Astronomy:PKS 0137+012

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PKS 0137+012
SDSS image of PKS 0137+012.
Observation data (J2000.0 epoch)
ConstellationCetus
Right ascension 01h 39m 57.30s[1]
Declination+01° 31′ 46.13″[1]
Redshift0.261680[1]
Helio radial velocity78,450 km/s
Distance3.143 Gly
Apparent magnitude (V)17.07
Apparent magnitude (B)17.12
Characteristics
TypeOpt.var. RLQ[1]
Size~366,000 ly (112.2 kpc) (estimated)[1]
Other designations
4C +01.04, 2MASX J01395752+0131461, PGC 6160, UM 355, PHL 1093, OC +062, TXS 0137+012, NVSS J013957+013151[1]

PKS 0137+012 also known as PHL 1093, is a radio-loud quasar located in the constellation Cetus. The quasar has a redshift of (z) 0.261, meaning it is estimated to be located 3.14 billion light-years away[1] and was first discovered as a discrete source by astronomers in 1968.[2]

Description

PKS 0137+012 is hosted by a large elliptical galaxy, specifically an early-type galaxy based on a two-dimensional modelling technique.[3][4] It is known to have a close companion located 1.0 arcseconds away suggestive of a close interaction.[5]

The estimated stellar population age for this galaxy suggests that it is 1.7 billion years old, and has a supermassive black hole with a mass of 2.2 x 109 Mʘ.[6][7] A bright knot feature is seen west of its nucleus.[7]

