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NRAO 530

From Wikipedia, the free encyclopedia
Flat spectrum radio quasar in the constellation Serpens
NRAO 530
The flat spectrum radio quasar NRAO 530.
Observation data (J2000.0epoch)
ConstellationSerpens
Right ascension17h 33m 02.705s
Declination−13° 04′ 49.548″
Redshift0.899000
Heliocentric radial velocity269,513km/s
Distance7.558Gly
Apparent magnitude (V)19.5
Apparent magnitude (B)18.0
Characteristics
Typeblazar;FRSQ;LPQBLLAC
Other designations
LEDA 2829294,PKS 1730-130, 4FGL J1733.0-1305, G4Jy 1417, Cul 1730-130, PKS 1730-13, PKS B1730-130

NRAO 530 orPKS 1730-13 is aflat-spectrum radio quasar[1] located in the southernconstellation ofSerpens. It has aredshift of 0.902.[2][3] and was first discovered by two astronomers, W.J. Welch andHyron Spinrad in 1973.[4] It is classified as ablazar because of its optical variability across theelectromagnetic spectrum in radio,gamma ray and X-ray bands.[5] This quasar is also further categorized anOVV quasar.[6][7]

Description

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Like many other blazars, NRAO 530 is shown to be in a flaring state. In 1994, it showed a striking flare that was observed in radio andmillimeterwavelengths in its 30-year history[8] with two of its distinctive flares nearly tripling the 90GHz flux.[6] A shortX-ray flare was detected in February 2004 byINTEGRAL, with the source being detected in the 20-40keV energy range at the level of ≈2 x 10−10 erg cm−2 s−1.[9] In 2010, there was increased gamma-ray flux from the blazar[10] leading to a high amplitude outburst.[11]

NRAO 530 contains a core-jet structure showing detections ofsuperluminal motions in 5 of the jet components with projectedvelocities between the range of 13.6 and 25.2c. Additionally, the structure's compact component (the radio core) is found to be the strongest withpolarized emission around it.[12] There is an extended radio structure present containing slight emission knots being aligned in a confined curved westernjet, terminating at a hot spot location. When situated close to the core, the jet abruptly bends, revealing an evolution of aposition angle from north at projectedVLBI scale distance of ~400 parsecs. This is then increased towards west at a larger VLBI scale of ~10kiloparsecs. In the eastern side, a faint and broad counter-jet is seen ending at another bright hot spot creating a diffused lobe.[13]

NRAO 530 has two-sidedradio lobes, which the western lobe is found stronger compared to the eastern lobe and is linked to the core.[14] Furthermore, the western lobe is located 11 arcsecs west by a position angle of -86°.[12] An expandinghalo was detected between 1994 and 1995 with an apparent projected velocity of 26 h−1 c.[15]

Thesupermassive black hole mass in NRAO 530 is uncertain with some studies estimating it between the ranges of 3 x 108 Mʘ[16] and 2 x 109 Mʘ.[17]

