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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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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 is 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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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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... | ... | @@ -362,7 +362,7 @@ These grids of non-LTE, line blanketed model atmospheres including stellar winds |
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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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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 upto 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 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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... | ... | @@ -370,7 +370,7 @@ This is the main grid of CSPN model atmospheres. It is described [here](http://a |
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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 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 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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... | ... | @@ -414,12 +414,12 @@ This is a huge 3-dimensional grid of model atmospheres consisting of hydrogen an |
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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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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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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 similar 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 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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... | ... | @@ -436,9 +436,13 @@ The remaining grids below are only used for testing purposes (Starburst99) or ha |
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[starburst99_2d.ascii.gz](https://data.nublado.org/stars/starburst99_2d.ascii.gz).
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The original file was created with the Starburst99 code, as described [here](http://www.stsci.edu/science/starburst99/). 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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The original file was created with the Starburst99 code, as described
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[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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The starburst99_2d.ascii file was produced by Christophe Morisset by manually joining several Starburst99 runs with different metallicities into a single 2D grid. This enables interpolation in both age and metallicity. This file is used to test that this works correctly. It serves no other purpose.
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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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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.ascii.gz](https://data.nublado.org/stars/kurucz79.ascii.gz).
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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 betweeen 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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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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... | ... | @@ -462,7 +466,7 @@ This is a subset of the Mihalas (Mihalas, D. 1972, Non-LTE Model Atmospheres for |
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[kwerner.ascii.gz](https://data.nublado.org/stars/kwerner.ascii.gz).
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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.
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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.
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------
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... | ... | |