Astronomy: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 ascension 13h 10m 28.6638s
Declination+32° 20′ 43.783″
Redshift0.997
Helio 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

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 of observations between 1976 and 1986 was obtained. Data from the light curve showed the total variability range of B2 1308+326 was 3.0 magnitude with the detection of multiple flares. According to observations in early 1987, it was found to be a faint state.[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

  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. doi:10.1086/162173. ISSN 0004-637X. Bibcode: 1984ApJ...282...29S. https://ui.adsabs.harvard.edu/abs/1984ApJ...282...29S/abstract. 
  2. ↑ Watson, D.; Smith, N.; Hanlon, L.; McBreen, B.; Quilligan, F.; Tashiro, M.; Metcalfe, L.; Doyle, P. et al. (2000-09-13), "ASCA and other contemporaneous observations of the blazar B2 1308+326", Astronomy and Astrophysics 364: 43, Bibcode: 2000A&A...364...43W 
  3. ↑ "Au CVn (B2 1308+326, OP+313)". http://quasar.square7.ch/fqm/1308+326.html. 
  4. ↑ Bachev, R. (2022-06-01). "An update on B2 1308+326". The Astronomer's Telegram 15447: 1. Bibcode: 2022ATel15447....1B. https://ui.adsabs.harvard.edu/abs/2022ATel15447....1B/abstract#:~:text=The%20blazar%20(flat%20spectrum%20radio%20quasar,%20FSRQ),state%20in%20optical,%20NIR%20and%20gamma-rays%20during. 
  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. https://ui.adsabs.harvard.edu/abs/2014ATel.6068....1S/abstract. 
  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. https://ui.adsabs.harvard.edu/abs/2022ATel15459....1V/abstract. 
  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. https://ui.adsabs.harvard.edu/abs/2022ATel15334....1C/abstract. 
  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" (in en). Astronomy & Astrophysics 681: A116. doi:10.1051/0004-6361/202347719. ISSN 0004-6361. Bibcode: 2024A&A...681A.116P. https://www.aanda.org/articles/aa/abs/2024/01/aa47719-23/aa47719-23.html. 
  9. ↑ Pandey, Ashwani; Hu, Chen; Wang, Jian-Min; Czerny, Bożena; Chen, Yong-Jie; Songsheng, Yu-Yang; Wang, Yi-Lin; Zhang, Hao et al. (December 2024). "B2 1308+326: A Changing-look Blazar or Not?" (in en). 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. doi:10.1086/182857. ISSN 0004-637X. Bibcode: 1979ApJ...227L..11P. https://articles.adsabs.harvard.edu/pdf/1979ApJ...227L..11P. 
  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 the Korean Astronomical Society 57 (1): 67, doi:10.5303/JKAS.2024.57.1.67, Bibcode: 2024JKAS...57...67L 
  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. et al. (2022-06-01). "Unprecedented Optical Flare Continues in Blazar 1308+326, Reaching Historic Maximum Brightness". The Astronomer's Telegram 15474: 1. Bibcode: 2022ATel15474....1H. https://ui.adsabs.harvard.edu/abs/2022ATel15474....1H/abstract. 
  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. https://ui.adsabs.harvard.edu/abs/2022ATel15496....1M/abstract. 
  14. ↑ Otero-Santos, J.; Piirola, V.; Pacciani, L.; Escudero, J.; Agudo, I.; Bonnoli, G.; Morcuende, D.; Casanova, V. et al. (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. https://ui.adsabs.harvard.edu/abs/2023ATel16360....1O/abstract. 
  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. https://articles.adsabs.harvard.edu//full/1997AstL...23...64A/0000066.000.html. 
  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. doi:10.1086/374619. ISSN 0004-637X. Bibcode: 2003ApJ...589..126Z. https://iopscience.iop.org/article/10.1086/374619/fulltext/. 
  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" (in en). Astronomy and Astrophysics Supplement Series 139 (3): 601–616. doi:10.1051/aas:1999511. ISSN 0365-0138. Bibcode: 1999A&AS..139..601C. https://aas.aanda.org/articles/aas/pdf/1999/18/ds1030.pdf. 
  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. 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. doi:10.1111/j.1365-2966.2007.12281.x. ISSN 0035-8711. Bibcode: 2007MNRAS.381..797P. 



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