The radio source of PKS 0137+012 is compact. Observations of it made in 1978 have shown this source to contain a flat-spectrum radio component at the quasar's position with a steep-spectrum component located at the ending point of an optical jet, making this similar to the radio source structure of 3C 273.[8] A radio map made by the Very Large Array also showed it has a complex radio lobe featuring a curved structure on its north-eastern side caused by precession of its jet.[9][10] Three other components were discovered with one of them being described as the strongest. It has a flux density of 0.801 ± 0.008 at 1125 MHz.[11]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 "NED Search results for PKS 0137+012". https://ned.ipac.caltech.edu/byname?objname=PKS+0137+012&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1. 
  2. ↑ Pauliny-Toth, I. I. K.; Kellermann, K. I. (December 1968). "Measurements of the flux density and spectra of discrete sources at centimeter wavelengths. II. The observations at 5 GHz (6cm)." (in en). The Astronomical Journal 73: 953–969. doi:10.1086/110754. ISSN 0004-6256. Bibcode: 1968AJ.....73..953P. https://articles.adsabs.harvard.edu/pdf/1968AJ.....73..953P. 
  3. ↑ Nolan, L. A.; Dunlop, J. S.; Kukula, M. J.; Hughes, D. H.; Boroson, T.; Jimenez, R. (2001-05-11). "The ages of quasar host galaxies". Monthly Notices of the Royal Astronomical Society 323 (2): 308–330. doi:10.1046/j.1365-8711.2001.04174.x. ISSN 0035-8711. Bibcode: 2001MNRAS.323..308N. 
  4. ↑ McLure, R. J.; Kukula, M. J.; Dunlop, J. S.; Baum, S. A.; O'Dea, C. P.; Hughes, D. H. (1999-09-19). "A comparative HST imaging study of the host galaxies of radio-quiet quasars, radio-loud quasars and radio galaxies -- I". Monthly Notices of the Royal Astronomical Society 308 (2): 377–404. doi:10.1046/j.1365-8711.1999.02676.x. ISSN 0035-8711. Bibcode: 1999MNRAS.308..377M. https://watermark02.silverchair.com/308-2-377.pdf?token=AQECAHi208BE49Ooan9kkhW_Ercy7Dm3ZL_9Cf3qfKAc485ysgAAA2AwggNcBgkqhkiG9w0BBwagggNNMIIDSQIBADCCA0IGCSqGSIb3DQEHATAeBglghkgBZQMEAS4wEQQMOshXkzySapP_8GfEAgEQgIIDE6TxQbzgMaf9mqpHsLcfjpE9cOr2tP-bMaxrNIXLV-5eTWZqiAHJ74ssLw9HufLtgULXr4NtqpDRPmeO6LOxr694mwyfmZBx2vircFJdGHF76QYb0ZIwFfWKE1PAG3aa6bVPH5bOEwI67Mdsc3u8T3Zp1fZ6s36bHFqdnz7sd3ndlrhHeLfme46PlRyFWwIIF_wYv94aw1ORWjU7sAS9PYlAemLH9_HUac0gKzV18HZPJSIsE1T0hSRU9EEpraE5Zq603x61hS2IPsEfjnmIu98fwbamecWlHyShcd_rMNmKKdAL0OWrvCakRaJooHhshpSzQsSXZnAfU9FMArnxB0tXfkb9vJu4xqYIO2v6mbOCMlmPFF5SptQ4U1nPX9UVW7ULiUD3iXN_J8XO__tuCIN0KRj8GxgDvrYZN2kmblYC9gjBmlzsUvWaDEQFjKhpnGGk_p9a3qdyapTTGG0sO8gtsHj5Id8JkxiPbPcp3xgcbdikl28IDTbIyqvhR3OKQTI6LecuGJcIL5X37re1zCIAQHKClVQBvvE0JUZLWvipDlicuMKeWwWtrd0cwwtrlpRYHlyegBdpjDEK32PBsfBNyU4D7ftLgNYd1pi9gLPc7944DAq5ZEKy19JCfdRg7e6BH7gkpb_z1olfYiWexkrJFrwh5cH0OH8MUOKeqgYc6ZTs9oFYmesh0BlxreUyWpXxvGT5578hIH8dp_A0j3AGGetgUVsZRlwdCjJuPB9HxkHj5__h9thB87wMBqAMw2vxweFHveFuF8twq8ILiwEM0mr-a_iaDHKUR5Y0oFbpeWtJqiwjoRj-I39yU5wnlx4d_dkgF9RN0mQN4UZyPCEcRtPHk1Jo38RTDeSvD4rIsqRa81FU9M3lyW0ui8Ih9f_Bt16cgBJBMXbYaGFDwQ_OrJvC8n3_P2AiI4K5nUB9w9P1UwtEANelgTFwvG5ySNwVE6L_95saupMAx6SiVTmM313Pi_kIXJ2uKKoeLdbLdRB92_22HOF_vM-nns8fND57cERy9tkuQAnEmK7rEHtlovw. 
