The Broken Power Sequence in RL AGN 1/14 The Broken Power Sequence of Radio-Loud AGN + Collective Evidence for Inverse Compton emission from External Photons in High-Power Blazars E. Meyer 1 , M. Georganopoulos 2 , G. Fossati 1 , M. Lister 3 Fermy meets Jansky St. Michael's, MD 10 November 2011 1 Rice University, Houston, TX 2 UMBC, Baltimore, MD NRL – 5 Nov 3 Purdue University, Lafayette, IN Fermi/Jansky, Nov 2011 2010
The Broken Power Sequence in RL AGN 2/14 BLRG Blazars NLRG Relativistic Jet NL NL BL BL Super-massive black hole BL (SMBH), 10 6 – 10 10 M ☼ NL BL NL Accretion Disk + Molecular Torus Seyfert 2 Open Questions: - Jet structure relate to Morphology? Seyfert 1 - Site of the Gamma-ray emission? - Role of the Black Hole mass, spin, accretion rate? NL → What can we learn from studying populations? NRL – 5 Nov Fermi/Jansky, Nov 2011 2010
The Broken Power Sequence in RL AGN 3/14 The Blazar View of the Relativistic Jet NRL – 5 Nov Fermi/Jansky, Nov 2011 2010
The Broken Power Sequence in RL AGN 4/14 The Blazar Sequence Broken Core dominance L ext Lext → Jet Power Core Dominance → Angle Meyer et al., 2011 NRL – 5 Nov Fermi/Jansky, Nov 2011 2010
The Broken Power Sequence in RL AGN 5/14 The Blazar Sequence Broken Core dominance (R) L ext Lext → Jet Power Core Dominance → Angle Meyer et al., 2011 NRL – 5 Nov Fermi/Jansky, Nov 2011 2010
The Broken Power Sequence in RL AGN 6/14 The Broken Blazar Sequence > Weak Jets consistent with velocity gradients in the radiating plasma (spine-sheath – Ghisellini 2005, Chiaberge 2000 and/or decelerating flow – Georganopoulos 2003) > Strong Jets drop quickly in Luminosity (1:4) > many BL LACS in the strong jet branch (more on this) > ISPs more misaligned versions of HSP? – explains many recent findings “at odds” with the sequence: – Caccianiga & March˜a (2004): high R, low Lum., low peak > Confusion at low synchrotron peaks/overlap with RG > There is not a continuous sequence NRL – 5 Nov Fermi/Jansky, Nov 2011 2010
The Broken Power Sequence in RL AGN 7/14 L kin , θ, … m? ° (2FGL) ° (Mass estimates from reverberation m = L kin /L Edd mapping, velocity dispersions, L Edd = 1.3x10 38 M BH NRL – 5 Nov mass-luminosity scalings) Fermi/Jansky, Nov 2011 2010
The Broken Power Sequence in RL AGN 8/14 The Broken Power Sequence Inefficient Case: Efficient - no broad lines, SSC - assume const Γ with L kin - assume n( γ ) = k γ -2 L peak ~ kB 2 ~ L kin 2 ν peak ~ B γ b 2 δ ~ L kin -3/2 -4/3 ~ L kin 2 L peak ~ ν peak Efficient Case: - BBB,IR emission, EC Inefficient - assume scaling L kin ~ Γ 2 -4/3 ~ L kin 2 L peak ~ ν peak NRL – 5 Nov Fermi/Jansky, Nov 2011 2010
The Broken Power Sequence in RL AGN 9/14 The Broken Power Sequence NRL – 5 Nov Fermi/Jansky, Nov 2011 2010
The Broken Power Sequence in RL AGN 10/14 The Broken Power Sequence NRL – 5 Nov Fermi/Jansky, Nov 2011 2010
The Broken Power Sequence in RL AGN 11/14 About those BL Lacs... 1:4 Δ frequency :Δ Luminosity δ/δ 0 = ν peak / ν 0 NRL – 5 Nov Fermi/Jansky, Nov 2011 2010
The Broken Power Sequence in RL AGN 12/14 About those BL Lacs... (Georganopoulos & Marscher 1998) NRL – 5 Nov Fermi/Jansky, Nov 2011 2010
The Broken Power Sequence in RL AGN 13/14 What can we learn from Fermi ? Gamma-ray spectral index hardens as they drop in luminosity (just like synchrotron sequence) Radio galaxies De-beamed luminosities R II mix here!) NRL – 5 Nov Fermi/Jansky, Nov 2011 2010
The Broken Power Sequence in RL AGN 14/14 What can we learn from Fermi ? NRL – 5 Nov Fermi/Jansky, Nov 2011 2010
The Broken Power Sequence in RL AGN 15/14 SSC versus EC SSC – upscatter synchrotron photons -IC peak is a “copy” of synch -beaming pattern is the same: L ~ δ 3+α synchrotron peak or IC peak EC – upscatter photons from outside the jet (BLR, molecular torus, accretion disk?) -beaming pattern is different: L ~ δ 3+α synchrotron peak L ~ δ 5+α IC peak (For radio, L core /L ext ~ L ~ δ 3+α , α ~ 0.2 ) NRL – 5 Nov Fermi/Jansky, Nov 2011 2010
