The T.H.E.R.M.A.L. Suite

UV Background


It is still standard in multiple hydrodynamical simulations that model the Intergalactic Medium and/or galaxy formation to account for radiative feedback via a spatially uniform, but time-varying ultraviolet background (UVB) radiation field, input to the code as a list of photoionization and photoheating rates that vary with redshift (e.g. Katz et al. 1996). For historical reasons the ascii table containing these rates that is provided to the code is usually called TREECOOL. These models are obtained using one-dimensional cosmological radiative transfer calculations. Below I list some of the more popular ones and where you can download the files:

The approximate ionization and thermal histories obtained using these models in ΛCDM hydrodynamical simulations, including the older versions, can be found in Figures 9 and 12 of this paper.

However, in order to fully explore the parameter space of ionization, and most specially, thermal histories in a consistent way in Onorbe et al. (2017), we created a new phenomenological method to develop UVB tables that will reliable produce different ionization and thermal histories during reionization. We provide here the tables for a list of UVB models that have been constructed using this methodology and that have already been used in several scientific papers.

Contact us if you are interested in running some other specific model of UVB in your simulation. We will be happy to provide it to you.

Caveats and warnings:

- The UVB models surely break down during reionization events as they assumed an homogeneous evolution during an intrinsically inhomogeneous process. Therefore the validity of using them in optically thin simulations (during reionization) is questionable. We refer the reader to Oñorbe et al. (2017) and Puchwein et al. (2018) for a more detailed discussion in this regard.

- Metal ionization and cooling: The UVB models provided here only have information about the photoionization and photoheating of H and He elements (so HI, HeI and HeII). Therefore these models do not provide any information about the photoionization of any metals or their photoheating. Also, the cooling associated with H and He as well as any other element has to be implemented independly in your code. Some codes used a look up table that provides the net cooling/heating of a resolution element as a function of its density, temperature, metal content, etc. Contact us if you are interested in running a model that uses this format.

- Mean flux: the HI, HeI and HeII photoionization in all the models provided here have been adjusted to match the HI and HeI mean flux observations. However the exact mean flux values obtained in a simulation will slightly vary depending on the exact cosmological paramaters used and the thermal state of the IGM (e.g. the specific heating/cooling processes considered). See Oñorbe et al. (2017) for more details about this.

© J. Oñorbe