CTD 135

CTD 135
SDSS image of CTD 135.
Observation data (J2000.0 epoch)
ConstellationPegasus
Right ascension22h 36m 22.47s
Declination+28° 28′ 57.41″
Redshift0.790000
Heliocentric radial velocity236,836 km/s
Distance6.976 Gly
Apparent magnitude (V)19.0
Apparent magnitude (B)19.1
Characteristics
TypeHPQ FSRQ
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

CTD 135 is a radio-loud quasar located in the constellation of Pegasus. The redshift of the object is (z) 0.790 and it was first discovered as an astronomical radio source in 1970 by astronomers. It is classified as a BL Lacertae object and has a flat radio spectrum thus categorizing it a flat-spectrum radio quasar.

Description

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. There is a radio core present that has a brightness temperature of 0.1 x 1012 Kelvin. 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. 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.

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. A near infrared flare was detected on 26 November 2010. On 12 January 2016, it had another near infrared flare, which its optical brightness corresponds to around 14.78 ± 0.04. In November 2024, the quasar had shown a new flare which increased its luminosity by a factor of 64 in H-band.

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.

References

  1. 1 2 3 4 5 6 7 8 "NED Search results for CTD 135". NASA/IPAC Extragalactic Database. Retrieved 2025-11-16.
  2. ↑ 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.
  3. ↑ 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.
  4. ↑ 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.
  5. ↑ 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)
  6. 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.
  7. ↑ 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.
  8. 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
  9. ↑ 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)
  10. ↑ "ATel #3056: NIR flaring of the FRSQSO B2 2234+28A". The Astronomer's Telegram. Retrieved 2025-11-16.
  11. ↑ "ATel #8572: A NIR Flare of the QSO B2 2234+28A". The Astronomer's Telegram. Retrieved 2025-11-16.
  12. ↑ "ATel #16872: Historical NIR light maximum of the blazar B2 2234+28A". The Astronomer's Telegram. Retrieved 2025-11-16.
  13. ↑ 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.