Find research datasets worth reusing
Search datasets from major research repositories and use ShareScore to quickly assess how well each record supports discovery, access, and reuse.
16
datasets available to search
ShareScore release 0.9.0
Dataset results
16 results for “atmospheric H2”
Reconstruction of atmospheric H2 from Greenland and Antarctic firn air
<p>This data set contains:</p> <ol> <li>firn air depth profiles of H<sub>2</sub> from 4 polar sites (South Pole and Megadunes in Antarctica) and NEEM and Summit in Greenland used to by Patterson et al., in press to reconstruct the history of atmospheric H<sub>2</sub> </li> <li>Matlab code for the UCI firn air model and data used in the reconstructions </li> </ol> <p>Reference: Patterson, J. D., Aydin, M., Crotwell, A. M., Pétron, G., Severinghaus, J. P., Krummel, P. B., Langenfelds, R. L., Petrenko, V. V., and Saltzman, E. S.: Reconstructing atmospheric H<sub>2</sub> over the past century from bi-polar firn air records, Clim. Past, https://doi.org/10.5194/cp-2023-27, in press.</p> <p>Note: The firn air depth profiles archived here are processed to remove outliers and average replicates. For raw data, please contact the laboratories at which the measurements were made (G. Petron, GML/NOAA; P. Krummel; CSIRO). </p>
Correlated k coefficients for H2-He atmospheres; 196 spectral windows and 1060 pressure-temperature points
<p>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.</p> <p>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.</p> <p> 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</p> <p>Each dataset contains the following files:</p> <p>ascii_data: the correlated k coefficients file in ascii format. This can be read by the included IDL code.</p> <p>binary_data: the correlated k coefficients file in binary format</p> <p>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.</p> <p>full_abunds: the relative abundances for all the species from the chemistry files, on the 1060-point pressure-temperature grid.</p> <p>sum_in_atoms: relative abundances for the alkali metals</p> <p>sum_in_cia: relative abundances for the species that could be used for calculating collision-induced absorption (CIA)</p> <p>sum_in_layer: relative abundances for all molecules included in the correlated k-coefficients calculations</p> <p><em>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.</em></p>
Correlated k coefficients for H2-He atmospheres; 11 spectral windows and 1060 pressure-temperature points
<p>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.</p> <p>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.</p> <p> 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</p> <p>Each dataset contains the following files:</p> <p>ascii_data: the correlated k coefficients file in ascii format. This can be read by the included IDL code.</p> <p>binary_data: the correlated k coefficients file in binary format</p> <p>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.</p> <p>full_abunds: the relative abundances for all the species from the chemistry files, on the 1060-point pressure-temperature grid.</p> <p>sum_in_atoms: relative abundances for the alkali metals</p> <p>sum_in_cia: relative abundances for the species that could be used for calculating collision-induced absorption (CIA)</p> <p>sum_in_layer: relative abundances for all molecules included in the correlated k-coefficients calculations</p> <p><em>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.</em></p>
Reconstruction of atmospheric H2 from Greenland and Antarctic firn air
Open the record for dataset details and reuse information.
