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PKS 0215+015

From Wikipedia, the free encyclopedia
Quasar in the constellation of Cetus
PKS 0215+015
The BL Lacertae object PKS 0215+015.
Observation data (J2000.0epoch)
ConstellationCetus
Right ascension02h 17m 48.954s[1]
Declination+01° 44′ 49.699″[1]
Redshift1.720000[1]
Heliocentric radial velocity515,643km/s[1]
Distance9.545Gly
Apparent magnitude (V)16.74
Apparent magnitude (B)16.09
Characteristics
TypeOpt var, FSRQ BLLAC[1]
Other designations
PKS B0215+015,LEDA 2823038, PMN J0217+0144, OD +026, WMAP 096,NVSS J021748+014448,FIRST J021748.9+014449[1]

PKS 0215+015 is aBL Lacertae object (BL Lac)[2] located in theconstellation ofCetus. It has a highredshift of (z) 1.72[3][1] and was first discovered in 1971 by J.V. Wall and his colleagues during theParkes Catalogue of Radio Sources survey.[4] Theradio spectrum of the source is flat, making it aflat-spectrum radio quasar,[5] a type ofblazar also known as anoptically violent variable quasar in literature.[6][7]

Description

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PKS 0215+015 is classified as a bona fide BL Lac object, displaying typical characteristics such as weak emission lines and high rapidpolarization changes.[8] It is variable on theelectromagnetic spectrum with its optical band displaying variations of more than 4magnitudes.[9] Rapid polarization swings at 50° and -100° were found associated with the rapid flux variations of the object.[10]

According tooptical continuum observations, PKS 0215+015 is found to undergo a flaring period, brightening up to 1.5 magnitude by September 10, 1980.[11] On October 20, 1984, the object reached its brightest state with aB magnitude of 14.5 while its faintest state was recorded on August 11, 1983. By 1986, its brightness flared up once more after being in a faint state in 1985.[12] Observations by theAustralia Telescope Compact Array (ATCA), also showed the source had a strong long-term increase in itsflux density since May 2021.[13]

The radio structure of PKS 0215+015 is compact. Based on radio observations, the source has an invertedspectrum which peaks over 10GHz.[3] It has a radio core which has a highbrightness temperature.[14]Very Large Array imaging showed there is also a bentjet pointing in a north to south direction near the core region, with a subsequent bend clearly shown pointing east.[15] The jet also has a component visible at 2 centimeter and 7 millimeter wavelength imaging which in turn is blended partially with the core.[16]

In February 2022, theIceCube Neutrino Observatory detected a new candidate high-track energymuon neutrino event. DubbedIceCube-220225A, it was found to be associated with PKS 0215+015 which at that time, was undergoing a powerful radio flare exceeding flux densities of 3Jy at bothcentimeter andmillimeter wavelengths.[6] Observations also suggested the neutrino production happened closer to the core.[16]

Severalabsorption lines have been identified in the quasar'sultraviolet spectrum,[17][18][11] with one of the lines at (z) 1.345 displaying evidence of ionized neutralmagnesium,manganese and ionizediron absorption.[19] Another absorption line located at (z) 1.721, showscerium andchromium oxide absorption.[20]

