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## Using stellar SEDs in C07.02 and later
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## Using stellar SEDs in C07.02 and later
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## Overview of the stellar SEDs
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## Overview of the stellar SEDs
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### Introduction
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### Introduction
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This page describes how to set up the grids of stellar spectral energy distributions (SEDs) in versions C07 and later of Cloudy. The ability to read in tables of stellar atmospheres was originally introduced into Cloudy by Kevin Volk around 1990. The current versions use [Peter van Hoof](http://homepage.oma.be/pvh/)'s unified treatment with a single code base and many more stellar SEDs. The [StellaratmosphereOld](StellaratmosphereOld) page describes the stellar atmospheres used in Cloudy versions C06.02 and before.
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This page describes how to set up the grids of stellar spectral energy distributions (SEDs) in versions C07 and later of Cloudy. The ability to read in tables of stellar atmospheres was originally introduced into Cloudy by Kevin Volk around 1990. The current versions use [Peter van Hoof](http://homepage.oma.be/pvh/)'s unified treatment with a single code base and many more stellar SEDs. The [StellaratmosphereOld](StellaratmosphereOld) page describes the stellar atmospheres used in Cloudy versions C06.02 and before.
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[Peter van Hoof](http://homepage.oma.be/pvh/) wrote this part of Cloudy and is the maintainer. Please post questions, comments, and suggestions for new stellar atmosphere grids on the
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[Peter van Hoof](http://homepage.oma.be/pvh/) wrote this part of Cloudy and is the maintainer. Please post questions, comments, and suggestions for new stellar atmosphere grids on the
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[Cloudy discussion board](https://cloudyastrophysics.groups.io/g/Main).
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[Cloudy discussion board](https://cloudyastrophysics.groups.io/g/Main).
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The following sections describe how to download the ASCII stellar SED files. Each grid of stellar SEDs, along with a link to the paper or web site describing it, is given below. *If you use one of these grids in a publication it is very important that you properly cite the original paper describing that grid!* It is intellectually lazy, and deprives the original authors of their proper citation, to simply state that you used an SED that was available in Cloudy.
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The following sections describe how to download the ASCII stellar SED files. Each grid of stellar SEDs, along with a link to the paper or web site describing it, is given below. *If you use one of these grids in a publication it is very important that you properly cite the original paper describing that grid!* It is intellectually lazy, and deprives the original authors of their proper citation, to simply state that you used an SED that was available in Cloudy.
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### Note for older Cloudy versions
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### Note for older Cloudy versions
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To avoid needless repetition, we will assume after this section that you are using Cloudy C22 or newer. The main differences between these and older Cloudy versions are briefly described here.
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To avoid needless repetition, we will assume after this section that you are using Cloudy C22 or newer. The main differences between these and older Cloudy versions are briefly described here.
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Some of the grids are very large and accessing them can be slow. They can be "compiled" to speed up the process. How this is done depends on the Cloudy version. In Cloudy versions C17 and older, compiling these grids resulted in files with names ending in ".mod". These binary files were platform-dependent. Compiling the grids was mandatory and the resulting *.mod files were the ones that needed to be placed in the Cloudy data directory. Starting with Cloudy version C22 all this changed. The code now works directly on the ASCII files and compiling them became optional. The latter now results in files with names ending in ".idx". These help speed up reading the ASCII file and are recommended for large ASCII files. Despite their simple appearance, these idx files are still (in principle) platform-dependent. Both the *.ascii files and the *.idx files (if you chose to create them) need to be placed in the Cloudy search path. An added advantage of the new setup is that there is no longer a dependence on the frequency mesh, so _you do not need to recompile the ASCII grids when you change the frequency mesh_ (this was mandatory in Cloudy versions C17 and older). Compiling grids that are not in the standard Cloudy format (e.g. Rauch grids or Starburst99 output) is still mandatory.
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Some of the grids are very large and accessing them can be slow. They can be "compiled" to speed up the process. How this is done depends on the Cloudy version. In Cloudy versions C17 and older, compiling these grids resulted in files with names ending in ".mod". These binary files were platform-dependent. Compiling the grids was mandatory and the resulting *.mod files were the ones that needed to be placed in the Cloudy data directory. Starting with Cloudy version C22 all this changed. The code now works directly on the ASCII files and compiling them became optional. The latter now results in files with names ending in ".idx". These help speed up reading the ASCII file and are recommended for large ASCII files. Despite their simple appearance, these idx files are still (in principle) platform-dependent. Both the *.ascii files and the *.idx files (if you chose to create them) need to be placed in the Cloudy search path. An added advantage of the new setup is that there is no longer a dependence on the frequency mesh, so _you do not need to recompile the ASCII grids when you change the frequency mesh_ (this was mandatory in Cloudy versions C17 and older). Compiling grids that are not in the standard Cloudy format (e.g. Rauch grids or Starburst99 output) is still mandatory.
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Since Cloudy release C22 the policy for reading data files (including stellar atmosphere grids) has been unified and made more flexible. The concept of the Cloudy data directory has been generalized to the Cloudy search path. See the section titled "The Search Path for Input Files" in Hazy 1 for more details. When the Cloudy search path is mentioned below, it should be implicitly replaced with the Cloudy data directory for Cloudy versions C17 and older.
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Since Cloudy release C22 the policy for reading data files (including stellar atmosphere grids) has been unified and made more flexible. The concept of the Cloudy data directory has been generalized to the Cloudy search path. See the section titled "The Search Path for Input Files" in Hazy 1 for more details. When the Cloudy search path is mentioned below, it should be implicitly replaced with the Cloudy data directory for Cloudy versions C17 and older.
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For Cloudy versions C17 and older, modify all commands that use explicit file names between double quotes by replacing the .ascii filename extension with .mod (except for the *compile stars* command, which always works on an .ascii file).
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For Cloudy versions C17 and older, modify all commands that use explicit file names between double quotes by replacing the .ascii filename extension with .mod (except for the *compile stars* command, which always works on an .ascii file).
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### Procedure for setting up a stellar SED grid
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### Procedure for setting up a stellar SED grid
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This describes the general procedure for setting up an individual stellar SED grid. The method is basically the same for all the grids.
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This describes the general procedure for setting up an individual stellar SED grid. The method is basically the same for all the grids.
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1) Cloudy should already have been set up by following the usual steps described on the [StepByStep](StepByStep) page.
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1) Cloudy should already have been set up by following the usual steps described on the [StepByStep](StepByStep) page.
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2) Download the SED files from the individual websites listed below. *It is OK to skip the grids you don't need* (or to skip all of them if you are not going to use stellar atmosphere files at all). Cloudy will work just fine without them as long as you are not explicitly requesting a stellar atmosphere from a missing grid. Some grids are on the original author's web site, while other files are located in the "stars" directory below the main Cloudy
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2) Download the SED files from the individual websites listed below. *It is OK to skip the grids you don't need* (or to skip all of them if you are not going to use stellar atmosphere files at all). Cloudy will work just fine without them as long as you are not explicitly requesting a stellar atmosphere from a missing grid. Some grids are on the original author's web site, while other files are located in the "stars" directory below the main Cloudy [data site](https://data.nublado.org/). Links are given at the top of each of the sections below describing the grids. Most files have names that end in "ascii". An example is *ostar2002_p03.ascii* (a file from the Tlusty web site). The downloaded grid files should be stored in the Cloudy search path. Most files have been compressed with gzip or xz. Explode the ASCII files using the command `gunzip *.gz` or `xz -d *.xz` as needed. If you downloaded any of the Rauch grids, explode the tarballs with `tar xfz *.tgz`.
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[data site](https://data.nublado.org/). Links are given at the top of each of the sections below describing the grids. Most files have names that end in "ascii". An example is *ostar2002_p03.ascii* (a file from the Tlusty web site). The downloaded grid files should be stored in the Cloudy search path. Most files have been compressed with gzip or xz. Explode the ASCII files using the command `gunzip *.gz` or `xz -d *.xz` as needed. If you downloaded any of the Rauch grids, explode the tarballs with `tar xfz *.tgz`.
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3) In most cases this step is optional, except when you downloaded files that are not in the native Cloudy format (i.e. files that do not end with the extension ".ascii"). Some of the grids are very large and accessing them can be slow. They can be "compiled" to speed up the process. Execute Cloudy with the single command *compile stars* in the directory where you placed the downloaded files. A convenient way to do this is running the code with the command `cloudy.exe -e compile stars`. One idx file will be created for each of the downloaded files. An example is *ostar2002_p03.idx* which is created from the file *ostar2002_p03.ascii*. Keep the original ASCII files as you will need them too. If you downloaded any of the Rauch grids you will probably want to remove the individual SED files with the command ```rm -f *0.1```. There may be a great many of them, and they are still contained in the tarballs you downloaded. Note that Cloudy will find input files on the entire search path, but output files will always be written in the local directory, regardless of where the corresponding input file resided. It is a good idea though to keep the ASCII and idx files together. For Cloudy versions prior to C25.00 RC2, some grids are not recognized by Cloudy (e.g., the BPASS grids) in which case you need to use an explicit filename on the command (e.g., *compile stars "BPASSv2.3_imf135_300.a-02_burst_binary.ascii"*). Later Cloudy versions will find any file with the extension ".ascii" on the search path.
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3) In most cases this step is optional, except when you downloaded files that are not in the native Cloudy format (i.e. files that do not end with the extension ".ascii"). Some of the grids are very large and accessing them can be slow. They can be "compiled" to speed up the process. Execute Cloudy with the single command *compile stars* in the directory where you placed the downloaded files. A convenient way to do this is running the code with the command `cloudy.exe -e compile stars`. One idx file will be created for each of the downloaded files. An example is *ostar2002_p03.idx* which is created from the file *ostar2002_p03.ascii*. Keep the original ASCII files as you will need them too. If you downloaded any of the Rauch grids you will probably want to remove the individual SED files with the command ```rm -f *0.1```. There may be a great many of them, and they are still contained in the tarballs you downloaded. Some grids are not recognized by Cloudy (e.g., the BPASS grids) in which case you need to use an explicit filename on the command (e.g., *compile stars "BPASSv2.3_imf135_300.a-02_burst_binary.ascii"*). Note that Cloudy will find input files on the entire search path, but output files will always be written in the local directory, regardless of where the corresponding input file resided. It is a good idea though to keep the ASCII and idx files together.
