Data from Dannen et al. (2019)
Photoionization calculations of the radiation force due to spectral lines in AGNs
(Accepted to ApJ)
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
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
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.
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
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.
Simple python reader
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
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.
Citing these tables
Please cite Dannen et al. (2019) if you publish results that utilized any of these tables.
These calculations were performed on the Cherry Creek cluster at UNLV.
Support for Program number HST-AR-14579.001-A was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555.
Work at LANL was done under the auspices of the National
Nuclear Security Administration of the US Department
of Energy at Los Alamos National Laboratory under
Contract No. DE-AC52-06NA25396. TW is partially supported by
LANL LDRD Exploratory Research Grant 20170317ER.