adsabs/AstroCLIMB huggingface dataset:
Paper: TOI-1685 b Is a Hot Rocky Super-Earth: Updates to the Stellar and Planet Parameters of a Popular JWST Cycle 2 Target
Authors: Jennifer A. Burt, Matthew J. Hooton, Eric E. Mamajek, Oscar Barragán, Sarah C. Millholland, Tyler R. Fairnington, Chloe Fisher, Samuel P. Halverson, Chelsea X. Huang, Madison Brady, Andreas Seifahrt, Eric Gaidos, Rafael Luque, David Kasper, Jacob L. Bean
Figure caption: Injection recovery analyses of the residual RVs generated by Pyaneti (left) and the combined TESS S19 and S59 light curves (right). Blue and red circles denote synthetic planets that were and were not successfully recovered, respectively. The black contours denote the 50% detection probability threshold as a function of orbital period. In both cases, small and low-mass planets could evade detection, leaving the possibility that TOI-1685 b is not the only low-mass planet in the system. We overplot the allowable parameter space for a perturbing planet if TOI-1685 b started on a 0.05 au orbit as blue lines, using the mass–radius relation from Müller et al. (2024) to convert the planet masses from Figure 8. For the perturber to remain undetected, it would need to have a mass ≤3 M ⊕ and a radius ≤3 R ⊕ if on the shorter (8 days) end of the allowable period range. The undetected planet limits relax to ≤5 M ⊕ and ≤3.75 R ⊕ when considering a perturber on the longer (27 days) end of the allowed orbital period range.
Paper: TOI-1685 b Is a Hot Rocky Super-Earth: Updates to the Stellar and Planet Parameters of a Popular JWST Cycle 2 Target
Authors: Jennifer A. Burt, Matthew J. Hooton, Eric E. Mamajek, Oscar Barragán, Sarah C. Millholland, Tyler R. Fairnington, Chloe Fisher, Samuel P. Halverson, Chelsea X. Huang, Madison Brady, Andreas Seifahrt, Eric Gaidos, Rafael Luque, David Kasper, Jacob L. Bean
Figure caption: Small planet mass vs radius diagram, using data taken from NASA’s Exoplanet Archive on 2023 October 17. Gray points with error bars show confirmed planets with mass and radius measurements better than 20%, and solid lines represent two-layer models as given by Zeng et al. (2016). Large colored circles are the previous characterizations of TOI-1685 b from B21 in blue and H21 in red, while the green square depicts the best-fit mass and radius for the planet derived here. Purple diamonds show planets that have been selected for observation with JWST in Cycle 1 or 2.
Paper: TOI-1685 b Is a Hot Rocky Super-Earth: Updates to the Stellar and Planet Parameters of a Popular JWST Cycle 2 Target
Authors: Jennifer A. Burt, Matthew J. Hooton, Eric E. Mamajek, Oscar Barragán, Sarah C. Millholland, Tyler R. Fairnington, Chloe Fisher, Samuel P. Halverson, Chelsea X. Huang, Madison Brady, Andreas Seifahrt, Eric Gaidos, Rafael Luque, David Kasper, Jacob L. Bean
Figure caption: Period and mass of a hypothetical perturber that could have caused TOI-1685 b to decay to its current orbit via obliquity tides. The shadings indicate different possible initial semimajor axes of TOI-1685 b before its decay. Each region is bounded on the left by a minimum initial period ratio, P pert/P  b,i  = 1.3, and on the right by ∣g∣/α = 1 (with ∣g∣/α increasing to the left). The dashed black lines indicate contours of constant RV semiamplitude.
Paper: TOI-1685 b Is a Hot Rocky Super-Earth: Updates to the Stellar and Planet Parameters of a Popular JWST Cycle 2 Target
Authors: Jennifer A. Burt, Matthew J. Hooton, Eric E. Mamajek, Oscar Barragán, Sarah C. Millholland, Tyler R. Fairnington, Chloe Fisher, Samuel P. Halverson, Chelsea X. Huang, Madison Brady, Andreas Seifahrt, Eric Gaidos, Rafael Luque, David Kasper, Jacob L. Bean
Figure caption: Left: SBGLS periodogram constructed using all of the 2020 RV data for TOI-1685 across the CARMENES, IRD, and MAROON-X instruments. The vertical lines denote the periods of TOI-1685 b (green) and the potential second planets suggested in H21 (red) and B21 (blue). Only TOI-1685 b shows a narrow peak with a roughly monotonic increase in power as a function of the number of observations, the two hallmarks of a Keplerian signal. The H21 signal does not manifest in the combined RVs with any significant power, while the B21 signal exhibits a local maxima in the 50–70 observation range and a broad peak, which suggest it is a signature of activity in the star. Right: detection significance of each period as a function of the number of observations. The signal at TOI-1685 b’s period exhibits the roughly monotonic increase expected from a true Keplerian signal, while the signals at the periods corresponding to the H21 and B21 planet candidates show early increases in power followed by a notable downturn or leveling off as more observations are added.
