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On estimators of the jet bolometric luminosity of Fermi 2LAC blazars

  • Zerui Wang
  • Rui Xue
  • Leiming DuEmail author
  • Zhaohua Xie
  • Dingrong Xiong
  • Tingfeng Yi
  • Yunbing Xu
  • Wenguang Liu
Original Article

Abstract

Bolometric luminosity is a basic physical parameter that is widely used in the study of blazars. Due to the lack of simultaneous full wavelength data, several estimators of the bolometric luminosity are being used in practice. In this paper, we study and evaluate the reliability and significance of six estimators, the \(5\mbox{GHz}\) luminosity, the 1keV luminosity, the \(\gamma\)-ray luminosity, the \(5\mbox{GHz}\) luminosity + the 1keV luminosity, the \(5\mbox{GHz}\) luminosity + the \(\gamma\)-ray luminosity and the 1keV luminosity + the \(\gamma\)-ray luminosity, by analyzing the linear correlations between the integrated bolometric luminosity and them. Our main results are as follows. (i) All the six estimators are reliable in the sense that they are all significant correlated with the bolometric luminosity. (ii) Ranking from the higher significance of the reliability to lower one the six estimators are the \(5\mbox{GHz}\) luminosity + the \(\gamma\)-ray luminosity, the 1keV luminosity + the \(\gamma\)-ray luminosity, \(\gamma\)-ray luminosity, the \(5\mbox{GHz}\) luminosity + the 1keV luminosity, the \(5\mbox{GHz}\) luminosity and the 1keV luminosity. (iii) We suggest that the bolometric luminosity can be well estimated by the \(\gamma\)-ray luminosity using the best linear equation that given in this paper for Fermi FSRQs. (iv) According to the linear regressions obtained in the analysis, we provide calibration for each estimator.

Keywords

Methods: statistical Radiation mechanisms: non-thermal Galaxies: active BL Lacertae objects: general 

Notes

Acknowledgements

Part of this work is based on archival data, software or online services provided by the ASI SCIENCE DATA CENTER (ASDC). We are very grateful to Professor Giommi and the supporting team in ASDC for their help. This work is supported by the Joint Research Fund in Astronomy (Grant Nos. U1431123, 10978019, 11263006, 11463001) under cooperative agreement between the National Natural Science Foundation of China (NSFC) and Chinese Academy of Sciences (CAS), the Provincial Natural Science Foundation of Yunnan (Grant No.: 2013FZ042) and the Yunnan province education department project (Grant No. 2014Y138, 2016ZZX066).

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Copyright information

© Springer Science+Business Media B.V. 2017

Authors and Affiliations

  • Zerui Wang
    • 1
  • Rui Xue
    • 2
  • Leiming Du
    • 1
    Email author
  • Zhaohua Xie
    • 1
  • Dingrong Xiong
    • 3
  • Tingfeng Yi
    • 1
  • Yunbing Xu
    • 1
  • Wenguang Liu
    • 1
  1. 1.Department of PhysicsYunnan Normal UniversityKunmingChina
  2. 2.School of Astronomy and Space ScienceNanjing UniversityNanjingChina
  3. 3.Yunnan ObservatoriesChinese Academy of SciencesKunmingChina

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