References

[edit]
  1. ^abcdefg"NED search results for PKS 0215+015".NASA/IPAC Extragalactic Database. Retrieved2025-05-18.
  2. ^Blades, J. C.; Hunstead, R. W.; Murdoch, H. S.; Pettini, M. (September 1982)."Optical absorption lines in the high redshift BL Lac object 0215+015".Monthly Notices of the Royal Astronomical Society.200 (4):1091–1111.Bibcode:1982MNRAS.200.1091B.doi:10.1093/mnras/200.4.1091.ISSN 0035-8711.
  3. ^abTorniainen, I.; Tornikoski, M.; Teräsranta, H.; Aller, M. F.; Aller, H. D. (2005-06-01)."Long term variability of gigahertz-peaked spectrum sources and candidates"(PDF).Astronomy & Astrophysics.435 (3):839–856.Bibcode:2005A&A...435..839T.doi:10.1051/0004-6361:20041886.ISSN 0004-6361.
  4. ^Wall, J. V.; Shimmins, A. J.; Merkelijn, J. K. (1971)."The Parkes 2700 MHz Survey. Catalogues for the ±4 declination zone and for the selected regions".Australian Journal of Physics Astrophysical Supplement.19:1–68.Bibcode:1971AuJPA..19....1W.
  5. ^Zheng, Y. G.; Yang, C. Y.; Zhang, L.; Wang, J. C. (December 2016)."Discerning the Gamma-Ray-Emitting Region in the Flat Spectrum Radio Quasars".The Astrophysical Journal Supplement Series.228 (1): 1.arXiv:1612.02394.doi:10.3847/1538-4365/228/1/1.ISSN 0067-0049.
  6. ^ab"The flaring radio-bright blazar PKS 0215+015 coincident with the high energy neutrino alert IceCube-220225A".The Astronomer's Telegram. Retrieved2025-05-18.
  7. ^Schramm, K.-J.; Borgeest, U.; Kuehl, D.; von Linde, J.; Linnert, M. D.; Schramm, T. (August 1994)."The Hamburg quasar monitoring program (HQM) at Calar Alto. III. Lightcurves of optically violent variable sources".Astronomy and Astrophysics Supplement Series.106:349–359.ISSN 0365-0138.
  8. ^Gaskell, C. M. (January 1982)."High redshift BL Lacertae object: PKS 0215+015".The Astrophysical Journal.252:447–454.Bibcode:1982ApJ...252..447G.doi:10.1086/159572.ISSN 0004-637X.
  9. ^Blades, J. C.; Pettini, M.; Hunstead, R. W.; Murdoch, H. S. (1982)."The ultraviolet spectrum of the high redshift BL Lac object 0215+015".NASA Conference Publication.2238:193–196.Bibcode:1982NASCP2238..193B.
  10. ^Kikuchi, Sen (1988)."Photometric and polarimetric behavior of the high-redshifted BL Lacertae object PKS 0215+015 in 1984-86".Publications of the Astronomical Society of Japan.40 (5):547–565.Bibcode:1988PASJ...40..547K.doi:10.1093/pasj/40.5.547.
  11. ^abBlades, J. C.; Hunstead, R. W.; Murdoch, H. S.; Pettini, M. (September 1982)."Optical absorption lines in the high redshift BL Lac object 0215+015".Monthly Notices of the Royal Astronomical Society.200 (4):1091–1111.Bibcode:1982MNRAS.200.1091B.doi:10.1093/mnras/200.4.1091.ISSN 0035-8711.
  12. ^Webb, James R.; Smith, Alex G.; Leacock, Robert J.; Fitzgibbons, Gregory L.; Gombola, Paul P.; Shepherd, David W. (February 1988)."Optical observations of 22 violently variable extragalactic sources - 1968-1986".The Astronomical Journal.95: 374.Bibcode:1988AJ.....95..374W.doi:10.1086/114641.ISSN 0004-6256.
  13. ^"ATCA finds a long-term radio flare of PKS0215+015 coincident with IceCube-220225A".The Astronomer's Telegram. Retrieved2025-05-18.
  14. ^Eppel, F.; Kadler, M.; Ros, E.; Benke, P.; Giroletti, M.; Hessdoerfer, J.; McBride, F.; Roesch, F. (2023-08-08),VLBI Probes of Jet Physics in Neutrino-Candidate Blazars,arXiv:2308.04311
  15. ^Sebastian, Biny; Kharb, Preeti; Lister, Matthew L.; Marshall, Herman L.; O’Dea, Christopher P.; Baum, Stefi A. (2022-08-01)."Investigating the Origin of X-Ray Jets: A Case Study of Four Hybrid Morphology MOJAVE Blazars".The Astrophysical Journal.935 (1): 59.arXiv:2206.13665.Bibcode:2022ApJ...935...59S.doi:10.3847/1538-4357/ac7c10.ISSN 0004-637X.
  16. ^abEppel, F.; Kadler, M.; Ros, E.; Roesch, F.; Hessdoerfer, J.; Benke, P.; Edwards, P. G.; Fromm, C. M.; Giroletti, M. (2023-02-24), "VLBI Scrutiny of a New Neutrino-Blazar Multiwavelength-Flare Coincidence",The Multimessenger Chakra of Blazar Jets,375: 91,arXiv:2301.13859,Bibcode:2023IAUS..375...91E,doi:10.1017/S1743921323000893
  17. ^Foltz, Craig B.; Chaffee Jr., Frederic H. (March 1987)."Confirmation of the emission-line redshift of the BL Lac object PKS 0215 + 015".The Astronomical Journal.93: 529.Bibcode:1987AJ.....93..529F.doi:10.1086/114334.ISSN 0004-6256.Archived from the original on 2022-11-07. Retrieved2025-05-18.
  18. ^Pettini, M.; Hunstead, R. W.; Murdoch, H. S.; Blades, J. C. (October 1983)."C IV absorption in the high-redshift BL Lac object 0215 + 015. II - New observations at 20 km/s resolution".The Astrophysical Journal.273: 436.Bibcode:1983ApJ...273..436P.doi:10.1086/161382.ISSN 0004-637X.Archived from the original on 2024-09-05. Retrieved2025-05-18.
  19. ^Bergeron, J.; D'Odorico, S. (1986-06-01)."Ionization state of the absorption systems in the BL Lac object 0215 + 015 and properties of low-excitation absorbers".Monthly Notices of the Royal Astronomical Society.220 (4):833–843.doi:10.1093/mnras/220.4.833.ISSN 0035-8711.
  20. ^P., Boisse; J., Bergeron (March 1988)."The BL Lac object PKS 0215+015 in a low state : variable emission lines at ze = 1.72 and no dust signature from the system at ZA = 1.345".Astronomy and Astrophysics.192: 1.Bibcode:1988A&A...192....1B.ISSN 0004-6361.Archived from the original on 2023-11-15. Retrieved2025-07-18.

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