Paper: TOI-1685 b Is a Hot Rocky Super-Earth: Updates to the Stellar and Planet Parameters of a Popular JWST Cycle 2 Target
Authors: Jennifer A. Burt, Matthew J. Hooton, Eric E. Mamajek, Oscar Barragán, Sarah C. Millholland, Tyler R. Fairnington, Chloe Fisher, Samuel P. Halverson, Chelsea X. Huang, Madison Brady, Andreas Seifahrt, Eric Gaidos, Rafael Luque, David Kasper, Jacob L. Bean
Figure caption: Color–magnitude diagram (G − K  s  vs. M  G , with the G magnitude taken from Gaia Collaboration et al. 2021 and the 2MASS K  s  magnitude from Cutri et al. 2003) for stars within 25 pc (ϖ > 40 mas) in SIMBAD, subtracting known white dwarfs, binary stars, and giants. The vast majority of the fiducial values for parallax ϖ and magnitudes G and K  s  in SIMBAD come from Gaia DR3 for the first two and 2MASS for the latter. The blue line is a ninth-order polynomial fit, with spectral types labeled at their mean colors from the updated online table from Pecaut & Mamajek (2013). TOI-1685, depicted as a pink star, is 0.57 mag brighter than the main-sequence locus.
Paper: TOI-1685 b Is a Hot Rocky Super-Earth: Updates to the Stellar and Planet Parameters of a Popular JWST Cycle 2 Target
Authors: Jennifer A. Burt, Matthew J. Hooton, Eric E. Mamajek, Oscar Barragán, Sarah C. Millholland, Tyler R. Fairnington, Chloe Fisher, Samuel P. Halverson, Chelsea X. Huang, Madison Brady, Andreas Seifahrt, Eric Gaidos, Rafael Luque, David Kasper, Jacob L. Bean
Figure caption: Best-fit SED for TOI-1685 from VOSA. Colored points are photometric magnitudes from the Gaia, 2MASS, and WISE surveys and magnitudes synthesized from spectrophotometrically calibrated Gaia DR3 Bp/Rp spectra into the photometric system of the OAJ J-PAS and J-PLUS. The gray line depicts the model flux measurements.
Paper: TOI-1685 b Is a Hot Rocky Super-Earth: Updates to the Stellar and Planet Parameters of a Popular JWST Cycle 2 Target
Authors: Jennifer A. Burt, Matthew J. Hooton, Eric E. Mamajek, Oscar Barragán, Sarah C. Millholland, Tyler R. Fairnington, Chloe Fisher, Samuel P. Halverson, Chelsea X. Huang, Madison Brady, Andreas Seifahrt, Eric Gaidos, Rafael Luque, David Kasper, Jacob L. Bean
Figure caption: All of the light curves used in the global transit fit of TOI-1685 b, detrended and phase-folded by common photometric bandpass. The two TESS sectors are shown separately. The median transit models are shown with black lines, and the light curves in 6 minute bins are shown as white circles, with error bars generally too small to be visible.
Paper: An HI-absorption-selected Cold Rotating Disk Galaxy at z ≈ 2.193
Authors: B. Kaur, N. Kanekar, M. Neeleman, M. Rafelski, J. X. Prochaska, R. Dutta
Figure caption: Panel (A) shows the expected HI disk of DLA-B1228g (large ellipse) and its expected velocity field based on the velocity field of the ALMA CO(3–2) emission (inner ellipse) and an assumed flat rotation curve (see main text for a description of the model for the HI disk). The magenta star indicates the location of the sight line toward the background QSO. The x- and y-axes are in kpc, relative to the kinematic center of the CO(3–2) emission (see Table 2). Panel (B) shows the VLT-UVES Ni II  λ1751 absorption profile from the z ≈ 2.1929 DLA, while panel (C) shows the integrated ALMA CO(3–2) flux density spectrum of DLA-B1228g, with the dashed line showing the ±1σ error, where σ is the rms noise per 35 km s−1 velocity resolution. The vertical blue line in panel (B) shows the expected absorption velocity if the absorption arises in an extended HI disk with a flat rotation curve (see main text for discussion). In both the right panels, the x-axis is velocity in km s−1 relative to the redshift of DLA-B1228g (z = 2.1933; see Table 2).
