1. Spectral Line Shapes from Black Hole Accretion Disks Tsing Wai Wong Advisors: Dr. Drew Milsom Dr. David Ballantyne (pictures from http://www.seasky.org/cosmic/sky7a09.html and http://www.nasa.gov ) http://www.seasky.org/cosmic/sky7a09.htmlhttp://www.nasa.gov

2. Fitting with model including Relativistic Iron Line Emission  From Fabian et. al. 2002 Source: MCG-6-30-15 (Observed with XMM-Newton)

3. Iron Line Profile Shown in (F v ) flux units, obtained from the ratio of the MOS data to best-fitting underlying continuum model. The crosses mark the data points and the solid line marks the line model  From Fabian et. al. 2002

4. Steps in Calculation 1. Determine which photons escape and their observed frequencies 2. Determine which angle they are observed at 3. Determine the flux at the observation point Image of XMM-Newton (from www.cnrs.fr )www.cnrs.fr  From Fanton et. al. 1997, Rauch and Blandford (1994)

5. Number of Geodesics reaching Infinity vs. Red Shift

6. Number of Geodesics Reaching Infinity at a certain Observation Angle

7. Summary: What we can tell from the line shape?  Temperature Gradient  Spin of the Black Hole  Observation angle (picture from http://web1.pas.rochester.edu/~dmw/ast102/)