PKS 0043−42
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| PKS 0043−42 | |
|---|---|
 DESI Legacy Surveys image of PKS 0043−42 | |
| Observation data (J2000.0 epoch) | |
| Constellation | Phoenix |
| Right ascension | 00h 46m 17.74s[1] |
| Declination | −42° 07′ 51.46″[1] |
| Redshift | 0.119776[1] |
| Heliocentric radial velocity | 35,908 km/s[1] |
| Distance | 1.589 Gly |
| Characteristics | |
| Type | Elliptical WRLG[1] |
| Size | ~232,500 ly (71.27 kpc) (estimated)[1] |
| Other designations | |
| 2MASX J00461775−4207512, PGC 2702, PMN J0046-4207, G4Jy 0085, 2MASS J00461774−4207515, LQAC 011−042 005, MRSS 295−105194, PAPER J011.58−42.11[1] | |
PKS 0043−42 is a low-excitation radio galaxy[2] located in the constellation of Phoenix. The redshift of the object is (z) 0.119[1] and it was first recorded as an extragalactic radio source in December 1965 in the Parkes Catalogue survey by astronomers.[3]
PKS 0043−42 is classified as a weak-line radio galaxy (WLRG), located at the center of a galaxy group.[4][5] The host galaxy of the object is best described as an early-type galaxy or an elliptical galaxy based on its stellar continuum.[6] Evidence also points to the host galaxy interacting with a companion object to the north.[7] A diffused halo structure is surrounding the entire host galaxy.[8]
K-band imaging showed PKS 0043−42 has evidence of isothope twisting and excessive radio emission in a north-south direction. It is suggested a dust lane might be present in the galaxy or be the result of the interaction with the companion. Surprisingly, although the galaxy displays an undisturbed appearance, a radio bridge is found connecting it to its companion.[8]
A radio image has found the source of PKS 0043−42 is mainly extended with a Fanaroff-Riley class Type 2 morphology. While the hotspots are clearly seen even in X-ray imaging, the radio core remains undetected, even at six centimeter frequencies.[9][10] Evidence of radio emission can be found bridging from the hotspots to the mid-point section of the source.[11] In optical wavelengths, the emission lines displayed in its spectrum contain traces of low ionization.[10] The linear polarization of the source is covered entirely over a large area.[12] A compact dusty torus was discovered in PKS 0043−42 in 2011, indicating cold gas is fueling the accretion process rather than warm gas. The active galactic nucleus luminosity is estimated to be around 3.7 × 1044 erg s−1.[5]
References
- 1 2 3 4 5 6 7 8 "NED Search results for PKS 0043-42". ned.ipac.caltech.edu. Retrieved 27 October 2025.
- ↑ Burgess, A. M.; Hunstead, R. W. (January 2006). "The Molonglo Southern 4 Jy Sample (MS4). II. ATCA Imaging and Optical Identification". The Astronomical Journal. 131 (1): 114–132. arXiv:astro-ph/0512590. Bibcode:2006AJ....131..114B. doi:10.1086/498679. ISSN 0004-6256.
- ↑ Bolton, JG; E Clarke, Margaret; Ekers, RD (1965). "Identification of Extragalactic Radio Sources Between Declinations 20° and 44°". Australian Journal of Physics. 18 (6): 627. Bibcode:1965AuJPh..18..627B. doi:10.1071/ph650627. ISSN 0004-9506.
- ↑ 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. doi:10.1111/j.1365-2966.2010.17542.x. ISSN 0035-8711.
- 1 2 Ramos Almeida, C.; Dicken, D.; Tadhunter, C.; Asensio Ramos, A.; Inskip, K. J.; Hardcastle, M. J.; Mingo, B. (20 May 2011). "Clear detection of dusty torus signatures in a weak-line radio galaxy: the case of PKS 0043−42". Monthly Notices of the Royal Astronomical Society. 413 (4): 2358–2364. arXiv:1101.1868. Bibcode:2011MNRAS.413.2358R. doi:10.1111/j.1365-2966.2011.18309.x. ISSN 0035-8711.
- ↑ Sadler, Elaine M.; Ekers, Ronald D.; Mahony, Elizabeth K.; Mauch, Tom; Murphy, Tara (December 2013). "The local radio-galaxy population at 20 GHz". Monthly Notices of the Royal Astronomical Society. 438 (1): 796–824. arXiv:1304.0268. doi:10.1093/mnras/stt2239. ISSN 0035-8711.
- ↑ Inskip, K. J.; Tadhunter, C. N.; Morganti, R.; Holt, J.; Ramos Almeida, C.; Dicken, D. (15 July 2010). "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. doi:10.1111/j.1365-2966.2010.17002.x. ISSN 0035-8711.
- 1 2 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. doi:10.1111/j.1365-2966.2010.17542.x. ISSN 0035-8711.
- ↑ Mingo, B.; Hardcastle, M. J.; Ineson, J.; Mahatma, V.; Croston, J. H.; Dicken, D.; Evans, D. A.; Morganti, R.; Tadhunter, C. (29 May 2017). "An X-ray survey of the 2 Jy sample – II. X-ray emission from extended structures". Monthly Notices of the Royal Astronomical Society. 470 (3): 2762–2779. doi:10.1093/mnras/stx1307. ISSN 0035-8711.
- 1 2 Morganti, R.; Oosterloo, T.; Tadhunter, C. N.; Aiudi, R.; Jones, P.; Villar-Martin, M. (December 1999). "The radio structures of southern 2-Jy radio sources: New ATCA and VLA radio images". Astronomy and Astrophysics Supplement Series. 140 (3): 355–372. arXiv:astro-ph/9910150. Bibcode:1999A&AS..140..355M. doi:10.1051/aas:1999427. ISSN 0365-0138.
- ↑ R., Morganti; Killeen, N. E. B.; N., Tadhunter, C. (August 1993). "The radio structures of southern 2-Jy radio sources". Monthly Notices of the Royal Astronomical Society. 263. doi:10.1093/mnra (inactive 27 October 2025). ISSN 0035-8711. Archived from the original on 7 November 2022.
{{cite journal}}: CS1 maint: DOI inactive as of October 2025 (link) CS1 maint: multiple names: authors list (link) - ↑ Morris, D; Whiteoak, JB (1968). "The Distribution of Linear Polarization over 13 Extended Sources at 21·2 cm Wavelength". Australian Journal of Physics. 21 (4): 475. Bibcode:1968AuJPh..21..475M. doi:10.1071/ph680475. ISSN 0004-9506.
External links
- PKS 0043−42 on WikiSky: DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images
