PG 1216+069
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| PG 1216+069 | |
|---|---|
 SDSS image of PG 1216+069. | |
| Observation data (J2000.0 epoch) | |
| Constellation | Virgo |
| Right ascension | 12h 19m 20.93s[1] |
| Declination | +06° 38′ 38.49″[1] |
| Redshift | 0.331300[1] |
| Heliocentric radial velocity | 99,321 km/s ± 90[1] |
| Distance | 3.822 Gly |
| Apparent magnitude (V) | 15.65 |
| Apparent magnitude (B) | 15.68 |
| Characteristics | |
| Type | Elliptical Sy1[1] |
| Size | ~405,500 ly (124.32 kpc) (estimated)[1] |
| Other designations | |
| 2MASS J12192094+0638384, PG 1216+069, RBS 1097, RX J1219.3+0638, SDSS J121920.93+063838.5[1] | |
PG 1216+069 is a quasar and also a Seyfert 1 galaxy located in the constellation of Virgo. The redshift of the object is (z) 0.331[1] and it was first discovered by astronomers from the Bright Quasar Survey (BQS) in June 1983.[2] It has also been classified as a radio intermediate quasar (RIQ) in literature.[3]
PG 1216+069 is radio-quiet.[4] It is hosted by a large elliptical galaxy, based on Hubble Space Telescope (HST) imaging, which has an absolute magnitude of around -20.9. It is also surrounded by a halo structure. Two close companions are found to be located from the galaxy by 13.6 and 20.4 kiloparsecs respectively.[5][6][7] A subdampened Lyman-alpha absorption line system was located towards the quasar.[8]
The radio structure of PG 1216+069 can be considered as compact. When imaged with the Very Long Baseline Array (VLBA), it has a compact radio core with a brightness temperature of >108 Kelvin, with it’s flux density peaking at around 1.04 mJy frequencies. Radio imaging made with Very Long Baseline Interferometry (VLBI) found the component radio spectrum is flat, with the spectral shape being described as inverted.[9] A slightly extended structure is found based on radio mapping at 5 and 8.4 GHz frequencies.[10]
A supermassive black hole mass has been estimated for PG 1216+069, and is estimated to be 8.30 ± 0.12 M☉.[11] There have also been detections of doubly ionized silicon absorption at high velocities towards the quasar, spread out evenly across two components that are separating from each other at 234 kilometers per second.[12]
References
- 1 2 3 4 5 6 7 8 "NED Search results for PG 1216+069". NASA/IPAC Extragalactic Database. Retrieved 2025-12-25.
- ↑ Schmidt, M.; Green, R. F. (June 1983). "Quasar evolution derived from the Palomar bright quasar survey and other complete quasar surveys". The Astrophysical Journal. 269: 352–374. Bibcode:1983ApJ...269..352S. doi:10.1086/161048. ISSN 0004-637X.
- ↑ Polletta, M.; Courvoisier, T. J.-L.; Hooper, E. J.; Wilkes, B. J. (October 2000). "The far-infrared emission of radio loud and radio quiet quasars". Astronomy and Astrophysics. 362: 75–96. arXiv:astro-ph/0006315. Bibcode:2000A&A...362...75P. ISSN 0004-6361.
- ↑ Laor, Ari; Baldi, Ranieri D; Behar, Ehud (2018-11-16). "What drives the radio slopes in radio-quiet quasars?". Monthly Notices of the Royal Astronomical Society. 482 (4): 5513–5523. arXiv:1810.10245. doi:10.1093/mnras/sty3098. ISSN 0035-8711.
- ↑ Wisotzki, L.; Kuhlbrodt, B.; Jahnke, K. (2001-03-07), The luminosity function of QSO host galaxies, arXiv:astro-ph/0103112, Bibcode:2001qhte.conf...83W
- ↑ Percival, W. J.; Miller, L.; McLure, R. J.; Dunlop, J. S. (2001), "The Host Galaxies of Luminous Radio-Quiet Quasars", QSO Hosts and Their Environments, Boston, MA: Springer US, pp. 21–26, doi:10.1007/978-1-4615-0695-9_3, ISBN 978-1-4613-5199-3, retrieved 2025-12-25
{{citation}}: CS1 maint: work parameter with ISBN (link) - ↑ Boyce, P. J.; Disney, M. J.; Blades, J. C.; Boksenberg, A.; Crane, P.; Deharveng, J. M.; Macchetto, F. D.; Mackay, C. D.; Sparks, W. B. (July 1998). "HST Planetary Camera images of quasar host galaxies" (PDF). Monthly Notices of the Royal Astronomical Society. 298 (1): 121–130. Bibcode:1998MNRAS.298..121B. doi:10.1046/j.1365-8711.1998.01617.x. ISSN 0035-8711.
- ↑ Chengalur, Jayaram N.; Ghosh, T.; Salter, C. J.; Kanekar, N.; Momjian, E.; Keeney, B. A.; Stocke, J. T. (2015-09-03). "H i 21cm emission from the subdamped Lyman-α absorber atz = 0.0063 towards PG 1216+069". Monthly Notices of the Royal Astronomical Society. 453 (3): 3136–3143. arXiv:1508.02825. doi:10.1093/mnras/stv1840. ISSN 0035-8711.
- ↑ Wang, Ailing; An, Tao; Zhang, Yingkang; Cheng, Xiaopeng; Ho, Luis C; Kellermann, Kenneth I; Baan, Willem A (2023-09-02). "VLBI Observations of a sample of Palomar-Green quasars II: characterizing the parsec-scale radio emission". Monthly Notices of the Royal Astronomical Society. 525 (4): 6064–6083. doi:10.1093/mnras/stad2651. ISSN 0035-8711.
- ↑ Chen, Sina; Laor, Ari; Behar, Ehud; Baldi, Ranieri D; Gelfand, Joseph D (2023-07-28). "The radio emission in radio-quiet quasars: the VLBA perspective". Monthly Notices of the Royal Astronomical Society. 525 (1): 164–182. doi:10.1093/mnras/stad2289. ISSN 0035-8711.
- ↑ Vestergaard, M. (2002-04-05), "Determining Central Black Hole Masses in Distant Active Galaxies", The Astrophysical Journal, 571 (2): 733–752, arXiv:astro-ph/0204106, Bibcode:2002ApJ...571..733V, doi:10.1086/340045
- ↑ Collins, Joseph A.; Shull, J. Michael; Giroux, Mark L. (2009-10-16). "HUBBLE SPACE TELESCOPESURVEY OF INTERSTELLAR HIGH-VELOCITY Si III". The Astrophysical Journal. 705 (1): 962–977. arXiv:0909.4900. Bibcode:2009ApJ...705..962C. doi:10.1088/0004-637x/705/1/962. ISSN 0004-637X.
