From X-ray Binaries to AGN: the Disk/Jet Connection Rich Plotkin University of Amsterdam ( Michigan) with Sera Markoff (Amsterdam), Scott Anderson (Washington), Niel Brandt (PSU), Brandon Kelly (UCSB), Elmar Körding (Nijmegen, NL), Ohad Shemmer (N. Texas), Jianfeng Wu (PSU CfA)
X-Ray Binaries Can Help Us Learn about Galaxy and SMBH (Co)-Evolution z=18.3; T=0.2 Gyr 31.25 Mpc/h z=0; T=13.6 Gyr 31.25 Mpc/h To better understand feedback, and to exploit AGN as probes of SMBHs, we need more constraints on how radiation Ṁ, MBH Understanding the connection between black hole accretion disks and outflows is crucial XRBs are scale models of AGN Springel et al. (2005) - Millenium Simulation
Outline: Advantages of Looking at All Types of Black Holes I. Two case studies: i. High-energy radiation near the disk/jet interface ii. Accretion mode, and how it affects AGN unification and feedback II. Future insights to be learned from XRBs
Luminosity Microquasar Outbursts Dunn et al. (2010) End Start Dunn et al. (2010) Thermal L jet or corona /L disk Non-Thermal Black Hole X-ray Binary ( ~ 10M Sun ) GX 339-4 During Outburst
Constraining how Radiation Ṁ, MBH The Fundamental Plane of Black Hole Activity (Merloni et al. 2003, Falcke et al. 2004) log Lx-ray + ξm log MBH (erg s -1 ) log L x (M) [erg s -1 ] 55 50 45 40 35 Data from Körding et al. (2006) Plotkin et al. (2012a) XRBs ~10 M sun Sgr A * ~10 6 M sun LLAGN ~10 7--8 M sun FR I s ~10 8--9 M sun BLLacs ~10 8--9 M sun L x-ray ~ (L radio ) ξr M ξm For low L/L Edd BHs: the conversion of the accretion flow into radiative output at the disk/jet interface is universal across the black hole mass scale 28 30 32 34 36 38 40 42 log L r [erg s -1 ] log Lradio (erg s -1 )
Constraining how Radiation Ṁ, MBH The Fundamental Plane of Black Hole Activity (Merloni et al. 2003, Falcke et al. 2004) log Lx-ray + ξm log MBH (erg s -1 ) log L x (M) [erg s -1 ] 55 50 45 40 35 Data from Körding et al. (2006) Plotkin et al. (2012a) XRBs ~10 M sun Sgr A * ~10 6 M sun LLAGN ~10 7--8 M sun FR I s ~10 8--9 M sun BLLacs ~10 8--9 M sun L x-ray ~ (L radio ) ξr M ξm What geometry produces the high-energy radiation? If Inverse Compton X-rays from Radiatively Inefficient Accretion: Lx-ray ~ (Lradio) 1.76 M -1.56 If Optically Thin Synchrotron X-rays: Lx-ray ~ (Lradio) 1.38 M -0.81 28 30 32 34 36 38 40 42 log L r [erg s -1 ] log Lradio (erg s -1 )
X-rays from an average low L/LEdd BH are Dominated by Optically Thin Jet Synchrotron ξm - Mass Coefficient -0.6-0.8-1.0-1.2-1.4-1.6 43 Galactic BHs, SgrA*, LLAGN 10 MSun - 10 7 MSun Optically Thin Synchrotron X-rays L X "ṁ 2 Inverse Compton X-rays 1.2 1.4 1.6 1.8 ξ R Contracted α R =0.00 L X "ṁ 2.3 ξr - Radio Coefficient Plotkin et al. (2012a) Lx-ray ~ (Lradio) ξr M ξm P12 Bayesian Regression Merit Function Merit Function is a modified χ 2 estimator (from Körding et al. 2006) Bayesian Linear Regression (mlinmix_err developed by Kelly 2007)
Geometry of a low-luminosity Hard Sate Black Hole Inefficient Inner Accretion Flow Most X-rays are optically <1-2% thin jet L Edd synchrotron No Wind/Torus Figure Adapted from Trump et al. 2011 e.g., above schematic helps inform us on how to use radiation from nearby low-luminosity AGN to probe the SMBH Mass Function at z=0