Correlated k coefficients for H2-He atmospheres; 622 spectral windows and 1460 pressure-temperature points
<p>There are 10 correlated k-coefficients datasets, using the naming convention sonora_2020_fehxxxx_co_yyy.data.622.tar.gz (5 models) or sonora_2020_fehxxxx_co_yyy_noTiOVO.data.622.tar.gz (5 models), where xxxx is the metallicity in 10x dex relative to solar, and yyy is the 100x C/O ratio relative to solar, as a multiplication factor. For example a metallicity of +000 and a C/O ratio of 100 indicates solar abundances, feh+070 should be read as a metallicity of +0.7 dex, feh-100 as -1.0 dex, co_100 should be read as 1x C/O relative to solar. We use the Lodders et al. 2010 value for the solar C/O=0.458. The files with “noTiOVO” in the filename contain the correlated k-coefficients calculated without the opacity of TiO and VO. The rest of the molecular abundances and opacities are the same as the equilibrium chemistry values in the regular files. These files are useful for calculating models without any TiO- and VO-induced temperature inversion in the atmosphere.</p> <p>The correlated-k coefficients are calculated using pre-mixed opacities, with abundances given by equilibrium chemistry for each metallicity-C/O combination, as described in Marley et al. 2021. There are 5 Fe/H values: 0.0, 0.5, 0.7, 1.0, and -0.3; and 1 C/O value: 1.0x solar. The k-coefficients 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, and can be read in using the IDL script read_k_coefficients.pro. The spectral windows are listed in the file 622_windows.txt (intervals defined as starting at lambda1 and ending at lambda2).</p> <p>The opacity sources included in the calculations are: 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 corresponding high resolution opacities for these atoms and molecules can be found in the Zenodo repository 10.5281/zenodo.6600976. The references for the line lists used in these opacity calculations are listed in the file Opacity_references_2021.pdf. Please include these references, as well as the reference to this Zenodo repository when publishing your paper.</p> <p>Each dataset contains the following files:</p> <p>ascii_data: the correlated k coefficients file in ascii format. This can be read by the included IDL code.</p> <p>binary_data: the correlated k coefficients file in binary format</p> <p>full_abunds: the relative abundances for all the species from the chemistry files, on the 1460-point pressure-temperature grid</p> <p>sum_in_atoms: relative abundances for the alkali metals</p> <p>sum_in_layer: relative abundances for all molecules included in the correlated k-coefficients calculations</p> <p><em>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.</em></p>
Correlated-k table for H2 dominated atmospheres for 3D Climate Modelling
<p>Correlated-k table for H2 dominated atmospheres with a variable amount of water vapour built by incorporating absorption data files from the HITRAN database and using the exo\_k code by J.Leconte. This correlated-k tables are created to use with Generic-PCM model to simulate the atmospheres of H2 dominated planets.</p> <p>The calculation of radiative transfer can be performed using the correlated-k method, which efficiently determines net radiative fluxes by categorizing spectral lines into infrared and visible bands (IR x VI) and assigning the average absorption coefficients to each band. These coefficients are pre-calculated based on detailed line-by-line radiative transfer calculations. The correlated-k method is an economic alternative to the line-by-line method, making it possible to accurately and rapidly compute atmospheric radiation.</p> <p> </p>
Limits of the Habitable Zone for H2 atmosphere with 3D climate Modelling
<p>Water is crucial for life, regardless of the environment. That's why in search of extraterrestrial life, we focus on planets in the habitable zone (HZ), where liquid water can exist. The size of this zone depends on factors like the star type and planet size. Using the Generic PCM model (https://lmdz-forge.lmd.jussieu.fr/mediawiki/Planets/index.php/Overview_of_the_Generic_PCM), we've defined the limits of the HZ for atmospheres dominated by H2 in 3D for the first time. You can access the dataset from the simulations in ".nc" file format. Temporal evolution of variables such as surface temperature, surface pressure, water vapour, liquid water, ice etc. are in a 3D grid for different orbital distances and with different surface pressures are present in the dataset. We have used the correlated-k table published in Zenodo for the simulations (https://doi.org/10.5281/zenodo.10978762).</p>
Chondritic reactivity under H2-rich atmospheres: Formation of H2S. Computational Data.