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4) You can add grids later (if newer ones become available, or if you change your mind about grids you initially skipped). Download the new files, place them in the search path and simply go through the same procedure outlined above. Cloudy will skip any grids for which it finds a valid idx file in the search path (i.e., it will skip any grids that are already compiled).
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4) You can add grids later (if newer ones become available, or if you change your mind about grids you initially skipped). Download the new files, place them in the search path and simply go through the same procedure outlined above. Cloudy will skip any grids for which it finds a valid idx file in the search path (i.e., it will skip any grids that are already compiled).
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### Installing Starburst99 grids
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### Installing Starburst99 grids
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The Starburst99 web page is [here](http://www.stsci.edu/science/starburst99/). The Starburst99 output needs to be converted into the standard Cloudy format and therefore needs to be compiled. The first step is to take the spectrum that was generated by Starburst99 (called *_xxx.spectrum*_) and give it a name that ends in *_.stb99*_. An example of the Starburst99 format that Cloudy expects is given [here](https://data.nublado.org/stars/starburst99.stb99.gz). You can compile the file by giving the single Cloudy command *compile stars "<yourname.stb99>"*. You should replace *<yourname.stb99>* by the name you chose and make sure it is surrounded by double quotes (as is always the case when you include filenames in Cloudy input).
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The Starburst99 web page is [here](http://www.stsci.edu/science/starburst99/). The Starburst99 output needs to be converted into the standard Cloudy format and therefore needs to be compiled. The first step is to take the spectrum that was generated by Starburst99 (called *_xxx.spectrum*_) and give it a name that ends in *_.stb99*_. An example of the Starburst99 format that Cloudy expects is given [here](https://data.nublado.org/stars/starburst99.stb99.gz). You can compile the file by giving the single Cloudy command *compile stars "<yourname.stb99>"*. You should replace *<yourname.stb99>* by the name you chose and make sure it is surrounded by double quotes (as is always the case when you include filenames in Cloudy input).
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Cloudy will then create two files: *yourname.ascii* and *yourname.idx*. Both files are needed by Cloudy.
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Cloudy will then create two files: *yourname.ascii* and *yourname.idx*. Both files are needed by Cloudy.
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Use the starburst file by specifying the file name and the log of the age.
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Use the starburst file by specifying the file name and the log of the age.
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An example might be *table star "starburst.ascii" age 6.7*
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An example might be *table star "starburst.ascii" age 6.7*
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The age will have whatever units are in the original Starburst99 file. The default is years.
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The age will have whatever units are in the original Starburst99 file. The default is years.
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The procedure for using Starburst99 grids was changed in C07.02. It was a special command in previous versions.
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The procedure for using Starburst99 grids was changed in C07.02. It was a special command in previous versions.
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### Installing PopStar grids
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### Installing PopStar grids
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This page describes the procedure for the 2009 grids. The PopStar models can be obtained [here](http://www.fractal-es.com/PopStar/). Next select "PopStar2009" and
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This page describes the procedure for the 2009 grids. The PopStar models can be obtained [here](http://www.fractal-es.com/PopStar/). Next select "PopStar2009" and
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click on "Download Models" on the left-hand side. Then you need to download 1 or more of the zip files in the column "Spectra zip file" on the right-hand side. Models are present for different initial mass functions (IMFs) and metallicities (Z).
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click on "Download Models" on the left-hand side. Then you need to download 1 or more of the zip files in the column "Spectra zip file" on the right-hand side. Models are present for different initial mass functions (IMFs) and metallicities (Z).
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You can choose to convert a single combination of IMF and Z into a 1-dimensional grid allowing interpolation in age, or combine several runs with the _same_ IMF but different Z values into a 2-dimensional grid allowing interpolation in age as well as log(Z) (the latter option is only supported from C10 onwards). The first step is to take an empty (temporary) directory and unzip the files you downloaded in that directory. Next, you run the script [convert_popstar.pl](https://data.nublado.org/stars/convert_popstar.pl) (make sure that the file has execute permission) and redirect the output to a file with a name of your choosing ending in *.ascii*.
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You can choose to convert a single combination of IMF and Z into a 1-dimensional grid allowing interpolation in age, or combine several runs with the _same_ IMF but different Z values into a 2-dimensional grid allowing interpolation in age as well as log(Z) (the latter option is only supported from C10 onwards). The first step is to take an empty (temporary) directory and unzip the files you downloaded in that directory. Next, you run the script [convert_popstar.pl](https://data.nublado.org/stars/convert_popstar.pl) (make sure that the file has execute permission) and redirect the output to a file with a name of your choosing ending in *.ascii*.
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An example for a single zip file would be:
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An example for a single zip file would be:
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```
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```
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<download sp-sal1-z0200.zip from PopStar website>
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<download sp-sal1-z0200.zip from PopStar website>
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unzip sp-sal1-z0200.zip
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unzip sp-sal1-z0200.zip
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<download convert_popstar.pl>
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<download convert_popstar.pl>
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chmod +x convert_popstar.pl
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chmod +x convert_popstar.pl
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convert_popstar.pl > sp-sal1-z0200.ascii
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convert_popstar.pl > sp-sal1-z0200.ascii
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```
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```
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You can optionally compile this grid with:
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You can optionally compile this grid with:
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```
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```
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compile star "sp-sal1-z0200.ascii"
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compile star "sp-sal1-z0200.ascii"
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```
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```
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This will produce a file "sp-sal1-z0200.idx". Both the files "sp-sal1-z0200.ascii" and "sp-sal1-z0200.idx" (if it was created) should be in the Cloudy search path. After you have done this, you can delete the temporary directory if you wish. Now the grid can be used as described in the next section. The procedure for a 2-dimensional grid is very similar. You need to download and unzip multiple files, but apart from that, the procedure is exactly the same. The conversion script will automatically detect that multiple metallicities are present and will alter the resulting *.ascii* file accordingly. It is not necessary to download all metallicities belonging to a certain IMF, you can also use a subset if you wish. The script will extract the stellar flux *only*.
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This will produce a file "sp-sal1-z0200.idx". Both the files "sp-sal1-z0200.ascii" and "sp-sal1-z0200.idx" (if it was created) should be in the Cloudy search path. After you have done this, you can delete the temporary directory if you wish. Now the grid can be used as described in the next section. The procedure for a 2-dimensional grid is very similar. You need to download and unzip multiple files, but apart from that, the procedure is exactly the same. The conversion script will automatically detect that multiple metallicities are present and will alter the resulting *.ascii* file accordingly. It is not necessary to download all metallicities belonging to a certain IMF, you can also use a subset if you wish. The script will extract the stellar flux *only*.
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The PopStar grids are described in [Molla et al. (2009)](http://cdsads.u-strasbg.fr/abs/2009MNRAS.398..451M).
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The PopStar grids are described in [Molla et al. (2009)](http://cdsads.u-strasbg.fr/abs/2009MNRAS.398..451M).
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### Installing BPASS grids
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### Installing BPASS grids
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The BPASS (Binary Population and Spectral Synthesis) stellar population synthesis models are available [here](http://bpass.auckland.ac.nz/index.html). We support the v2.0 through v2.3 releases. These have been converted into Cloudy format and can be downloaded [here](https://data.nublado.org/stars/bpass). The grids are available for several different choices of the initial mass function. There are grids for either an instantaneous starburst of 1e6 Msol, or continuous star formation of 1 Msol/yr lasting 1e6 years (the latter only for v2.0). Each of these releases has separate grids for single-star and binary-star evolution. Grids are available for metallicities ranging from Z=0.001 to 0.040 (v2.0) or Z=0.00001 to 0.040 (all later versions). The first step is to download the compressed ASCII file. Below we will use the v2.3 release as an example.
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The BPASS (Binary Population and Spectral Synthesis) stellar population synthesis models are available [here](http://bpass.auckland.ac.nz/index.html). We support the v2.0 through v2.3 releases. These have been converted into Cloudy format and can be downloaded [here](https://data.nublado.org/stars/bpass). The grids are available for several different choices of the initial mass function. There are grids for either an instantaneous starburst of 1e6 Msol, or continuous star formation of 1 Msol/yr lasting 1e6 years (the latter only for v2.0). Each of these releases has separate grids for single-star and binary-star evolution. Grids are available for metallicities ranging from Z=0.001 to 0.040 (v2.0) or Z=0.00001 to 0.040 (all later versions). The first step is to download the compressed ASCII file. Below we will use the v2.3 release as an example.
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```
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```
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<download BPASSv2.3_imf135_300.a+00_burst_single.ascii.xz>
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<download BPASSv2.3_imf135_300.a+00_burst_single.ascii.xz>
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<download BPASSv2.3_imf135_300.a+00_burst_binary.ascii.xz>
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<download BPASSv2.3_imf135_300.a+00_burst_binary.ascii.xz>
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xz -d *.ascii.xz
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xz -d *.ascii.xz
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```
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```
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In the file name "burst" refers to the single starburst models and "cont" to the continuous star formation models. Furthermore, "single" refers to the single-star evolution models and "binary" to the binary-star evolution models.
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In the file name "burst" refers to the single starburst models and "cont" to the continuous star formation models. Furthermore, "single" refers to the single-star evolution models and "binary" to the binary-star evolution models.
