Astronomy:OI 287

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OI 287
File:Image of OI 287.png
SDSS image of OI 287
Observation data (J2000.0 epoch)
ConstellationGemini
Right ascension 07h 55m 37.03s[1]
Declination+25° 42′ 39.02″[1]
Redshift0.444241[1]
Helio radial velocity133,180 km/s ± 12[1]
Distance4.779 Gly
Apparent magnitude (V)18.04
Apparent magnitude (B)18.50
Characteristics
TypeBLLAC[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]

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 its 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. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 "NED Search results for OI 287". https://ned.ipac.caltech.edu/byname?objname=OI+287&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1. 
  2. ↑ Antonucci, Robert; Kinney, Anne L.; Hurt, Todd (September 1993). "Hubble Space Telescope Ultraviolet Spectroscopy of the Highly Polarized but Quiescent Quasar OI 287" (in en). The Astrophysical Journal 414: 506. doi:10.1086/173098. ISSN 0004-637X. Bibcode: 1993ApJ...414..506A. https://ui.adsabs.harvard.edu/abs/1993ApJ...414..506A/abstract. 
  3. ↑ Moore, R. L.; Stockman, H. S. (January 1981). "The class of highly polarized quasars : observations and description." (in en). The Astrophysical Journal 243: 60–75. doi:10.1086/158567. ISSN 0004-637X. Bibcode: 1981ApJ...243...60M. https://ui.adsabs.harvard.edu/abs/1981ApJ...243...60M/abstract. 
  4. ↑ 4.0 4.1 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". Monthly Notices of the Royal Astronomical Society 228 (1): 203–216. doi:10.1093/mnras/228.1.203. ISSN 0035-8711. https://watermark02.silverchair.com/mnras228-0203.pdf?token=AQECAHi208BE49Ooan9kkhW_Ercy7Dm3ZL_9Cf3qfKAc485ysgAAA1wwggNYBgkqhkiG9w0BBwagggNJMIIDRQIBADCCAz4GCSqGSIb3DQEHATAeBglghkgBZQMEAS4wEQQMky84-wMdI3xkmGb5AgEQgIIDD5AhxLtsNRbELyTjvARbpV7y9mLGgLYiiMV_Z8Es3yLyecxnSxHiSU2BLWoyZ_6T6rWbuiVMXREiYIYXQIgzvHPFfNOACeL0rc1HTnWM4wbunfp9s3GvobAYiqjeeICtxKO-FU9GxrMfkQbvhIZ4tgxV0WQ5JDw2wWobJDvzE5AiQ8GYKhQZtcs8hJcBtD0PyMU0LmRKzEEMuvhZ-918bre2f6A6U7aoJyZ4FX0l5dVfIXJUGCZgmIVb2a6Va9OcOCdktc6Ui7bMqcO-anOM-5vIMI0ibnIJZqHmnHFxPvmyVnQesXX8znUIsIvlHNCegycXXH8rCgLeQjeDc1cXmK0hV4AnCciQmHYvLyj4LgA6QfO8ATvnBjZlVt9fBgCZVcgrFoMJw1rkufgGc7R7qvToOkG9MF9ZlcmGsQEnnpmyEXG75Q5_ZUcd2s6XFYB_yyFjP6wmCs48bu-Hjb0XQ_FszY2W_i8Xa-Wb0DNT-y7FJfQKWALuf3WmAkDRsJfa22021cr6rQBYgF35rt5Zln7lyAqaz1NxGTugQ5g5qPNUgOC_p3iwIflp6Z9jzYDzf4M2gYfqzRJlDxFWFsuW6F6OyBd_7L5Ocslc7nQMtICfcKOAx1nzhIh8XTVtD4GquLI-EkqMrZtDRuenwluK6ke-kIXnI22kz9tWm_pdty35lf3q_uTqsp3vF8Fxu3ew2ZBy0pYTJ7Hhko2fKpSuqOLJCSlzI9SeClpMucTKBfK663mZso0l9UpgD5HTicLu1ThD4b-9pYoljcqe_Jt1C3_j7G1moaJ4lQ-VFQebaqfmj8Ypmae1tIVjBto2Vu6qV1meRjOenhMmiMIlXXQ0TjdjhWvA5GyqCyxQverYy0MoaYCnx1RFEKJfBNXzMW6K_V6otwkj6ANaaJQ1QXDPoxCGglr0twcu5jliCftCRVL0FL_jBokTD1j3HOXrSnr7V8G44od4zCBTBXwM19XFcO2rTNHfACg3iCg1voq-wsSf4u7uOzLYp9Ji_r9NwzcBfeljo7V8UbiZXvitLkT7Cg. 