Outline: Advantages of Looking at All Types of Black Holes I. Two case studies: i. High-energy radiation near the disk/jet interface ii. Accretion mode, and how it affects AGN unification and feedback II. Future insights to be learned from XRBs
Explore Accretion Mode with BL Lacs (beamed low-luminosity radio galaxies) JET 80 SDSS Optical Spectrum Flux. Dens. (erg s 1 cm 2 Å 1 ) Flux Dens. 60 40 20 0 SDSS J110021.06+401928.0 (z spec =?, z hg > 0.275) 4000 5000 6000 7000 8000 9000 Wavelength (Å) [Obs. Frame] Wavelength (Å) Plotkin et al. (2010) Urry & Padovani (1995)
Explore Accretion Mode with BL Lacs (beamed low-luminosity radio galaxies) JET 20 SDSS Optical Spectrum Flux. Dens. (erg s 1 cm 2 Å 1 ) Flux Dens. 15 10 5 Mg Na Ca II H/K Weakly Beamed BL Lac SDSS J080018.79+164557.1 (z spec = 0.309) 500 Wavelength (Å) Plotkin et al. (2010) Urry & Padovani (1995)
Mid-Infrared Colors with WISE: Most BL Lacs are Missing Dusty Torus Emission Plotkin et al. 2012b WISE Infrared Color 1 [3.4µm]-[4.6µm] (mag) W1 W2 1.4 1.2 1.0 0.8 0.6 0.4 (a) Redder RL BL Lacs (0.1<z<0.3) Quasars (Point like) Quasars (Extended) Early Type Galaxies Weakly Beamed BL Lacs Contours: Simulated IR Colors Simulated Jet (b) Simulated Jet WISE Blazar Strip (Massaro et al. 2011) 0.2 Redder 0.0 1.4 1.2 Simulated Jet+Galaxy (c) Simulated Jet + Galaxy Simulated Jet+Galaxy+Torus (d) Simulated Jet + Galaxy + Torus 1.0 WISE Infrared Color 1 [3.4µm]-[4.6µm] (mag) W1 W2 0.8 0.6 0.4 0.2 0.0 0 1 2 3 4 W2 W3 WISE Infrared Color 2 [4.6µm]-[12µm] (mag) 0 1 2 3 4 W2 W3 WISE Infrared Color 2 [4.6µm]-[12µm] (mag)
Luminosity XRB accretion state (and jet properties) are likely connected to the inner accretion flow adapted from Dunn et al. 2010 adapted from Trump et al. 2011 Disk Wind Feeding Torus High-Luminosity ~10% L Edd Inefficient Inner Accretion Flow Low-Luminosity <1-2% L Edd No Wind/Torus Thermal L jet or corona /L disk End Start Non-Thermal GX 339-4 ( ~ 10 M Sun ) Nature of Inner Accretion Flow Likely Evolves
Lack of torus emission suggests an accretion mode divide for AGN, similar to XRBs (e.g., see Jackson & Wall 1999; Nicastro 2000; Ghisellini & Celotti 2001; Böttcher & Dermer 2002; Wold et al. 2007; Ghisellini et al. 2009, Hardcastle et al. 2009; Trump et al. 2011; Antonucci et al. 2011, Plotkin et al. 2012b) Wind Mode? Disk Wind Feeding Torus ~10% L Edd Radio Mode? Inefficient Inner Accretion Flow <1-2% L Edd No Wind/Torus Figure Adapted from Trump et al. 2011
Outline: Advantages of Looking at All Types of Black Holes I. Two case studies: i. High-energy radiation near the disk/jet interface ii. Accretion mode, and how it affects AGN unification and feedback II. Future insights to be learned from XRBs
Do distinct accretion states launch winds vs. jets, or can wind vs radio feedback co-exist? XRB winds not detected in hard (i.e jetted) state? Radio-loud QSOs generally show weaker disk winds Luminosity Radio Loud Radio Quiet weaker disk wind Ljet or corona/ldisk Ponti et al. (2012) Richards et al. (2011)
Conclusions 1. X-ray binaries help us see the bigger picture 2. There is a robust disk/jet coupling for Hard State Black Holes X-rays are predominantly optically thin synchrotron Constraints on geometry near the black hole help us go from radiation Ṁ, M BH 3. BL Lac objects have weak or missing tori New evidence for an AGN accretion mode divide Implications for wind vs radio feedback?