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The ASCII files can be compiled by starting Cloudy and typing:
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The ASCII files can be compiled by starting Cloudy and typing:
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```
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```
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compile stars "BPASSv2_imf135_100_burst_single.ascii"
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compile stars "BPASSv2_imf135_100_burst_single.ascii"
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```
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```
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This step is optional for Cloudy versions C22 and later, but still recommended as the ASCII files are large and compiling them will speed up reading them. Now you need to move the *.ascii and *.idx (if present) files into the search path. After this, they can then be used in Cloudy.
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This step is optional for Cloudy versions C22 and later, but still recommended as the ASCII files are large and compiling them will speed up reading them. Now you need to move the *.ascii and *.idx (if present) files into the search path. After this, they can then be used in Cloudy.
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These are 2D grids allowing interpolation in age and metallicity. You can produce a mix of single and binary stars using e.g.:
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These are 2D grids allowing interpolation in age and metallicity. You can produce a mix of single and binary stars using e.g.:
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```
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```
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table star "BPASSv2.3_imf135_300.a+00_burst_single.ascii" 2e8 -1.8
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table star "BPASSv2.3_imf135_300.a+00_burst_single.ascii" 2e8 -1.8
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intensity <xxx>
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intensity <xxx>
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table star "BPASSv2.3_imf135_300.a+00_burst_binary.ascii" 2e8 -1.8
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table star "BPASSv2.3_imf135_300.a+00_burst_binary.ascii" 2e8 -1.8
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intensity <yyy>
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intensity <yyy>
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```
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```
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The BPASS v2.3 release is described in [Byrne et al. (2022)](https://ui.adsabs.harvard.edu/abs/2022MNRAS.512.5329B/abstract) and [Stanway & Eldridge (2018)](https://ui.adsabs.harvard.edu/abs/2018MNRAS.479...75S/abstract). For the older releases, each [subdirectory](http://data.nublado.org/stars/bpass) contains a README file that contains instructions how to cite the release.
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The BPASS v2.3 release is described in [Byrne et al. (2022)](https://ui.adsabs.harvard.edu/abs/2022MNRAS.512.5329B/abstract) and [Stanway & Eldridge (2018)](https://ui.adsabs.harvard.edu/abs/2018MNRAS.479...75S/abstract). For the older releases, each [subdirectory](http://data.nublado.org/stars/bpass) contains a README file that contains instructions how to cite the release.
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### Installing your own grids
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### Installing your own grids
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It is possible to install your own atmosphere grids. For this you need to create your own ASCII file. Instructions for this are given in Appendix B of Hazy 1 (starting from C10.00). Once you created the ASCII file, compiling it and using it is quite similar to Starburst99 files. To (optionally) compile, issue the command *compile stars "<yourname.ascii>"*. To use it, issue the command *table star "<yourname.ascii>" <par1> <par2> ...* (the number of parameters here should exactly match the number of parameters you defined in the grid).
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|
It is possible to install your own atmosphere grids. For this you need to create your own ASCII file. Instructions for this are given in Appendix B of Hazy 1 (starting from C10.00). Once you created the ASCII file, compiling it and using it is quite similar to Starburst99 files. To (optionally) compile, issue the command *compile stars "<yourname.ascii>"*. To use it, issue the command *table star "<yourname.ascii>" <par1> <par2> ...* (the number of parameters here should exactly match the number of parameters you defined in the grid).
|
|
|
|
|
|
|
|
|
|
|
|
### If you don't set up all the stellar SED grids
|
|
|
### If you don't set up all the stellar SED grids
|
|
|
|
|
|
|
The Cloudy download includes a large body of test cases that are designed to confirm that the code gets the right answer. Running the test suite is an important part of setting up the code and is described on the TestSuite page.
|
|
|
The Cloudy download includes a large body of test cases that are designed to confirm that the code gets the right answer. Running the test suite is an important part of setting up the code and is described on the TestSuite page.
|
|
|
|
|
|
|
The test suite includes a number of test cases that are designed to check that the stellar SEDs can be correctly accessed with the *table stars* command. These tests are in the _tsuite/auto_ directory and have names that start with "stars". The command `ls stars\*.in` will list them all. You would need to download all of the stellar grids for all of the star tests to work.
|
|
|
The test suite includes a number of test cases that are designed to check that the stellar SEDs can be correctly accessed with the *table stars* command. These tests are in the _tsuite/auto_ directory and have names that start with "stars". The command `ls stars\*.in` will list them all. You would need to download all of the stellar grids for all of the star tests to work.
|
|
|
|
|
|
|
If you decide not to download all of the stellar grids then the *stars\** tests that use the missing SEDs will fail. This is *not a problem*, but is a reminder that some of the *table stars* commands will not work.
|
|
|
If you decide not to download all of the stellar grids then the *stars\** tests that use the missing SEDs will fail. This is *not a problem*, but is a reminder that some of the *table stars* commands will not work.
|
|
|
|
|
|
|
|
|
|
|
|
### How to find out which grids you have installed
|
|
|
### How to find out which grids you have installed
|
|
|
|
|
|
|
Two commands will generate information about available grids. You can use these to document which grids are installed after the code has been set up.
|
|
|
Two commands will generate information about available grids. You can use these to document which grids are installed after the code has been set up.
|
|
|
|
|
|
|
The command *table star available* will list the available grids with parameters. Some of the lines of the output it generates may look as follows (the example below shows the output produced by Cloudy versions C25.00 RC2 and later):
|
|
|
The command *_table star available*_ will list the available grids with parameters. Some of the lines of the output it generates may look as follows:
|
|
```
|
|
|
|
|
... <snip> ...
|
|
|
```
|
|
File name: obstar_merged_3d.ascii: valid, index file: present.
|
|
|
... <snip> ...
|
|
Grid parameters: ndim: 3 npar: 3 nmods 1082
|
|
|
table star tlusty Ostar 3-dim <Teff> <log(g)> <log(Z)>
|
|
Cloudy command: table star "obstar_merged_3d.ascii" <Teff> <log(g)> <log(Z)>
|
|
|
table star werner <Teff> [ <log(g)> ]
|
|
... <snip> ...
|
|
|
table star wmbasic <Teff> <log(g)> <log(Z)>
|
|
File name: rauch_h-ni_solar.ascii: valid, index file: present.
|
|
|
... <snip> ...
|
|
Grid parameters: ndim: 2 npar: 2 nmods 51
|
|
|
```
|
|
Cloudy command: table star "rauch_h-ni_solar.ascii" <Teff> [ <log(g)> ]
|
|
|
|
|
... <snip> ...
|
|
|
This shows that the _Tlusty_ O star 3-dimensional grid has three parameters, temperature, gravity, and metallicity. The *Werner* star grid has two parameters (the square brackets indicate that the second parameter is optional), and the *WMbasic* grid again has three parameters. This output lists all the grids installed on your computer, excluding any grids that you defined yourself (since Cloudy doesn't know the names you gave to those files).
|
|
```
|
|
|
|
|
|
|
|
Starting with Cloudy C17 the output of the *table star available* command will also list several forms of the *table star hm05* and *table hm12* commands.
|
|
This shows that the merged *Tlusty* O- and B-star 3-dimensional grid has three parameters, temperature, gravity, and metallicity. The *Rauch* grid on the other hand has two parameters (the square brackets indicate that the second parameter is optional). This output lists all the grids that can be found on the search path (Cloudy versions before C25.00 RC2 would exclude any grids that you defined yourself since Cloudy didn't know the names you gave to those files).
|
|
|
These grids differ in certain aspects from the standard stellar atmosphere grids (e.g., they implicitly set the intensity). But they use the same underlying code infrastructure and the data files are fully compatible with standard stellar atmosphere grids. This is why they are included in the output.
|
|
|
|
|
|
|
Starting with Cloudy C17 the output of the *table star available* command will also list several forms of the *table hm05*, *table hm12*, and *table ks19* commands.
|
|
|
The command *table star <grid> list* will list the models contained in that grid.
|
|
These grids differ in certain aspects from the standard stellar atmosphere grids (e.g., they implicitly set the intensity). But they use the same underlying code infrastructure and the data files are fully compatible with standard stellar atmosphere grids. This is why they are included in the output.
|
|
|
The parameter *<grid>* should use the same syntax as given in the output from
|
|
|
|
|
the *table star available* command (without the parameters).
|
|
The command *table star <grid> list* will list the models contained in that grid.
|
|
|
An example would be *table star tlusty Ostar Z+0.3 list*,
|
|
The parameter *<grid>* should use the same syntax as given in the output from
|
|
|
which produces (assuming the grid is installed on your computer):
|
|
the *table star available* command (without the parameters).
|
|
|
|
|
An example would be *table star tlusty Ostar Z+0.3 list*,
|
|
|
```
|
|
which produces (assuming the grid is installed on your computer):
|
|
|
Teff\lg g| 3.00 3.25 3.50 3.75 4.00 4.25 4.50 4.75
|
|
|
|
|
---------|------------------------------------------------
|
|
```
|
|
|
27500 | 1 2 3 4 5 6 7 8
|
|
Teff\lg g| 3.00 3.25 3.50 3.75 4.00 4.25 4.50 4.75
|
|
|
30000 | 9 10 11 12 13 14 15 16
|
|
---------|------------------------------------------------
|
|
|
32500 | -- 17 18 19 20 21 22 23
|
|
27500 | 1 2 3 4 5 6 7 8
|
|
|
35000 | -- 24 25 26 27 28 29 30
|
|
30000 | 9 10 11 12 13 14 15 16
|
|
|
37500 | -- -- 31 32 33 34 35 36
|
|
32500 | -- 17 18 19 20 21 22 23
|
|
|
40000 | -- -- 37 38 39 40 41 42
|
|
35000 | -- 24 25 26 27 28 29 30
|
|
|
42500 | -- -- -- 43 44 45 46 47
|
|
37500 | -- -- 31 32 33 34 35 36
|
|
|
45000 | -- -- -- 48 49 50 51 52
|
|
40000 | -- -- 37 38 39 40 41 42
|
|
|
47500 | -- -- -- 53 54 55 56 57
|
|
42500 | -- -- -- 43 44 45 46 47
|
|
|
50000 | -- -- -- -- 58 59 60 61
|
|
45000 | -- -- -- 48 49 50 51 52
|
|
|
52500 | -- -- -- -- 62 63 64 65
|
|
47500 | -- -- -- 53 54 55 56 57
|
|
|
55000 | -- -- -- -- 66 67 68 69
|
|
50000 | -- -- -- -- 58 59 60 61
|
|
|
```
|
|
52500 | -- -- -- -- 62 63 64 65
|
|
|
|
|
55000 | -- -- -- -- 66 67 68 69
|
|
|
Entries with a number indicate models that are present in the grid. The number is the sequence number in the input file. The command will also work for user-defined grids by supplying the name of the ASCII file between quotes, e.g. *table star "usergrid.ascii" list*.
