cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.5281/zenodo.4755012
title: Correlated k coefficients for H2-He atmospheres; 180 spectral windows and 1060 pressure-temperature points

description: There are 72 correlated k-coefficients datasets, using the naming convention m-xxx_coyyy.data.180.tar.zip, where xxx is the metallicity in dex relative to solar, and yyy is the C/O ratio relative to solar, as a multiplication factor. For example a metallicity of 0.0 and a C/O ratio of 1.0 indicates solar abundances. We use the Lodders et al. 2010 value for the solar C/O=0.458. The spectral windows are listed in the file 180_windows.txt (intervals defined as starting at lambda1 and ending at lambda2), and the k-coefficients can be read in and checked using the script in the IDL code read_k_coefficients.pro. The k-coefficients are calculated for a grid of 1060 pressure-temperature points listed in the file PT_list_1060.

The correlated-k coefficients are calculated using pre-mixed opacities, where the abundances for each metallicity-C/O combination have been calculated using equilibrium chemistry, as described in Marley et al. 2021. There are 12 Fe/H values: 0.0, 0.5, 0.7, 1.0, 1.5, 1.5, 1.7, 2.0, -0.25, -0.3, -0.5, -0.75, and -1.0; and 6 C/O values: 0.25, 0.5, 1.0, 1.5, 2.0 and 2.5.

 The opacity sources included in the calculations are: C2H2, C2H4, C2H6, CH4, CO, CO2, CrH, FeH, H2O, H2S, HCN, LiCl, MgH, N2,  NH3, OCS, PH3, SiO, TiO, and VO, in addition to alkali metals (Li, Na, K, Rb, Cs). The references for the line lists and broadening parameters used in these opacity calculations can also be found in Marley et al 2021, and are included here for convenience in the file Table_2_Marley_et.al.2021.png Please include these references, as well as the reference to this Zenodo repository when publishing your paper.

Each dataset contains the following files:

ascii_data: the correlated k coefficients file in ascii format. This can be read by the included IDL code.

binary_data: the correlated k coefficients file in binary format

cp_all: contains the mean molecular weight for each layer. The head capacity values do not include the proper H2 heat capacity and should not be used.

full_abunds: the relative abundances for all the species from the chemistry files, on the 1060-point pressure-temperature grid.

sum_in_atoms: relative abundances for the alkali metals

sum_in_cia: relative abundances for the species that could be used for calculating collision-induced absorption (CIA)

sum_in_layer: relative abundances for all molecules included in the correlated k-coefficients calculations

Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center.
DOI: 10.5281/zenodo.6476019
title: Opacities for atoms and molecules relevant to the spectra of hot rocky planets

description: This dataset contains opacities for atoms and molecules that are relevant to the sector of hot rocky planets, such as magma ocean planets, post-giant impact atmospheres, or planets in ultra-short period orbits. These species can arise above a magma ocean with a composition specific to the continental crust or bulk silicate earth. We do not include opacities for major species that are not specific to hot rocky planet atmospheres, such as water, methane, carbon dioxide, ammonia, etc., as these can be found elsewhere, for example in datasets related to brown dwarf and hot Jupiter atmospheres. 

Most of the species included in this dataset can be seen in the attached plot, hot_spectra.pdf, which shows a secondary eclipse model of a lava planet and the contributions of individual species to this spectrum. The references for the line lists used to generate these opacities can be found in the file reference_table.pdf.

Each *.zip file contains a set of 1060 opacity layers in ASCII format, each identified with the temperature and pressure it corresponds to. Each layer file contains a header showing the layer number, the temperature (in K), and pressure (in mbar). The data consists of to columns: wavelength in microns and opacity in cm2/molecule. The wavelength grid goes from 0.4 to 50 microns. A list of all the layers calculated for each molecule is given in the file layer_list.

Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center.
DOI: 10.5281/zenodo.6476020
title: Opacities for atoms and molecules relevant to the spectra of hot rocky planets

description: This dataset contains opacities for atoms and molecules that are relevant to the sector of hot rocky planets, such as magma ocean planets, post-giant impact atmospheres, or planets in ultra-short period orbits. These species can arise above a magma ocean with a composition specific to the continental crust or bulk silicate earth. We do not include opacities for major species that are not specific to hot rocky planet atmospheres, such as water, methane, carbon dioxide, ammonia, etc., as these can be found elsewhere, for example in datasets related to brown dwarf and hot Jupiter atmospheres. 

Most of the species included in this dataset can be seen in the attached plot, hot_spectra.pdf, which shows a secondary eclipse model of a lava planet and the contributions of individual species to this spectrum. The references for the line lists used to generate these opacities can be found in the file reference_table.pdf.

Each *.zip file contains a set of 1060 opacity layers in ASCII format, each identified with the temperature and pressure it corresponds to. Each layer file contains a header showing the layer number, the temperature (in K), and pressure (in mbar). The data consists of to columns: wavelength in microns and opacity in cm2/molecule. The wavelength grid goes from 0.4 to 50 microns. A list of all the layers calculated for each molecule is given in the file layer_list.

Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center.
DOI: 10.15468/dl.7k42fq
title: Occurrence Download

description: A dataset containing 57050 species occurrences available in GBIF matching the query:
{
 "and" : [
 "DatasetKey is UTA Reptiles",
 "TaxonKey is Squamata"
 ]
}

 The dataset includes 57050 records from 1 constituent datasets; see https://api.gbif.org/v1/occurrence/download/0002476-250127130748423/datasets/export for details.
 
Data from some individual datasets included in this download may be licensed under less restrictive terms.
DOI: 10.5281/zenodo.6600975
title: High resolution opacities for H2/He atmospheres

description: This set of molecular and atomic opacities has been built based on the same opacity sources used for calculating the correlated-k coefficients in the following repositories:

10.5281/zenodo.5590997 (11 windows)

10.5281/zenodo.5590995 (30 windows)

10.5281/zenodo.5590986 (180 windows)

10.5281/zenodo.5590989 (196 windows)

These opacities can be used to generate high resolution spectra for the atmospheric structures computed with the correlated-k coefficients above.

The set includes C2H2, C2H4, C2H6, CH4, CO, CO2, CrH, Fe, FeH, H2, H3+, H2O, H2S, HCN, LiCl, LiF, LiH, MgH, N2, NH3, OCS, PH3, SiO, TiO, and VO, in addition to alkali metals (Li, Na, K, Rb, Cs). The opacities are calculated for a grid of 1460 pressure-temperature points, from10^−6 to 3000 bar and from 75 to 4000 K, listed in the file 1460_layer_list. Each *.zip file contains one opacity file for each pressure-temperature layer, with the species’ name, the pressure, and the temperature given in the filename. The opacity is given in units of cm^2/molecule. For completeness, each *.zip file also contains a file named wavelengths.txt, listing the wavelengths corresponding to each opacity point, in units of microns. All the opacities are calculated on the same wavelength grid. 

The references for the line lists used in these opacity calculations can be found in the file Opacity_references_2021.pdf. Please include these references, as well as the reference to this Zenodo repository when publishing your paper. 

Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center.
DOI: 10.5281/zenodo.4710968
title: Correlated k coefficients for H2-He atmospheres; 11 spectral windows and 1060 pressure-temperature points

description: There are 72 correlated k-coefficients datasets, using the naming convention m-xxx_coyyy.data.11.tar.zip, where xxx is the metallicity in dex relative to solar, and yyy is the C/O ratio relative to solar, as a multiplication factor. For example a metallicity of 0.0 and a C/O ratio of 1.0 indicates solar abundances. There are an additional 10 datasets that do not include the TiO and VO opacities, as indicated by the "_noTiOVO" designation in the file name. We use the Lodders et al. 2010 value for the solar C/O=0.458. The spectral windows are listed in the file 11_windows.txt (intervals defined as starting at lambda1 and ending at lambda2), and the k-coefficients can be read in and checked using the script in the IDL code read_k_coefficients.pro. The k-coefficients are calculated for a grid of 1060 pressure-temperature points listed in the file PT_list_1060.

