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\@writefile{lof}{\contentsline {figure}{\numberline {1.1}{\ignorespaces The left panel shows the radius of the black hole horizon $r_{\rm  Hor}$ (dashed line) and the {\it  Innermost Circular Stable Orbit (ISCO)} around it $r_{\rm  ISCO}$ (solid line), in units of the Schwarzschild radius $r_{\rm  Sch}$ (see Eq. 1.2\hbox {}), as functions of the black hole spin parameter $a$. The limiting value of $a=1$ ($a=-1$) corresponds to a corotating (counter-rotating) orbit around a maximally-spinning black hole. The binding energy of a test particle at the ISCO determines the radiative efficiency $\epsilon $ of a thin accretion disk around the black hole, shown on the right panel. }}{\fontsize  {8.75}{11pt}\selectfont  \sffamily  3}}
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\@writefile{lof}{\contentsline {figure}{\numberline {1.2}{\ignorespaces Simulated image of an  accretion flow around a  black hole spinning at half its maximum rate, from a viewing angle of $10^\circ $ relative to the  rotation axis. The coordinate grid in the equatorial plane of the spiraling flow shows how strong lensing around the black hole bends the back of the apparent disk up. The left side of the image is brighter due its rotational motion towards the observer. The bright arcs are generated by gravitational lensing. A dark silhouette appears around the location of the  black hole because the light emitted by gas behind it disappears into the  horizon and cannot be seen by an observer on the other side. Recently, the technology for observing such an image from the supermassive black holes at the centers of the Milky Way and M87 galaxies has been demonstrated as feasible [Doeleman, S., et al. {\it  Nature} {\bf  455}, 78 (2008)]. To obtain the required resolution of tens of micro-arcseconds, signals are being correlated over an array (interferometer) of observatories operating at a millimeter wavelength across the Earth. Figure credit: Broderick, A., \& Loeb, A. {\it  Journal of Physics Conf. Ser.} {\bf  54}, 448 (2006); {\it  Astrophys. J.} {\bf  697} 1164 (2009). }}{\fontsize  {8.75}{11pt}\selectfont  \sffamily  10}}
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\@writefile{lof}{\contentsline {figure}{\numberline {1.3}{\ignorespaces Multi-wavelength images of the highly collimated jet emanating from the supermassive  black hole at the center of the giant elliptical galaxy M87. The X-ray image (top) was obtained with the Chandra X-ray satellite, the  radio image (bottom left) was obtained with the Very Large Array (VLA), and the optical image (bottom right) was obtained with the Hubble Space Telescope (HST). }}{\fontsize  {8.75}{11pt}\selectfont  \sffamily  12}}
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\@writefile{lof}{\contentsline {figure}{\numberline {1.4}{\ignorespaces Numerical  simulation of the collapse of an early dwarf galaxy with a  virial temperature just above the  cooling threshold of atomic hydrogen and no H$_2$. The image shows a snapshot of the gas density distribution 500 million years after the  Big Bang, indicating the formation of two compact objects near the center of the galaxy with masses of $2.2\times 10^{6}M_{\odot }$ and $3.1\times 10^{6}M_{\odot }$, respectively, and radii $<1$ pc.  Sub-fragmentation into lower mass clumps is inhibited because hydrogen atoms cannot cool the gas significantly below its initial temperature. These circumstances lead to the formation of  supermassive stars that inevitably collapse to make massive seeds of supermassive  black holes. The simulated box size is 200 pc on a side. Figure credit: Bromm, V. \& Loeb, A. {\it  Astrophys. J.} {\bf  596}, 34 (2003). }}{\fontsize  {8.75}{11pt}\selectfont  \sffamily  16}}
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