Fluxes obtained with simple disk plus power law model |
Setup for relativistic disk modeling
Different values of mass, distance and inclination were chosen:
Mass/Msun: 5, 10, 15
Dist/kpc: 5, 10, 15, 20
incl/deg: 55, 65, 75, 85
=>48 {M, d, i} triplets.
Model: phabs*kerrbb
Frozen parameters:
kerrbb.norm=1,
kerrbb.eta=0 (standard Keplerian disk with zero torque
at the inner boundary),
kerrbb.Mbh=one of the choices from above,
kerrbb.dist=one of the choices from above,
kerrbb.incl=one of the choices from above,
kerrbb.rflag=1 (self-irradiation is included),
kerrbb.lflag=1 (limb-darkening is included).
Global parameters (allowed to vary, but tied between observations):
phabs.nh,
kerrbb.spin.
Local parameters (allowed to vary between observations):
kerrbb.Mdd (mass accretion rate of the disk in units of 10^18
g/sec),
kerrbb.hd (spectral hardening factor).
Number of free parameters in the simultaneous fits = 54
Degrees of freedom = 14,822
Fit results
* Click here to see variation of mass accretion rate and spectral hardening (color correction) factor.* Click here to see individual fits.
* Click here to see individual best-fit parameter files.
Heat maps ...
... based on reduced-χ2 values (i.e. χ2ν=χ2/14822)
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... based on derived spin values
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...based on values of averaged spectral hardening factors
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... based on values of average best-fit Eddington luminosities
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... heat maps based on isotropic Eddington luminosities assuming a flux of 1.5x10-9 erg/s/cm^2.
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... based on derived column density
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Chernoff faces for {M,D,i} triplets
Control faces
The leftmost face is a `neutral' face where
the parameter values of
The remaining figures show how the faces/expressions change when any one of these parameters above change.
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Mass=5 solar
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Mass=10 solar
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Mass=15 solar
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Last update: 2013 June 05 (DM).