CTD 135
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| CTD 135 | |
|---|---|
 SDSS image of CTD 135. | |
| Observation data (J2000.0 epoch) | |
| Constellation | Pegasus |
| Right ascension | 22h 36m 22.47s[1] |
| Declination | +28° 28′ 57.41″[1] |
| Redshift | 0.790000[1] |
| Heliocentric radial velocity | 236,836 km/s[1] |
| Distance | 6.976 Gly |
| Apparent magnitude (V) | 19.0 |
| Apparent magnitude (B) | 19.1 |
| Characteristics | |
| Type | HPQ FSRQ[1] |
| Other designations | |
| 2MASS J22362246+2828570, NVSS J223622+282858, OY +256, TXS 2234+282, IRCF J223622.4+282857, B2 2234+82A, 87GB 223359.9+281325, FL8Y J2236.4+2828[1] | |
CTD 135 is a radio-loud[2] quasar located in the constellation of Pegasus. The redshift of the object is (z) 0.790[1] and it was first discovered as an astronomical radio source in 1970 by astronomers.[3] It is classified as a BL Lacertae object and has a flat radio spectrum thus categorizing it a flat-spectrum radio quasar.[4][1][5]
CTD 135 is found to have a compact radio structure. When observed at both 4.8 and 1.4 GHz frequencies, it has one component that is found to be unsolved with an extend of 5 milliarcseconds. At 8.4 GHz, the source has a radio jet that is positioned at 60° with multiple bright component features.[6][7] There is a radio core present that has a brightness temperature of 0.1 x 1012 Kelvin.[6] This core is also suggested to be self-absorbed and weak at frequency range below 15 GHz. Two other components are found; a southwest component that has a flat radio spectrum and a northern east component that contains a steep radio spectrum. The flux density of the core is estimated to be 755 ± 39 mJy at 15 GHz.[8] The host galaxy of CTD 135 has been suggested to be a luminous giant elliptical galaxy with a total host magnitude of -25.30 ± 0.41.[9]
Studies have found CTD 135 is a blazar. When observed, it is known to display significant variability on long-term light curves and also within the a short timespan of a few day period.[8] A near infrared flare was detected on 26 November 2010.[10] On 12 January 2016, it had another near infrared flare, which its optical brightness corresponds to around 14.78 ± 0.04.[11] In November 2024, the quasar had shown a new flare which increased its luminosity by a factor of 64 in H-band.[12]
A possible quasi-periodic oscillation signature was detected in CTD 135 in October 2021. Based on its long-term light curve data, it is estimated to be 460 days long. The central supermassive black hole of the quasar is 108.35 M☉ with the accretion disk luminosity being 6.03 × 1045 erg s−1.[13]
References
- 1 2 3 4 5 6 7 8 "NED Search results for CTD 135". NASA/IPAC Extragalactic Database. Retrieved 2025-11-16.
- ↑ Cheng, X.-P.; An, T.; Frey, S.; Hong, X.-Y.; He, X.; Kellermann, K. I.; Lister, M. L.; Lao, B.-Q.; Li, X.-F.; Mohan, P.; Yang, J.; Wu, X.-C.; Zhang, Z.-L.; Zhang, Y.-K.; Zhao, W. (2020-04-01). "Compact Bright Radio-loud AGNs. III. A Large VLBA Survey at 43 GHz". The Astrophysical Journal Supplement Series. 247 (2): 57. arXiv:2003.01382. Bibcode:2020ApJS..247...57C. doi:10.3847/1538-4365/ab791f. ISSN 0067-0049.
- ↑ Ames, Susan (February 1970). "Flux Measurements of Radio Sources at 2695 MHz". The Astronomical Journal. 75: 71. Bibcode:1970AJ.....75...71A. doi:10.1086/110944. ISSN 0004-6256.
- ↑ Altschuler, D. R. (February 1982). "The short-term radio variability of BL Lacertae objects". The Astronomical Journal. 87: 387–394. Bibcode:1982AJ.....87..387A. doi:10.1086/113110. ISSN 0004-6256.
- ↑ Abe, S; Abhir, J; Abhishek, A; Acciari, V A; Aguasca-Cabot, A; Agudo, I; Aniello, T; Ansoldi, S; Antonelli, L A; Arbet Engels, A; Arcaro, C; Artero, M; Asano, K; Babić, A; Baquero, A (2024-11-07). "Constraints on VHE gamma-ray emission of flat spectrum radio quasars with the MAGIC telescopes". Monthly Notices of the Royal Astronomical Society. 535 (2). doi:10.1093/mnra (inactive 30 November 2025). ISSN 0035-8711. Archived from the original on 2024-12-05.
{{cite journal}}: CS1 maint: DOI inactive as of November 2025 (link) - 1 2 Airapetyan, E. A.; Matveenko, L. I. (January 1997). "The fine structure of compact radio sources from geodetic data". Astronomy Letters. 23 (1): 64–70. Bibcode:1997AstL...23...64A. ISSN 0320-0108.
- ↑ Hodge, M. A.; Lister, M. L.; Aller, M. F.; Aller, H. D.; Kovalev, Y. Y.; Pushkarev, A. B.; Savolainen, T. (August 2018). "Mojave XVI: Multiepoch Linear Polarization Properties of Parsec-scale AGN Jet Cores". The Astrophysical Journal. 862 (2): 151. arXiv:1806.07312. Bibcode:2018ApJ...862..151H. doi:10.3847/1538-4357/aacb2f. ISSN 0004-637X.
- 1 2 Frey, S.; Gabányi, K. É; An, T. (2022-02-02), "The Quasar CTD 135 is Not a Compact Symmetric Object", Symmetry, 14 (2): 321, arXiv:2202.00950, Bibcode:2022Symm...14..321F, doi:10.3390/sym14020321, retrieved 2025-11-16
- ↑ Olguín-Iglesias, A.; León-Tavares, J.; Kotilainen, J. K.; Chavushyan, V.; Tornikoski, M.; Valtaoja, E.; Añorve, C.; Valdés, J.; Carrasco, L. (2016-08-11). "The host galaxies of active galactic nuclei with powerful relativistic jets". Monthly Notices of the Royal Astronomical Society. 460 (3). doi:10.1093/mnra (inactive 30 November 2025). ISSN 0035-8711. Archived from the original on 2024-04-29.
{{cite journal}}: CS1 maint: DOI inactive as of November 2025 (link) - ↑ "ATel #3056: NIR flaring of the FRSQSO B2 2234+28A". The Astronomer's Telegram. Retrieved 2025-11-16.
- ↑ "ATel #8572: A NIR Flare of the QSO B2 2234+28A". The Astronomer's Telegram. Retrieved 2025-11-16.
- ↑ "ATel #16872: Historical NIR light maximum of the blazar B2 2234+28A". The Astronomer's Telegram. Retrieved 2025-11-16.
- ↑ Gan, Ying-Ying; Zhang, Hai-Ming; Zhang, Jin; Yang, Xing; Yi, Ting-Feng; Liang, Yun-Feng; Liang, En-Wei (October 2021). "Highly variable γ-ray emission of CTD 135 and implications for its compact symmetric structure". Research in Astronomy and Astrophysics. 21 (8): 201. arXiv:2104.04436. Bibcode:2021RAA....21..201G. doi:10.1088/1674-4527/21/8/201. ISSN 1674-4527.
External links
- CTD 135 on WikiSky: DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images
- CTD 135 on SIMBAD