Paper: Obliquity Constraints for the Extremely Eccentric Sub-Saturn Kepler-1656 b
Authors: Ryan A. Rubenzahl, Andrew W. Howard, Samuel Halverson, Cristobal Petrovich, Isabel Angelo, Guđmundur Stefánsson, Fei Dai, Aaron Householder, Benjamin Fulton, Steven R. Gibson, Arpita Roy, Abby P. Shaum, Howard Isaacson, Max Brodheim, William Deich, Grant M. Hill, Bradford Holden, Daniel Huber, Russ R. Laher, Kyle Lanclos, Joel N. Payne, Erik A. Petigura, Christian Schwab, Josh Walawender, Sharon X. Wang, Lauren M. Weiss, Joshua N. Winn, Jason T. Wright
Figure caption: Projected obliquity λ for measured systems as a function of eccentricity, for single-star systems (left) and multistar systems. The shaded bar on the left plot covers ±20°, the range of obliquities for which CHEM could operate given an appropriate companion with zero stellar obliquity. The shaded bands on the multistar plot highlight ±10° around the angles ±40° and ±130° corresponding to the bimodal peaks of the expected true obliquity distribution from star-planet Kozai (Anderson et al. 2016). Note that these angles refer to the true orbital inclinations, while the data points are for λ, the sky projection. The true obliquity ψ is between λ and sign(λ)90°. The data are the same from Figure 1, supplemented with updates for HD 80606 b (42° ± 8°; Hébrard et al. 2010) and 55 Cnc e (﹩{11}_{-20}^{+17}﹩ deg; Zhao et al. 2023), and the addition of TIC 241249530 b (﹩{163.5}_{-7.7}^{+9.4}﹩ deg; Gupta et al. 2024), TOI-3362 b (1.°2 ± 2.°8; Espinoza-Retamal et al. 2023), TOI 677 b (0.°3 ± 1.°3; Sedaghati et al. 2023; Hu et al. 2024), and of course Kepler-1656 b, where we have drawn the 1σ upper limit of 50° (this work).
Paper: Obliquity Constraints for the Extremely Eccentric Sub-Saturn Kepler-1656 b
Authors: Ryan A. Rubenzahl, Andrew W. Howard, Samuel Halverson, Cristobal Petrovich, Isabel Angelo, Guđmundur Stefánsson, Fei Dai, Aaron Householder, Benjamin Fulton, Steven R. Gibson, Arpita Roy, Abby P. Shaum, Howard Isaacson, Max Brodheim, William Deich, Grant M. Hill, Bradford Holden, Daniel Huber, Russ R. Laher, Kyle Lanclos, Joel N. Payne, Erik A. Petigura, Christian Schwab, Josh Walawender, Sharon X. Wang, Lauren M. Weiss, Joshua N. Winn, Jason T. Wright
Figure caption: Three-body simulations of the orbits of Kepler-1656 b (black) and c (gray), for variable initial mutual inclinations i bc, (5°, 10°, 15°, and 120° from left to right). The top row shows the evolution of the mutual inclination (gray) and the inner planet’s obliquity (black), as a function of the semimajor axis. The lower panel shows the eccentricity evolution of planet b (black) and c (gray). The first three (i bc ≤ 15°) are initialized as described in Section 3.1. The fourth (i bc = 120°) is an example of a simulation from Angelo et al. (2022) initialized in situ with a circular planet b. All four scenarios can reproduce the observed Kepler-1656 system (red and yellow data points). Though, i bc ≤ 15° requires starting planet b at a more distant orbit that subsequently migrates through its present-day location, before circularizing in ∼100 Myr; larger mutual inclinations excite large eccentricities without triggering migration, with brief excursions to low obliquity over many ∼Gyr. The measured projected obliquity is plotted for the positive-λ scenario (to match ψ b > 0) in the top panel at 35° with error bars covering 0°–50°.
