Astronomy:CTD 135

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CTD 135
SDSS image of CTD 135.
Observation data (J2000.0 epoch)
ConstellationPegasus
Right ascension 22h 36m 22.47s[1]
Declination+28° 28′ 57.41″[1]
Redshift0.790000[1]
Helio radial velocity236,836 km/s[1]
Distance6.976 Gly
Apparent magnitude (V)19.0
Apparent magnitude (B)19.1
Characteristics
TypeHPQ 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]

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.[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 Mʘ with the accretion disk luminosity being 6.03 x 1045 erg s-1.[13]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 "NED Search results for CTD 135". https://ned.ipac.caltech.edu/byname?objname=CTD+135&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1. 
  2. ↑ Cheng, X.-P.; An, T.; Frey, S.; Hong, X.-Y.; He, X.; Kellermann, K. I.; Lister, M. L.; Lao, B.-Q. et al. (2020-04-01). "Compact Bright Radio-loud AGNs. III. A Large VLBA Survey at 43 GHz". The Astrophysical Journal Supplement Series 247 (2): 57. doi:10.3847/1538-4365/ab791f. ISSN 0067-0049. Bibcode: 2020ApJS..247...57C. 
  3. ↑ Ames, Susan (February 1970). "Flux Measurements of Radio Sources at 2695 MHz" (in en). The Astronomical Journal 75: 71. doi:10.1086/110944. ISSN 0004-6256. Bibcode: 1970AJ.....75...71A. https://articles.adsabs.harvard.edu/pdf/1970AJ.....75...71A. 
  4. ↑ Altschuler, D. R. (February 1982). "The short-term radio variability of BL Lacertae objects." (in en). The Astronomical Journal 87: 387–394. doi:10.1086/113110. ISSN 0004-6256. Bibcode: 1982AJ.....87..387A. https://ui.adsabs.harvard.edu/abs/1982AJ.....87..387A/abstract. 
  5. ↑ Abe, S; Abhir, J; Abhishek, A; Acciari, V A; Aguasca-Cabot, A; Agudo, I; Aniello, T; Ansoldi, S et al. (2024-11-07). "Constraints on VHE gamma-ray emission of flat spectrum radio quasars with the MAGIC telescopes" (in en). Monthly Notices of the Royal Astronomical Society 535 (2). doi:10.1093/mnra. ISSN 0035-8711. https://academic.oup.com/mnras/article/535/2/1484/7815912. 
  6. ↑ 6.0 6.1 Airapetyan, E. A.; Matveenko, L. I. (January 1997). "The fine structure of compact radio sources from geodetic data" (in en). Astronomy Letters 23 (1): 64–70. ISSN 0320-0108. Bibcode: 1997AstL...23...64A. https://articles.adsabs.harvard.edu//full/1997AstL...23...64A/0000069.000.html. 
  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" (in en). The Astrophysical Journal 862 (2): 151. doi:10.3847/1538-4357/aacb2f. ISSN 0004-637X. Bibcode: 2018ApJ...862..151H. 
  8. ↑ 8.0 8.1 Frey, S.; Gabányi, K. É; An, T. (2022-02-02), "The Quasar CTD 135 is Not a Compact Symmetric Object", Symmetry 14 (2): 321, doi:10.3390/sym14020321, Bibcode: 2022Symm...14..321F, http://arxiv.org/abs/2202.00950, retrieved 2025-11-16 
  9. ↑ Olguín-Iglesias, A.; León-Tavares, J.; Kotilainen, J. K.; Chavushyan, V.; Tornikoski, M.; Valtaoja, E.; Añorve, C.; Valdés, J. et al. (2016-08-11). "The host galaxies of active galactic nuclei with powerful relativistic jets" (in en). Monthly Notices of the Royal Astronomical Society 460 (3). doi:10.1093/mnra. ISSN 0035-8711. https://academic.oup.com/mnras/article/460/3/3202/2609461. 
  10. ↑ "ATel #3056: NIR flaring of the FRSQSO B2 2234+28A". https://www.astronomerstelegram.org/?read=3056. 
  11. ↑ "ATel #8572: A NIR Flare of the QSO B2 2234+28A". https://www.astronomerstelegram.org/?read=8572. 
  12. ↑ "ATel #16872: Historical NIR light maximum of the blazar B2 2234+28A". https://www.astronomerstelegram.org/?read=16872. 
  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" (in en). Research in Astronomy and Astrophysics 21 (8): 201. doi:10.1088/1674-4527/21/8/201. ISSN 1674-4527. Bibcode: 2021RAA....21..201G. 



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