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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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## Future changes
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### Future changes
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In Cloudy versions up to and including C17, the code was set up in such a way that in order to compile the stellar atmosphere grids they had to reside in the local directory. On the other hand, when you wanted to use the compiled grids, they had to be in the data directory. So either you had to move the compiled files into the data directory, or place the downloaded ascii files in the data directory in the first place. After C17, the rules for searching input files will be the same for all commands, which includes the stellar grids. This means that both during compilation and when using the grids during a run, the files are searched along the entire search path. That implies that during compilation the code will find ascii files in other locations (such as the data directory) as long as they are on the search path. On the other hand, during a run the code will be able to use a compiled atmosphere grid that is stored in the local directory. This gives the user more freedom to organize the files.
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... | ... | @@ -13,10 +13,10 @@ The page below describes the situation as it exists for C17. The changes describ |
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------
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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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... | ... | @@ -30,7 +30,7 @@ The following sections describe how to download the original ASCII stellar SED f |
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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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## 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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... | ... | @@ -52,7 +52,7 @@ There may be a great many of them, and they are still contained in the tarballs |
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5) 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 data directory and simply go through the same procedure outlined above. Cloudy will skip any grids for which it finds a valid mod file in the data directory (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/). This uses the common code base for stellar atmosphere grids and therefore need to be compiled just like any other grid. 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.mod*. Keep the ASCII file as you will need it in the next version of Cloudy. To use the Starburst99 grid in a simulation, simply include the command *table star "<yourname.mod>" <age>*.
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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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The PopStar models can be obtained [here](http://www.fractal-es.com/PopStar/).
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Click on "Download Models" on the left-hand side, and 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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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 importing the v2.0 grids that can be downloaded [here](http://bpass.auckland.ac.nz/2.html) under the header "SEDs", as well as the v2.1 grids that are available [here](http://bpass.auckland.ac.nz/8.html). The grids are available as tarballs for several different choices of the initial mass function. The tarball contains grids assuming 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 grids has separate models for single-star and binary-star evolution. Grids are available for a range of metallicities ranging from Z=0.001 to 0.040 (v2.0) or Z=0.00001 to 0.040 (v2.1). The first step is to download one or more of the tarballs from the BPASS website. Next you run the script [convert_bpassv2.x.pl](https://data.nublado.org/stars/convert_bpassv2.x.pl) (make sure that the file has execute permission). Below we describe the process for a BPASS v2.0 grid:
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... | ... | @@ -154,12 +154,12 @@ As was already mentioned above, continuous star formation files are no longer pr |
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This version of the grid is described in [Eldridge et al. (2017)](https://arxiv.org/abs/1710.02154)
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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 included in the file [vanhoof_atmosphere_grids.pdf](../tree/master/trunk/docs/vanhoof_atmosphere_grids.pdf?format=raw) which is also included as 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 compile, issue the command *compile stars "<yourname.ascii>"*. To use it, issue the command *table star "<yourname.mod>" <par1> <par2> ...* (the number of parameters here should exactly match the number of parameters you defined in the grid).
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## If you don't set up all the stellar SED grids
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### If you don't set up all the stellar SED grids
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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.
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... | ... | @@ -168,7 +168,7 @@ The test suite includes a number of test cases that are designed to check that t |
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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.
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## How to find out which grids you have installed
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### How to find out which grids you have installed
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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.
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... | ... | @@ -213,16 +213,16 @@ Teff\lg g| 3.00 3.25 3.50 3.75 4.00 4.25 4.50 4.75 |
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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 mod file between quotes, e.g. *table star "usergrid.mod" list*.
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## Using the grids
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### Using the grids
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### Standard grids in Cloudy
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#### Standard grids in Cloudy
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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*
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are both valid and will both produce the exact same model.