Paper: An HI-absorption-selected Cold Rotating Disk Galaxy at z ≈ 2.193
Authors: B. Kaur, N. Kanekar, M. Neeleman, M. Rafelski, J. X. Prochaska, R. Dutta
Figure caption: ALMA CO(3–2) integrated line flux density image (black contours; both panels) overlaid on (A) the HST-WFC3 F160W image (color scale) and (B) the HST-WFC3 F105W image (color scale). The images also show the VLT-SINFONI integrated Hα intensity image (magenta contours starting at ±3σ and increasing in steps of ﹩\sqrt{2}﹩). The x-axis and y-axis are, respectively, R.A. and decl. relative to the kinematic center of the CO(3–2) emission (see Table 2). The inset on the bottom left shows the ALMA synthesized beam. In both panels, the yellow cross indicates the possible NUV counterpart of DLA-B1228g identified in the HST-WFC3 F105W image by Kaur et al. (2022a). The new ALMA CO(3–2) image shows that this object is clearly offset from the CO emission and is thus unlikely to be related to DLA-B1228g. See main text for discussion.
Paper: An HI-absorption-selected Cold Rotating Disk Galaxy at z ≈ 2.193
Authors: B. Kaur, N. Kanekar, M. Neeleman, M. Rafelski, J. X. Prochaska, R. Dutta
Figure caption: (A) The CO(3–2) mean velocity field after blanking all spatial locations where the integrated CO(3–2) flux density has <3σ significance. The velocity field is seen to be similar to that of a rotating disk. The red cross indicates the kinematic center of the CO(3–2) emission (see Table 2). (B) A PV slice along the major axis of the galaxy, indicated by the dashed line in the left panel. The y-axis contains velocity in km s−1 relative to the DLA redshift, z = 2.1929, while the x-axis is the distance from the peak of the CO(3–2) emission (see Table 2) in arcseconds. The flux density contours start at ±2σ and increase in steps of ﹩\sqrt{2}﹩, where σ is the rms noise per 35 km s−1 channel.
Paper: An HI-absorption-selected Cold Rotating Disk Galaxy at z ≈ 2.193
Authors: B. Kaur, N. Kanekar, M. Neeleman, M. Rafelski, J. X. Prochaska, R. Dutta
Figure caption: The three rows show the CO(3–2) integrated line flux density (Jy km s−1), the CO(3–2) velocity field (km s−1), and the CO(3–2) velocity dispersion (km s−1), while the three columns show the ALMA image, the best-fit rotating disk model image, and the residual image obtained after subtracting the model image from the corresponding ALMA image. The x-axis and y-axis are, respectively, R.A. and decl. (in arcseconds) relative to the peak of the CO(3–2) emission measured from the best-fit rotating disk model (see Table 2). In the top left panel, the contours start at ±3σ and increase in steps of ﹩\sqrt{2};﹩ negative features are shown with dashed contours. We note that the top right panel, showing the residual integrated line flux density image, does not contain any residual emission with ≥3σ or ≤−3σ significance and hence does not have any marked contours. The images of the middle and bottom panels have been blanked at spatial locations where the integrated CO(3–2) flux density has <3σ significance. The inset in the left panels shows the ALMA synthesized beam.
Paper: An HI-absorption-selected Cold Rotating Disk Galaxy at z ≈ 2.193
Authors: B. Kaur, N. Kanekar, M. Neeleman, M. Rafelski, J. X. Prochaska, R. Dutta
Figure caption: The velocity-integrated CO(3–2) image, with contours at (−3, 3, 4.2, 6) × σ, where σ is the rms noise on the image. The magenta star indicates the QSO position. The right panel shows a zoom-in on DLA-B1228g. The x-axis and y-axis are R.A. and decl. relative to the kinematic center of the CO(3–2) emission (see Table 2) in arcseconds. The synthesized beam is shown in the bottom left corner of each panel.