|
|
```
|
|
|
|
|
|
|
|
|
|
Entries with a number indicate models that are present in the grid. The number is the sequence number in the input file. The command will also work for user-defined grids by supplying the name of the ASCII file between quotes, e.g. *table star "usergrid.ascii" list*.
|
|
|
### Using the grids
|
|
|
|
|
|
|
|
|
|
|
|
### Using the grids
|
|
|
#### Standard grids in Cloudy
|
|
|
|
|
|
|
|
|
|
The *table star available* command which was explained in the previous section will not only list the available grids on your computer, it will also show the correct syntax to include a stellar atmosphere in your simulation. Parameters between pointed brackets must be replaced by actual numbers. A valid example would be *table star tlusty Ostar 3-dim 42300 4.22 -0.73* to get a Tlusty O-star model with Teff = 42,300 K, log g = 4.22, and log Z = -0.73. Parameters between square brackets may be omitted. This is only the case for the log g parameter in 2-dimensional grids. If it is omitted, it will default to the highest log g available in the grid. Hence the commands *table star tlusty Ostar Z+0.3 42300 4.75* and *table star tlusty Ostar Z+0.3 42300*
|
|
#### Standard grids in Cloudy
|
|
|
are both valid and will both produce the exact same model.
|
|
|
|
|
|
|
The *table star available* command which was explained in the previous section will not only list the available grids on your computer, it will also show the correct syntax to include a stellar atmosphere in your simulation. Parameters between pointed brackets must be replaced by actual numbers. A valid example would be *table star "obstar_merged_3d.ascii" 42300 4.22 -0.73* to get a Tlusty model with Teff = 42,300 K, log g = 4.22, and log Z = -0.73. For certain standard grids, the filename between double quotes may be replaced by keywords. For instance, the command *table star tlusty OBStar 3-dim 42300 4.22 -0.73* would produce the exact same model as the command shown above. Parameters between square brackets may be omitted. This is only the case for the log g parameter in 2-dimensional grids. If it is omitted, it will default to the highest log g available in the grid. Hence the commands *table star tlusty Ostar Z+0.3 42300 4.75* and *table star tlusty Ostar Z+0.3 42300* are both valid and will both produce the exact same model.
|
|
|
|
|
|
|
|
#### User-defined grids (including Starburst99, PopStar, and BPASS grids)
|
|
#### User-defined grids (including Starburst99, PopStar, and BPASS grids)
|
|
|
|
|
|
|
|
For user-defined grids a slightly different syntax is used to include them in a simulation: *table star "<yourname.mod>" <par1> <par2> ...*
|
|
For user-defined grids only the syntax with the filename between double quotes is accepted:
|
|
|
The number of parameters supplied must exactly match the number of parameters in the grid.
|
|
*table star "<yourname.ascii>" <par1> <par2> ...*
|
|
|
For grids that were generated from Starburst99 output, there is only a single parameter:
|
|
The number of parameters supplied must exactly match the number of parameters in the grid.
|
|
|
the age. For other grids, there may be more, depending on how the grid was defined by the user.
|
|
For grids that were generated from Starburst99 output, there is only a single parameter:
|
|
|
|
|
the age. For other grids, there may be more, depending on how the grid was defined.
|
|
|
|
|
|
|
|
### Using ASCII files directly
|
|
-------
|
|
|
|
|
|
|
|
We are in the process of removing the need for compiled binary files and allow the code to work directly on the ASCII files. This work is still in progress, but some of the new functionality is already available. Starting with Cloudy version C17 you can use the command *table star "<yourname.ascii>" <par1> <par2> ...* to interpolate directly on the data in the ASCII file and skip the compilation stage. This works well for small grids (roughly 1 to 10 MB in size, depending on the speed of the computer). For large grids, we will likely introduce a new (and optional) form of compilation that is independent of the frequency mesh in Cloudy to help speed up the reading process.
|
|
|
|
|
|
|
## Details about individual stellar grids
|
|
|
Starting with Cloudy C17 we also support the command *table star "<yourname.ascii>" list* to list the contents of an ASCII file. All other *table star* commands still require the use of compiled binary files.
|
|
|
|
|
|
|
The following subsections describe details of each of the standard grids now in the code. People who wish to install all the available grids should download all the ASCII files in our [stars directory](https://data.nublado.org/stars) as well as visit the links shown below in the Tlusty, Rauch, and CoStar sections.
|
|
|
-------
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
## Details about individual stellar grids
|
|
### Atlas grids
|
|
|
|
|
|
|
|
The following subsections describe details of each of the standard grids now in the code. People who wish to install all the available grids should download all the ASCII files in our [stars directory](https://data.nublado.org/stars) as well as visit the links shown below in the Tlusty, Rauch, and CoStar sections.
|
|
[atlas_fp05k2_odfnew.ascii.gz (log Z = +0.5)](https://data.nublado.org/stars/atlas_fp05k2_odfnew.ascii.gz)
|
|
|
|
|
|
|
|
|
|
[atlas_fp02k2_odfnew.ascii.gz (log Z = +0.2)](https://data.nublado.org/stars/atlas_fp02k2_odfnew.ascii.gz)
|
|
|
|
|
|
|
|
### Atlas grids
|
|
[atlas_fp00k2_odfnew.ascii.gz (log Z = +0.0)](https://data.nublado.org/stars/atlas_fp00k2_odfnew.ascii.gz)
|
|
|
|
|
|
|
|
[atlas_fp05k2_odfnew.ascii.gz (log Z = +0.5)](https://data.nublado.org/stars/atlas_fp05k2_odfnew.ascii.gz)
|
|
[atlas_fm05k2_odfnew.ascii.gz (log Z = -0.5)](https://data.nublado.org/stars/atlas_fm05k2_odfnew.ascii.gz)
|
|
|
|
|
|
|
|
[atlas_fp02k2_odfnew.ascii.gz (log Z = +0.2)](https://data.nublado.org/stars/atlas_fp02k2_odfnew.ascii.gz)
|
|
[atlas_fm10k2_odfnew.ascii.gz (log Z = -1.0)](https://data.nublado.org/stars/atlas_fm10k2_odfnew.ascii.gz)
|
|
|
|
|
|
|
|
[atlas_fp00k2_odfnew.ascii.gz (log Z = +0.0)](https://data.nublado.org/stars/atlas_fp00k2_odfnew.ascii.gz)
|
|
[atlas_fm15k2_odfnew.ascii.gz (log Z = -1.5)](https://data.nublado.org/stars/atlas_fm15k2_odfnew.ascii.gz)
|
|
|
|
|
|
|
|
[atlas_fm05k2_odfnew.ascii.gz (log Z = -0.5)](https://data.nublado.org/stars/atlas_fm05k2_odfnew.ascii.gz)
|
|
[atlas_fm20k2_odfnew.ascii.gz (log Z = -2.0)](https://data.nublado.org/stars/atlas_fm20k2_odfnew.ascii.gz)
|
|
|
|
|
|
|
|
[atlas_fm10k2_odfnew.ascii.gz (log Z = -1.0)](https://data.nublado.org/stars/atlas_fm10k2_odfnew.ascii.gz)
|
|
[atlas_fm25k2_odfnew.ascii.gz (log Z = -2.5)](https://data.nublado.org/stars/atlas_fm25k2_odfnew.ascii.gz)
|
|
|
|
|
|
|
|
[atlas_fm15k2_odfnew.ascii.gz (log Z = -1.5)](https://data.nublado.org/stars/atlas_fm15k2_odfnew.ascii.gz)
|
|
|
|
|
|
|
|
|
|
[atlas_fm20k2_odfnew.ascii.gz (log Z = -2.0)](https://data.nublado.org/stars/atlas_fm20k2_odfnew.ascii.gz)
|
|
[atlas_3d_odfnew.ascii.gz (all metallicities)](https://data.nublado.org/stars/atlas_3d_odfnew.ascii.gz)
|
|
|
|
|
|
|
|
[atlas_fm25k2_odfnew.ascii.gz (log Z = -2.5)](https://data.nublado.org/stars/atlas_fm25k2_odfnew.ascii.gz)
|
|
|
|
|
|
|
These are the Castelli & Kurucz
|
|
|
|
|
([Castelli, F., Kurucz R. L. 2004, astro-ph/0405087](http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2004astro.ph..5087C&db_key=PRE&data_type=HTML&format=&high=456aed1c0813147)) LTE, plane-parallel, hydrostatic model atmospheres using the newest opacity distribution functions. The original versions of the files are from the [Kurucz web site](http://kurucz.harvard.edu/grids.html). These grids come in various metallicities, ranging from log Z = +0.5 to -2.5, all with a turbulent velocity of 2 km/s. There is also a single file *atlas_3d_odfnew.ascii.gz* which contains all metallicities and which enables interpolation in log Z. If you download the latter file, *you do not need any of the other odfnew files*, unless you want to run the entire test suite. *The ODFNEW models are the most up-to-date and preferred versions of the Atlas models.*
|
|
|
|
|
|
|
|
[atlas_3d_odfnew.ascii.gz (all metallicities)](https://data.nublado.org/stars/atlas_3d_odfnew.ascii.gz)