<p>This supporting material includes:</p> <ul> <li>Cartesian coordinates of the PBE-optimized minima and transition states for the studied reactions, provided in both XYZ and CIF formats.</li> <li>Examples of input and output files used with the <a href="https://www.cp2k.org/">CP2K</a> package.</li> <li>Vibrational analysis, including all calculated frequencies.</li> </ul>
Correlated k coefficients for H2-He atmospheres; 196 spectral windows and 1460 pressure-temperature points
<p>There are 108 correlated k-coefficients datasets, using the naming convention sonora_2020_fehxxxx_co_yyy.data.196.tar.gz (78 models) or sonora_2020_fehxxxx_co_yyy_noTiOVO.data.196.tar.gz (78 models), where xxxx is the metallicity in 10x dex relative to solar, and yyy is the 100x C/O ratio relative to solar, as a multiplication factor. For example a metallicity of +000 and a C/O ratio of 100 indicates solar abundances, feh+070 should be read as a metallicity of +0.7 dex, feh-100 as -1.0 dex, co_025 should be read as 0.25x C/O relative to solar, and co_200 as 2x C/O relative to solar. We use the Lodders et al. 2010 value for the solar C/O=0.458. The files with “noTiOVO” in the filename contain the correlated k-coefficients calculated without the opacity of TiO and VO. The rest of the molecular abundances and opacities are the same as the equilibrium chemistry values in the regular files. These files are useful for calculating models without any TiO- and VO-induced temperature inversion in the atmosphere.</p> <p>The correlated-k coefficients are calculated using pre-mixed opacities, with abundances given by equilibrium chemistry for each metallicity-C/O combination, as described in Marley et al. 2021. There are 13 Fe/H values: 0.0, 0.3, 0.5, 0.7, 1.0, 1.3, 1.5, 1.7, 2.0, -0.3, -0.5, -0.7, and -1.0; and 6 C/O values: 0.25, 0.5, 1.0, 1.5, 2.0 and 2.5. The k-coefficients 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, and can be read in using the IDL script read_k_coefficients.pro. The spectral windows are listed in the file 196_windows.txt (intervals defined as starting at lambda1 and ending at lambda2). NB Please note that for metallicities between 1.3 and 2.0 the value of <em>max_windows</em> has changed from 200 to 1000.</p> <p>The opacity sources included in the calculations are: 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 corresponding high resolution opacities for these atoms and molecules can be found in the Zenodo repository 10.5281/zenodo.6600976. The references for the line lists used in these opacity calculations are listed in the file Opacity_references_2021.pdf. Please include these references, as well as the reference to this Zenodo repository when publishing your paper.</p> <p>Each dataset contains the following files:</p> <p>ascii_data: the correlated k coefficients file in ascii format. This can be read by the included IDL code.</p> <p>binary_data: the correlated k coefficients file in binary format</p> <p>full_abunds: the relative abundances for all the species from the chemistry files, on the 1460-point pressure-temperature grid</p> <p>sum_in_atoms: relative abundances for the alkali metals</p> <p>sum_in_layer: relative abundances for all molecules included in the correlated k-coefficients calculations</p> <p><em>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.</em></p>
Correlated k coefficients for H2-He atmospheres; 180 spectral windows and 1460 pressure-temperature points
<p>There are 108 correlated k-coefficients datasets, using the naming convention sonora_2020_fehxxxx_co_yyy.data.196.tar.gz (78 models) or sonora_2020_fehxxxx_co_yyy_noTiOVO.data.196.tar.gz (78 models), where xxxx is the metallicity in 10x dex relative to solar, and yyy is the 100x C/O ratio relative to solar, as a multiplication factor. For example a metallicity of +000 and a C/O ratio of 100 indicates solar abundances, feh+070 should be read as a metallicity of +0.7 dex, feh-100 as -1.0 dex, co_025 should be read as 0.25x C/O relative to solar, and co_200 as 2x C/O relative to solar. We use the Lodders et al. 2010 value for the solar C/O=0.458. The files with “noTiOVO” in the filename contain the correlated k-coefficients calculated without the opacity of TiO and VO. The rest of the molecular abundances and opacities are the same as the equilibrium chemistry values in the regular files. These files are useful for calculating models without any TiO- and VO-induced temperature inversion in the atmosphere.