  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." (in en). The Astrophysical Journal 279: 93–111. doi:10.1086/161868. ISSN 0004-637X. Bibcode: 1984ApJ...279...93W. https://ui.adsabs.harvard.edu/abs/1984ApJ...279...93W/abstract. 
  6. ↑ Ulvestad, James S.; Antonucci, Robert R. J. (May 1988). "Radio Properties of the Highly Polarized, Quiescent Quasar OI 287" (in en). The Astrophysical Journal 328: 569. doi:10.1086/166314. ISSN 0004-637X. Bibcode: 1988ApJ...328..569U. https://ui.adsabs.harvard.edu/abs/1988ApJ...328..569U/abstract. 
  7. ↑ Hutchings, J. B.; Crampton, D.; Campbell, B. (May 1984). "Optical imaging of 78 quasars and host galaxies." (in en). The Astrophysical Journal 280: 41–50. doi:10.1086/161966. ISSN 0004-637X. Bibcode: 1984ApJ...280...41H. https://ui.adsabs.harvard.edu/abs/1984ApJ...280...41H/abstract. 
  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". Monthly Notices of the Royal Astronomical Society 296 (4): 961–976. doi:10.1046/j.1365-8711.1998.01463.x. ISSN 0035-8711. Bibcode: 1998MNRAS.296..961W. https://watermark02.silverchair.com/296-4-961.pdf?token=AQECAHi208BE49Ooan9kkhW_Ercy7Dm3ZL_9Cf3qfKAc485ysgAAA2IwggNeBgkqhkiG9w0BBwagggNPMIIDSwIBADCCA0QGCSqGSIb3DQEHATAeBglghkgBZQMEAS4wEQQM6NZUM-61ZIdapPoDAgEQgIIDFQNG9fuXL2klZncsWe20zADTyVJXbwhjHoWZYBVzjxaI-H_Deo7WZqkcDlQbITaf-Y7X5VmngLP-b8DXWVx7OTe95jWHKIbvoolr3-TQS9j3_OCWwx5YIpQntivSSiPK2dpBOX8vOuWCLNArUiFKJWH2kXI0_Zv1SepHGxeBUIpZtg5Y0arv7V1tg3IchASV_bouCsqXPE7usr1gz_87Dc6ZZsZfwusjmWEGt0bqVDg00xbY5ckzRnzJaHkZN8FXlIS4T3KrTar657R1LSZcRxMckiBxSA9_IwaB3n8u0B1XuKUFm9Z-IifgD791a1PbOFg18-eTuS9gGE-TmVo1_TltG-n-P2t2nCxROwS2QhbV7wBLfjejybrl0u0yXmL_kpuNQPfxbN2801GE5pkAv809oYS7xZ41UuIRw2G6JIHkEnrimNeEFffsdSKDzADaQJMifFXcAinc0NkkHYyw8jNv0JWwJUfmYL0SqWTC0UBq9VKq9WzrvSal_VfeYq9Yc-kR0PU_ohl_fDLjEWT0sDv0kK1dUKuviJbGFBbOQjhDyvnCMQ2qzqYVrsEC8pAoUF45TAXCgK03Q9OfsKQcX3k0GdPzDUNX7-qDaadTk4L907l0D1usUl0B6aYIQOFwSa8FfZVAY5PBfIGenPjH-uU3JgaPzTeNeF3yYz_eZAxklK3ghL1jxyE4Jo5wTEA998jrPhThRggoL8GLWW4TE5IhpkJqxRvbLRYgT1EbiKQnKIke1LENOCpiWFL8gobAmBohPWUcAceQa0mAAY9QX2-Az9zc3UhJJ247_03FYUkOVRNIuB-L41mDaWJBlO-WeKpMG0PhxfQCqs28SgzkyB3XS-nrfIBxS0ZFxR4oxFXp7UD7Cr_io8nVtvng3kwgEFlwll6-Fl8vNfTG4aKBPFaO2ULpBgTQ6RlhK-dzZEfwYVr04rjw5k68CPZx9q15FDkdnqg2XVA2WZmn7WYUKWuRaAYHaDiJgRclvbF1u-0oaNr76xPOS-Pp56mJ410yUJ9ovmut1RNuPWXthRtrxtb5x_7CMA. 
  9. ↑ Rudy, Richard J.; Schmidt, Gary D. (August 1988). "The Nature of the Strong, Static Polarization of the Quasar OI 287" (in en). The Astrophysical Journal 331: 325. doi:10.1086/166557. ISSN 0004-637X. Bibcode: 1988ApJ...331..325R. https://ui.adsabs.harvard.edu/abs/1988ApJ...331..325R/abstract. 
  10. ↑ Li, Zhenzhen; Zhou, Hongyan; Hao, Lei; Wang, Huiyuan; Ji, Tuo; Shi, Xiheng; Liu, Bo; Zhang, Shaohua et al. (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. doi:10.1088/0004-637x/812/2/99. ISSN 1538-4357. Bibcode: 2015ApJ...812...99L. https://doi.org/10.1088/0004-637x/812/2/99. 



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