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B2 1308+326

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B2 1308+326
The BL Lac object B2 1308+326.
Observation data (J2000.0 epoch)
ConstellationCanes Venatici
Right ascension13h 10m 28.6638s
Declination+32° 20′ 43.783″
Redshift0.997
Heliocentric radial velocity503,199 km/s
Apparent magnitude (V)15.24
Apparent magnitude (B)15.61
Characteristics
TypeOpt var; FSRQ, BL LAC
Other designations
IRAS F13080+3237, OHIO P 313, US 371, QSO B1308+326, CSO 836, INTREF 546, NVSS J131028+322044, V* AU CVn, H-ATLAS J131028.7+322043, 5C 12.659, 7C 1308+3236, 2E 2979, B2 1308+32

B2 1308+326 known as OP 313 or AU CVn, is a BL Lacertae object[1] located in the constellation of Canes Venatici. It has a redshift of (z) 0.997[2] and was initially discovered as a variable star in 1959 before being identified with its optical counterpart in 1972.[3] Its radio spectrum is flat, making it a FRSQ (flat-spectrum radio quasar).[4][5][6]

Description

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B2 1308+326 is found variable on the electromagnetic spectrum. It is classified a blazar[7] although some studies described it as a transitional or change-looking due to it experiencing a shift in synchrotron peak frequencies.[8][9] It is known to show an outburst in 1978 which it displayed extreme degrees of polarization, found rapidly variable in both position and degree angles on a time scale for 15 minutes.[10]

A gamma ray flare was detected in 2014.[11] In June 2022, B2 1308+326 showed an optical flare, subsequently reaching a historic maximum brightness with a slight decreased flux of 0.2-0.3 magnitude in R-band observed a month later.[12][13] Significant gamma ray activity was detected on 1 December 2023.[14]

Radio imaging of B2 1308+326 made by Very long baseline interferometry at 5 GHz showed it has an extended region and simple radio core structure measuring 1.3 x 0.6 in size with an orientation along the 30° position angle. When shown at 8.4 GHz, the source is then resolved into a bright core with a brightness temperature of 1012 Kelvin and a jet structure.[15] Subsequent observations found the core has a 3% polarization with a flat spectrum and contains perpendicular electric field vectors to the jet's direction which turns almost parallel upon 2 mas from the core.[16] Imaging by Very Large Array showed it has a dominant component and secondary component located 12 arcseconds north as well as a diffused halo surrounding the structure.[17]

A light curve of B2 1308+326 during 10 years between 1976 and 1986, its total range of variability was shown to be 3.0 magnitude with the detection of multiple flares. According to observations in early 1987, it was found to be a faint state indicating the light curve showed an overall decline.[18] The light curve at 4.8–90 GHz frequencies also showed B2 1308+326 had two complex outbursts, one between 1980-1988 and the second between 1988 and 2001 accompanied by three flares.[19]

