OI 287

Last updated
OI 287
Image of OI 287.png
SDSS image of OI 287
Observation data (J2000.0 epoch)
Constellation Gemini
Right ascension 07h 55m 37.03s [1]
Declination +25° 42′ 39.02″ [1]
Redshift 0.444241 [1]
Heliocentric radial velocity 133,180 km/s ± 12 [1]
Distance 4.779 Gly
Apparent magnitude  (V)18.04
Apparent magnitude  (B)18.50
Characteristics
Type BLLAC [1]
Size~240,000  ly (73.7  kpc) (estimated) [1]
Other designations
B2 0752+25A, NVSS J075537+254236, SDSS J075537.02+254238.9, THING 587732156852142361, 2MASS J07553702+2542389 [1] LEDA 3506791

OI 287 is a quasar [2] located in the constellation of Gemini. The redshift of the object is (z) 0.444 [1] and it was first discovered as a highly polarized object by astronomers in January 1981, [3] but it also has been classified as a blazar in a 1982 study. [4]

Contents

Description

The source of OI 287 has a double-lobed structure based on Very Large Array (VLA) observations made in 1984, however at that time it was unresolved. [5] Radio maps made at 20 and 6 centimeters (cm), would reveal the source has a twin-jet structure, depicted as oscillating. The radio spectrum of the source also has a steep appearance between frequencies of 0.36 and 5 GHz. There is a radio core present with an inverted spectrum between 1.4 and 5 GHz but no variability of its flux density. [4] The core is lowly polarized with polarization levels of only 0.25%. [6]

The host galaxy of OI 287 has a circular appearance with an M-R apparent magnitude of -23.0 based on optical imaging. [7] However a study published in 1998, suggested it has a disk morphology when observed through near-infrared imaging, displaying the presence of radio emission. The host is also described as slightly elongated towards its companion located 4.9 kiloparsecs away from it. [8]

The optical spectrum of OI 287 shows the presence of rich emission lines featuring both narrow and broad Balmer components, as well as detections of doubly ionized oxygen [O III] emission. The optical continuum of the spectrum is found to be increasing sharply towards the near-infrared, but gets flatter at around 10 microns. [9] A broad-line region was located inside the quasar, described as having an obscured appearance, with it's accretion disk also likely obscured as well. The mass range of the torus is 105-107 Mʘ and the total thickness of the narrow-line region is approximately 2 x 10-8 parsecs. The supermassive black hole located in the center of OI 287 has an estimated mass of 1.46+1.89-0.82 x 109 Mʘ. [10]

References

  1. 1 2 3 4 5 6 7 8 "NED Search results for OI 287". NASA/IPAC Extragalactic Database. Retrieved 2025-12-25.
  2. ↑ Antonucci, Robert; Kinney, Anne L.; Hurt, Todd (September 1993). "Hubble Space Telescope Ultraviolet Spectroscopy of the Highly Polarized but Quiescent Quasar OI 287". The Astrophysical Journal. 414: 506. Bibcode:1993ApJ...414..506A. doi:10.1086/173098. ISSN   0004-637X.
  3. ↑ Moore, R. L.; Stockman, H. S. (January 1981). "The class of highly polarized quasars : observations and description". The Astrophysical Journal. 243: 60–75. Bibcode:1981ApJ...243...60M. doi:10.1086/158567. ISSN   0004-637X.
  4. 1 2 Saikia, D. J.; Salter, C. J.; Neff, S. G.; Gower, A. C.; Sinha, R. P.; Swarup, G. (1987-09-01). "Radio observations of a few selected blazars" (PDF). Monthly Notices of the Royal Astronomical Society. 228 (1): 203–216. doi: 10.1093/mnras/228.1.203 . ISSN   0035-8711.
  5. ↑ Wardle, J. F. C.; Moore, R. L.; Angel, J. R. P. (April 1984). "The radio morphology of blazars and relationships to optical polarization and to normal radio galaxies". The Astrophysical Journal. 279: 93–111. Bibcode:1984ApJ...279...93W. doi:10.1086/161868. ISSN   0004-637X.
  6. ↑ Ulvestad, James S.; Antonucci, Robert R. J. (May 1988). "Radio Properties of the Highly Polarized, Quiescent Quasar OI 287". The Astrophysical Journal. 328: 569. Bibcode:1988ApJ...328..569U. doi:10.1086/166314. ISSN   0004-637X.
  7. ↑ Hutchings, J. B.; Crampton, D.; Campbell, B. (May 1984). "Optical imaging of 78 quasars and host galaxies". The Astrophysical Journal. 280: 41–50. Bibcode:1984ApJ...280...41H. doi:10.1086/161966. ISSN   0004-637X.
  8. ↑ Wright, S.C.; McHardy, I.M.; Abraham, R.G.; Crawford, C.S. (June 1998). "Near-infrared imaging of the host galaxies of BL Lacertae objects" (PDF). Monthly Notices of the Royal Astronomical Society. 296 (4): 961–976. Bibcode:1998MNRAS.296..961W. doi: 10.1046/j.1365-8711.1998.01463.x . ISSN   0035-8711.
  9. ↑ Rudy, Richard J.; Schmidt, Gary D. (August 1988). "The Nature of the Strong, Static Polarization of the Quasar OI 287". The Astrophysical Journal. 331: 325. Bibcode:1988ApJ...331..325R. doi:10.1086/166557. ISSN   0004-637X.
  10. ↑ Li, Zhenzhen; Zhou, Hongyan; Hao, Lei; Wang, Huiyuan; Ji, Tuo; Shi, Xiheng; Liu, Bo; Zhang, Shaohua; Liu, Wen-Juan; Pan, Xiang; Jiang, Peng (2015-10-12). "Detection of the Intermediate-Width Emission Line Region in Quasar Oi 287 with the Broad Emission Line Region Obscured by the Dusty Torus". The Astrophysical Journal. 812 (2): 99. arXiv: 1512.02824 . Bibcode:2015ApJ...812...99L. doi:10.1088/0004-637x/812/2/99. ISSN   1538-4357.
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