Multi-criteria samples of architecturally-characterized multi-planet systems

Multi-criteria samples of architecturally-characterized multi-planet systems from the study "Two families of multi-planet systems with distinct architectures and stellar hosts" by Turrini, Danielski et al. (2026). Dataset Samples The dataset is divided into four main samples of multi-planet systems: Sample L (Large): The first sample is composed of all multi-planet systems for which we know both the semi-major axis (a_p) and mass (m_p) of all planets. Following [Laskar & Petit 2017], we consider as valid masses both the absolute mass (M_p) and the minimum mass (M_p sin(i_p)). To investigate the dynamical excitation of these systems, we retrieved the orbital eccentricity (e_p) of the planets whenever available. For systems where eccentricities are not known for all planets, we filled the gaps using the correlation between the number of planets (N) and their average eccentricity derived from Kepler's observations [He et al. 2020]. Sample L is populated by n_L = 298 multi-planet systems (28% of the known population). Sample H (Homogeneous): The second sample is created by cross-matching Sample L with the SWEET-Cat catalogue [Santos et al. 2013, Sousa et al. 2021], which provides homogeneous stellar atmospheric parameters (i.e., effective temperature, surface gravity, and [Fe/H]). The homogeneous stellar masses are estimated using isochrone fitting. Sample H contains n_H = 189 multi-planet systems and is designed to validate observed trends involving the host stars' properties. Sample E (Excitation): The third sample is the subset of Sample L for which the orbital eccentricity (e_p) is known for all planets. Sample E contains n_E = 89 systems and is designed to validate any trend in dynamical excitation [Turrini el al. 2020, 2022] emerging from samples L and H. Sample S (Strict): The fourth sample includes only those systems from Sample E for which the absolute planetary mass (M_p) and its relative uncertainty are known for all planets. Sample S is composed of n_S = 68 systems and is designed to validate parameter trends involving planetary mass against possible biases introduced by the inclusion of minimum mass. The complete architectural and dynamical characterization of the samples requires knowledge of the inclinations of the planetary orbits [Laskar & Petit 2017, Turrini et al. 2020, He et al. 2020, Bocchieri et al. 2026]. Because this information is available for only a handful of systems, we assumed the average equipartition of dynamical excitation among its secular degrees of freedom [Laskar & Petit 2017, He et al. 2020] to statistically constrain the relative inclinations of the planets. We adopted different approaches across the samples: For Samples L and H (where orbital eccentricities are not always known), we adopted the multiplicity-inclination correlation from He et al. (2020). For Samples E and S (where eccentricities are known by definition), we used the eccentricity-inclination correlation from Turrini et al. (2020). Sample Characterization All samples are homogeneously characterized through the following normalized parameters: i) Normalized System Mass (NSM): The ratio between the total planetary mass and the stellar mass within each system [Gilbert et al. 2020, Zhu & Dong 2021]. ii) Outermost Period (P_out): The orbital period of the outermost planet, quantifying how wide the systems are. iii) Planetary Multiplicity (N): The number of planets within each system. iv) Mass Fraction (S_m): The fraction of the total planetary mass contained in the most massive planet [Chambers 2001]. v) Orbital Spacing Metric (S_s): Quantifies how spatially and gravitationally compact the systems are [Chambers 2001]. vi) Normalized Angular Momentum Deficit (NAMD): Quantifies the global dynamical excitation of the system and provides a "dynamical temperature" scale [Chambers 2001, Turrini 2020, 2022]. vii) Stellar Metallicity: Measured as [Fe/H] using the iron abundance of the star as proxy. viii) Stellar Mass: Expressed in units of solar masses. ix) Planet-Building Material (PBM): Quantifies the amount of solids in the now-lost Class II protoplanetary discs (expressed in dex as Log_10(M_dust / M_Earth)). This combines information from stellar mass and metallicity taking advantage of the observational star mass-disc mass correlation [Pascucci et al. 2016, Testi et al. 2022]. CSV Files Structure All files are structured as comma-separated values (CSV) tables. Each row represents an individual multi-planet system. Below is the sequential column-by-column breakdown of the data included in the files, detailing each parameter and its corresponding uncertainty (in the case of the normalized angular momentum, due to the high skewness of its posterior distribution, we provide the 16th and 84th quantiles separately): Column 1 (source_id_DR2): The unique GAIA DR2 identifier for the host star as catalogued by the Gaia mission. Column 2 (NAMD): The normalized angular momentum deficit (NAMD), representing the system's dynamical excitation. Column 3 (NAMD_LO68): The lower 68% confidence bound for the NAMD value. Column 4 (NAMD_UP68): The upper 68% confidence bound for the NAMD value. Column 5 (NSM): The normalized system mass (ratio of total planetary mass to stellar mass). Column 6 (SIGMA_NSM): The computed statistical uncertainty for the normalized system mass. Column 7 (P_OUT): The orbital period of the outermost planet in the system. Column 8 (SIGMA_P_OUT): The computed statistical uncertainty for the outermost planet's orbital period. Column 9 (PBM): The planet-building material metric, estimating the original mass of solids in the protoplanetary disc (expressed in dex). Column 10 (SIGMA_PBM): The computed statistical uncertainty for the Planet-Building Material metric. Column 11 (M_STAR): The mass of the host star in solar masses. Column 12 (SIGMA_M_STAR): The computed statistical uncertainty for the stellar mass. Column 13 (FeH): Iron abundance of the star normalized from the solar value (proxy for metallicity, in dex). Column 14 (SIGMA_FeH): The computed statistical uncertainty for the Iron abundance. Column 15 (S_M): The mass fraction of the most massive planet in the system. Column 16 (SIGMA_S_M): The computed statistical uncertainty for the mass fraction metric. Column 17 (S_S): The orbital spacing metric, indicating the spatial and gravitational compactness of the system. Column 18 (SIGMA_S_S): The computed statistical uncertainty for the orbital spacing metric. Column 19 (NPLANETS): The total number of confirmed planets in the system (planetary multiplicity).