References

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  1. ^ Sitko, M. L.; Stein, W. A.; Schmidt, G. D. (1984-07-01). "Wavelength-dependent polarization in the optical flux of the BL Lacertae object B2 1308+326". The Astrophysical Journal. 282: 29–32. Bibcode:1984ApJ...282...29S. doi:10.1086/162173. ISSN 0004-637X.
  2. ^ Watson, D.; Smith, N.; Hanlon, L.; McBreen, B.; Quilligan, F.; Tashiro, M.; Metcalfe, L.; Doyle, P.; Teraesranta, H. (2000-09-13), "ASCA and other contemporaneous observations of the blazar B2 1308+326", Astronomy and Astrophysics, 364: 43, arXiv:astro-ph/0009202, Bibcode:2000A&A...364...43W
  3. ^ "Au CVn (B2 1308+326, OP+313)". Frankfurt Quasar Monitoring. Retrieved 2025-01-05.
  4. ^ Bachev, R. (2022-06-01). "An update on B2 1308+326". The Astronomer's Telegram. 15447: 1. Bibcode:2022ATel15447....1B.
  5. ^ Buson, Sara (April 2014). "Fermi LAT Detection of a GeV Flare from OP 313 (B2 1308+32)". The Astronomer's Telegram. 6068: 1. Bibcode:2014ATel.6068....1S.
  6. ^ Vlasyuk, V. V.; Spiridonova, O. I.; Maslennikova, O. A. (2022-06-01). "The FSRQ B2 1308+326: reaching the new absolute maximum and still brightening". The Astronomer's Telegram. 15459: 1. Bibcode:2022ATel15459....1V.
  7. ^ Corcoran, Riley M.; Slater, John J.; Neal, Warner S.; Balonek, Thomas J. (2022-04-01). "Continued Optical Flaring in Blazar 1308+326". The Astronomer's Telegram. 15334: 1. Bibcode:2022ATel15334....1C.
  8. ^ Pandey, Ashwani; Kushwaha, Pankaj; Wiita, Paul J.; Prince, Raj; Czerny, Bożena; Stalin, C. S. (2024-01-01). "Origin of the broadband emission from the transition blazar B2 1308+326". Astronomy & Astrophysics. 681: A116. arXiv:2310.05096. Bibcode:2024A&A...681A.116P. doi:10.1051/0004-6361/202347719. ISSN 0004-6361.
  9. ^ Pandey, Ashwani; Hu, Chen; Wang, Jian-Min; Czerny, Bożena; Chen, Yong-Jie; Songsheng, Yu-Yang; Wang, Yi-Lin; Zhang, Hao; Aceituno, Jesús (December 2024). "B2 1308+326: A Changing-look Blazar or Not?". The Astrophysical Journal. 978 (2): 120. doi:10.3847/1538-4357/ad9b7c. ISSN 0004-637X.
  10. ^ Puschell, J. J.; Stein, W. A.; Jones, T. W.; Warner, J. W.; Owen, F.; Rudnick, L.; Aller, H.; Hodge, P. (1979-01-01). "B2 1308+326: photometry and polarization during the outburst of 1978 spring". The Astrophysical Journal. 227: L11 – L16. Bibcode:1979ApJ...227L..11P. doi:10.1086/182857. ISSN 0004-637X.
  11. ^ Li, Shan; Lee, Sang-Sung; Cheong, Whee Yeon (2024-04-11), "A Multi-wavelength Study on A Gamma-ray Bright AGN 1308+326 Using KVN at 22 and 43 GHz", Journal of Korean Astronomical Society, 57 (1): 67, arXiv:2404.06882, Bibcode:2024JKAS...57...67L, doi:10.5303/JKAS.2024.57.1.67, retrieved 2025-01-05
  12. ^ Hulburt, Madeline L.; Choi, Ha-Eun H.; Du, Norah; Balonek, Thomas J.; Corcoran, Riley M.; Slater, John J.; Neal, Warner S.; Malinowski, Chloe R.; Sampson, Matthew J.; Unnone, Victor K.; Heatherton, James F.; Tockstein, Jordan L. (2022-06-01). "Unprecedented Optical Flare Continues in Blazar 1308+326, Reaching Historic Maximum Brightness". The Astronomer's Telegram. 15474: 1. Bibcode:2022ATel15474....1H.
  13. ^ Minev, M.; Valcheva, A. (2022-07-01). "B2 1308+326 is dimming after the highest optical state". The Astronomer's Telegram. 15496: 1. Bibcode:2022ATel15496....1M.
  14. ^ Otero-Santos, J.; Piirola, V.; Pacciani, L.; Escudero, J.; Agudo, I.; Bonnoli, G.; Morcuende, D.; Casanova, V.; Aceituno, F. J.; Sota, A.; Marchini, A.; Stiaccini, L.; Leonini, S.; Conti, M.; Rosi, P. (2023-12-01). "Optical follow-up of the gamma-ray flare of the blazar OP 313 reveals a bright state with high polarization degree". The Astronomer's Telegram. 16360: 1. Bibcode:2023ATel16360....1O.
  15. ^ 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.
  16. ^ Zavala, R. T.; Taylor, G. B. (2003-05-20). "A View through Faraday's Fog: Parsec-Scale Rotation Measures in Active Galactic Nuclei". The Astrophysical Journal. 589 (1): 126–146. arXiv:astro-ph/0302367. Bibcode:2003ApJ...589..126Z. doi:10.1086/374619. ISSN 0004-637X.
  17. ^ Cassaro, P.; Stanghellini, C.; Bondi, M.; Dallacasa, D.; Ceca, R. Della; Zappalà, R. A. (1999-11-01). "Extended radio emission in BL Lac objects - I. The images" (PDF). Astronomy and Astrophysics Supplement Series. 139 (3): 601–616. arXiv:astro-ph/9910209. Bibcode:1999A&AS..139..601C. doi:10.1051/aas:1999511. ISSN 0365-0138.
  18. ^ Schramm, K.-J; Borgeest, U.; K¨uhl, D.; von Linde, J.; Linnert, M.D.; Schramm, T. (1994). "The Hamburg Quasar Monitoring Program (HQM) at Calar Alto: III. Lightcurves of optically violent variable sources". Astronomy & Astrophysics Supplement Series. arXiv:astro-ph/9403050. Bibcode:1994astro.ph..3050B.
  19. ^ Pyatunina, T. B.; Kudryavtseva, N. A.; Gabuzda, D. C.; Jorstad, S. G.; Aller, M. F.; Aller, H. D.; Teräsranta, H. (2007-09-26). "Frequency-dependent time delays for strong outbursts in selected blazars from the Metsähovi and UMRAO monitoring data bases – II". Monthly Notices of the Royal Astronomical Society. 381 (2): 797–808. Bibcode:2007MNRAS.381..797P. doi:10.1111/j.1365-2966.2007.12281.x. ISSN 0035-8711.
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