The Broken Power Sequence in RL AGN 16/14 EC in powerful jets? NRL – 5 Nov Fermi/Jansky, Nov 2011 2010
The Broken Power Sequence in RL AGN 17/14 EC in powerful jets? NRL – 5 Nov Fermi/Jansky, Nov 2011 2010
The Broken Power Sequence in RL AGN 18/14 EC versus SSC NRL – 5 Nov Fermi/Jansky, Nov 2011 2010
The Broken Power Sequence in RL AGN 19/14 Conclusions/Key Observations From the Blazar (synchrotron) Envelope: + No High-Luminosity, High-Peak sources + Suggestion of Two populations: “weak” / “strong” + Jet Power important, but not fundamental: spin, M BH , or accretion rate? + ISP sources are a key diagnostic population + spectral types are not clearly associated with a pop., this may be explained as jets overtaking lines + no high-synchrotron-peak radio galaxies New Orientation Scheme: + Observations consistent with a change in accretion mode at a critical rate of ~ 10 -2 Eddington mass rate, linked to a divide in jet SED characteristics. + The sequence remains in 'broken' form, power increasing along the theoretically predicted line NRL – 5 Nov Fermi/Jansky, Nov 2011 2010
The Broken Power Sequence in RL AGN 20/14 Conclusions/Key Observations From new Fermi analysis + Verify the presence of an 'envelope' in the IC peak frequency-peak luminosity plane + Gamma-ray output depends primarily on orientation and the power in the jet + We find evidence for External Compton emission mechanisms for the IC component in powerful blazars (log L kin > 45.5 ergs s -1 ), though from our analysis the slope of the L G /L S – CD relation is much higher than expected from a single velocity flow, indicating a more complext jet structure. NRL – 5 Nov Fermi/Jansky, Nov 2011 2010
The Broken Power Sequence in RL AGN 21/14 Next Steps - Complete the high-energy characterization of the IC spectra for the 3-year data set, with additional data from TeV, X-ray - Expand the sample to include NLSy1 - Look at VLBI data: jet speeds, morphologies - Expand the sample (small) - Apply to evolution studies, EGRB NRL – 5 Nov Fermi/Jansky, Nov 2011 2010
The Broken Power Sequence in RL AGN 22/14 The end (this slide intentionally left blank) NRL – 5 Nov Fermi/Jansky, Nov 2011 2010
The Broken Power Sequence in RL AGN 23/14 NRL – 5 Nov Fermi/Jansky, Nov 2011 2010
The Broken Power Sequence in RL AGN 24/14 Measuring the Power of Relativistic Jets NRL – 5 Nov Fermi/Jansky, Nov 2011 2010
The Broken Power Sequence in RL AGN 25/14 How does Beaming affect the SED? ∂ = Γ -1 (1 – βcosΘ) -1 Γ = 5 – 50 L ~ L 0 ∂ p p = 2+α, 3+α NRL – 5 Nov Fermi/Jansky, Nov 2011 2010
The Broken Power Sequence in RL AGN 26/14 Simple/Complex are co-spatial as radio galaxies As a theoretical source is aligned: + fast component of complex jets is revealed → dramatically higher peak frequencies + simple jets follow 1:4 rule NRL – 5 Nov Fermi/Jansky, Nov 2011 2010
The Broken Power Sequence in RL AGN 27/14 Are two populations expected? The updated theoretical sequence (Ghisellini 2008) predicts blue quasars, low power FSRQ, but is still a continuous sequence → ← Alternative: Spin Paradigm Rapidly retrograde-spinning black holes able to extract more energy, forming powerful FR II, spin down to moderately powerful FR I (Garofalo 2010) Verified Simple/Complex population divide would NRL – 5 Nov support the spin-based unification scheme Fermi/Jansky, Nov 2011 2010
The Broken Power Sequence in RL AGN 28/14 Methods: 1. Fit the average synchrotron spectrum All sources from every flux-limited blazar sample =~4000 candidates NED + SIMBAD, literature search =~ 1700 Fitted with phenomenological SED,hand CANNOT use selection = 737 sources with accurate simple ratios for v peak , L peak determining peak GOOD BAD NRL – 5 Nov Fermi/Jansky, Nov 2011 2010
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