QSO B1038+528A

QSO B1038+528A
The quasar QSO B1038+528A. On the left side of the image is QSO B1038+528B.
Observation data (J2000.0 epoch)
ConstellationUrsa Major
Right ascension10h 41m 46.78s[1]
Declination+52° 33′ 28.23″[1]
Redshift0.678425[1]
Heliocentric radial velocity203,387 km/s[1]
Distance6.367 Gly
Apparent magnitude (V)18.5
Apparent magnitude (B)16.96
Characteristics
TypeHPQ FSRQ[1]
Size~233,000 ly (71.4 kpc) (estimated)[1]
Other designations
OL +564, SDSS J104146.77+523328.2, SBS 1038+538, RX J1041.7+5233, 2MASS J10414679+5233283, 6C B103844.1+524909, ICRF J104146.7+523328, JVAS J1041+5233, VIPS 0362, VLSS J1041.7+5233[1] PGC 3510279

QSO B1038+528A, also known as OL 564,[2] is a radio-loud quasar located in the constellation of Ursa Major. The redshift of the quasar is (z) 0.678[1][3] and it was first discovered via a NRAO interferometer survey by a team of astronomers lead by F.N. Owen in 1980, who described it along with QSO B1038+528B as an extremely close pair of quasars.[4] The radio spectrum of the quasar is considered as flat, making it a flat-spectrum radio quasar.[5]

Description

QSO B1038+528A makes up one of the quasar pair alongside QSO B1038+528B. While the primary quasar is found to be brighter with a redshift at 0.67, the secondary quasar is faint and located at (z) 2.296.[4] The absolute magnitude of the quasars are estimated to be 17.5 and 18.5 respectively.[6] The separation between the quasar pair is 33 arcseconds.[7][8]

The radio structure of QSO B1038+528A is compact. When observed, the radio morphology is shown to be of core-jet type with a long radio jet that is extending outwards from the radio core with a distance spanning at least 50 milliarcseconds (400 parsecs) and a position angle of 22°. This jet is also found to contain a steep spectrum. Two other components are discovered in the quasar, mainly a strong component and a much weaker component.[9] Traces of diffused radio emission have been found to surround the quasar based on radio mapping made by the Very Large Array (VLA).[3]

A study published in 1988 showed that QSO B1038+528A has evidence of superluminal motion. Based on observations, a component is found ejecting from the position of the core towards direction of north-east, travelling at a speed of 100 kilometers per second.[10] The proper motion value for its core is found to be estimated as 31 ± 22 per year and it is also said to be shifting by 0.7 milliarcseconds between 2.3 and 8.4 GHz frequencies.[3][11]

References

  1. ^ a b c d e f g h "NED Search Results for QSO B1038+528A (OL 564)". NASA/IPAC Extragalactic Database. Retrieved 2025-11-29.
  2. ^ Hintzen, P. (July 1984). "Wide-angle radio tail QSOs as members of clusters of galaxies. II. Direct optical observations and spectroscopy of QSO fields". The Astrophysical Journal Supplement Series. 55: 533–550. Bibcode:1984ApJS...55..533H. doi:10.1086/190966. ISSN 0067-0049.
  3. ^ a b c Marcaide, J. M.; Elosegui, P.; Shapiro, I. I. (Aug 1994). "On the Relative Proper Motion of Quasars 1038+528 A,B". The Astronomical Journal. 108: 368. Bibcode:1994AJ....108..368M. doi:10.1086/117075. ISSN 0004-6256.
  4. ^ a b Owen, F. N.; Wills, B. J.; Wills, D. (Jan 1980). "A close pair of radio-emitting quasi-stellar objects". The Astrophysical Journal. 235: L57–L60. Bibcode:1980ApJ...235L..57O. doi:10.1086/183158. ISSN 0004-637X.
  5. ^ Rioja, M. J.; Porcas, R. W. (March 2000). "A phase-reference study of the quasar pair 1038+528A,B". Astronomy and Astrophysics. 355: 552–563. arXiv:astro-ph/0002097. Bibcode:2000A&A...355..552R. ISSN 0004-6361.
  6. ^ Marcaide, J. M.; Shapiro, I. I. (Jan 1984). "VLBI study of 1038+528A and B : discovery of wavelength dependence of peak brightness location". The Astrophysical Journal. 276: 56–59. Bibcode:1984ApJ...276...56M. doi:10.1086/161592. ISSN 0004-637X.
  7. ^ Elosegui, Pedro; Marcaide, Juan-Maria; Shapiro, Irwin I. (1991). "Errors in high precision source position determination". IAU Colloquium 131: Radio Interferometry. Theory, Techniques, and Applications. 19: 307–311. Bibcode:1991ASPC...19..307E. ISSN 1050-3390.
  8. ^ Marcaide, J. M.; Shapiro, I. I. (Aug 1983). "High precision astrometry via very-long-baseline radio interferometry : estimate of the angular separation between the quasars 1038+528A and B." The Astronomical Journal. 88: 1133–1137. Bibcode:1983AJ.....88.1133M. doi:10.1086/113402. ISSN 0004-6256.
  9. ^ Marcaide, J. M.; Shapiro, I. I.; Corey, B. E.; Cotton, W. D.; Gorenstein, M. V.; Rogers, A. E. E.; Romney, J. D.; Schild, R. E.; Baath, L.; Bartel, N.; Cohen, N. L.; Clark, T. A.; Preston, R. A.; Ratner, M. I.; Whitney, A. R. (Jan 1985). "The quasars 1038+528 A and B." Astronomy and Astrophysics. 142: 71–84. Bibcode:1985A&A...142...71M. ISSN 0004-6361.
  10. ^ Marcaide, J. M.; Bartel, N.; Bonometti, R. J.; Corey, B. E.; Cotton, W. D.; Gorenstein, M. V.; Preston, R. A.; Ratner, M. I.; Rogers, A. E. E.; Shapiro, I. I. (1988). "Second Epoch of Simultaneous λ 3.6 and λ 13 CM Observations of the Pair of Quasars 1038 + 528 A, B". The Impact of VLBI on Astrophysics and Geophysics. 129: 101. ISSN 1743-9221.
  11. ^ Lobanov, A. P. (Feb 1998). "Ultracompact jets in active galactic nuclei". Astronomy and Astrophysics. 330: 79–89. arXiv:astro-ph/9712132. Bibcode:1998A&A...330...79L. ISSN 0004-6361.
This article is issued from Wikipedia. The text is available under Creative Commons Attribution-Share Alike 4.0 unless otherwise noted. Additional terms may apply for the media files.