The Spectral Energy Distributions and Beaming Effect for Fermi Blazars Junhui Fan Guangzhou University Collaborators: J H Yang, Y Liu, C Lin, Y.H. Yuan, H B Xiao Black Holes and Friends 2 11-13 April 2016, Fudan Univ. China
Outline 1. Introduction 2. Spectral Energy Distributions 3. Beaming Effect in Fermi Blazars 4. Summary 2016-4-13 Black Holes and Friends 2, 11-13 2 April 2016, Fudan Univ. China
Outline 1. Introduction 2. Spectral Energy Distributions 3. Beaming Effect in Fermi Blazars 4. Summary 2016-4-13 Black Holes and Friends 2, 11-13 3 April 2016, Fudan Univ. China
INTRODUCTION Observations show that some sources with AGNs particular observational properties RBLs LBLs 1) BL Lacertae objects--BLs, XBLs HBLs 2) Flat Spectrum Radio Quasars—FSRQs 2016-4-13 Black Holes and Friends 2, 11-13 4 April 2016, Fudan Univ. China
What is a BL Lac Object? BL Lacertae objects. 1) Absence of emission lines in the core sources; weak emission lines were found in BLs (Miller et al. 1978) 2) Rapid and large amplitude variability 3) Nonthermal continuum 4) High and rapidly variable polarization 2016-4-13 Black Holes and Friends 2, 11-13 5 April 2016, Fudan Univ. China
What is an FSRQ? Optically violently variable quasars--OVVs, ( m>1.0m) ( Penston & Cannon,1970) Kinman (1975) OVVs tend to have steep optical spectra and be associated with compact variable radio sources which have flat radio spectra at GHz frequencies. Highly polarized quasars--HPQs ( p>3.0%), (Moore and Stockman 1981, ApJ, 243 ) , 45% Core-dominated quasars--CDQs ( R = Lc/Le > 1.0) Superluminal Sources--SM β = v/c > 1.0 (Zhang & Fan, 2008, 123 sources) 2016-4-13 Black Holes and Friends 2, 11-13 6 April 2016, Fudan Univ. China
INTRODUCTION BLAZARS Objects with one of the above properties BLAZARS (BL Lacs and FSRQs) extragalactic objects with rapid variability, high luminosity, high and variable polarization, or superluminal motions. The term “blazar” was coined, half in jest, by Ed Speigel at the first conference on BL lac objects in Pittsburg, 1978. Fan et al. 2013, RAA, Strong gamma-ray emissions 2016-4-13 Black Holes and Friends 2, 11-13 7 Fan et al. 2013, IAUS 290 April 2016, Fudan Univ. China
INTRODUCTION INTRODUCTION BLAZARS BLAZARS (BL Lacs and FSRQs) Special subclass of AGNs: extragalactic objects with rapid variability, high luminosity, high and variable polarization, have/no strong emission lines, gamma-ray emissions, or superluminal motions. 2016-4-13 Black Holes and Friends 2, 11-13 8 April 2016, Fudan Univ. China
窄线区 F ob = p F in AGN Model = ( , ) 宽线区 喷流 黑洞 吸积盘 Standard Model for AGNs 活动星系核的标准模型 2016-4-13 Black Holes and Friends 2, 11-13 9 April 2016, Fudan Univ. China
SEDs of Blazars 2016-4-13 Black Holes and Friends 2, 11-13 10 April 2016, Fudan Univ. China
2016-4-13 Black Holes and Friends 2, 11-13 11 April 2016, Fudan Univ. China
Classification of BL Lac Objects From surveys Radio selected BL Lacertae objects-RBLs, X-ray Selected BL Lacertae objects-XBLs From Spectral Energy Distributions RBLs, energy cutoff frequency at opt/IR XBLs, frequency at UV/X-ray 121 BL Sample (Giommi, Ansari, Micol, Feb, 1995) 2016-4-13 Black Holes and Friends 2, 11-13 12 April 2016, Fudan Univ. China
Classification of BL Lac Objects Padovani & Giommi 1995, ApJ, 444 2016-4-13 Black Holes and Friends 2, 11-13 13 April 2016, Fudan Univ. China
Classification of BL Lac Objects Padovani & Giommi 1996 2016-4-13 Black Holes and Friends 2, 11-13 14 April 2016, Fudan Univ. China
Classification of BL Lac Objects LBLs: RBLs XBLs HBLs Low-frequency peaked LBLs HBLs: High-frequency peaked Padovani & XBL HBL, RBL LBL 2016-4-13 Black Holes and Friends 2, 11-13 15 Giommi 1996 April 2016, Fudan Univ. China
SED of Blazars Fossati et al. 1998 Compiled 3 subclasses of 126 blazars (RBLs, XBLs, FSRQs) 2016-4-13 Black Holes and Friends 2, 11-13 16 April 2016, Fudan Univ. China
Sequence of Blazars 2016-4-13 Black Holes and Friends 2, 11-13 17 April 2016, Fudan Univ. China
Giommi et al. 2005, A&A, 434, 385 Detected luminous high frequency BL Lacs low frequency low luminosity BL Lacs Contradict with the “blazar sequence” since there are no lower luminous low frequency or high frequency luminous BL Lacs in Fossati et al. (1998). 2016-4-13 Black Holes and Friends 2, 11-13 18 April 2016, Fudan Univ. China