The correlated-k coefficients are calculated using pre-mixed opacities, where the abundances for each metallicity-C/O combination have been calculated using equilibrium chemistry, as described in Marley et al. 2021. There are 12 Fe/H values: 0.0, 0.5, 0.7, 1.0, 1.5, 1.5, 1.7, 2.0, -0.25, -0.3, -0.5, -0.75, and -1.0; and 6 C/O values: 0.25, 0.5, 1.0, 1.5, 2.0 and 2.5.

 The opacity sources included in the calculations are: C2H2, C2H4, C2H6, CH4, CO, CO2, CrH, FeH, H2O, H2S, HCN, LiCl, MgH, N2,  NH3, OCS, PH3, SiO, TiO, and VO, in addition to alkali metals (Li, Na, K, Rb, Cs). The references for the line lists and broadening parameters used in these opacity calculations can also be found in Marley et al 2021, and are included here for convenience in the file Table_2_Marley_et.al.2021.png

Each dataset contains the following files:

ascii_data: the correlated k coefficients file in ascii format. This can be read by the included IDL code.

binary_data: the correlated k coefficients file in binary format

cp_all: contains the mean molecular weight for each layer. The head capacity values do not include the proper H2 heat capacity and should not be used.

full_abunds: the relative abundances for all the species from the chemistry files, on the 1060-point pressure-temperature grid.

sum_in_atoms: relative abundances for the alkali metals

sum_in_cia: relative abundances for the species that could be used for calculating collision-induced absorption (CIA)

sum_in_layer: relative abundances for all molecules included in the correlated k-coefficients calculations

Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center.
DOI: 10.5281/zenodo.4710969
title: Correlated k coefficients for H2-He atmospheres; 11 spectral windows and 1060 pressure-temperature points

description: There are 72 correlated k-coefficients datasets, using the naming convention m-xxx_coyyy.data.11.tar.zip, where xxx is the metallicity in dex relative to solar, and yyy is the C/O ratio relative to solar, as a multiplication factor. For example a metallicity of 0.0 and a C/O ratio of 1.0 indicates solar abundances. We use the Lodders et al. 2010 value for the solar C/O=0.458. The spectral windows are listed in the file 11_windows.txt (intervals defined as starting at lambda1 and ending at lambda2), and the k-coefficients can be read in and checked using the script in the IDL code read_k_coefficients.pro. The k-coefficients are calculated for a grid of 1060 pressure-temperature points listed in the file PT_list_1060. The correlated-k coefficients are calculated using pre-mixed opacities, where the abundances for each metallicity-C/O combination have been calculated using equilibrium chemistry, as described in Marley et al. 2021. There are 12 Fe/H values: 0.0, 0.5, 0.7, 1.0, 1.5, 1.5, 1.7, 2.0, -0.25, -0.3, -0.5, -0.75, and -1.0; and 6 C/O values: 0.25, 0.5, 1.0, 1.5, 2.0 and 2.5. The opacity sources included in the calculations are: C2H2, C2H4, C2H6, CH4, CO, CO2, CrH, FeH, H2O, H2S, HCN, LiCl, MgH, N2, NH3, OCS, PH3, SiO, TiO, and VO, in addition to alkali metals (Li, Na, K, Rb, Cs). The references for the line lists and broadening parameters used in these opacity calculations can also be found in Marley et al 2021, and are included here for convenience in the file Table_2_Marley_et.al.2021.png Each dataset contains the following files: ascii_data: the correlated k coefficients file in ascii format. This can be read by the included IDL code. binary_data: the correlated k coefficients file in binary format cp_all: contains the mean molecular weight for each layer. The head capacity values do not include the proper H2 heat capacity and should not be used. full_abunds: the relative abundances for all the species from the chemistry files, on the 1060-point pressure-temperature grid. sum_in_atoms: relative abundances for the alkali metals sum_in_cia: relative abundances for the species that could be used for calculating collision-induced absorption (CIA) sum_in_layer: relative abundances for all molecules included in the correlated k-coefficients calculations
description: {"references": ["Marley, M et al. (2021)"]}
DOI: 10.5281/zenodo.6707793
title: Correlated k coefficients for H2-He atmospheres; 11 spectral windows and 1060 pressure-temperature points

