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;277:1475-1479
Published by AAAS
Figure 1 from A Rotating Molecular Jet from a Perseus Protostar
Gerardo Pech et al. 2012 ApJ 751 78 doi:10.1088/0004-637X/751/1/78
Figure 2 from A Rotating Molecular Jet from a Perseus Protostar
Gerardo Pech et al. 2012 ApJ 751 78 doi:10.1088/0004-637X/751/1/78
Figure 2 from The Topological Changes of Solar Coronal Magnetic Fields. III. Reconnected Field Topology Produced by Currentsheet Dissipation
Å. M. Janse and B. C. Low 2010 ApJ 722 1844 doi:10.1088/0004-637X/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;378:409-415
© 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;295:1688-1691
Published by AAAS
Figure 2 Three-dimensional graphics of magnetic field lines around a Kerr black hole at t = 7
S Koide et al. Science 2002;295:1688-1691
Published by AAAS
Figure 12 from Transport of Large-Scale Poloidal Flux in Black Hole Accretion
Kris Beckwith et al. 2009 ApJ 707 428 doi:10.1088/0004-637X/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;421:3522-3537
© 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)
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.
from de breuck et al. 2001, AJ, 121, 1241
x-ray data
Chandra 0.5-7 keV, 0.5-2 keV, 2-7 keV and HST/ACS z-band cutouts of a 20x13 arcsec region around
the z=4.1 radiogalaxy TN J1338-1942 (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=-0.15 +- 0.28 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
SED decomposition
de breuck et al. 2010
ApJ 725 36
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
• 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