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
These are the Castelli & Kurucz
|
|
[atlas_fp10k2.ascii.gz (log Z = +1.0)](https://data.nublado.org/stars/atlas_fp10k2.ascii.gz)
|
|
|
([Castelli, F., Kurucz R. L. 2004, astro-ph/0405087](http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2004astro.ph..5087C&db_key=PRE&data_type=HTML&format=&high=456aed1c0813147)) LTE, plane-parallel, hydrostatic model atmospheres using the newest opacity distribution functions. The original versions of the files are from the [Kurucz web site](http://kurucz.harvard.edu/grids.html). These grids come in various metallicities, ranging from log Z = +0.5 to -2.5, all with a turbulent velocity of 2 km/s. There is also a single file *atlas_3d_odfnew.ascii.gz* which contains all metallicities and which enables interpolation in log Z. If you download the latter file, *you do not need any of the other odfnew files*, unless you want to run the entire test suite. *The ODFNEW models are the most up-to-date and preferred versions of the Atlas models.*
|
|
|
|
|
|
|
[atlas_fp05k2.ascii.gz (log Z = +0.5)](https://data.nublado.org/stars/atlas_fp05k2.ascii.gz)
|
|
|
|
|
|
|
|
|
|
[atlas_fp03k2.ascii.gz (log Z = +0.3)](https://data.nublado.org/stars/atlas_fp03k2.ascii.gz)
|
|
|
|
|
|
|
|
[atlas_fp10k2.ascii.gz (log Z = +1.0)](https://data.nublado.org/stars/atlas_fp10k2.ascii.gz)
|
|
[atlas_fp02k2.ascii.gz (log Z = +0.2)](https://data.nublado.org/stars/atlas_fp02k2.ascii.gz)
|
|
|
|
|
|
|
|
[atlas_fp05k2.ascii.gz (log Z = +0.5)](https://data.nublado.org/stars/atlas_fp05k2.ascii.gz)
|
|
[atlas_fp01k2.ascii.gz (log Z = +0.1)](https://data.nublado.org/stars/atlas_fp01k2.ascii.gz)
|
|
|
|
|
|
|
|
[atlas_fp03k2.ascii.gz (log Z = +0.3)](https://data.nublado.org/stars/atlas_fp03k2.ascii.gz)
|
|
[atlas_fp00k2.ascii.gz (log Z = +0.0)](https://data.nublado.org/stars/atlas_fp00k2.ascii.gz)
|
|
|
|
|
|
|
|
[atlas_fp02k2.ascii.gz (log Z = +0.2)](https://data.nublado.org/stars/atlas_fp02k2.ascii.gz)
|
|
[atlas_fm01k2.ascii.gz (log Z = -0.1)](https://data.nublado.org/stars/atlas_fm01k2.ascii.gz)
|
|
|
|
|
|
|
|
[atlas_fp01k2.ascii.gz (log Z = +0.1)](https://data.nublado.org/stars/atlas_fp01k2.ascii.gz)
|
|
[atlas_fm02k2.ascii.gz (log Z = -0.2)](https://data.nublado.org/stars/atlas_fm02k2.ascii.gz)
|
|
|
|
|
|
|
|
[atlas_fp00k2.ascii.gz (log Z = +0.0)](https://data.nublado.org/stars/atlas_fp00k2.ascii.gz)
|
|
[atlas_fm03k2.ascii.gz (log Z = -0.3)](https://data.nublado.org/stars/atlas_fm03k2.ascii.gz)
|
|
|
|
|
|
|
|
[atlas_fm01k2.ascii.gz (log Z = -0.1)](https://data.nublado.org/stars/atlas_fm01k2.ascii.gz)
|
|
[atlas_fm05k2.ascii.gz (log Z = -0.5)](https://data.nublado.org/stars/atlas_fm05k2.ascii.gz)
|
|
|
|
|
|
|
|
[atlas_fm02k2.ascii.gz (log Z = -0.2)](https://data.nublado.org/stars/atlas_fm02k2.ascii.gz)
|
|
[atlas_fm10k2.ascii.gz (log Z = -1.0)](https://data.nublado.org/stars/atlas_fm10k2.ascii.gz)
|
|
|
|
|
|
|
|
[atlas_fm03k2.ascii.gz (log Z = -0.3)](https://data.nublado.org/stars/atlas_fm03k2.ascii.gz)
|
|
[atlas_fm15k2.ascii.gz (log Z = -1.5)](https://data.nublado.org/stars/atlas_fm15k2.ascii.gz)
|
|
|
|
|
|
|
|
[atlas_fm05k2.ascii.gz (log Z = -0.5)](https://data.nublado.org/stars/atlas_fm05k2.ascii.gz)
|
|
[atlas_fm20k2.ascii.gz (log Z = -2.0)](https://data.nublado.org/stars/atlas_fm20k2.ascii.gz)
|
|
|
|
|
|
|
|
[atlas_fm10k2.ascii.gz (log Z = -1.0)](https://data.nublado.org/stars/atlas_fm10k2.ascii.gz)
|
|
[atlas_fm25k2.ascii.gz (log Z = -2.5)](https://data.nublado.org/stars/atlas_fm25k2.ascii.gz)
|
|
|
|
|
|
|
|
[atlas_fm15k2.ascii.gz (log Z = -1.5)](https://data.nublado.org/stars/atlas_fm15k2.ascii.gz)
|
|
[atlas_fm30k2.ascii.gz (log Z = -3.0)](https://data.nublado.org/stars/atlas_fm30k2.ascii.gz)
|
|
|
|
|
|
|
|
[atlas_fm20k2.ascii.gz (log Z = -2.0)](https://data.nublado.org/stars/atlas_fm20k2.ascii.gz)
|
|
[atlas_fm35k2.ascii.gz (log Z = -3.5)](https://data.nublado.org/stars/atlas_fm35k2.ascii.gz)
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[atlas_fm25k2.ascii.gz (log Z = -2.5)](https://data.nublado.org/stars/atlas_fm25k2.ascii.gz)
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[atlas_fm40k2.ascii.gz (log Z = -4.0)](https://data.nublado.org/stars/atlas_fm40k2.ascii.gz)
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[atlas_fm30k2.ascii.gz (log Z = -3.0)](https://data.nublado.org/stars/atlas_fm30k2.ascii.gz)
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[atlas_fm45k2.ascii.gz (log Z = -4.5)](https://data.nublado.org/stars/atlas_fm45k2.ascii.gz)
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[atlas_fm35k2.ascii.gz (log Z = -3.5)](https://data.nublado.org/stars/atlas_fm35k2.ascii.gz)
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[atlas_fm50k2.ascii.gz (log Z = -5.0)](https://data.nublado.org/stars/atlas_fm50k2.ascii.gz)
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[atlas_fm40k2.ascii.gz (log Z = -4.0)](https://data.nublado.org/stars/atlas_fm40k2.ascii.gz)
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[atlas_fm45k2.ascii.gz (log Z = -4.5)](https://data.nublado.org/stars/atlas_fm45k2.ascii.gz)
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[atlas_3d.ascii.gz (all metallicities)](https://data.nublado.org/stars/atlas_3d.ascii.gz)
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[atlas_fm50k2.ascii.gz (log Z = -5.0)](https://data.nublado.org/stars/atlas_fm50k2.ascii.gz)
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These are the final versions of the original Kurucz (Kurucz, R.L. 1991, in "Proceedings of the Conference on Precision Photometry: Astrophysics of the Galaxy", Eds. A.G.D. Philip, A.R. Upgren and K.A. Janes. Schenectady, NY: Davis Press, p. 27) LTE, plane-parallel, hydrostatic model atmospheres. The original versions of the files are from the [Kurucz web site](http://kurucz.harvard.edu/grids.html). These grids come in various metallicities, ranging from log Z = +1.0 to -5.0, all with a turbulent velocity of 2 km/s. There is also a single file *atlas_3d.ascii.gz* which contains all metallicities and which enables interpolation in log Z. If you download the latter file, *you do not need any of the other files*, unless you want to run the entire test suite. These models are included for backward compatibility and also because they cover a larger range of metallicities. The ODFNEW models further up are the most up-to-date and preferred versions of the Atlas models.
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[atlas_3d.ascii.gz (all metallicities)](https://data.nublado.org/stars/atlas_3d.ascii.gz)
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### Tlusty O and B star grids
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[Tlusty SEDs for Cloudy](http://tlusty.oca.eu/Tlusty2002/tlusty-frames-cloudy.html)
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These are the final versions of the original Kurucz (Kurucz, R.L. 1991, in "Proceedings of the Conference on Precision Photometry: Astrophysics of the Galaxy", Eds. A.G.D. Philip, A.R. Upgren and K.A. Janes. Schenectady, NY: Davis Press, p. 27) LTE, plane-parallel, hydrostatic model atmospheres. The original versions of the files are from the [Kurucz web site](http://kurucz.harvard.edu/grids.html). These grids come in various metallicities, ranging from log Z = +1.0 to -5.0, all with a turbulent velocity of 2 km/s. There is also a single file *atlas_3d.ascii.gz* which contains all metallicities and which enables interpolation in log Z. If you download the latter file, *you do not need any of the other files*, unless you want to run the entire test suite. These models are included for backward compatibility and also because they cover a larger range of metallicities. The ODFNEW models further up are the most up-to-date and preferred versions of the Atlas models.
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The [Tlusty](http://tlusty.oca.eu/) code is maintained by Ivan Hubeny & Thierry Lanz. They have produced extensive grids of non-LTE, line-blanketed, plane-parallel, hydrostatic O, and B star SEDs. The [_SEDs for Cloudy_](http://tlusty.oca.eu/Tlusty2002/tlusty-frames-cloudy.html) link on their main web site gives links to the files we use.
