3.600 Gly
Characteristics
TypeNLRG Sy2[1]
Other designations
LEDA 2831507, PKS J2253−4057, G4Jy 1795, Cul 2250−412, PMN J2253−4057[1]

PKS 2250−41 is an intermediate redshifted radio galaxy[2][3] located in the southern constellation of Grus. The redshift of the object is (z) 0.309[1] and it was first discovered as a strong radio source in 1992 by astronomers via a 6 centimeter Australia Telescope.[4]

Description

PKS 2250−41 is classified as a Fanaroff-Riley Class Type 2 radio galaxy. Its host is an elliptical galaxy belonging to a small galaxy group. A faint companion disc galaxy is found northeast from the host galaxy with a magnitude of 20.57 ± 0.12 and has the same redshift.[5][6] Evidence pointed out the disc galaxy is also interacting, based on a faint radio bridge and its disturbed appearance towards the direction of the host galaxy. A much smaller galaxy is located southwest and it is also heavily involved in the interaction, given the presence of a western arc-like tail extension.[7]

The host galaxy also displays an extended arc structure found measuring an approximate length of 50 kiloparsecs and located west from the continuum nucleus. There is evidence of fainter emission line arcs in the direction of east. An X-shaped structure is found forming from these emission lines at the center of the nucleus.[8]

Studies showed PKS 2250−41 has an extended emission-line region (EELR). Based on studies, the structure of the region is described as elliptical with the ellipse's major axis being aligned along the position angle of 80°. The region is also showed to be slightly offset in between its emission line and continuum peaks, with the lines mainly peaking at 0.55 ± 0.03 arcseconds east.[8] An observation made in 1999, resolved the emission lines into two kinetic components, mainly a narrow component and a broad component. The narrow component has a higher ionization level but has weak helium emission. Meanwhile, the broad component has a lower ionization level.[9]

The radio structure of the source is mainly made up of two asymmetrical radio lobes on opposite sides, only slightly resolved at 5 GHz frequencies. At 8 GHz, the two radio lobes are still slightly resolved but an extended structure of low-surface brightness, is now seen. No evidence of a radio core is found. Both the lobes are positioned 4.9 and 11.9 arcseconds from the nucleus shown on V-bands.[8] Evidence has confirmed the emission-line arc is wrapping around the western lobe on its outer rim area.[10]

References

  1. ^ a b c d e f g "NED Search results for PKS 2250-41". NASA/IPAC Extragalactic Database. Retrieved 2025-10-20.
  2. ^ Tadhunter, C.; Shaw, M.; Clark, N.; Morganti, R. (August 1994). "A giant emission line arc in the intermediate redshift radio galaxy PKS 2250-41". Astronomy and Astrophysics. 288: L21 – L24. Bibcode:1994A&A...288L..21T. ISSN 0004-6361.
  3. ^ Morganti, R.; Tadhunter, C. N.; Clark, N.; Killeen, N. (1996). "A Powerful Jet/Cloud Interaction in the Radio Galaxy PKS 2250-41". In Ekers, R.; Fanti, C.; Padrielli, L. (eds.). Extragalactic Radio Sources. Dordrecht: Springer Netherlands. pp. 227–229. doi:10.1007/978-94-009-0295-4_79. ISBN 978-94-009-0295-4.
  4. ^ Duncan, R. A.; Sproats, L. N. (1992). "Synthesis 6 CM images of 22 strong southern radio sources". Publications of the Astronomical Society of Australia. 10 (1): 16–20. Bibcode:1992PASA...10...16D. doi:10.1017/S1323358000019135. ISSN 0066-9997.
  5. ^ 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. ISSN 0035-8711.
  6. ^ Inskip, K. J.; Villar-Martín, M.; Tadhunter, C. N.; Morganti, R.; Holt, J.; Dicken, D. (June 2008). "PKS2250−41: a case study for triggering". Monthly Notices of the Royal Astronomical Society. 386 (4): 1797–1810. arXiv:0803.0084. Bibcode:2008MNRAS.386.1797I. doi:10.1111/j.1365-2966.2008.13171.x. ISSN 0035-8711.
  7. ^ 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. ISSN 0035-8711.
  8. ^ a b c Clark, N. E.; Tadhunter, C. N.; Morganti, R.; Killeen, N. E. B.; Fosbury, R. a. E.; Hook, R. N.; Siebert, J.; Shaw, M. A. (April 1997). "Radio, optical and X-ray observations of PKS 2250-41: a jet/galaxy collision?". Monthly Notices of the Royal Astronomical Society. 286 (3): 558–582. doi:10.1093/mnras/286.3.558. ISSN 0035-8711.
  9. ^ Villar-Martín, M.; Tadhunter, C.; Morganti, R.; Axon, D.; Koekemoer, A. (July 1999). "PKS 2250—41 and the role of jet-cloud interactions in powerful radio galaxies". Monthly Notices of the Royal Astronomical Society. 307 (1): 24–40. arXiv:astro-ph/9902376. Bibcode:1999MNRAS.307...24V. doi:10.1046/j.1365-8711.1999.02603.x. ISSN 0035-8711.
  10. ^ Tilak, Avanti; O'Dea, Christopher P.; Tadhunter, Clive; Wills, Karen; Morganti, Raffaella; Baum, Stefi A.; Koekemoer, Anton M.; Dallacasa, Daniele (December 2005). "Resolving the Shocks in Radio Galaxy Nebulae: Hubble Space Telescope and Radio Imaging of 3C 171, 3C 277.3, and PKS 2250-41". The Astronomical Journal. 130 (6): 2513–2521. arXiv:astro-ph/0507652. Bibcode:2005AJ....130.2513T. doi:10.1086/497265. ISSN 0004-6256.
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