Paper: Obliquity Constraints for the Extremely Eccentric Sub-Saturn Kepler-1656 b
Authors: Ryan A. Rubenzahl, Andrew W. Howard, Samuel Halverson, Cristobal Petrovich, Isabel Angelo, Guđmundur Stefánsson, Fei Dai, Aaron Householder, Benjamin Fulton, Steven R. Gibson, Arpita Roy, Abby P. Shaum, Howard Isaacson, Max Brodheim, William Deich, Grant M. Hill, Bradford Holden, Daniel Huber, Russ R. Laher, Kyle Lanclos, Joel N. Payne, Erik A. Petigura, Christian Schwab, Josh Walawender, Sharon X. Wang, Lauren M. Weiss, Joshua N. Winn, Jason T. Wright
Figure caption: Top: representative snippet of the Kepler photometry. Transit windows are highlighted by the vertical blue bands, with in-transit data marked in red. Lower left: autocorrelation function of the full Kepler photometry using spinspotter. Lower right: corresponding true obliquity distribution (orange) given the measured sky-projected obliquity (blue).
Paper: Did Binary Neutron Star Merger GW170817 Leave Behind a Long-lived Neutron Star?
Authors: Marcus DuPont, Andrew MacFadyen
Figure caption: Radio (upper) and X-ray (lower) emission profiles from GW170817 as detected by CXO and VLA instruments (pink circles, data provided by Hajela et al. 2022). The black dashed curve is a representative structured ring afterglow, the black dashed–dotted curve is a structured jet afterglow, and the solid black curve is the sum of both components. The fainter purple dashed curves represent a family of structured ring afterglows for various θ 0 ∈ [0.01, π/2] and therefore E iso. All curves are computed using the afterglowpy code with the relevant parameters for the structured ring annotated in the upper left corner of both plots.
Paper: Did Binary Neutron Star Merger GW170817 Leave Behind a Long-lived Neutron Star?
Authors: Marcus DuPont, Andrew MacFadyen
Figure caption: Similar to Figure 2 except now we assume all of the spin-down energy is beamed in the magnetic rotator’s equatorial plane. The light-curve parameters are also slightly modified from what is shown in Figure 2 in order for the representative dashed black curve to fit within the constraints of the observations.
Paper: The Neutron Star Mass, Distance, and Inclination from Precision Timing of the Brilliant Millisecond Pulsar J0437-4715
Authors: Daniel J. Reardon, Matthew Bailes, Ryan M. Shannon, Chris Flynn, Jacob Askew, N. D. Ramesh Bhat, Zu-Cheng Chen, Małgorzata Curyło, Yi Feng, George B. Hobbs, Agastya Kapur, Matthew Kerr, Xiaojin Liu, Richard N. Manchester, Rami Mandow, Saurav Mishra, Christopher J. Russell, Mohsen Shamohammadi, Lei Zhang, Andrew Zic
Figure caption: Band-averaged timing residuals for PSR J0437–4715 from PPTA-DR3. Residuals at observing frequencies near 800 MHz, 1400 MHz, and 3100 MHz are shown in red, teal, and blue, respectively. Top panel shows post-fit residuals with all modeled Gaussian random processes present, including the dominant DM variations that increase in amplitude ∝ν −2. The middle panel shows the residuals after removal of the maximum likelihood realizations of these Gaussian processes. The bottom panel shows these noise-subtracted residuals divided by the uncertainty. The top and middle panels have labels that show the weighted rms of the residuals in each band.
Paper: Did Binary Neutron Star Merger GW170817 Leave Behind a Long-lived Neutron Star?
Authors: Marcus DuPont, Andrew MacFadyen
Figure caption: Illustration of the two-component emission model for GW170817 considered in this work. We assume the magnetized rotator slings a relativistically expanding, thin ring in the equatorial plane, and a structured jet forms along its rotation axis. θ obs is taken to be the viewing angle with respect to the source’s rotation axis. For brevity, the dynamical ejecta is not depicted. The arrow sizes are indicative of the relative velocity magnitudes.
Paper: The Neutron Star Mass, Distance, and Inclination from Precision Timing of the Brilliant Millisecond Pulsar J0437-4715
Authors: Daniel J. Reardon, Matthew Bailes, Ryan M. Shannon, Chris Flynn, Jacob Askew, N. D. Ramesh Bhat, Zu-Cheng Chen, Małgorzata Curyło, Yi Feng, George B. Hobbs, Agastya Kapur, Matthew Kerr, Xiaojin Liu, Richard N. Manchester, Rami Mandow, Saurav Mishra, Christopher J. Russell, Mohsen Shamohammadi, Lei Zhang, Andrew Zic
Figure caption: Measured ToAs for PSR J0437–4715 across multiple PPTA data sets. The colors of the points indicate the observing frequency on a linear scale. The data set is labeled on each panel and described in Section 2.
