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To find and download HEASARC data in the cloud, you can use astroquery.heasarc or download our new tool, hark.

The HEASARC and NuSTAR teams are greatly saddened by the sudden passing of Katja Pottschmidt. Most recently Katja was the lead scientist for the NuSTAR Guest Observer Facility (GOF), a role she had supported for many years. During her science career she worked on many other high energy astrophysics missions and played an integral role in advancing our knowledge of the universe. She was a wonderful colleague and friend and will be keenly missed by all who knew her.

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kyconv: convolution using a relativistic line from axisymmetric accretion disk

Convolution using as a kernel the relativistic line from an axisymmetic accretion disk. See Dovciak et al. (2004).

par1 a/M; BH angular momentum (GM/c)
par2 theta_o; observer inclination (0 = pole on, degrees)
par3 rin; inner radius (GM/c$^2$)
par4 ms; 0 means integrate from rin, 1 means integrate emission from above the marginally stable orbit only
par5 rout; outer radius (GM/c$^2$)
par6 alpha; accretion disk emissivity scales as $r^{-alpha}$ for $r<rb$
par7 beta; accretion disk emissivity scales as $r^{-beta}$ for $r>rb$
par8 rb; boundary radius between inner and outer emissivity laws (GM/c$^2$)
par9 zshift; overall Doppler shift
par10 limb; 0 means isotropic emission, 1 means Laor's limb darkening ($1+0.26\mu$), 2 means Haardt's limb brightening ($\ln{1+1/\mu}$
par11 ne_loc; number of grid points in local energy (energy resolution of local flux, the grid is equidistant in logarithmic scale)
par12 normal; 0 means normalize total flux to unity, +ve value means normalize to unity at the energy given by the parametervalue, -ve value means unnormalized.

next up previous contents
Next: lsmooth: lorentzian smoothing Up: Convolution Model Components Previous: kerrconv: accretion disk line   Contents