Published January 1, 2017
| Version v1
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Radio and optical intra-day variability observations of five blazars
Creators
- 1. Chinese Acad Sci, Grad Univ, Beijing 100049, Peoples R China
- 2. Guangxi Univ, Guangxi Key Lab Relativist Astrophys, Nanning 530004, Guangxi, Peoples R China
- 3. Shandong Univ, Inst Space Sci, Shandong Prov Key Lab Opt Astron & Solar Terr Env, Weihai 264209, Weihai, Peoples R China
- 4. Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany
- 5. Univ Athens, Sect Astrophys Astron & Mech, GR-15784 Athens, Greece
- 6. Osaka Kyoiku Univ, Astron Inst, 4-698 Asahigaoka, Kashiwara, Osaka 5828582, Japan
- 7. Univ Turku, Dept Phys & Astron, Tuorla Observ, F-21500 Turku, Finland
- 8. Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA
- 9. European Space Agcy, Herschel Sci Ctr, ESAC, C Bajo Castillo S-N, E-28692 Madrid, Spain
- 10. Tohoku Univ, Planetary Plasma & Atmospher Res Ctr, Sendai, Miyagi 9808578, Japan
- 11. Pedag Univ, Mt Suhora Observ, Ul Podchorazych 2, PL-30084 Krakow, Poland
- 12. Nordic Opt Telescope, Apartado 474, E-38700 Santa Cruz De La Palma, Spain
Description
We carried out a pilot campaign of radio and optical band intra-day variability (IDV) observations of five blazars (3C66A, S5 0716+714, OJ287, B0925+504 and BL Lacertae) on 2015 December 18-21 by using the radio telescope in Effelsberg (Germany) and several optical telescopes in Asia, Europe and America. After calibration, the light curves from both 5 GHz radio band and the optical R band were obtained, although the data were not smoothly sampled over the sampling period of about four days. We tentatively analyse the amplitudes and time-scales of the variabilities, and any possible periodicity. The blazars vary significantly in the radio (except 3C66A and BL Lacertae with only marginal variations) and optical bands on intra-and inter-day time-scales, and the source B0925+504 exhibits a strong quasi-periodic radio variability. No significant correlation between the radio-and optical-band variability appears in the five sources, which we attribute to the radio IDV being dominated by interstellar scintillation whereas the optical variability comes from the source itself. However, the radio and optical-band variations appear to be weakly correlated in some sources and should be investigated based on well-sampled data from future observations.
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