# Read me for Cloudy data files

Overview
Compiling ancillary files with the *.in input files
The *.ini files
Hummer and Storey Case B data files
FeII
Star files
Other data files
The resolution of the continuum energy mesh

## Overview

This file documents the files included in the Cloudy data distribution. It is meant as a reminder of the various files and is not intended as instructions for setting up the code. Those instructions are on the web site.

## Compiling ancillary files with the *.in input files

Certain sets of ancillary files must be generated before the code will function. These include the stellar atmospheres, grain data files, and possibly the opacities. A series of simple input scripts are included here to do this. Each source be executed after compiling the source. The following gives the script name and says what it does.

### Emergent continua from stellar atmospheres

These need need to be compiled before the Atlas, Costar, Rauch, and Werner options on the `table star` command will function. See Stellar Atmospheres in C96 for more details. This step does not need to be done if these stellar continua are not needed.

`compilestars.in` - will compile all the stellar atmospheres
`compile1star.in` - will compile only one of the stellar atmospheres (edit the file to determine which one).
`compileatlas.in` - will compile only the atlas stellar atmospheres
`compilecostar.in` - will compile only the CoStar stellar atmospheres
`compilerauch.in` - compile only the Rauch stellar atmospheres
`compile werner.in` - compiles only the Werner stellar atmospheres

### (Possibly) compiling the size-distributed grains

Compiled grain opacities must exist before the `pgrains` command will function. Compiled opacities are already included in the data files (the *.opc files), so nothing need be done if you are happy with the default setup. They would need to be recompiled if you change the energy grid of the code, or wish to use a different grain refractive index or size distribution. Distributed grains are new in C96 and were added in collaboration with Peter van Hoof and Peter G. Martin. These use optical properties for each grain material (the *.rfi files) and size distribution files (the *.szd files) to create grain opacities (the *.opc files) that are a function of grain size. The code can then do a more realistic simulation of the grain emission and physics

`compilegrains.in` - This will compile all the standard grains.

`compile1grain.in` - example of compiling a single grain type for the `pgrain`s command to use.

`vanhoof_grain_model.pdf` - written by Peter van Hoof, describes the file formats needed to modify grain properties.

### The grain properties files, * szd, *.rfi, *.opc

These files specify the size distribution (*.szd) and refractive indices (*.rfi) for the new treatment of grain physics that is used with the `pgrains` command. The *.opc files give the actual opacities used by the code.

## The *.ini files

These are a series of files that add commands to the input stream. They are added by including an `init` command that names one of the following files.

`c84.ini` - makes code behave more like version 84
`honly.ini` - hydrogen only init file
`hheonly.ini` - init file for H, He only
`ism.ini` turns off level 2 lines, only includes prominent elements for depleted mixture. NB This does not add grains to the mix even though many elements are strongly depleted. This is not consistent, and so grains should be added separately

## Hummer and Storey Case B data files

The files HS_e1b.dat through HS_e8b.dat, and HS_e1a.dat through HS_e8a.dat are from Storey P.J., Hummer D.G. 1995, MNRAS 272, 41
http://adc.gsfc.nasa.gov/adc-cgi/cat.pl?/catalogs/6/6064/

## Kaastra and Mewe inner shell process files

The files auger.dat, mewecoef.dat, and kalpha.dat are tables of atomic data from Kaastra, J.S., & Mewe, R., 1993, A&AS, 97, 443

## FeII

Three files contain the data needed to set up the large FeII model ion, described in Verner et al. (1999, ApJS 120, 101. The data formats are described following the name of the file and the reference for the data it contains.

### fe2rad.dat:

This file contains Einstein transition probabilities. The original sources were Nahar (1995; A&A 293, 967), Quinet, LeDourneuf, & Zeipppen (1996; A&AS 120, 361), Furh, Martin, & Wiese (1988; J Phys Chem Ref Data 17, Suppl 4), Giridhar & Arellano Ferro (1995; Ref Mexicana Astron Astrofis 31, 23), and the Kurucz (1995; SAO CD ROM 23) data base if nothing else was available.

lower level number
upper level number
lower level statistical weight
upper level statistical weight
Einstein A coefficient, s**(-1)
Energy, cm**(-1)
type of transition (1 - allowed, 2 - semiforbidden, 3 - forbidden)

### fe2col.dat :

This file contains collision data. These data are from Zhang & Pradhan (1995; A&A 293, 953), Bautista (private communication), and the g-bar approximation (Mewe 1972; A&AS 20, 215).

lower level number in Zhang and Pradhan notation, from 1 to 141
upper level number in Zhang and Pradhan notation, from 2 to 142
collision strengths at 20 temperatures,
1e3,3e3,5e3,7e3,1e4,12e3,15e3,17e3,2e4,25e3,3e4,35e3,4e4,45e3,5e4,6e4,7e4,8e
4,9e4,1e5

### fe2nn.dat

nn(142) - actual level numbers for each of Zhang and Pradhan levels

### fe2levels.dat

This gives the spectroscopic levels sorted in increasing order within the model atom.

fe2bands.dat

These are the bands that will be entered into the main output created by the code. This is designed to be edited by a human. All FeII emission within these bands is co-added and entered as a single emission line.

## Other data files

BLRLineList.dat, the list of lines that can be entered into an array by calling cdGetLineList

level1.dat, the main set of level 1 lines, this file is designed to be edited by humans.

level2.dat, the level 2 lines, do not edit this file!

## The resolution of the continuum mesh

The file continuum_mesh.dat contains data the defines the continuum mesh used during a calculation. It is possible to make the continuum have any resolution at all by changing this file. The continuum resolution largely sets the execution time so be careful. The file contains documentation of its use.

Visit http://nimbus.pa.uky.edu/cloudy for more details, the latest updates, and to get on the mailing list.

Good luck!
Gary J. Ferland