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was never intended to be supported. This is now checked and the code will abort when this is attempted. The reason for this change is that saving files outside the local directory does not work in grid runs.
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The restriction to NKRD (4000) input lines has been removed. Also the restriction on the input line length (was 2000 characters) has been removed. The code now accepts an arbitrary number of input lines of arbitrary length.
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The restriction to NKRD (4000) input lines has been removed. Also, the restriction on the input line length (was 2000 characters) has been removed. The code now accepts an arbitrary number of input lines of arbitrary length.
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The parser now supports line disambiguation. The Cloudy line stack may contain seemingly duplicate entries with the same label and wavelength, but which are actually different lines. This can create problems if you want to use such a line in a command like _save line list_. One example is the H I 4.65247 micron line, which may be either the 7 -> 5 or the 35 -> 7 line. You can now optionally supply the lower and upper level index, or the energy of the lower level, to indicate which line you want. The _save line labels_ output contains the necessary information to do this. This new syntax is supported by the _save lines emissivity, save line list, set blend, print line sum, table lines, monitor line_, and _optimize lines_ commands. It is also supported by the subroutines cdLine(), cdEmis(), and cdGetLineList(). This type of disambiguation is not possible for all lines on the line stack. See Hazy for further information. The code will print a warning when you use a line that is ambiguous.
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The parser now supports line disambiguation. The Cloudy line stack may contain seemingly duplicate entries with the same label and wavelength, but which are actually different lines. This can create problems if you want to use such a line in a command like _save line list_. One example is the H I 4.65247 micron line, which may be either the 7 -> 5 or the 35 -> 7 line. You can now optionally supply the lower and upper-level index, or the energy of the lower level, to indicate which line you want. The _save line labels_ output contains the necessary information to do this. This new syntax is supported by the _save lines emissivity, save line list, set blend, print line sum, table lines, monitor line_, and _optimize lines_ commands. It is also supported by the subroutines cdLine(), cdEmis(), and cdGetLineList(). This type of disambiguation is not possible for all lines on the line stack. See Hazy for further information. The code will print a warning when you use a line that is ambiguous.
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## Changed commands or options
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We have incorporated the [Jenkins 2009](https://ui.adsabs.harvard.edu/abs/2009ApJ...700.1299J/abstract) empirical fit to interstellar deletions. The new command `metals deplete Jenkins2009 Fstar=0.5` command will interpolate on his fits to generate consistent metal depletions.
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We have incorporated the [Jenkins 2009](https://ui.adsabs.harvard.edu/abs/2009ApJ...700.1299J/abstract) empirical fit to interstellar deletions. The new command `metals deplete Jenkins2009 Fstar=0.5` will interpolate on his fits to generate consistent metal depletions.
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The executable now accepts the `-e` option which allows you to supply Cloudy commands directly on the command line, e.g.
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... | ... | @@ -117,7 +117,6 @@ A new command \`\`no absorption escape'' has been introduced to ignore absorptio |
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A new command \`\`no scattering escape'' has been introduced to ignore scattering of photons off of thermal electrons.
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Please find the links to the the first three papers of the series “X-ray spectroscopy in the microcalorimeter era”, which described the improvements mentioned above:
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[https://iopscience.iop.org/article/10.3847/1538-4357/abaaab](https://iopscience.iop.org/article/10.3847/1538-4357/abaaab)
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... | ... | @@ -126,17 +125,17 @@ Please find the links to the the first three papers of the series “X-ray spect |
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[https://iopscience.iop.org/article/10.3847/1538-4357/abed4a](https://iopscience.iop.org/article/10.3847/1538-4357/abed4a)
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## The atomic, molecular, and grain database
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The molecular hydrogen level energies, which we use to derive line wavelengths, have been updated to Komasa (2011). This results in small (about one wavenumber) changes in level energies.
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We now use the Lique 2015 H - H,,2,, collisional data by default. Compared with previous calculations, these data extend to higher vibrational manifolds and include ortho-para changing reactive collisions. Tests show that the 2.121 micron line intensity changes by roughly 50%, becoming stronger in some PDR sims.
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Gargi Shaw has _updated some of the UMIST chemistry, H2, and LAMDA molecular emission models._ The treatment or ArH+ has been improved significantly. This work is described in Shaw, Ferland & Chatzikos ApJ submitted 2021.
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We now use the Lique 2015 H - H<sub>2</sub> collisional data by default. Compared with previous calculations, these data extend to higher vibrational manifolds and include ortho-para changing reactive collisions. Tests show that the 2.121 micron line intensity changes by roughly 50%, becoming stronger in some PDR sims.
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Fe III collision strengths are updated to Badnell and Balance 2014. We had previously used data from Zhang 1996. Tests show that the total Fe III cooling increases by nearly 50%.
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In c17.02 a bug had been fixed that could lead to a failed sanity check when running with a very high resolution frequency mesh. As a result the photoionization thresholds got a slightly different energy. In this release also _the radiative recombination continuum entries on the line stack have a slightly different wavelength_ to make them consistent with the new threshold values.
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In c17.02 a bug had been fixed that could lead to a failed sanity check when running with a very high-resolution frequency mesh. As a result the photoionization thresholds got a slightly different energy. In this release also _the radiative recombination continuum entries on the line stack have a slightly different wavelength_ to make them consistent with the new threshold values.
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The refractive index data for astronomical silicate and graphite from Draine, 2003, ApJ, 598, 1026 have been added. These can be found in the files sdraine03.rfi and gdraine03.rfi.
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