description: There are 72 correlated k-coefficients datasets, using the naming convention m-xxx_coyyy.data.11.tar.zip, where xxx is the metallicity in dex relative to solar, and yyy is the C/O ratio relative to solar, as a multiplication factor. For example a metallicity of 0.0 and a C/O ratio of 1.0 indicates solar abundances. There are an additional 10 datasets that do not include the TiO and VO opacities, as indicated by the "_noTiOVO" designation in the file name. We use the Lodders et al. 2010 value for the solar C/O=0.458. The spectral windows are listed in the file 11_windows.txt (intervals defined as starting at lambda1 and ending at lambda2), and the k-coefficients can be read in and checked using the script in the IDL code read_k_coefficients.pro. The k-coefficients are calculated for a grid of 1060 pressure-temperature points listed in the file PT_list_1060.

The correlated-k coefficients are calculated using pre-mixed opacities, where the abundances for each metallicity-C/O combination have been calculated using equilibrium chemistry, as described in Marley et al. 2021. There are 12 Fe/H values: 0.0, 0.5, 0.7, 1.0, 1.5, 1.5, 1.7, 2.0, -0.25, -0.3, -0.5, -0.75, and -1.0; and 6 C/O values: 0.25, 0.5, 1.0, 1.5, 2.0 and 2.5.

 The opacity sources included in the calculations are: C2H2, C2H4, C2H6, CH4, CO, CO2, CrH, FeH, H2O, H2S, HCN, LiCl, MgH, N2,  NH3, OCS, PH3, SiO, TiO, and VO, in addition to alkali metals (Li, Na, K, Rb, Cs). The references for the line lists and broadening parameters used in these opacity calculations can also be found in Marley et al 2021, and are included here for convenience in the file Table_2_Marley_et.al.2021.png

Each dataset contains the following files:

ascii_data: the correlated k coefficients file in ascii format. This can be read by the included IDL code.

binary_data: the correlated k coefficients file in binary format

cp_all: contains the mean molecular weight for each layer. The head capacity values do not include the proper H2 heat capacity and should not be used.

full_abunds: the relative abundances for all the species from the chemistry files, on the 1060-point pressure-temperature grid.

sum_in_atoms: relative abundances for the alkali metals

sum_in_cia: relative abundances for the species that could be used for calculating collision-induced absorption (CIA)

sum_in_layer: relative abundances for all molecules included in the correlated k-coefficients calculations

Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center.
DOI: 10.5281/zenodo.4755387
title: Correlated k coefficients for H2-He atmospheres; 196 spectral windows and 1060 pressure-temperature points

description: There are 72 correlated k-coefficients datasets, using the naming convention m-xxx_coyyy.data.196.tar.zip, where xxx is the metallicity in dex relative to solar, and yyy is the C/O ratio relative to solar, as a multiplication factor. For example a metallicity of 0.0 and a C/O ratio of 1.0 indicates solar abundances. There are an additional 5 datasets that do not include the TiO and VO opacities, as indicated by the "_noTiOVO" designation in the file name. We use the Lodders et al. 2010 value for the solar C/O=0.458. The spectral windows are listed in the file 196_windows.txt (intervals defined as starting at lambda1 and ending at lambda2), and the k-coefficients can be read in and checked using the script in the IDL code read_k_coefficients.pro. The k-coefficients are calculated for a grid of 1060 pressure-temperature points listed in the file PT_list_1060.

