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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kerrd: optically thick accretion disk around a Kerr black hole
Optically thick extreme-Kerr disk model based on the same tranfer-function used in the laor Kerr disk-line model. Local emission is simply assumed to be the diluted blackbody. See Laor (1991) for an explanation of the transfer function. See Ebisawa et al. (2003) for examples of using this model.
| par1 | distance (kpc) |
| par2 | spectral hardening factor, Tcol/Teff. Should be greater than 1.0, and considered to be 1.5–1.9 for accretion disks around a stellar-mass black hole. See, e.g., Shimura & Takahara (1995) 445, 780 |
| par3 | mass of the central object (solar unit) |
| par4 | mass accretion rate ( g/s) |
| par5 | disk inclination angle (deg; 0 for face-on) |
| par6 | inner radius (units of  ). 1.235 is the last stable
orbit. |
| par7 | outer radius (units of ) |
| K | normalization factor. should be fixed to 1. |