The “Blazar Sequence” in the TeV Band
The “blazar sequence” has been proposed for more than 20 yr, yet its nature is still unclear. In this work, for the first time we expand this topic to the TeV band by using a sample of 58 TeV blazars, including 48 blazars in the quiescent state and 21 blazars in the flaring state (11 blazars show in...
| Main Authors: | , , , , , , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
| Subjects: | |
| Online Access: | https://doi.org/10.3847/1538-4357/acc329 |
| _version_ | 1827827585231355904 |
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| author | Zhihao Ouyang Hubing Xiao Jianzhen Chen Junhui Fan Anton A. Strigachev Rumen S. Bachev Xiangtao Zeng Marina Manganaro Rui Xue Zelin Li |
| author_facet | Zhihao Ouyang Hubing Xiao Jianzhen Chen Junhui Fan Anton A. Strigachev Rumen S. Bachev Xiangtao Zeng Marina Manganaro Rui Xue Zelin Li |
| author_sort | Zhihao Ouyang |
| collection | DOAJ |
| description | The “blazar sequence” has been proposed for more than 20 yr, yet its nature is still unclear. In this work, for the first time we expand this topic to the TeV band by using a sample of 58 TeV blazars, including 48 blazars in the quiescent state and 21 blazars in the flaring state (11 blazars show in both quiescent and flaring state). We investigate the correlation between the TeV luminosity, which has been compensated for attenuation from extragalactic background light, and the synchrotron peak frequency. We note that there is no correlation between TeV luminosity and peak frequency in the quiescent state and a strong anticorrelation in the flaring state for the observed value. However, there is a strong positive correlation in both the quiescent state and the flaring state for the intrinsic value. This indicates that the blazar sequence is shown in the flaring state rather than in the quiescent state for the observed value and the blazar sequence is not present in both states after removing the beaming effect. In addition, to confirm whether the beaming effect results in the blazar sequence, we compare the Fermi γ -ray luminosity between the quiescent state and the flaring state. We find the Fermi γ -ray luminosity in the flaring state is greater than that in the quiescent state, and the Doppler factor in the flaring state is greater. We suggest the blazar sequence in the flaring state may be due to a stronger beaming effect. |
| first_indexed | 2024-03-12T03:34:54Z |
| format | Article |
| id | doaj.art-961199aabacb44f5990a5c7c6f4cfdd0 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-12T03:34:54Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-961199aabacb44f5990a5c7c6f4cfdd02023-09-03T13:20:16ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-0194925210.3847/1538-4357/acc329The “Blazar Sequence” in the TeV BandZhihao Ouyang0Hubing Xiao1https://orcid.org/0000-0001-8244-1229Jianzhen Chen2Junhui Fan3https://orcid.org/0000-0002-5929-0968Anton A. Strigachev4Rumen S. Bachev5https://orcid.org/0000-0002-0766-864XXiangtao Zeng6https://orcid.org/0000-0002-0551-5615Marina Manganaro7Rui Xue8https://orcid.org/0000-0003-1721-151XZelin Li9Shanghai Key Lab for Astrophysics, Shanghai Normal University , Shanghai, 200234, People's Republic of China ; hubing.xiao@shnu.edu.cn, jzchen@shnu.edu.cnShanghai Key Lab for Astrophysics, Shanghai Normal University , Shanghai, 200234, People's Republic of China ; hubing.xiao@shnu.edu.cn, jzchen@shnu.edu.cnShanghai Key Lab for Astrophysics, Shanghai Normal University , Shanghai, 200234, People's Republic of China ; hubing.xiao@shnu.edu.cn, jzchen@shnu.edu.cnCenter for Astrophysics, Guangzhou University , Guangzhou, 510006, People's Republic of China ; fjh@gzhu.edu.cn; Key Laboratory for Astronomical Observation and Technology of Guangzhou , Guangzhou, 510006, People's Republic of China; Astronomy Science and Technology Research Laboratory of Department of Education of Guangdong Province , Guangzhou, 510006, People's Republic of ChinaInstitute of Astronomy and National Astronomical Observatory , Bulgarian Academy of Sciences, 72 Tsarigradsko shosse Blvd., 1784 Sofia, BulgariaInstitute of Astronomy and National Astronomical Observatory , Bulgarian Academy of Sciences, 72 Tsarigradsko shosse Blvd., 1784 Sofia, BulgariaCenter for Astrophysics, Guangzhou University , Guangzhou, 510006, People's Republic of China ; fjh@gzhu.edu.cn; Key Laboratory for Astronomical Observation and Technology of Guangzhou , Guangzhou, 510006, People's Republic of China; Astronomy Science and Technology Research Laboratory of Department of Education of Guangdong Province , Guangzhou, 510006, People's Republic of ChinaDepartment of Physics, University of Rijeka , Rijeka, 51000, CroatiaDepartment of Physics, Zhejiang Normal University , Jinhua, 321004, People's Republic of ChinaCollege of Microelectronics, Feicuihu Campus of Hefei University of Technology , Hefei, 230601, People's Republic of ChinaThe “blazar sequence” has been proposed for more than 20 yr, yet its nature is still unclear. In this work, for the first time we expand this topic to the TeV band by using a sample of 58 TeV blazars, including 48 blazars in the quiescent state and 21 blazars in the flaring state (11 blazars show in both quiescent and flaring state). We investigate the correlation between the TeV luminosity, which has been compensated for attenuation from extragalactic background light, and the synchrotron peak frequency. We note that there is no correlation between TeV luminosity and peak frequency in the quiescent state and a strong anticorrelation in the flaring state for the observed value. However, there is a strong positive correlation in both the quiescent state and the flaring state for the intrinsic value. This indicates that the blazar sequence is shown in the flaring state rather than in the quiescent state for the observed value and the blazar sequence is not present in both states after removing the beaming effect. In addition, to confirm whether the beaming effect results in the blazar sequence, we compare the Fermi γ -ray luminosity between the quiescent state and the flaring state. We find the Fermi γ -ray luminosity in the flaring state is greater than that in the quiescent state, and the Doppler factor in the flaring state is greater. We suggest the blazar sequence in the flaring state may be due to a stronger beaming effect.https://doi.org/10.3847/1538-4357/acc329BL Lacertae objectsFlat-spectrum radio quasars |
| spellingShingle | Zhihao Ouyang Hubing Xiao Jianzhen Chen Junhui Fan Anton A. Strigachev Rumen S. Bachev Xiangtao Zeng Marina Manganaro Rui Xue Zelin Li The “Blazar Sequence” in the TeV Band The Astrophysical Journal BL Lacertae objects Flat-spectrum radio quasars |
| title | The “Blazar Sequence” in the TeV Band |
| title_full | The “Blazar Sequence” in the TeV Band |
| title_fullStr | The “Blazar Sequence” in the TeV Band |
| title_full_unstemmed | The “Blazar Sequence” in the TeV Band |
| title_short | The “Blazar Sequence” in the TeV Band |
| title_sort | blazar sequence in the tev band |
| topic | BL Lacertae objects Flat-spectrum radio quasars |
| url | https://doi.org/10.3847/1538-4357/acc329 |
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