  5. ↑ Disney, M. J.; Boyce, P. J.; Blades, J. C.; Boksenberg, A.; Crane, P.; Deharveng, J. M.; Macchetto, F.; Mackay, C. D. et al. (July 1995). "Interacting elliptical galaxies as hosts of intermediate-redshift quasars" (in en). Nature 376 (6536): 150–153. doi:10.1038/376150a0. ISSN 0028-0836. Bibcode: 1995Natur.376..150D. https://ui.adsabs.harvard.edu/abs/1995Natur.376..150D/abstract. 
  6. ↑ Dunlop, J. S.; McLure, R. J.; Kukula, M. J.; Baum, S. A.; O'Dea, C. P.; Hughes, D. H. (April 2003). "Quasars, their host galaxies and their central black holes" (in en). Monthly Notices of the Royal Astronomical Society 340 (4): 1095–1135. doi:10.1046/j.1365-8711.2003.06333.x. ISSN 0035-8711. Bibcode: 2003MNRAS.340.1095D. https://watermark02.silverchair.com/340-4-1095.pdf?token=AQECAHi208BE49Ooan9kkhW_Ercy7Dm3ZL_9Cf3qfKAc485ysgAAA2IwggNeBgkqhkiG9w0BBwagggNPMIIDSwIBADCCA0QGCSqGSIb3DQEHATAeBglghkgBZQMEAS4wEQQMTTjOTPRdr4l7EhMSAgEQgIIDFTKeTCsVqnNMXcYQvfz22kYhPwhLROMfUxdNsNA8qa6Tuzy4F6wTzhrnIP8VIeEIhYuDA342cazoBP7yT-2jxwY1-TLxEXXUg84DRbhF0fyejyjhN0Gl5ZvqMKg2aR_FIY3bTbnVfS9DkDHDS7GewzGC3iS99E5YLK7ABSAwrg9E52feV3gEW_4gaWPcf_FjqOknEF-6GaXxTGQt1r8eBp68OnsGdFWCsaw3_JmAGz6DSlUp66gy64vi1qcjz4QFrtp6kgLpdkdzwjfbCIiPYST-pkZzEk7WmIQ-88o_9OHfuf8i0nGx3EpMvJatYI0MEBPEjPkP_XfRFZFm8Epau5ZOVP7MogkeD4nRwKr8SLFAAIlFYwsgVTP5AZktqfZoczUeS8fpfzuKe3ZE2T1JMflomUvn8-pMzg8YJhQ-F3mzM4gd-Zpabajkg77nU9oAcRyK7jE0lgLd_Dw-XAOSHKBb-ZWXGI-4It2cQLVAIZO5i1g2pVR_xuTLUxwq_WjomqXboucQsNs0RP4BlxN8Pdifkua17YapVPGz-l6wK-mbgQRqQAuMv-qadS48JB8c1k6CdZiZcO9QDePtG8wVdfz25Yua0K0RTm7FlBFqYR9n1vnRsUn1R48PIa1VJapTwYCXY8ZMfO2SXpZp0HlZriA8ajO82oijz6uZLNwrBW6auApvYgvPhvtIKnbs4o2a4PvraIEgqLXKDHIieFvbmjK8iOx6hbeg2LrNskemDwarRZw0YzuefRV_AacLv1lVW1XHb_poevkfkjuqKwkjSYMq45ypQJR8aj55z2SVcP8gMTSLYYVn1eazFHHZyeHAqY4TP5EBUgl7_9_58uwkY6lisI3Dqu1vuNGF-weEnTgq3mPRBHIAWaGawOwAWlmb7MK-gc6mQnPlyRxE0eNn5sTqB2Jl0wOWWVPIdaVqUEe9xVV60IShDGLwTIb6SNAWYg5cDnG44d4aVq_8K-vdlMAB-JYnm0hFHSSYZ9_3jFub35I7I7jZTMy_iePERBtkyoeJVkjTec8-eOHa3OJH5TycqkfvBw. 
  7. ↑ 7.0 7.1 Canalizo, Gabriela; Stockton, Alan (2013-07-16). "Intermediate-Age Stellar Populations in Classical Quasi-Stellar Object Host Galaxies". The Astrophysical Journal 772 (2): 132. doi:10.1088/0004-637x/772/2/132. ISSN 0004-637X. Bibcode: 2013ApJ...772..132C. https://doi.org/10.1088/0004-637x/772/2/132. 
  8. ↑ Ghigo, F. D. (November 1978). "Structures of 18 radio sources with peculiar optical features." (in en). The Astronomical Journal 83: 1363–1373. doi:10.1086/112325. ISSN 0004-6256. Bibcode: 1978AJ.....83.1363G. https://articles.adsabs.harvard.edu/pdf/1978AJ.....83.1363G. 
  9. ↑ Gower, A. C.; Hutchings, J. B. (January 1984). "The radio quasar 0137+012 - A case for damped jet precession". Publications of the Astronomical Society of the Pacific 96: 19. doi:10.1086/131296. ISSN 0004-6280. Bibcode: 1984PASP...96...19G. https://iopscience.iop.org/article/10.1086/131296/pdf. 
  10. ↑ Gower, A. C.; Hutchings, J. B. (November 1984). "Radio and optical morphology of low-redshift quasars." (in en). The Astronomical Journal 89: 1658–1687. doi:10.1086/113669. ISSN 0004-6256. Bibcode: 1984AJ.....89.1658G. https://articles.adsabs.harvard.edu/pdf/1984AJ.....89.1658G. 
  11. ↑ Curran, S. J.; Whiting, M. T.; Allison, J. R.; Tanna, A.; Sadler, E. M.; Athreya, R. (2017-02-21). "Atomic and molecular absorption in redshifted radio sources". Monthly Notices of the Royal Astronomical Society 467 (4): 4514–4525. doi:10.1093/mnras/stx408. ISSN 0035-8711. 



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