Potential sublimating exocomets around the young star PDS 70

The following figures and tables are from: Novais et al. (2026) "Potential sublimating exocomets around the young star PDS 70", XXXX, XXXX. We ask to please refer to the publication, as well as this Zenodo DOI 10.5281/zenodo.21628743, if these are used anywhere. figure1.csv: Data corresponding to Figure 1b. “rv” is the radial velocity in km/s and “norm_flux” is the normalised flux. figure2.csv: Data corresponding to Figure 2. The top part of the table corresponds to Figure 2a, where “rv” is the radial velocity in km/s, “norm_flux” is the normalised flux, and “flux_error” is the flux uncertainty. The “data” column corresponds to data points, while the “fit” column corresponds to the best-fit model. The bottom part of the table corresponds to Figure 2b, where “rv” corresponds to the radial velocity in km/s, “fill_fraction” corresponds to the surface fill fraction, and “optical_depth” corresponds to the optical depth, all measured at line centre. “median” corresponds to the median value of the posterior distribution (50th percentile), while “16pct”, “84pct”, “0p135pct”, and “99p865pct” correspond to the 16th, 84th, 0.135th, and 99.865th percentiles. figure3.csv: Data corresponding to Figure 3. “components” correspond to different variable absorption components present in the sodium lines, numbered from 1 (blue-most) to 4 (red-most). “log10_column_density” corresponds to the logarithm of the column density in cm-2, “line_width” is the Gaussian line width in km/s, “radial_velocity” is the radial velocity in km/s “optical_depth” is the optical depth, and “fill_fraction” is the surface fill fraction, all measured at line centre. “median” corresponds to the median value of the posterior distribution (50th percentile), while “16pct” and “84pct” correspond to the 16th and 84th percentiles. figure4.csv: Data corresponding to Figure 4. The top part of the table corresponds to the simulations including 2 planets (Figures 4a, b, c, d), while the bottom part of the table corresponds to the simulations including 3 planets (Figures 4e, f, g, h). The top part is divided in 3 tables. The first part shows the data from Figure 4a: “time0_bin” and “time1_bin” are the edges of the time bins in Myr, while “crossed_gap_fraction” and “ejected_fraction” are the fraction (percentage) of particles that crossed the gap or were ejected. The second part shows the data from Figure 4b and 4c: “a” corresponds to the semi-major axis in AU, “q” is the periastron distance in AU, “e” is the eccentricity, and “i” is the inclination in degrees. “initial” and “crossed_gap” correspond to parameters at the start of the simulations and when they crossed the gap, respectively. The last part shows the data from Figure 4d: “a_initial0_bin” and “a_initial1_bin” correspond to the edges of the semi-major axis bins in AU, “crossed_gap_fraction_low_inc” and “crossed_gap_fraction_high_inc” are the fractions (percentage) that crossed the gap with inclinations lower than and higher than the disc inclination, respectively, “ejected_fraction” is the fraction of ejected particles, and “survived_fraction” is the fraction of particles that did not cross the gap or got ejected. figure5.csv: Data corresponding to Figure 5. “wave_telluric_model” and “flux_telluric_model” are the wavelength in nm and flux of the telluric model generated with Molecfit. “wave_before_telluric_correction” and “norm_flux_before_telluric_correction” are the wavelength in nm and normalised flux before telluric correction, which appear in Figure 5a. “wave_after_telluric_correction” and “norm_flux_after_telluric_correction” are the wavelength in nm and normalised flux after telluric correction, which appear in Figure 5b. figure7.csv: Data corresponding to Figure 7. The top part of the table corresponds to Figure 7a, where “rv” is the radial velocity in km/s, “norm_flux” is the normalised flux, and “flux_error” is the flux uncertainty. The “data” column corresponds to data points, while the “fit” column corresponds to the best-fit model. The bottom part of the table corresponds to Figure 7b, where “rv” corresponds to the radial velocity in km/s, “fill_fraction” corresponds to the surface fill fraction, and “optical_depth” corresponds to the optical depth, all measured at line centre. “median” corresponds to the median value of the posterior distribution (50th percentile), while “16pct”, “84pct”, “0p135pct”, and “99p865pct” correspond to the 16th, 84th, 0.135th, and 99.865th percentiles. figure8.csv: Data corresponding to Figure 8. “time_after_first_epoch” is the time after first epoch in days, while “stellar_rotation_phase” is the stellar rotation phase. “rv” is the radial velocity in km/s and “line_depth” is the line depth, both at line centre. “median” corresponds to the median value of the posterior distribution (50th percentile), while “16pct” and “84pct” correspond to the 16th and 84th percentiles. supplementary_figure1.csv: Data corresponding to Supplementary Figure 1. “rv” and “norm_flux” are the radial velocity in km/s and normalised flux. supplementary_figure2.csv: Data corresponding to Supplementary Figure 2. “A” is the amplitude of the Voigt, “vsys” is the systemic velocity in km/s, “vsini” is the projected rotational velocity of the star in km/s, “sigma” is the Gaussian line width in km/s, “gamma” is the Lorentzian width in km/s, and “c1”, “c2”, “c3”, and “c4” are the polynomial coefficients. “median” corresponds to the median value of the posterior distribution (50th percentile), while “16pct” and “84pct” correspond to the 16th and 84th percentiles. supplementary_table1.csv: Data corresponding to Supplementary Table 1. “mu” is the centre wavelength of the line in nm, “sigma_v” is the Gaussian line width in km/s, “gamma_v” is the Lorentzian line width in km/s, “tau” is the optical depth, and “f” is the surface fill fraction. “c0” and “c1” are the offset and linear polynomial coefficients, respectively, for the first spectral section (around Na I D2), while “d0” and “d1” are the same coefficients for the second section (around Na I D1). “min” and “max” correspond to the minimum and maximum edge of the priors of each parameter. supplementary_table2.csv: Data corresponding to Supplementary Table 2. “mu” is the centre wavelength of the line in nm and “sigma” is the Gaussian line width in km/s. “min” and “max” correspond to the minimum and maximum edge of the priors of each parameter. Components are numbered from 1 (blue-most) to 4 (red-most). supplementary_table3.csv: Data corresponding to Supplementary Table 3. “v” is the radial velocity in km/s, “sigma” is the Gaussian line width in km/s, “gamma” is the Lorentzian line width in km/s, “tau” is the optical depth, “f” is the surface fill fraction, and “ncol” is the column density in cm-2. “phabs” corresponds to the stellar photospheric absorption line, “statem” is the stationary emission line, and “statabs1” and “statabs2” are the stationary absorption lines, where 1 is the blue-most and 2 is the red-most. Values correspond to the median value of the posterior distribution, and “loerr” and “uperr” are the difference between the median and the 16th and 84th percentiles of the posterior distributions. supplementary_table4.csv: Data corresponding to Supplementary Table 4. “v” is the radial velocity in km/s, “sigma” is the Gaussian line width in km/s, “tau” is the optical depth, “f” is the surface fill fraction, and “ncol” is the column density in cm-2. Components are numbered from 1 (blue-most) to 4 (red-most). Values correspond to the median value of the posterior distribution, and “loerr” and “uperr” are the difference between the median and the 16th and 84th percentiles of the posterior distributions.