Here you can download gzipped tar files of sets of accretion disk spectra:

• tot5models - all available spectra (9.0 Mbytes)
• kerrmodels - Kerr disk spectra (8.6 Mbytes)
• schwmodels - Schwarzschild disk spectra (400 kbytes)

The parameters of each model can be determined from the 20 character file name, for example

am-3f-Cr01a01nc.tot5

This is interpreted as follows:

• The first two characters determine whether the black hole was Kerr ("am") or Schwarzschild ("bm"). (The Kerr holes all have a/m=0.998.)
• The next two characters specify the black hole mass as a power of two times 10^9 solar masses. The example above corresponds to a black hole mass of 2^(-3)=0.125 times 10^9 solar masses.
• The two characters following "f" determine the accretion rate. For Kerr holes, this is a power of two times 1 solar mass per year. We use hexadecimal notation, so that the example above corresponds to 2^(-C)=2^(-12) solar masses per year. For Schwarzschild holes, the accretion rates are a power of two times 5.613 solar masses per year, in order to give the same Eddington ratios.
• The two characters following "r" determine the alpha viscosity parameter. "01" corresponds to alpha=0.01, while "10" corresponds to alpha=0.10.
• The two characters follwing "a" determine the cosine of the observer viewing angle, defined as the angle between the rotation axis of the disk and the line of sight. The choices are "01" for 0.01, "20" for 0.20, "40" for 0.40, "50" for 0.50, "60" for 0.60, "80" for 0.80, and "99" for 0.99.
• The final two characters before the decimal point specify the treatment of atomic level populations that was used: "lt" = LTE, "nc" = non-LTE.
• "tot5" specifies the version of these model spectra, and this is the version that was used in the paper by Hubeny, Agol, Blaes, and Krolik (2000).

The contents of each file consist of five columns of numbers, all corresponding to properties that an observer measures at infinity:

• Column 1 is the frequency in Hz.
• Column 2 is the specific luminosity at that frequency, in ergs/s/Hz. This is the luminosity at that frequency that an observer along a particular viewing angle would infer the source to have if it were assumed to be isotropic, i.e. 4 pi times (source distance squared) times measured specific flux.
• Columns 3 and 4 are respectively the Stokes parameters Q and U at that frequency, again in ergs/s/Hz.
• Column 5 is a quality flag set by our relativistic transfer function code which translates the locally emitted disk spectrum to that observed at infinity. This flag is usually zero, indicating that the calculated values at that frequency are trustworthy.

A detailed discussion of these models can be found in the paper by Hubeny, Agol, Blaes, and Krolik (2000, ApJ, 533,710).

If you would like to see additional models calculated, please send us an email at blaes@physics.ucsb.edu. Also, please contact us anyway if you use these models so we can keep you updated on our future progress.