Figure 1 Schematic drawing of the magnetic field geometry and gas flow in the x-wind model for the production of CAIs and chondrules. F H Shu et al. Science 1997;277: Published by AAAS

Figure 1 from A Rotating Molecular Jet from a Perseus Protostar Gerardo Pech et al ApJ doi: / X/751/1/78

Figure 2 from A Rotating Molecular Jet from a Perseus Protostar Gerardo Pech et al ApJ doi: / X/751/1/78

Figure 2 from The Topological Changes of Solar Coronal Magnetic Fields. III. Reconnected Field Topology Produced by Current- sheet Dissipation Å. M. Janse and B. C. Low 2010 ApJ doi: / X/722/2/1844

Individual field line (P= 0.3F) at t= 30, 50, 90 for simple model and p ∝ (z+ 0.1)−3. Sherwin B D, and Lynden-Bell D MNRAS 2007;378: © 2007 The Authors. Journal compilation © 2007 RAS

Figure 1 Time evolution of a simple system of a large-scale magnetic field, thin plasma, and a Kerr black hole at (A) t = 0, (B)t = 1 τS, (C)t = 4 τS, and (D)t = 7 τS. S Koide et al. Science 2002;295: Published by AAAS

Figure 2 Three-dimensional graphics of magnetic field lines around a Kerr black hole at t = 7 τS. S Koide et al. Science 2002;295: Published by AAAS

Figure 12 from Transport of Large-Scale Poloidal Flux in Black Hole Accretion Kris Beckwith et al ApJ doi: / X/707/1/428

Fig. 1 3D snapshot for an evolved model with j = 0.99, initial relative tilt θtilt,0 ≈ 90°, and disk thickness H/R ~ 0.3. J C McKinney et al. Science 2013;339:49-52 Published by AAAS

Asada and Makamura, 2012

Galactic Outflows and Winds Similarity solution Bardeen and Berger Chevalier and Clegg Hi Res simulations Breezes not winds

Edge ‐ on gas morphologies (as Fig. 1), with different feedback mechanisms enabled. Hopkins P F et al. MNRAS 2012;421: © 2012 The Author Monthly Notices of the Royal Astronomical Society © 2012 RAS

Accretion onto Black Holes is mostly (80-90%) hidden, ~50% C-thick? From XRB modeling: space density of C-thick AGN is thought to be comparable to that of less obscured AGN (with large uncertainties) thick thin unobscured total

ACS image Zirm et al. 2005, ApJ, 630, 28, 2005 Color composite image of the r625, i775, and z850 images from ACS, with the VLA 5 GHz radio map overlaid. Note the blue wedge emanating from the southwestern side of the radio galaxy: this appears only in the r625 band and is likely due entirely to Ly emission. The rest of the emission is clearly alignedwith the axis defined by the two radio lobes. The continuum in the i775 and z850 bands is dominated by the two clumps along the same axis.

optical spectrum from de breuck et al. 2001, AJ, 121, 1241

x-ray data Chandra keV, keV, 2-7 keV and HST/ACS z-band cutouts of a 20x13 arcsec region around the z=4.1 radiogalaxy TN J (circle radius is 4”). The Chandra exposure is 80ks. This is sufficient to detect i) the nuclear emission from the radiogalaxy with 15 counts, i.e. at more than 4; ii) estimate a nuclear hardness ratio of HR= which, for a source at z = 4.1, points towards heavy absorption (NH ~4e23 cm−2 for Gamma fixed to 1.8); iii) reveal an elongated diffuse emission in the soft band (10 counts) likely associated to the jet/interaction with the ambient medium

Radio galaxy SEDs and model fits. Lower abscissas are marked with observed wavelengths. Upper abscissas are marked with rest-frame wavelengths. Filled circles with error bars denote data points used in the fit; open circles denote data points that could be contaminated by emission lines and are therefore not used in the fits. Model components are a stellar population (green dashed lines) and two or three pure blackbodies (red dotted lines) representing dust emission. The sum of the model components is shown by solid black line. A downward arrow at λrest = 1.6 or 5 μm indicates an upper limit on the stellar or hot dust emission, respectively. the source seems well detected in the MIPS 24um image de breuck says 500MHz radio correlates with 5um rest, so agn-heated hot dust from de breuck et al ApJ SED decomposition

Questions What spins up Black Holes at High z? Difference in spinning and non-spinning black holes population From Type 2/HzRGs get populations, ages, metallicities, morphologies, SFR distributions? Large molecular masses inferred Clustering properties- likely highly biased