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### Tlusty O and B star grids
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There are 11 sets of O star SEDs compiled from the [OSTAR2002 grid](http://tlusty.oca.eu/Tlusty2002/tlusty-frames-OS02.html) with names "ostar2002_*.ascii.gz". They are described in the reference [Lanz, T., & Hubeny, I. 2003, ApJS, 146, 417](http://adsabs.harvard.edu/cgi-bin/nph-bib_query?2003ApJS..146..417L&db_key=AST). These SEDs are used by the *stars_ostar2002\*.in* simulations in the test suite.
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[Tlusty SEDs for Cloudy](http://tlusty.oca.eu/Tlusty2002/tlusty-frames-cloudy.html)
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There are 7 sets of B star SEDs compiled from the [BSTAR2006 grid](http://tlusty.oca.eu/Tlusty2002/tlusty-frames-BS06.html) with names *bstar2006\*.ascii.gz*. They are described in the reference [Lanz, T., & Hubeny, I. 2007, ApJS, 169, 83](http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=2007ApJS..169...83L&db_key=AST&data_type=HTML&format=&high=45d30ec84024291). These SEDs are used by the *stars_bstar2006\*.in* simulations in the test suite.
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The [Tlusty](http://tlusty.oca.eu/) code is maintained by Ivan Hubeny & Thierry Lanz. They have produced extensive grids of non-LTE, line-blanketed, plane-parallel, hydrostatic O, and B star SEDs. The [_SEDs for Cloudy_](http://tlusty.oca.eu/Tlusty2002/tlusty-frames-cloudy.html) link on their main web site gives links to the files we use.
|
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Starting with the C10 release of Cloudy, we have added support for merged OSTAR2002/BSTAR2006 grids. The resulting grids have a temperature coverage from 15 to 55 kK. In the overlap region between 27.5 and 30 kK, the BSTAR2006 models have been adopted. The merged grids have been produced for all metallicities supported by the BSTAR2006 grid. They have names *obstar\_merged\*.ascii.gz*. When you use one of these grids, you should cite both [Lanz, T., & Hubeny, I. 2003, ApJS, 146, 417](http://adsabs.harvard.edu/cgi-bin/nph-bib_query?2003ApJS..146..417L&db_key=AST) and [Lanz, T., & Hubeny, I. 2007, ApJS, 169, 83](http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=2007ApJS..169...83L&db_key=AST&data_type=HTML&format=&high=45d30ec84024291).
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These SEDs are used by the *stars\_obstar\_merged\*.in* simulations in the test suite.
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There are 11 sets of O star SEDs compiled from the [OSTAR2002 grid](http://tlusty.oca.eu/Tlusty2002/tlusty-frames-OS02.html) with names "ostar2002_*.ascii.gz". They are described in the reference [Lanz, T., & Hubeny, I. 2003, ApJS, 146, 417](http://adsabs.harvard.edu/cgi-bin/nph-bib_query?2003ApJS..146..417L&db_key=AST). These SEDs are used by the *stars_ostar2002\*.in* simulations in the test suite.
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In general, you will not need all the files listed on the Tlusty website (unless you want to run the entire test suite cleanly) and you will have a couple of choices. If you are only interested in solar metallicity stars then one of the *ostar2002_p00.ascii.gz*, *bstar2006_p00.ascii.gz* or *obstar_merged\_p00.ascii.gz* files are enough. If you want to interpolate in metallicity you will need one of the *ostar2002_3d.ascii.gz*, *bstar2006_3d.ascii.gz* or *obstar\_merged_3d.ascii.gz* files, but none of the other ones. If you want to run models at other metallicities, but not interpolate in metallicity, you can choose from the remaining files.
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There are 7 sets of B star SEDs compiled from the [BSTAR2006 grid](http://tlusty.oca.eu/Tlusty2002/tlusty-frames-BS06.html) with names *bstar2006\*.ascii.gz*. They are described in the reference [Lanz, T., & Hubeny, I. 2007, ApJS, 169, 83](http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=2007ApJS..169...83L&db_key=AST&data_type=HTML&format=&high=45d30ec84024291). These SEDs are used by the *stars_bstar2006\*.in* simulations in the test suite.
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Starting with the C10 release of Cloudy, we have added support for merged OSTAR2002/BSTAR2006 grids. The resulting grids have a temperature coverage from 15 to 55 kK. In the overlap region between 27.5 and 30 kK, the BSTAR2006 models have been adopted. The merged grids have been produced for all metallicities supported by the BSTAR2006 grid. They have names *obstar\_merged\*.ascii.gz*. When you use one of these grids, you should cite both [Lanz, T., & Hubeny, I. 2003, ApJS, 146, 417](http://adsabs.harvard.edu/cgi-bin/nph-bib_query?2003ApJS..146..417L&db_key=AST) and [Lanz, T., & Hubeny, I. 2007, ApJS, 169, 83](http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=2007ApJS..169...83L&db_key=AST&data_type=HTML&format=&high=45d30ec84024291).
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### WMbasic O and B stars
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These SEDs are used by the *stars\_obstar\_merged\*.in* simulations in the test suite.
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[wmbasic.ascii.gz](https://data.nublado.org/stars/wmbasic.ascii.gz).
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In general, you will not need all the files listed on the Tlusty website (unless you want to run the entire test suite cleanly) and you will have a couple of choices. If you are only interested in solar metallicity stars then one of the *ostar2002_p00.ascii.gz*, *bstar2006_p00.ascii.gz* or *obstar_merged\_p00.ascii.gz* files are enough. If you want to interpolate in metallicity you will need one of the *ostar2002_3d.ascii.gz*, *bstar2006_3d.ascii.gz* or *obstar\_merged_3d.ascii.gz* files, but none of the other ones. If you want to run models at other metallicities, but not interpolate in metallicity, you can choose from the remaining files.
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The WMbasic code was maintained by [Adi Pauldrach](http://www.usm.uni-muenchen.de/people/adi/Programs/Contact.html) who still has a home page [here](http://www.usm.uni-muenchen.de/people/adi/adi.html). He computed a small grid of non-LTE, line-blanketed, and wind-blanketed hot stars with metallicities log Z = 0.0 and -0.3. The original grid of models is [here](http://www.usm.uni-muenchen.de/people/adi/Models/Model.html) and is described in
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### WMbasic O and B stars
|
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[Pauldrach et al., 2001](http://www.usm.uni-muenchen.de/people/adi/Programs/Summary.html#History). The grid has been rebinned to create the file that is available above.
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This is a three-dimensional grid so you must specify temperature, log g, and log Z, in that order.
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[wmbasic.ascii.gz](https://data.nublado.org/stars/wmbasic.ascii.gz).
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### CoStar O and B stars
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The WMbasic code was maintained by [Adi Pauldrach](http://www.usm.uni-muenchen.de/people/adi/Programs/Contact.html) who still has a home page [here](http://www.usm.uni-muenchen.de/people/adi/adi.html). He computed a small grid of non-LTE, line-blanketed, and wind-blanketed hot stars with metallicities log Z = 0.0 and -0.3. The original grid of models is [here](http://www.usm.uni-muenchen.de/people/adi/Models/Model.html) and is described in
|
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[Pauldrach et al., 2001](http://www.usm.uni-muenchen.de/people/adi/Programs/Summary.html#History). The grid has been rebinned to create the file that is available above.
|
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These grids of non-LTE, line blanketed model atmospheres including stellar winds have been developed by Daniel Schaerer and are described in [Schaerer, D., & de Koter, A. 1997, A&A, 322, 598](http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=1997A%26A...322..598S&db_key=AST&data_type=HTML&format=&high=45b49b8de123609). There are two abundance sets, halo and solar. They are available from the [STScI web site](http://www.stsci.edu/science/starburst99/docs/SdK96/). You need the files Sc1_costar_z020_lb.fluxes (solar abundances) and Sc1_costar_z004_lb.fluxes (halo abundances).
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This is a three-dimensional grid so you must specify temperature, log g, and log Z, in that order.
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### Rauch PN Nuclei
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### CoStar O and B stars
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[Thomas Rauch](http://astro.uni-tuebingen.de/~rauch/) has developed several grids of non-LTE, line-blanketed, plane-parallel, hydrostatic model atmospheres for central stars of planetary nebulae (CSPN). Each of those grids will be discussed separately below. The grids are described in [Rauch, T. 2003, A&A, 403, 709](http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=2003A%26A...403..709R&db_key=AST&data_type=HTML&format=&high=45b49b8de106294).
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|
These grids of non-LTE, line blanketed model atmospheres including stellar winds have been developed by Daniel Schaerer and are described in [Schaerer, D., & de Koter, A. 1997, A&A, 322, 598](http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=1997A%26A...322..598S&db_key=AST&data_type=HTML&format=&high=45b49b8de123609). There are two abundance sets, halo and solar. They are available from the [STScI web site](http://www.stsci.edu/science/starburst99/docs/SdK96/). You need the files Sc1_costar_z020_lb.fluxes (solar abundances) and Sc1_costar_z004_lb.fluxes (halo abundances).
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#### The H-Ni grid
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### Rauch PN Nuclei
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[The H-Ni grid](http://astro.uni-tuebingen.de/~rauch/NLTE/H-Ni/TTTTTTT_GG_H-Ni.tgz)
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|
[Thomas Rauch](http://astro.uni-tuebingen.de/~rauch/) has developed several grids of non-LTE, line-blanketed, plane-parallel, hydrostatic model atmospheres for central stars of planetary nebulae (CSPN). Each of those grids will be discussed separately below. The grids are described in [Rauch, T. 2003, A&A, 403, 709](http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=2003A%26A...403..709R&db_key=AST&data_type=HTML&format=&high=45b49b8de106294).
