PKS 0428+205
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| PKS 0428+205 | |
|---|---|
 SDSS image of PKS 0428+205 | |
| Observation data (J2000.0 epoch) | |
| Constellation | Taurus |
| Right ascension | 04h 31m 03.76s[1] |
| Declination | +20° 37′ 34.26″[1] |
| Redshift | 0.220200[1] |
| Heliocentric radial velocity | 66,014 km/s[1] |
| Distance | 2.723 Gly |
| Apparent magnitude (B) | 22.17 |
| Characteristics | |
| Type | CSS[1] |
| Size | ~307,900 ly (94.39 kpc) (estimated)[1] |
| Other designations | |
| NVSS J043103+203734, OF +247, DA 138, 2MASX J04310377+2037346, TXS 0428+205, PKS J0431+2037, IERS B0428+205, VLSS J0431.0+2037[1] | |
PKS 0428+205 known as OF 247, is a radio galaxy located in the constellation of Taurus. The redshift of the galaxy is (z) 0.220[1] and it was first discovered as an extragalatic compact source in October 1971 by astronomers.[2] It is classified as a compact steep spectrum (CSS) object.[3][4]
PKS 0428+205 displays a gigahertz-peaked radio spectrum at various frequencies.[5][6] Its source is classified as compact, with radio emission separating into two individual components based on radio imaging made by the Very Large Array (VLA).[3] Another component described as both faint and extended is located 30 milliarcseconds away in the position angle of -30° and has a flux density of 120 mJy.[7]
The radio core of PKS 0428+205 is described as elongated along the position angle of -35° with some evidence of a lower surface brightness extension extending towards the northwest.[8] Observations with Very Long Baseline Interferometry (VLBI) at 5 GHz frequencies found there is an undetected northern radio lobe and southern radio lobe that is mainly dominated by a hotspot feature located at a distance of 175 parsecs from the core.[9] An arc of emission can be seen extending in an eastern direction from the northern hotspot.[10] The radiative age of the source is estimated to be 1.2 × 103 years.[11]
The host galaxy of PKS 0428+205 is a large normal elliptical galaxy, based on its absolute magnitude and surface brightness profiles not displaying the same characteristics like brightest cluster galaxies. Imaging made with Hubble Space Telescope (HST) described it having a reddened nucleus and is surrounded by a halo mainly extending in the directions of both south and east.[12] There are also fainter objects located within the space of 10 arcseconds[10] A study published in 2013 suggested PKS 0428+205 might be a young radio galaxy in the midst of an early evolution stage.[13]
References
- 1 2 3 4 5 6 7 8 "NED Search results for PKS 0428+205". NASA/IPAC Extragalactic Database. Retrieved 2025-09-13.
- ↑ Kellermann, K. I.; Jauncey, D. L.; Cohen, M. H.; Shaffer, B. B.; Clark, B. G.; Broderick, J.; Rönnäng, B.; Rydbeck, O. E. H.; Matveyenko, L.; Moiseyev, I.; Vitkevitch, V. V.; Cooper, B. F. C.; Batchelor, R. (October 1971). "High-Resolution Observations of Compact Radio Sources at 6 and 18 Centimeters". The Astrophysical Journal. 169: 1. Bibcode:1971ApJ...169....1K. doi:10.1086/151113. ISSN 0004-637X.
- 1 2 Spencer, R. E.; McDowell, J. C.; Charlesworth, M.; Fanti, C.; Parma, P.; Peacock, J. A. (October 1989). "MERLIN and VLA observations of compact steep-spectrum radio sources". Monthly Notices of the Royal Astronomical Society. 240 (3): 657–687. Bibcode:1989MNRAS.240..657S. doi:10.1093/mnras/240.3.657. ISSN 0035-8711.
- ↑ O'Dea, C. P.; Baum, S. A.; Stanghellini, C. (October 1991). "What Are the Gigahertz Peaked-Spectrum Radio Sources?". The Astrophysical Journal. 380: 66. Bibcode:1991ApJ...380...66O. doi:10.1086/170562. ISSN 0004-637X.
- ↑ Tyul'Bashev, S. A.; Chernikov, P. A. (May 2000). "Physical Conditions in Steep-Spectrum Radio Sources". Astronomy Reports. 44 (5): 286–297. Bibcode:2000ARep...44..286T. doi:10.1134/1.163852. ISSN 1063-7729.
- ↑ Dallacasa, D.; Fanti, C.; Fanti, R. (January 1994). "VLBI Morphology of GHZ-Peaked Spectrum Radio Galaxies". Symposium - International Astronomical Union. 159: 425. doi:10.1017/S0074180900176107. ISSN 0074-1809.
- ↑ Dallacasa, D.; Fanti, C.; Fanti, R.; Schilizzi, R. T.; Spencer, R. E. (March 1995). "A sample of small size compact steep-spectrum radio sources. I. VLBI images at 18 cm". Astronomy and Astrophysics. 295: 27–42. Bibcode:1995A&A...295...27D. ISSN 0004-6361.
- ↑ Phillips, R. B.; Mutel, R. L. (February 1981). "Milliarcsecond structure of 0428+205, 1518+047, and 2050+364 at 1.67 GHz". The Astrophysical Journal. 244: 19–26. Bibcode:1981ApJ...244...19P. doi:10.1086/158679. ISSN 0004-637X.
- ↑ D., Dallacasa; M., Orienti; C., Fanti; R., Fanti; C., Stanghellini (2013-07-21). "A sample of small-sized compact steep-spectrum radio sources: VLBI images and VLA polarization at 5 GHz". Monthly Notices of the Royal Astronomical Society. 433 (1). doi:10.1093/mnra (inactive 13 September 2025). ISSN 0035-8711. Archived from the original on 2022-03-03.
{{cite journal}}: CS1 maint: DOI inactive as of September 2025 (link) - 1 2 Stanghellini, C.; Orienti, M.; Spingola, C.; Zanichelli, A.; Dallacasa, D.; Cassaro, P.; O’Dea, C. P.; Baum, S. A.; Pérez-Torres, M. (2025-03-01). "Jetted subgalactic-size radio sources in merging galaxies - A jet redirection scenario". Astronomy & Astrophysics. 695: A179. arXiv:2407.02029. Bibcode:2025A&A...695A.179S. doi:10.1051/0004-6361/202451334. ISSN 0004-6361.
- ↑ Murgia, M.; Fanti, C.; Fanti, R.; Gregorini, L.; Klein, U.; Mack, K.-H.; Vigotti, M. (May 2002). "Synchrotron spectra and ages of compact steep spectrum radio sources". New Astronomy Reviews. 46 (2–7): 307–311. arXiv:astro-ph/9904141. Bibcode:2002NewAR..46..307M. doi:10.1016/S1387-6473(01)00200-7. ISSN 1387-6473.
- ↑ de Vries, W. H.; O'Dea, C. P.; Barthel, P. D.; Fanti, C.; Fanti, R.; Lehnert, M. D. (November 2000). "Hubble Space Telescope NICMOS Observations of the Host Galaxies of Powerful Radio Sources: Does Size Matter?". The Astronomical Journal. 120 (5): 2300–2330. arXiv:astro-ph/0007424. Bibcode:2000AJ....120.2300D. doi:10.1086/316825. ISSN 0004-6256.
- ↑ Artyukh, V. S.; Tyul'bashev, S. A.; Chernikov, P. A. (June 2013). "The radio sources CTA 21 and OF+247: The hot spots of radio galaxies". Astronomy Reports. 57 (6): 423–428. Bibcode:2013ARep...57..423A. doi:10.1134/S1063772913050016. ISSN 1063-7729.