References

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  1. ^Jorstad, Svetlana; Wielgus, Maciek; Lico, Rocco; Issaoun, Sara; Broderick, Avery E.; Pesce, Dominic W.; Liu, Jun; Zhao, Guang-Yao; Krichbaum, Thomas P.; Blackburn, Lindy; Chan, Chi-kwan; Janssen, Michael; Ramakrishnan, Venkatessh; Akiyama, Kazunori; Alberdi, Antxon (February 2023)."The Event Horizon Telescope Image of the Quasar NRAO 530".The Astrophysical Journal.943 (2): 170.arXiv:2302.04622.Bibcode:2023ApJ...943..170J.doi:10.3847/1538-4357/acaea8.ISSN 0004-637X.
  2. ^Junkkarinen, V. (1984-07-01)."Spectrophotometry of the QSO NRAO 530".Publications of the Astronomical Society of the Pacific.96:539–542.Bibcode:1984PASP...96..539J.doi:10.1086/131374.ISSN 0004-6280.
  3. ^Torniainen, I.; Tornikoski, M.; Teräsranta, H.; Aller, M. F.; Aller, H. D. (2005-05-13)."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. ^Welch, W. J.; Spinrad, Hyron (1973-08-01)."High-Frequency Observations of the Radio Source NRAO 530".Publications of the Astronomical Society of the Pacific.85 (506): 456.Bibcode:1973PASP...85..456W.doi:10.1086/129485.ISSN 0004-6280.
  5. ^An, Tao; Baan, Willem A.; Wang, Jun-Yi; Wang, Yu; Hong, Xiao-Yu (2013-08-08)."Periodic radio variabilities in NRAO 530: a jet–disc connection?".Monthly Notices of the Royal Astronomical Society.434 (4):3487–3496.doi:10.1093/mnras/stt1265.ISSN 0035-8711.
  6. ^abFeng, S.-W.; Shen, Z.-Q.; Cai, H.-B.; Chen, X.; Lu, R.-S.; Huang, L. (2006-08-23)."Multi-frequency VLBI observations of NRAO 530"(PDF).Astronomy & Astrophysics.456 (1):97–104.arXiv:astro-ph/0605578.Bibcode:2006A&A...456...97F.doi:10.1051/0004-6361:20054678.ISSN 0004-6361.
  7. ^Starr, Michelle (2023-02-13)."EHT Peers Into The Heart of One of The Brightest Lights in The Universe".ScienceAlert. Retrieved2024-10-26.
  8. ^Bower, Geoffrey C.; Backer, Donald C.; Wright, Melvyn; Forster, James R.; Aller, Hugh D.; Aller, Margo F. (1997-07-20)."A Dramatic Millimeter Wavelength Flare in the Gamma-Ray Blazar NRAO 530".The Astrophysical Journal.484 (1):118–130.Bibcode:1997ApJ...484..118B.doi:10.1086/304314.ISSN 0004-637X.
  9. ^Foschini, L.; Pian, E.; Maraschi, L.; Raiteri, C. M.; Tavecchio, F.; Ghisellini, G.; Tosti, G.; Malaguti, G.; Di Cocco, G. (2006-04-01)."A short hard X-ray flare from the blazar NRAO 530 observed by INTEGRAL".Astronomy and Astrophysics.450 (1):77–81.arXiv:astro-ph/0601101.Bibcode:2006A&A...450...77F.doi:10.1051/0004-6361:20064804.ISSN 0004-6361.
  10. ^D'Ammando, F.; Vandenbroucke, J. (2010-11-01)."Fermi LAT detection of increasing gamma-ray activity from the FSRQ PKS 1730-13".The Astronomer's Telegram.3002: 1.Bibcode:2010ATel.3002....1D.
  11. ^Williamson, Karen E.; Jorstad, Svetlana G.; Marscher, Alan P.; Larionov, Valeri M.; Smith, Paul S.; Agudo, Iván; Arkharov, Arkady A.; Blinov, Dmitry A.; Casadio, Carolina; Efimova, Natalia V.; Gómez, José L.; Hagen-Thorn, Vladimir A.; Joshi, Manasvita; Konstantinova, Tatiana S.; Kopatskaya, Evgenia N. (2014-06-23)."Comprehensive Monitoring of Gamma-ray Bright Blazars. I. Statistical Study of Optical, X-ray, and Gamma-ray Spectral Slopes".The Astrophysical Journal.789 (2): 135.arXiv:1406.2719.Bibcode:2014ApJ...789..135W.doi:10.1088/0004-637x/789/2/135.ISSN 0004-637X.
  12. ^abHong, Xiao-Yu; Sun, Chuan-Hao; Zhao, Jun-Hui; Jiang, Dong-Rong; Shen, Zhi-Qiang; An, Tao; Wang, Wei-Hua; Yang, Jun (2008-04-01)."Bending of Jets in the QSO NRAO 530".Chinese Journal of Astronomy and Astrophysics.8 (2):179–194.Bibcode:2008ChJAA...8..179H.doi:10.1088/1009-9271/8/2/05.ISSN 1009-9271.
  13. ^Zhao, Jun-Hui; Morris, Mark R.; Goss, W. M. (April 2019)."A Procedure for Making High Dynamic-range Radio Images: Deep Imaging of the Kiloparsec-scale Radio Structures of a Distant Blazar, NRAO 530, with JVLA Data".The Astrophysical Journal.875 (2): 134.arXiv:1903.08586.Bibcode:2019ApJ...875..134Z.doi:10.3847/1538-4357/ab11c4.ISSN 0004-637X.
  14. ^Lu, R.-S.; Krichbaum, T. P.; Zensus, J. A. (2011-11-18)."High-frequency very long baseline interferometry studies of NRAO 530".Monthly Notices of the Royal Astronomical Society.418 (4):2260–2272.arXiv:1108.0152.Bibcode:2011MNRAS.418.2260L.doi:10.1111/j.1365-2966.2011.19537.x.ISSN 0035-8711.
  15. ^Jorstad, Svetlana G.; Marscher, Alan P.; Mattox, John R.; Wehrle, Ann E.; Bloom, Steven D.; Yurchenko, Alexei V. (June 2001)."Multiepoch Very Long Baseline Array Observations of EGRET-detected Quasars and BL Lacertae Objects: Superluminal Motion of Gamma-Ray Bright Blazars".The Astrophysical Journal Supplement Series.134 (2):181–240.arXiv:astro-ph/0101570.Bibcode:2001ApJS..134..181J.doi:10.1086/320858.ISSN 0067-0049.
  16. ^Keck, Mason L. (2019-01-01).Probing the inner regions of supermassive black hole accretion disks and jets (Thesis).Bibcode:2019PhDT.......127K.
  17. ^Liang, E. W.; Liu, H. T. (April 2003)."The masses of central supermassive black holes and the variability time-scales in gamma-ray loud blazars".Monthly Notices of the Royal Astronomical Society.340 (2):632–638.Bibcode:2003MNRAS.340..632L.doi:10.1046/j.1365-8711.2003.06327.x.ISSN 0035-8711.

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