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This is the main grid of CSPN model atmospheres. It is described [here](http://astro.uni-tuebingen.de/~rauch/TMAF/flux_H-Ni.html). The reference for this grid is [Rauch, T. 2003, A&A, 403, 709](http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=2003A%26A...403..709R&db_key=AST&data_type=HTML&format=&high=45b49b8de106294). It consists of a set of models ranging between Teff = 50 and 190 kK and log g = 5 and 8. There are two grids included in this file, one for solar abundances (log Z = 0.0) and one for halo abundances (log Z = -1.0). The models treat line blanketing for all elements up to calcium as well as iron group elements. Cloudy will create three ASCII files out of this data set: one for the solar abundance grid, one for the halo grid, and a 3-dimensional grid that allows interpolation in log Z.
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#### The H-Ni grid
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[The H-Ni grid](http://astro.uni-tuebingen.de/~rauch/NLTE/H-Ni/TTTTTTT_GG_H-Ni.tgz)
|
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#### The H-Ca grid
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[The H-Ca grid](http://astro.uni-tuebingen.de/~rauch/NLTE/H-Ca/TTTTTTT_GG_H-Ca_final_bin_0.1.tgz)
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|
|
This is the main grid of CSPN model atmospheres. It is described [here](http://astro.uni-tuebingen.de/~rauch/TMAF/flux_H-Ni.html). The reference for this grid is [Rauch, T. 2003, A&A, 403, 709](http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=2003A%26A...403..709R&db_key=AST&data_type=HTML&format=&high=45b49b8de106294). It consists of a set of models ranging between Teff = 50 and 190 kK and log g = 5 and 8. There are two grids included in this file, one for solar abundances (log Z = 0.0) and one for halo abundances (log Z = -1.0). The models treat line blanketing for all elements up to calcium as well as iron group elements. Cloudy will create three ASCII files out of this data set: one for the solar abundance grid, one for the halo grid, and a 3-dimensional grid that allows interpolation in log Z.
|
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This is an earlier version of the H-Ni grid that only treats line blanketing by elements upto calcium. It is described [here](http://astro.uni-tuebingen.de/~rauch/TMAF/flux_H-Ca.html). The reference for this grid is [Rauch, T. 1997, A&A 320, 237](http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=1997A%26A...320..237R&db_key=AST&data_type=HTML&format=&high=45d30ec84029599). _For most purposes it is superseded by the H-Ni grid shown above_. However, it consists of a set of models ranging between Teff = 50 and 1000 kK and log g = 5 and 9 and therefore covers a larger parameter space than the H-Ni grid. There are two grids included in this file, one for solar abundances (log Z = 0.0) and one for halo abundances (log Z = -1.0). Cloudy will create three ASCII files out of this data set: one for the solar abundance grid, one for the halo grid, and a 3-dimensional grid that allows interpolation in log Z.
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#### The H-Ca grid
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[The H-Ca grid](http://astro.uni-tuebingen.de/~rauch/NLTE/H-Ca/TTTTTTT_GG_H-Ca_final_bin_0.1.tgz)
|
|
#### The PG1159 grid (aka He+C+N+O)
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[The PG1159 grid](http://astro.uni-tuebingen.de/~rauch/NLTE/He+C+N+O/TTTTTTT_GGGG_33_50_02_15_00005-02000A.tgz)
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This is an earlier version of the H-Ni grid that only treats line blanketing by elements upto calcium. It is described [here](http://astro.uni-tuebingen.de/~rauch/TMAF/flux_H-Ca.html). The reference for this grid is [Rauch, T. 1997, A&A 320, 237](http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=1997A%26A...320..237R&db_key=AST&data_type=HTML&format=&high=45d30ec84029599). _For most purposes it is superseded by the H-Ni grid shown above_. However, it consists of a set of models ranging between Teff = 50 and 1000 kK and log g = 5 and 9 and therefore covers a larger parameter space than the H-Ni grid. There are two grids included in this file, one for solar abundances (log Z = 0.0) and one for halo abundances (log Z = -1.0). Cloudy will create three ASCII files out of this data set: one for the solar abundance grid, one for the halo grid, and a 3-dimensional grid that allows interpolation in log Z.
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This is a grid specifically designed for hydrogen-deficient central stars of PNe. It treats an atmosphere consisting only of He and CNO. It is described [here](http://astro.uni-tuebingen.de/~rauch/TMAF/flux_He+C+N+O.html). The reference for this grid is [Rauch, T. 2003, A&A, 403, 709](http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=2003A%26A...403..709R&db_key=AST&data_type=HTML&format=&high=45b49b8de106294). It consists of a set of models ranging between Teff = 40 and 190 kK and log g = 5 and 9.
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#### The PG1159 grid (aka He+C+N+O)
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[The PG1159 grid](http://astro.uni-tuebingen.de/~rauch/NLTE/He+C+N+O/TTTTTTT_GGGG_33_50_02_15_00005-02000A.tgz)
|
|
#### The C/O white dwarf grid (aka C+O+Ne+Mg)
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[rauch_cowd.ascii.gz](https://data.nublado.org/stars/rauch_cowd.ascii.gz)
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This is a grid specifically designed for hydrogen-deficient central stars of PNe. It treats an atmosphere consisting only of He and CNO. It is described [here](http://astro.uni-tuebingen.de/~rauch/TMAF/flux_He+C+N+O.html). The reference for this grid is [Rauch, T. 2003, A&A, 403, 709](http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=2003A%26A...403..709R&db_key=AST&data_type=HTML&format=&high=45b49b8de106294). It consists of a set of models ranging between Teff = 40 and 190 kK and log g = 5 and 9.
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This is a small grid specifically designed for helium-deficient central stars. It treats an atmosphere consisting only of C, O, Ne, and Mg. It is described [here](http://astro.uni-tuebingen.de/~rauch/TMAF/flux_C+O+Ne+Mg.html). The model atmospheres have been downloaded using [TheoSSA](http://vo.ari.uni-heidelberg.de/ssatr-0.01/TrSpectra.jsp?) and have been converted to the Cloudy format. The resulting file rauch_cowd.ascii.gz provided above should be downloaded for use with Cloudy. A paper describing the grid will be submitted in the near future. The grid contains a set of models ranging between Teff = 170 and 250 kK and log g = 8.
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#### The C/O white dwarf grid (aka C+O+Ne+Mg)
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#### The pure hydrogen grid
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[rauch_cowd.ascii.gz](https://data.nublado.org/stars/rauch_cowd.ascii.gz)
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[The hydrogen grid](http://astro.uni-tuebingen.de/~rauch/NLTE/H/TTTTTTT_GGGG_H_00005-02000A.tgz)
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|
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This is a small grid specifically designed for helium-deficient central stars. It treats an atmosphere consisting only of C, O, Ne, and Mg. It is described [here](http://astro.uni-tuebingen.de/~rauch/TMAF/flux_C+O+Ne+Mg.html). The model atmospheres have been downloaded using [TheoSSA](http://vo.ari.uni-heidelberg.de/ssatr-0.01/TrSpectra.jsp?) and have been converted to the Cloudy format. The resulting file rauch_cowd.ascii.gz provided above should be downloaded for use with Cloudy. A paper describing the grid will be submitted in the near future. The grid contains a set of models ranging between Teff = 170 and 250 kK and log g = 8.
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This is a grid of pure hydrogen model atmospheres. It is described [here](http://astro.uni-tuebingen.de/~rauch/TMAF/flux_H.html). It consists of a set of models ranging between Teff = 20 and 1000 kK and log g = 4 and 9. Hence it covers a larger parameter space than any of the other grids.
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#### The pure hydrogen grid
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[The hydrogen grid](http://astro.uni-tuebingen.de/~rauch/NLTE/H/TTTTTTT_GGGG_H_00005-02000A.tgz)
|
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#### The pure helium grid
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[The helium grid](http://astro.uni-tuebingen.de/~rauch/NLTE/He/TTTTTTT_GGGG_He_00005-02000A.tgz)
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This is a grid of pure hydrogen model atmospheres. It is described [here](http://astro.uni-tuebingen.de/~rauch/TMAF/flux_H.html). It consists of a set of models ranging between Teff = 20 and 1000 kK and log g = 4 and 9. Hence it covers a larger parameter space than any of the other grids.
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This is a grid of pure helium model atmospheres. It is described [here](http://astro.uni-tuebingen.de/~rauch/TMAF/flux_He.html). It consists of a set of models ranging between Teff = 50 and 1000 kK and log g = 5 and 9.
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#### The pure helium grid
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[The helium grid](http://astro.uni-tuebingen.de/~rauch/NLTE/He/TTTTTTT_GGGG_He_00005-02000A.tgz)
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#### The H+He grid
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[The H+He grid](http://astro.uni-tuebingen.de/~rauch/NLTE/H+He/TTTTTTT_GGGG_H+He_X.XXX_Y.YYY_00005-02000A.tgz)
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|
This is a grid of pure helium model atmospheres. It is described [here](http://astro.uni-tuebingen.de/~rauch/TMAF/flux_He.html). It consists of a set of models ranging between Teff = 50 and 1000 kK and log g = 5 and 9.
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This is a huge 3-dimensional grid of model atmospheres consisting of hydrogen and helium. The helium fraction (by mass) can be set by the user. It is described [here](http://astro.uni-tuebingen.de/~rauch/TMAF/flux_H+He.html). It consists of a set of models ranging between Teff = 50 and 190 kK, log g = 5 and 9, and the H/He abundance ratio by mass between 1e9/1 and 1/1e9.
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#### The H+He grid
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[The H+He grid](http://astro.uni-tuebingen.de/~rauch/NLTE/H+He/TTTTTTT_GGGG_H+He_X.XXX_Y.YYY_00005-02000A.tgz)
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### The Haardt & Madau grids
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These grids give the cosmic ultraviolet background radiation as a function of redshift. The necessary data files are included in the Cloudy distribution by default, so no separate download is necessary. They were calculated with the [CUBA code](http://www.ucolick.org/~pmadau/CUBA/HOME.html). Three versions are available: from 1996, 2005, and 2012. The first data set gives the background for a single redshift, while the latter two give a grid of SEDs as a function of redshift. Since Cloudy version C17, the 2005 and 2012 data sets are implemented using the stellar atmosphere grid infrastructure. These grids differ in certain aspects from the standard stellar atmosphere grids (e.g., they implicitly set the intensity) which is why they have a separate command syntax: *table hm96*, *table hm05*, and *table hm12*. See Hazy 1 for further details. The first two data sets are described in [Haardt & Madau (1996) ApJ 461, 20](http://arxiv.org/abs/astro-ph/9509093). The 2012 grid is described in [Haardt & Madau (2012) ApJ 746, 125](http://arxiv.org/abs/1105.2039).
