# Data from Dannen et al. (2019)

### Photoionization calculations of the radiation force due to spectral lines in AGNs

(Accepted to ApJ)

arXiv posting

## XSTAR CALCULATIONS

Here we make publicly available the results of our photoionization calculations for force multipliers and associated heating/cooling rates for the Type 1 and 2 AGN SEDs from Mehdipour et al. (2015). A tarball containing all of the data is available for download here.These tables provide the essential data needed to perform many types of state-of-the-art radiation-hydrodynamical calcuations. For example, these tables now make it possible to model line-driven winds with self-consistent heating and cooling rates to also account for thermal driving - a task that has yet to be performed! Alternatively, these tables can be used together to self-consistently model cloud formation and acceleration in AGN using the methods developed by Proga & Waters (2015). If used in combination with MHD simulations, these force multipliers and heating/cooling rates can be used to compute the first ever self-consistent models of magnetothermal line-driven winds or cloud formation and acceleration in the presence of magnetic fields. As a final example, they can be used to compute models of clumpy accretion flows following the methods of Moscibrodzka & Proga (2013), as both of these AGN equilibrium curves (see below) feature large, thermally unstable regions.

### FORCE MULTIPLIER TABLES

AGN1_Fmult.datAGN2_Fmult.dat

These tables are formatted to be easy to parse (see the python example below), and a C++ interface to simulation codes is provided. The first entry in each table is N_xi, the number of photoionization parameter values. The remainder of the first row contains the N_xi values of log10(xi). The remainder of the first column is all the log10 values of the optical depth parameter, t. The entries corresponding to a given (t,xi) pair are the values of log10(M), where M is the force multiplier.

### HEATING/COOLING TABLES

AGN1_heating.datAGN1_cooling.dat

AGN1_net.dat

AGN2_heating.dat

AGN2_cooling.dat

AGN2_net.dat

For each SED (AGN1 or AGN2), there are three tables with labels 'heating', 'cooling', and 'net' (heating - cooling). The first entry in each table is N_xi, the number of photoionization parameter values. The remainder of the first row contains the N_xi values of xi (in cgs units this time). The remainder of the first column is all of the temperature values (in Kelvin). The entries corresponding to a given (T,xi) pair are the rates in units of erg cm^3 s^-1.

### Radiative equilibrium curves

AGN1_eq_curve.datAGN2_eq_curve.dat

These are the equlibrium curves (where heating balances cooling) corresponding to the Type 1/2 AGN SEDs. These curves can be extracted from the tables above, so we provide them separately as a means to verify the table parser.

## SUPPORTIVE CODE

### Simple python reader

Here is a sample script that parses the tables and generates a contour plot of the equlibirum curves and cooling rates.### Hydro interface/interpolation routine

VegasTables is a sophisticated routine written in C++ that is intended for use with hydrodynamical codes. This code first parses a table and then performs either bilinear or bicubic interpolation to evaluate the rates at any given (xi,T) or the force multipliers at any given (xi,t). We employed an earlier version of this interface (which was applied to Athena++) in the hydrodynamical calculations published by Dyda et al. (2017), where the bilinear interpolation method is documented (see the Appendix). The routines in vegas_tables.h now perform bicubic interpolation using the GSL library, as bicubic interpolation is found to be about 5x more accurate than bilinear interpolation.See the documentation within vegas_tables.h for example usage.

This is a general routine that works for any ordered tabular data. The data being 'ordered' is important, as it permits immediate indexing of the entry locations, obviating the need for a table search.