The correlated-k coefficients are calculated using pre-mixed opacities, where the abundances for each metallicity-C/O combination have been calculated using equilibrium chemistry, as described in Marley et al. 2021. There are 12 Fe/H values: 0.0, 0.5, 0.7, 1.0, 1.5, 1.5, 1.7, 2.0, -0.25, -0.3, -0.5, -0.75, and -1.0; and 6 C/O values: 0.25, 0.5, 1.0, 1.5, 2.0 and 2.5.

 The opacity sources included in the calculations are: C2H2, C2H4, C2H6, CH4, CO, CO2, CrH, FeH, H2O, H2S, HCN, LiCl, MgH, N2,  NH3, OCS, PH3, SiO, TiO, and VO, in addition to alkali metals (Li, Na, K, Rb, Cs). The references for the line lists and broadening parameters used in these opacity calculations can also be found in Marley et al 2021, and are included here for convenience in the file Table_2_Marley_et.al.2021.png

Each dataset contains the following files:

ascii_data: the correlated k coefficients file in ascii format. This can be read by the included IDL code.

binary_data: the correlated k coefficients file in binary format

cp_all: contains the mean molecular weight for each layer. The head capacity values do not include the proper H2 heat capacity and should not be used.

full_abunds: the relative abundances for all the species from the chemistry files, on the 1060-point pressure-temperature grid.

sum_in_atoms: relative abundances for the alkali metals

sum_in_cia: relative abundances for the species that could be used for calculating collision-induced absorption (CIA)

sum_in_layer: relative abundances for all molecules included in the correlated k-coefficients calculations

Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center.
DOI: 10.5281/zenodo.4755388
title: Correlated k coefficients for H2-He atmospheres; 196 spectral windows and 1060 pressure-temperature points

description: There are 72 correlated k-coefficients datasets, using the naming convention m-xxx_coyyy.data.196.tar.zip, where xxx is the metallicity in dex relative to solar, and yyy is the C/O ratio relative to solar, as a multiplication factor. For example a metallicity of 0.0 and a C/O ratio of 1.0 indicates solar abundances. We use the Lodders et al. 2010 value for the solar C/O=0.458. The spectral windows are listed in the file 196_windows.txt (intervals defined as starting at lambda1 and ending at lambda2), and the k-coefficients can be read in and checked using the script in the IDL code read_k_coefficients.pro. The k-coefficients are calculated for a grid of 1060 pressure-temperature points listed in the file PT_list_1060. The correlated-k coefficients are calculated using pre-mixed opacities, where the abundances for each metallicity-C/O combination have been calculated using equilibrium chemistry, as described in Marley et al. 2021. There are 12 Fe/H values: 0.0, 0.5, 0.7, 1.0, 1.5, 1.5, 1.7, 2.0, -0.25, -0.3, -0.5, -0.75, and -1.0; and 6 C/O values: 0.25, 0.5, 1.0, 1.5, 2.0 and 2.5. The opacity sources included in the calculations are: C2H2, C2H4, C2H6, CH4, CO, CO2, CrH, FeH, H2O, H2S, HCN, LiCl, MgH, N2, NH3, OCS, PH3, SiO, TiO, and VO, in addition to alkali metals (Li, Na, K, Rb, Cs). The references for the line lists and broadening parameters used in these opacity calculations can also be found in Marley et al 2021, and are included here for convenience in the file Table_2_Marley_et.al.2021.png Each dataset contains the following files: ascii_data: the correlated k coefficients file in ascii format. This can be read by the included IDL code. binary_data: the correlated k coefficients file in binary format cp_all: contains the mean molecular weight for each layer. The head capacity values do not include the proper H2 heat capacity and should not be used. full_abunds: the relative abundances for all the species from the chemistry files, on the 1060-point pressure-temperature grid. sum_in_atoms: relative abundances for the alkali metals sum_in_cia: relative abundances for the species that could be used for calculating collision-induced absorption (CIA) sum_in_layer: relative abundances for all molecules included in the correlated k-coefficients calculations
description: {"references": ["Marley et al. (2021)"]}