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This is a huge 3-dimensional grid of model atmospheres consisting of hydrogen and helium. The helium fraction (by mass) can be set by the user. It is described [here](http://astro.uni-tuebingen.de/~rauch/TMAF/flux_H+He.html). It consists of a set of models ranging between Teff = 50 and 190 kK, log g = 5 and 9, and the H/He abundance ratio by mass between 1e9/1 and 1/1e9.
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### The Khaire & Srianand grids
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### The Haardt & Madau grids
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These grids provide the extragalactic background radiation at any redshift between z = 0 and 15. The necessary data files are included in the Cloudy distribution by default, so no separate download is necessary. They work very similarly to the Haardt & Madau grids described above, except that an additional (optional) Q parameter may be needed. These grids differ from the standard stellar atmosphere grids as described in the previous section and they also have a separate command syntax: *table ks18* (in version C17) and *table ks19* (in all later versions). See Hazy 1 for further details. The grids are described in [Khaire & Srianand (2019) MNRAS 484, 4174](http://adsabs.harvard.edu/abs/2019MNRAS.484.4174K).
|
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|
These grids give the cosmic ultraviolet background radiation as a function of redshift. The necessary data files are included in the Cloudy distribution by default, so no separate download is necessary. They were calculated with the [CUBA code](http://www.ucolick.org/~pmadau/CUBA/HOME.html). Three versions are available: from 1996, 2005, and 2012. The first data set gives the background for a single redshift, while the latter two give a grid of SEDs as a function of redshift. Since Cloudy version C17, the 2005 and 2012 data sets are implemented using the stellar atmosphere grid infrastructure. These grids differ in certain aspects from the standard stellar atmosphere grids (e.g., they implicitly set the intensity) which is why they have a separate command syntax: *table hm96*, *table hm05*, and *table hm12*. See Hazy 1 for further details. The first two data sets are described in [Haardt & Madau (1996) ApJ 461, 20](http://arxiv.org/abs/astro-ph/9509093). The 2012 grid is described in [Haardt & Madau (2012) ApJ 746, 125](http://arxiv.org/abs/1105.2039).
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----
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### The Khaire & Srianand grids
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### Historic and test grids
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|
These grids provide the extragalactic background radiation at any redshift between z = 0 and 15. The necessary data files are included in the Cloudy distribution by default, so no separate download is necessary. They work very similarly to the Haardt & Madau grids described above, except that an additional (optional) Q parameter may be needed. These grids differ from the standard stellar atmosphere grids as described in the previous section and they also have a separate command syntax: *table ks18* (in version C17) and *table ks19* (in all later versions). See Hazy 1 for further details. The grids are described in [Khaire & Srianand (2019) MNRAS 484, 4174](http://adsabs.harvard.edu/abs/2019MNRAS.484.4174K).
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The remaining grids below are only used for testing purposes (Starburst99) or have been obsoleted by newer grids (Kurucz79, Mihalas, Werner). They are only needed for backward compatibility or if you want to run the entire test suite. *Please do not use the grids below for any new scientific research.*
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----
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#### Starburst99
|
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### Historic and test grids
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[starburst99.ascii.gz](https://data.nublado.org/stars/starburst99.ascii.gz).
|
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|
The remaining grids below are only used for testing purposes (Starburst99) or have been obsoleted by newer grids (Kurucz79, Mihalas, Werner). They are only needed for backward compatibility or if you want to run the entire test suite. *Please do not use the grids below for any new scientific research.*
|
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|
[starburst99_2d.ascii.gz](https://data.nublado.org/stars/starburst99_2d.ascii.gz).
|
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#### Starburst99
|
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The original file was created with the Starburst99 code, as described
|
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[starburst99.ascii.gz](https://data.nublado.org/stars/starburst99.ascii.gz).
|
|
[here](http://www.stsci.edu/science/starburst99/).
|
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|
|
This file is used by the Cloudy test suite to assure that access to the Starburst99 files still works correctly. It serves no other purpose.
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|
[starburst99_2d.ascii.gz](https://data.nublado.org/stars/starburst99_2d.ascii.gz).
|
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The *starburst99_2d.ascii* file was produced by Christophe Morisset by manually joining several Starburst99 runs with different metallicities into a single 2D grid.
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This enables interpolation in both age and metallicity.
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|
The original file was created with the Starburst99 code, as described
|
|
This file is used to test that this works correctly. It serves no other purpose.
|
|
|
[here](http://www.stsci.edu/science/starburst99/).
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|
|
This file is used by the Cloudy test suite to assure that access to the Starburst99 files still works correctly. It serves no other purpose.
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|
#### Kurucz79 O stars
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|
|
The *starburst99_2d.ascii* file was produced by Christophe Morisset by manually joining several Starburst99 runs with different metallicities into a single 2D grid.
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|
|
This enables interpolation in both age and metallicity.
|
|
[kurucz79.ascii.gz](https://data.nublado.org/stars/kurucz79.ascii.gz).
|
|
|
This file is used to test that this works correctly. It serves no other purpose.
|
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|
|
This is a subset of the Kurucz ([Kurucz, R. L. 1979, ApJS, 40, 1](http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=1979ApJS...40....1K&db_key=AST&data_type=HTML&format=&high=454351ce9528041)) grid of stellar SEDs. They have solar metallicity, log g = 4.0 or 4.5, and temperatures between 30,000 K and 50,000 K. This grid has been obsoleted by the Atlas ODFNEW grids listed above and is only maintained for backward compatibility.
|
|
|
#### Kurucz79 O stars
|
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|
|
|
[kurucz79.ascii.gz](https://data.nublado.org/stars/kurucz79.ascii.gz).
|
|
#### Mihalas NLTE hot stars
|
|
|
|
|
|
|
|
|
|
[mihalas.ascii.gz](https://data.nublado.org/stars/mihalas.ascii.gz).
|
|
|
This is a subset of the Kurucz ([Kurucz, R. L. 1979, ApJS, 40, 1](http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=1979ApJS...40....1K&db_key=AST&data_type=HTML&format=&high=454351ce9528041)) grid of stellar SEDs. They have solar metallicity, log g = 4.0 or 4.5, and temperatures between 30,000 K and 50,000 K. This grid has been obsoleted by the Atlas ODFNEW grids listed above and is only maintained for backward compatibility.
|
|
|
|
|
|
|
|
|
|
|
|
This is a subset of the Mihalas (Mihalas, D. 1972, Non-LTE Model Atmospheres for B & O Stars, NCAR-TN/STR-76) non-LTE O and B star SEDs. They have log g = 4.0. The temperature range is from 30,000 K to 55,000 K. This grid has been obsoleted by the Tlusty, WMbasic, and CoStar non-LTE grids listed above and is only maintained for backward compatibility.
|
|
|
#### Mihalas NLTE hot stars
|
|
|
|
|
|
|
|
|
|
[mihalas.ascii.gz](https://data.nublado.org/stars/mihalas.ascii.gz).
|
|
#### Werner PN Nuclei
|
|
|
|
|
|
|
|
|
|
[kwerner.ascii.gz](https://data.nublado.org/stars/kwerner.ascii.gz).
|
|
|
This is a subset of the Mihalas (Mihalas, D. 1972, Non-LTE Model Atmospheres for B & O Stars, NCAR-TN/STR-76) non-LTE O and B star SEDs. They have log g = 4.0. The temperature range is from 30,000 K to 55,000 K. This grid has been obsoleted by the Tlusty, WMbasic, and CoStar non-LTE grids listed above and is only maintained for backward compatibility.
|
|
|
|
|
|
|
|
|
|
|
|
This is the Werner & Heber [Werner, K., & Heber, U. 1991, in *Stellar Atmospheres: Beyond Classical Models*, p 341, NATO ASI Series C, eds. L. Crivellari, I. Hubney, & D. G. Hummer, (Dordrect: Kluwer)] grid of non-LTE planetary nebula nuclei model atmospheres. This grid has been obsoleted by the Rauch non-LTE grids listed above and is only maintained for backward compatibility.
|
|
|
#### Werner PN Nuclei
|
|
|
|
|
|
|
------
|
|
|
[kwerner.ascii.gz](https://data.nublado.org/stars/kwerner.ascii.gz).
|
|
|
|
|
|
|
Running the [TestSuite](TestSuite) is the next step
|
|
|
|
|
|
|
|
This is the Werner & Heber [Werner, K., & Heber, U. 1991, in *Stellar Atmospheres: Beyond Classical Models*, p 341, NATO ASI Series C, eds. L. Crivellari, I. Hubney, & D. G. Hummer, (Dordrect: Kluwer)] grid of non-LTE planetary nebula nuclei model atmospheres. This grid has been obsoleted by the Rauch non-LTE grids listed above and is only maintained for backward compatibility.
|
|
Return to the [CompileStars](CompileStars) page
|
|
|
|
|
|
|
|
------
|
|
Return to the [StepByStep](StepByStep) instructions or go [home](home)
|
|
|
|
|
|
|
|
Running the [TestSuite](TestSuite) is the next step
|
|
----- |
|
|
|
|
|
|
|
Return to the [CompileStars](CompileStars) page
|
|
|
|
|
|
|
|
|
|
Return to the [StepByStep](StepByStep) instructions or go [home](home)
|
|
|
|
|
|
|
|
|
|
----- |
|
|