Nieppola et al. 2006, A&A, 445, 441 2016-4-13 Black Holes and Friends 2, 11-13 19 April 2016, Fudan Univ. China
Fermi/LAT 2016-4-13 Black Holes and Friends 2, 11-13 20 April 2016, Fudan Univ. China
Abdo, et al. 2010, ApJ, 715, 429 set frequency boundary for subclasses of ~ 48 blazars (based on P & G criteria, according to their position in the effective spectral index plot). LSPs: ISPs: HSPs: Lower, Intermediate, High Synchrotron Peak 2016-4-13 Black Holes and Friends 2, 11-13 21 April 2016, Fudan Univ. China
Boundaries for Classifications LBL IBL HBL Ref Log ν(Hz) Log ν(Hz) Log ν(Hz) Padovani & Giommi, < 15 > 15 1996 Nieppola et al. 2006 < 14.5 14.5 ~ 16.5 > 16.5 Abdo et al. 2010 <14 14 ~ 15 > 15 Non 2016-4-13 Black Holes and Friends 2, 11-13 22 Consensus April 2016, Fudan Univ. China
Outline 1. Introduction 2. Spectral Energy Distributions 3. Beaming Effect in Fermi Blazars 4. Summary 2016-4-13 Black Holes and Friends 2, 11-13 23 April 2016, Fudan Univ. China
2.1 SEDs for 1425 Fermi Blazars from 3FGL 2016-4-13 Black Holes and Friends 2, 11-13 24 April 2016, Fudan Univ. China
Fan et al 2016, in preparation Multi-wavelength data are compiled for 1425 Fermi blazars to calculate the SEDs 2016-4-13 Black Holes and Friends 2, 11-13 25 April 2016, Fudan Univ. China
2.1 Fitting Results for some sources 2016-4-13 Black Holes and Friends 2, 11-13 26 April 2016, Fudan Univ. China
2.2 Distribution of Peak Frequencies 1392 2016-4-13 Black Holes and Friends 2, 11-13 27 April 2016, Fudan Univ. China
2016-4-13 Black Holes and Friends 2, 11-13 28 April 2016, Fudan Univ. China
2.2 Distribution of Peak Frequencies 999 at observer frame 2016-4-13 Black Holes and Friends 2, 11-13 29 April 2016, Fudan Univ. China
2.2 Distribution of Peak Frequencies 999 at source frame 2016-4-13 Black Holes and Friends 2, 11-13 30 April 2016, Fudan Univ. China
Bayesian information criterion for model selection, we used 4 components to fit the distribution, but 3 components are enough. 2016-4-13 Black Holes and Friends 2, 11-13 31 April 2016, Fudan Univ. China
2.3 Classifications of Fermi Blazars 14.0 14.0 2016-4-13 Black Holes and Friends 2, 11-13 32 April 2016, Fudan Univ. China
Boundaries for Classifications LBL IBL HBL Ref Log ν(Hz) Log ν(Hz) Log ν(Hz) < 15 > 15 Padovani & Giommi, 1996 < 14.5 14.5 ~ 16.5 > 16.5 Nieppola et al. 2006 <14 14 ~ 15 > 15 Abdo et al. 2010 <14.0 14.0 ~ 15.3 >15.3 This work 2016-4-13 Black Holes and Friends 2, 11-13 33 April 2016, Fudan Univ. China
Luminosity-luminosity Correlations 2016-4-13 Black Holes and Friends 2, 11-13 34 April 2016, Fudan Univ. China
Luminosity-luminosity Correlations 2016-4-13 Black Holes and Friends 2, 11-13 35 April 2016, Fudan Univ. China
Correlation after removing the effect of redshift Gamma-Radio correlation still exist 2016-4-13 Black Holes and Friends 2, 11-13 36 April 2016, Fudan Univ. China
2016-4-13 Black Holes and Friends 2, 11-13 37 April 2016, Fudan Univ. China
2016-4-13 Black Holes and Friends 2, 11-13 38 April 2016, Fudan Univ. China
Tramacere-2007 Tramacere-2011 2016-4-13 Black Holes and Friends 2, 11-13 39 April 2016, Fudan Univ. China
2016-4-13 Black Holes and Friends 2, 11-13 40 April 2016, Fudan Univ. China
Outline 1. Introduction 2. Spectral Energy Distributions 3. Beaming Effect in Fermi Blazars 4. Summary 2016-4-13 Black Holes and Friends 2, 11-13 41 April 2016, Fudan Univ. China
3. Beaming Effect in Fermi Blazars 3.1 Variability Index 3.2 Doppler factor and viewing angle 3.3 Radio polarization 3.4 Radio and Gamma-Ray Correlation 3.5 Other Correlations and Doppler factor determination 3.6 etc …… 2016-4-13 Black Holes and Friends 2, 11-13 42 April 2016, Fudan Univ. China
3.5. Other Correlations and Doppler Factors i. Gamma-Ray luminosity vs. Radio Doppler Factor ii. Gamma-Ray luminosity VS. Superluminal Velocity iii.Gamma-Ray Luminosity vs. Core-dominance parameter iv.Gamma-Ray Luminosity vs. peak frequency v. Gamma-Ray Doppler Factors 2016-4-13 Black Holes and Friends 2, 11-13 43 April 2016, Fudan Univ. China
3.1 Variability Index vs Peak Frequency Ackermann et al. 2015 Bastieri, 2016 2016-4-13 Black Holes and Friends 2, 11-13 44 April 2016, Fudan Univ. China
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