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### User-defined grids (including Starburst99 and PopStar grids)
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#### User-defined grids (including Starburst99 and PopStar grids)
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For user-defined grids a slightly different syntax is used to include them in a simulation: *table star "<yourname.mod>" <par1> <par2> ...*
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The number of parameters supplied must exactly match the number of parameters in the grid.
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the age. For other grids, there may be more, depending on how the grid was defined by the user.
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## Using ASCII files directly
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### Using ASCII files directly
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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.
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... | ... | @@ -239,13 +239,13 @@ Starting with Cloudy C17 we also support the command *table star "<yourname.asci |
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-------
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# Details about individual stellar grids
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## Details about individual stellar grids
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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.
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## Atlas grids
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### Atlas grids
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[atlas_fp05k2_odfnew.ascii.gz (log Z = +0.5)](https://data.nublado.org/stars/atlas_fp05k2_odfnew.ascii.gz)
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... | ... | @@ -320,7 +320,7 @@ These are the Castelli & Kurucz |
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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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## Tlusty O and B star grids
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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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... | ... | @@ -337,7 +337,7 @@ These SEDs are used by the *stars\_obstar\_merged\*.in* simulations in the test |
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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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## WMbasic O and B stars
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### WMbasic O and B stars
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[wmbasic.ascii.gz](https://data.nublado.org/stars/wmbasic.ascii.gz).
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... | ... | @@ -347,17 +347,17 @@ The WMbasic code is maintained by [Adi Pauldrach](http://www.usm.uni-muenchen.de |
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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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## CoStar O and B stars
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### CoStar O and B stars
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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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## Rauch PN Nuclei
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### Rauch PN Nuclei
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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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### The H-Ni grid
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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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... | ... | @@ -365,7 +365,7 @@ These grids of non-LTE, line blanketed model atmospheres including stellar winds |
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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-Ca grid
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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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... | ... | @@ -373,7 +373,7 @@ This is the main grid of CSPN model atmospheres. It is described [here](http://a |
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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 PG1159 grid (aka He+C+N+O)
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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)
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... | ... | @@ -381,14 +381,14 @@ This is an earlier version of the H-Ni grid that only treats line blanketing by |
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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 C/O white dwarf grid (aka C+O+Ne+Mg)
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#### 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 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 pure hydrogen grid
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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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... | ... | @@ -396,7 +396,7 @@ This is a small grid specifically designed for helium-deficient central stars. I |
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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 helium grid
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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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... | ... | @@ -404,7 +404,7 @@ This is a grid of pure hydrogen model atmospheres. It is described [here](http:/ |
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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 H+He grid
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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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... | ... | @@ -412,24 +412,24 @@ This is a grid of pure helium model atmospheres. It is described [here](http://a |
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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 Haardt & Madau grids
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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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## The Khaire & Srianand grids
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### The Khaire & Srianand 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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----
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## Historic and test grids
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### Historic and test grids
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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
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#### Starburst99
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[starburst99.ascii.gz](https://data.nublado.org/stars/starburst99.ascii.gz).
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... | ... | @@ -445,7 +445,7 @@ This enables interpolation in both age and metallicity. |
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This file is used to test that this works correctly. It serves no other purpose.
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### Kurucz79 O stars
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#### Kurucz79 O stars
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[kurucz79.ascii.gz](https://data.nublado.org/stars/kurucz79.ascii.gz).
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... | ... | @@ -453,7 +453,7 @@ 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.
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### Mihalas NLTE hot stars
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#### Mihalas NLTE hot stars
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[mihalas.ascii.gz](https://data.nublado.org/stars/mihalas.ascii.gz).
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... | ... | @@ -461,7 +461,7 @@ This is a subset of the Kurucz ([Kurucz, R. L. 1979, ApJS, 40, 1](http://adsabs. |
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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.
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### Werner PN Nuclei
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#### Werner PN Nuclei
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[kwerner.ascii.gz](https://data.nublado.org/stars/kwerner.ascii.gz).
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... | ... | |