Spectral Line Shapes from Black Hole Accretion Disks

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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/sky7a0
9.html and http//www.nasa.gov )
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Fitting with model including Relativistic Iron
Line Emission
Source MCG-6-30-15 (Observed with XMM-Newton)

• From Fabian et. al. 2002

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Iron Line Profile

• Shown in (Fv) 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

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Steps in Calculation

• Determine which photons escape and their observed
  frequencies
• Determine which angle they are observed at
• Determine the flux at the observation point

• From Fanton et. al. 1997,
• Rauch and Blandford (1994)

Image of XMM-Newton (from www.cnrs.fr )
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Number of Geodesics reaching Infinity vs. Red
Shift
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Number of Geodesics Reaching Infinity at a
certain Observation Angle
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SummaryWhat we can tell from the line shape?

• Temperature Gradient
• Spin of the Black Hole
• Observation angle

(picture from http//web1.pas.rochester.edu/dmw/a
st102/)