Hostname: page-component-78c5997874-v9fdk Total loading time: 0 Render date: 2024-11-16T21:13:47.347Z Has data issue: false hasContentIssue false
  • English
  • Français

The Correlation between the Gamma-Ray Luminosity and the Core-Dominance Parameters for a Fermi Blazar Sample

Published online by Cambridge University Press:  25 July 2014

J. H. Fan ,
J. H. Yang ,
D. X. Wu ,
S. H. Li ,
Y. Liu  and
Z. Y. Ji
J. H. Fan
Affiliation:
CfA, Guangzhou University, Guangzhou 510006, China email: fjh@gzhu.edu.cn Astron. Sci. & Tech. Res. Lab. of Dept of Edu. of Guangdong Province, China
J. H. Yang
Affiliation:
CfA, Guangzhou University, Guangzhou 510006, China email: fjh@gzhu.edu.cn Dept. of Phys. & Electron. Sci., Hunan Uni. of Arts and Sci., Changde 415000, China
D. X. Wu
Affiliation:
CfA, Guangzhou University, Guangzhou 510006, China email: fjh@gzhu.edu.cn Astron. Sci. & Tech. Res. Lab. of Dept of Edu. of Guangdong Province, China
S. H. Li
Affiliation:
CfA, Guangzhou University, Guangzhou 510006, China email: fjh@gzhu.edu.cn Astron. Sci. & Tech. Res. Lab. of Dept of Edu. of Guangdong Province, China
Y. Liu
Affiliation:
CfA, Guangzhou University, Guangzhou 510006, China email: fjh@gzhu.edu.cn Astron. Sci. & Tech. Res. Lab. of Dept of Edu. of Guangdong Province, China
Z. Y. Ji
Affiliation:
School of Astronomy and Space science, Nanjing University, Nanjing, China
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

In this work, we investigated the correlation between the γ-ray luminosity, logLγ and the core-dominance parameter, log (1+R), for a sample of 124 Fermi blazars with available core and extended radio emissions. Our analysis shows that there is no correlation between the γ-ray luminosity, log Lγ and the core-dominance parameter, log (1+R). However, there is a closely linear correlation between log Lγ − log LExt and log (1+R), log Lγ−log LExt = (0.95 ± 0.08) log (1+R) + (2.72 ± 0.11), for the whole sample. The result suggests that the γ-ray emissions are composed of two components, one is beamed, the other is unbeamed.

Keywords

galaxies:active-galaxies:BL Lacertae objects-galaxies:quasars-galaxies:jets
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S304: Multiwavelength AGN Surveys and Studies , October 2013 , pp. 157 - 158
Copyright
Copyright © International Astronomical Union 2014 

References

Abdo, A. A., Ackermann, M., Ajello, M., et al., 2009, ApJ, 700, 597Google Scholar
Abdo, A. A., Ackermann, M., Ajello, M., et al., 2010, ApJS, 188, 405Google Scholar
Ackermann, M., Ajello, M., Allafort, A., et al., 2011, ApJ, 743, 171CrossRefGoogle Scholar
Arshakian, T. G., Torrealba, J., Chavushyan, V. H., et al., 2010, A&A, 520, A62Google Scholar
Bastieri, D., 2012, “Variability of Blazars: From Jansky to Fermi”, Dec. 13-16, 2012, GuangzhouGoogle Scholar
Fan, J. H., Yang, J. H., Pan, J., & Hua, T. X., 2011, RAA, 11, 1413Google Scholar
Fan, J. H., Yang, J. H., Zhang, J. Y., et al., 2013a, PASJ, 65, 25Google Scholar
Fan, J. H., Yang, J. H., Liu, Y., & Zhang, J. Y., 2013b, RAA, 13, 259Google Scholar
Ghisellini, G., Tavecchio, F., Foschini, L., et al., 2010, MNRAS, 402, 497Google Scholar
Giovannini, G., 2013, IAUS 304, Multiwavelength AGN Surveys and Studies, this proceedingsGoogle Scholar
Giroletti, M., Reimer, A., Fuhrmann, L., & Pavlidou, V. 2010, ASPC, 427, 283Google Scholar
Giroletti, M., Pavlidou, V., Reimer, A., et al. 2012, AdSpR, 49, 1320Google Scholar
Gupta, A. C., 2011, JApA, 32, 155Google Scholar
Ivezić, Z. & MacLeod, C., 2013, IAUS 304, Multiwavelength AGN Surveys and Studies, this proceedingsGoogle Scholar
Kovalev, Y. Y., 2009, ApJ, 707, 56CrossRefGoogle Scholar
Marscher, A., et al., 2011, JApA, 32, 233Google Scholar
Massaro, E., Giommi, P., Leto, C., et al., 2011, Multifrequency Catalogue of Blazars (3rd Edition), Edited by Massaro, E., Giommi, P., Leto, C., Marchegiani, P., Maselli, A., Perri, M. and Piranomonte, S.. ARACNE Editrice, Rome, ItalyGoogle Scholar
Massaro, F., Giroletti, M., & Paggi, A., et al. 2013a, ApJS, 207, 4Google Scholar
Massaro, F., DAbrusco, R., Giroletti, M., et al. 2013b, ApJS, 208, 15Google Scholar
Massaro, F. & Ajello, M. 2011, ApJ, 729, 12CrossRefGoogle Scholar
Nolan, P. L., Abdo, A. A., Ackermann, M., et al., 2012, ApJS, 199, 31Google Scholar
Pushkarev, A. B., Kovalev, Y. Y., & Lister, M. L., 2010, ApJ, 722L, 7Google Scholar
Sarajedini, V., 2013, IAUS 304, Multiwavelength AGN Surveys and Studies, this proceedingsGoogle Scholar
Savolainen, T., Homan, D. C., Hovatta, T., et al., 2010, A&A, 512A, 24Google Scholar
Sol, H., 2013, IAUS 304, Multiwavelength AGN Surveys and Studies, this proceedingsGoogle Scholar
Urry, C. M. & Shafer, R. A., 1984, ApJ, 280, 569Google Scholar
Urry, M., 2011, JApA, 32, 139Google Scholar
Wills, B. J., Wills, D., Breger, M., et al., 1992 ApJ, 398, 454Google Scholar