</p> <p>The correlated-k coefficients are calculated using pre-mixed opacities, with abundances given by equilibrium chemistry for each metallicity-C/O combination, as described in Marley et al. 2021. There are 13 Fe/H values: 0.0, 0.3, 0.5, 0.7, 1.0, 1.3, 1.5, 1.7, 2.0, -0.3, -0.5, -0.7, and -1.0; and 6 C/O values: 0.25, 0.5, 1.0, 1.5, 2.0 and 2.5. The k-coefficients 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, and can be read in using the IDL script read_k_coefficients.pro. The spectral windows are listed in the file 180_windows.txt (intervals defined as starting at lambda1 and ending at lambda2). NB Please note that for metallicities between 1.3 and 2.0 the value of <em>max_windows</em> has changed from 200 to 1000.</p> <p>The opacity sources included in the calculations are: 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 corresponding high resolution opacities for these atoms and molecules can be found in the Zenodo repository 10.5281/zenodo.6600976. The references for the line lists used in these opacity calculations are listed in the file Opacity_references_2021.pdf. Please include these references, as well as the reference to this Zenodo repository when publishing your paper.</p> <p>Each dataset contains the following files:</p> <p>ascii_data: the correlated k coefficients file in ascii format. This can be read by the included IDL code.</p> <p>binary_data: the correlated k coefficients file in binary format</p> <p>full_abunds: the relative abundances for all the species from the chemistry files, on the 1460-point pressure-temperature grid</p> <p>sum_in_atoms: relative abundances for the alkali metals</p> <p>sum_in_layer: relative abundances for all molecules included in the correlated k-coefficients calculations</p> <p><em>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.</em></p>
Correlated k coefficients for H2-He atmospheres; 11 spectral windows and 1460 pressure-temperature points
<p>There are 108 correlated k-coefficients datasets, using the naming convention sonora_2020_fehxxxx_co_yyy.data.196.tar.gz (78 models) or sonora_2020_fehxxxx_co_yyy_noTiOVO.data.196.tar.gz (78 models), where xxxx is the metallicity in 10x dex relative to solar, and yyy is the 100x C/O ratio relative to solar, as a multiplication factor. For example a metallicity of +000 and a C/O ratio of 100 indicates solar abundances, feh+070 should be read as a metallicity of +0.7 dex, feh-100 as -1.0 dex, co_025 should be read as 0.25x C/O relative to solar, and co_200 as 2x C/O relative to solar. We use the Lodders et al. 2010 value for the solar C/O=0.458. The files with “noTiOVO” in the filename contain the correlated k-coefficients calculated without the opacity of TiO and VO. The rest of the molecular abundances and opacities are the same as the equilibrium chemistry values in the regular files. These files are useful for calculating models without any TiO- and VO-induced temperature inversion in the atmosphere.</p> <p>The correlated-k coefficients are calculated using pre-mixed opacities, with abundances given by equilibrium chemistry for each metallicity-C/O combination, as described in Marley et al. 2021. There are 13 Fe/H values: 0.0, 0.3, 0.5, 0.7, 1.0, 1.3, 1.5, 1.7, 2.0, -0.3, -0.5, -0.7, and -1.0; and 6 C/O values: 0.25, 0.5, 1.0, 1.5, 2.0 and 2.5. The k-coefficients 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, and can be read in using the IDL script read_k_coefficients.pro. The spectral windows are listed in the file 11_windows.txt (intervals defined as starting at lambda1 and ending at lambda2). NB Please note that for metallicities between 1.3 and 2.0 the value of <em>max_windows</em> has changed from 200 to 1000.</p> <p>The opacity sources included in the calculations are: 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 corresponding high resolution opacities for these atoms and molecules can be found in the Zenodo repository 10.5281/zenodo.6600976. The references for the line lists used in these opacity calculations are listed in the file Opacity_references_2021.pdf. Please include these references, as well as the reference to this Zenodo repository when publishing your paper.