This README describes the contents of "Dataset for Analytic Stability Maps of Unknown Exoplanet Companions for Imaging Prioritization."
Analysis of this dataset is presented in:
Carlos Gascon, Dmitry Savransky, and Miquel Sureda, "Analytic Stability Maps of Unknown Exoplanet Companions for Imaging Prioritization," The Astronomical Journal (2020) vol. 160, no. 2. https://doi.org/10.3847/1538-3881/ab9b21
This data set was generated and analyzed using codes available at:
https://github.com/CarlosGascon/NumSim
https://github.com/CarlosGascon/StableDoS
https://github.com/dgarrett622/DoS
The dataset is composed entirely of *.mat files: Mathworks (c) MATLAB 5.0 MAT-file. The format specification and MATLAB version compatibility are detailed in: https://www.mathworks.com/help/pdf_doc/matlab/matfile_format.pdf. Multiple open source resources also exist for handling MAT files, including GNU Octave.
The dataset is composed of numerical simulations producing Figure 1 in the paper, and system prioritizations, corresponding to paper Appendix A. These are divided into two subdirectories: "Numerical_Simulation" and "System_Prioritization".
Numerical Simulations
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Results of the simulations used to generate the numerical stability maps presented in Figure 1.
Comments
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* Data files follow the naming convention "Target_element", where "Target" is the name of the system and "element" can be:
- a (or e or m) centers: Arrays defining the bin centers corresponding to the grids where StabNum is calculated (see General Comments). Eccentricity (e) values are linearly spaced, while semi-major axis (a) and planetary mass (m) values are logarithmically spaced.
- StabNum: Simulation lifetime matrix in [log10(yr)].
- info: Struct containing the target's main information.
* When needed, "mplot" and "eplot" are appended to the file name in order to determine which kind of plot the file is referring to.
Systems Prioritization
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Data used to calculate the dynamically stable completeness and generate the single-planet systems prioritization.
Comments
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* Data is divided into the following subdirectories:
- Datalimits: 4-element array containing the semi-major axis (a) and planetary radius (R) imageable limits [amin, amax, Rmin, Rmax], calculated, together with the depth-of-search grids, using Garrett's code (see General Comments).
- Edges: Arrays containing the a and R bin edges (logarithmically spaced) corresponding to the grids where the calculations are performed (see General Comments).
- DoSGrids: Depth-of-search grids calculated using Garrett's code (see General Comments).
- StabGrids: Stability grids for each stability criterion considered.
- StabDoSGrids: Stable depth-of-search grids (calculated as StabGrid .* DoSGrid).
- OccGrids: Occurrence rates grids calculated using the SAG13 parametric fit, where each bin value is also multiplied by the bin area.
- StabCompGrids: Stable completeness grids (calculated as StabDoSGrid .* OccGrid).
* Res.mat contains the stable depth-of-search and completeness results for all 213 single-planet systems, stored in a table with the following columns:
- Target: Name of the system and planet letter.
- Distance: System's distance in [pc].
- sma: Known planet's semi-major axis in [AU].
- ecc: Known planet's eccentricity.
- mp: Known planet's mass in [Mjup] (see General Comments).
- StabDoS: Stable depth-of-search (this column is calculated for each stability criterion).
- StabComp: Stable completeness (this column is calculated for each stability criterion).
General Comments
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* Planetary mass (m), planetary radius (R) and semi-major axis (a) are always expressed in [Mjup], [Rearth] and [AU], respectively.
* When center values are given (e.g., in Numerical Simulations), the corresponding matrices account for the results obtained exactly at the grid points defined by acenters and ecenters (or mcenters). Therefore, if matrices are Nm x Na, then acenters and mcenters have Na and Nm points, respectively.
* When edge values are given (e.g., in Systems Prioritization), the corresponding matrices contain the bin values obtained by averaging the results at the edges of each bin defined by aedges and Redges. Therefore, if matrices are Nr x Na, then aedges and Redges have Na + 1 and Nr + 1 points, respectively. Note that, in the case of the occurrence grids (OccGrids), the average bin values are also multiplied by the bin area defined by the corresponding bin edges.
* In most cases, the known planet's mass corresponds to the minimum value mp * sinI.
* G, H and P refer to Giuppone's, the Hill AMD and Petrovich's stability criteria, respectively.
* Depth-of-search is calculated using Garrett's code, available at: https://github.com/dgarrett622/DoS
License
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This dataset is shared under a Creative Commons Attribution 4.0 International license (https://creativecommons.org/licenses/by/4.0/). You may:
* Share — copy and redistribute the material in any medium or format
* Adapt — remix, transform, and build upon the material
for any purpose, even commercially.
Under the following terms:
* Attribution — You must give appropriate credit, provide a link to the license, and indicate if changes were made. You may do so in any reasonable manner, but not in any way that suggests the licensor endorses you or your use.
* No additional restrictions — You may not apply legal terms or technological measures that legally restrict others from doing anything the license permits.