Paper: The Neutron Star Mass, Distance, and Inclination from Precision Timing of the Brilliant Millisecond Pulsar J0437-4715
Authors: Daniel J. Reardon, Matthew Bailes, Ryan M. Shannon, Chris Flynn, Jacob Askew, N. D. Ramesh Bhat, Zu-Cheng Chen, Małgorzata Curyło, Yi Feng, George B. Hobbs, Agastya Kapur, Matthew Kerr, Xiaojin Liu, Richard N. Manchester, Rami Mandow, Saurav Mishra, Christopher J. Russell, Mohsen Shamohammadi, Lei Zhang, Andrew Zic
Figure caption: Gaussian probability densities for the pulsar mass, distance, and orbital inclination measurements from various PPTA data sets, relative to the broad prior adopted for NICER early analyses and model selection.
Paper: GRB 211211A: The Case for an Engine-powered over r-process-powered Blue Kilonova
Authors: Hamid Hamidani, Masaomi Tanaka, Shigeo S. Kimura, Gavin P. Lamb, Kyohei Kawaguchi
Figure caption: Same as Figure 3. The SED of our alternative central engine model, where a low-power jet launched by late engine activity interacts with the lanthanide-rich ejecta to explain the early (5−10 hr) blue KN emission in GRB 211211A (double lines), while the r-process explains the late (1.4−4.2 days) red KN emission (black line; same model as in Figures 2 and 3). The central engine model, combined with the red KN model (solid colored lines), can explain both early and late emission data (see Figure 5 for the bolometric luminosity).
Paper: Eddington Envelopes: The Fate of Stars on Parabolic Orbits Tidally Disrupted by Supermassive Black Holes
Authors: Daniel J. Price, David Liptai, Ilya Mandel, Joanna Shepherd, Giuseppe Lodato, Yuri Levin
Figure caption: Disk formation in an isentropic simulation (radiatively efficient cooling) with a nonspinning black hole, as in Figure 1. After ∼120 days, a narrow, circular ring of material forms in the orbital plane. In the second panel, we show the ballistic trajectories of three selected particles in the debris stream (solid white lines), showing how relativistic orbital precession leads to repeated self-intersection of the stream and subsequent disk formation. Dashed white lines show the corresponding Newtonian trajectories (i.e., without relativistic precession). The view is inclined by 60° to match Figure 7. Data and scripts used to create the figure are available on Zenodo: doi:10.5281/zenodo.11438154.
Paper: Eddington Envelopes: The Fate of Stars on Parabolic Orbits Tidally Disrupted by Supermassive Black Holes
Authors: Daniel J. Price, David Liptai, Ilya Mandel, Joanna Shepherd, Giuseppe Lodato, Yuri Levin
Figure caption: Thermodynamics of the accretion flow, showing line-of-sight averaged internal energy 〈u〉 ≡ ∫ρ u d z/∫ρ d z (left) and Mach number (right) in the adiabatic calculation from Figure 1 (with β = 1, a = 0). The stream itself remains cold apart from mild heating caused by the nozzle shock at pericenter passage and some shock heating caused by stream–stream collisions near apocenter. The outflowing Eddington envelope is powered by the accretion flow toward the innermost regions near the black hole. Data and scripts used to create the figure are available on Zenodo: doi:10.5281/zenodo.11438154.
Paper: Eddington Envelopes: The Fate of Stars on Parabolic Orbits Tidally Disrupted by Supermassive Black Holes
Authors: Daniel J. Price, David Liptai, Ilya Mandel, Joanna Shepherd, Giuseppe Lodato, Yuri Levin
Figure caption: Effect of resolution in calculations with a = θ = 0 and β = 1, as in Figure 1. Top row: comparison of the large-scale structure, where each panel is 500 au × 500 au. Bottom row: comparison of the stream fanning at small scales, where each panel is 100 au × 100 au. The total number of particles increases by approximately a factor of 8 between columns from left to right, with the third column corresponding to the resolution used in our main calculations. Data and scripts used to create the figure are available on Zenodo: doi:10.5281/zenodo.11438154.