</p> <p>Each dataset contains the following files:</p> <p>ascii_data: the correlated k coefficients file in ascii format. This can be read by the included IDL code.</p> <p>binary_data: the correlated k coefficients file in binary format</p> <p>full_abunds: the relative abundances for all the species from the chemistry files, on the 1460-point pressure-temperature grid</p> <p>sum_in_atoms: relative abundances for the alkali metals</p> <p>sum_in_layer: relative abundances for all molecules included in the correlated k-coefficients calculations</p> <p><em>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.</em></p>
Correlated k coefficients for H2-He atmospheres; 30 spectral windows and 1460 pressure-temperature points
<p>There are 108 correlated k-coefficients datasets, using the naming convention sonora_2020_fehxxxx_co_yyy.data.196.tar.gz (78 models) or sonora_2020_fehxxxx_co_yyy_noTiOVO.data.196.tar.gz (78 models), where xxxx is the metallicity in 10x dex relative to solar, and yyy is the 100x C/O ratio relative to solar, as a multiplication factor. For example a metallicity of +000 and a C/O ratio of 100 indicates solar abundances, feh+070 should be read as a metallicity of +0.7 dex, feh-100 as -1.0 dex, co_025 should be read as 0.25x C/O relative to solar, and co_200 as 2x C/O relative to solar. We use the Lodders et al. 2010 value for the solar C/O=0.458. The files with “noTiOVO” in the filename contain the correlated k-coefficients calculated without the opacity of TiO and VO. The rest of the molecular abundances and opacities are the same as the equilibrium chemistry values in the regular files. These files are useful for calculating models without any TiO- and VO-induced temperature inversion in the atmosphere.</p> <p>The correlated-k coefficients are calculated using pre-mixed opacities, with abundances given by equilibrium chemistry for each metallicity-C/O combination, as described in Marley et al. 2021. There are 13 Fe/H values: 0.0, 0.3, 0.5, 0.7, 1.0, 1.3, 1.5, 1.7, 2.0, -0.3, -0.5, -0.7, and -1.0; and 6 C/O values: 0.25, 0.5, 1.0, 1.5, 2.0 and 2.5. The k-coefficients 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, and can be read in using the IDL script read_k_coefficients.pro. The spectral windows are listed in the file 30_windows.txt (intervals defined as starting at lambda1 and ending at lambda2). NB Please note that for metallicities between 1.3 and 2.0 the value of <em>max_windows</em> has changed from 200 to 1000.</p> <p>The opacity sources included in the calculations are: 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 corresponding high resolution opacities for these atoms and molecules can be found in the Zenodo repository 10.5281/zenodo.6600976. The references for the line lists used in these opacity calculations are listed in the file Opacity_references_2021.pdf. Please include these references, as well as the reference to this Zenodo repository when publishing your paper.</p> <p>Each dataset contains the following files:</p> <p>ascii_data: the correlated k coefficients file in ascii format. This can be read by the included IDL code.</p> <p>binary_data: the correlated k coefficients file in binary format</p> <p>full_abunds: the relative abundances for all the species from the chemistry files, on the 1460-point pressure-temperature grid</p> <p>sum_in_atoms: relative abundances for the alkali metals</p> <p>sum_in_layer: relative abundances for all molecules included in the correlated k-coefficients calculations</p> <p><em>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.</em></p>
Molecular Absorption Cross Sections for H2-He Dominated Substellar Atmospheres (using exocross and ExoMol line lists as of ~2021)
