Overview
Compiling
ancillary files with the *.in input files
The *.ini files
Hummer and Storey Case B data
files
FeII
Star files
This file documents the files included in the Cloudy data distribution. There are several types of definitions here.
The first describe the purpose of the Cloudy input files that are included in the data distribution. These have file names ending in *.in. These are used to
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.
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.
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
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 pgrains command to use.
new_grain_model.pdf - written by Peter van Hoof, describes the file formats needed to modify grain properties.
compileopac.in
A large amount of atomic opacity data is generated by the code when it starts up. If you execute the script compmileopac.in the code will compile the opacities and then save this information to disk. In later calculation a small amount of time may be saved by reading this file rather than recomputing all the opacities. This saves about 2 seconds on my PC, where the file is stored on a local SCSI disk. Note that this option may actually loose time if you have a very fast CPU and the files are on a network drive.
Compiled opacities are stored as the files opacity.opc and opacity.pnt. .
If the opacities are not compiled by executing this file the code will function normally, and will compute the opacities at each initialization.
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 does not
add grains to the mix even though many elements are strongly depleted. NB
This is not consistent, and so grains should be added separately
from Storey P.J., Hummer D.G. Mon. Not. R. Astron. Soc. 272, 41 (1995)
http://adc.gsfc.nasa.gov/adc-cgi/cat.pl?/catalogs/6/6064/
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.
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.
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)
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
nn(142) - actual level numbers for each of Zhang and Pradhan levels
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.
This web page describes how to gather all the needed star data files together, and what to then do with them.
auger.dat, mewecoef.dat, kalpha.dat, tables of atomic data from the Kaastra & Mewe compilations
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, edited by humans
level2.dat, the level 2 lines, do not edit this file
Visit http://nimbus.pa.uky.edu/cloudy
for details and latest updates.
Good luck,
Gary J. Ferland