<p>This data set consists of molecular absorption cross sections for the following molecules assuming collisional broadening by a H2-He dominated atmosphere: H2O, CH4, NH3, PH3, CO2, CO, HCN, H2S, H2, FeH, SiO CrH, TiH, MgH, CaH, TiO, VO</p> <p>The cross section grid has a constant spectral resolution of R~20,000 from 0.3 microns to 50 microns. It ranges in temperature from 50-5000 K and in pressure from 10^6 to 3000 bars. When decompressed, the full set of files takes up 22 GB.</p> <p>These molecular absorption cross sections were calculated using the exocross code created and distributed by the ExoMol collaboration. A description of the procedure I followed for their calculation is included in the appendix of Lacy & Burrows 2023. A description of the file format and brief summary of the line lists used can be found in README.txt. Please cite these line lists as well as Lacy & Burrows 2023 if you make use of these cross sections in your work. (See https://www.exomol.com/bibliography/)</p>
Climate model results for H2-H2O atmospheres
<p>This dataset is a realization of a greenhouse climate model for H2-H2O atmospheres</p>
Data underlying the publication: Callisto's atmosphere: First evidence for H2 and constraints on H2O
<p>We explore the parameter space for the contribution to Callisto's H corona observed by the Hubble Space Telescope (Roth et al. 2017a) from sublimated H<sub>2</sub>O and radiolytically produced H<sub>2</sub> using the Direct Simulation Monte Carlo (DSMC) method. The spatial morphology of this corona produced via photo- and magnetospheric electron impact-induced dissociation is described by tracking the motion of and simulating collisions between the hot H atoms and thermal molecules including a near-surface O<sub>2</sub> component. Our results indicate that sublimated H<sub>2</sub>O produced from the surface ice, whether assumed to be intimately mixed with or distinctly segregated from the dark non-ice or ice-poor regolith, cannot explain the observed structure of the H corona. On the other hand, a global H<sub>2</sub> component can reproduce the observation, and is also consistent with enhanced electron densities observed at high altitudes by <em>Galileo</em>'s plasma-wave instrument (Gurnett et al. 1997, 2000), providing the first evidence of H<sub>2</sub> in Callisto's atmosphere. The range of H<sub>2</sub> surface densities explored, under a variety of conditions, that are consistent with these observations is ∼(0.4-1)×10<sup>8</sup> cm<sup>-3</sup>. The simulated H<sub>2</sub> escape rates and estimated lifetimes suggest that Callisto has a neutral H<sub>2</sub> torus. We also place a rough upper limit on the peak H<sub>2</sub>O number density (<∼10<sup>8</sup> cm<sup>-3</sup>), column density (<∼10<sup>15</sup> cm<sup>-2</sup>), and sublimation flux (<∼10<sup>12</sup> cm<sup>-2</sup> s<sup>-1</sup>), all of which are 1-2 orders of magnitude less than that assumed in previous models. Finally, we discuss the implications of these results, as well as how they compare to Europa and Ganymede.</p>
Data underlying the publication: Callisto's atmosphere: First evidence for H2 and constraints on H2O
Open the record for dataset details and reuse information.
ScienceDex guides
Understand access before you commit
These curated guides explain access requirements, typical timelines, costs, and reuse considerations for widely used research datasets.
Allen Brain Atlas
Allen Brain Atlas is an Allen Institute collection of brain map atlases, datasets, APIs, and analysis tools covering mouse, human, and non-human primate brain resources.
Annotated Behaviour and Observability Dataset (ABODe)
ABODe is a University of Edinburgh DataShare dataset for behavior classification in group-housed mice using home-cage video, identities, bounding boxes, ground-plate positions, and annotator labels.
DANDI Archive for NWB datasets
DANDI is a BRAIN Initiative archive for publishing and sharing neurophysiology data, including electrophysiology, optophysiology, and behavioral data packaged as NWB and related standards.
International Brain Laboratory public data
The International Brain Laboratory public data releases expose standardized mouse decision-making experiments, including Neuropixels recordings, widefield calcium imaging, behavior, and session metadata accessed through the ONE API.
OpenNeuro
OpenNeuro is a free, open platform for sharing neuroimaging datasets, with public search, dataset pages, and download paths for web, S3, DataLad, and the OpenNeuro CLI.