adsabs/AstroCLIMB huggingface dataset:
Paper: The Supersonic Project: Lighting Up the Faint End of the JWST UV Luminosity Function
Authors: Claire E. Williams, William Lake, Smadar Naoz, Blakesley Burkhart, Tommaso Treu, Federico Marinacci, Yurina Nakazato, Mark Vogelsberger, Naoki Yoshida, Gen Chiaki, Yeou S. Chiou, Avi Chen
Figure caption: Top: UVLF at z = 12 with (pink) and without (blue) the stream velocity compared to the theoretical models of Yung et al. (2023), Mason et al. (2023), and Dayal et al. (2014) and observational constraints close to the redshift presented from Pérez-González et al. (2023), Naidu et al. (2022), Finkelstein et al. (2023), Leung et al. (2023), Harikane et al. (2023b), Donnan et al. (2023a), Bouwens et al. (2023), and Bouwens et al. (2023). The UVLF is then averaged over bins with ΔM UV = 1, with the shaded regions showing the minimum and maximum values in that box. Bottom: Distributions of galaxies by AB absolute UV magnitude with and without the stream velocity between z = 13 and 12.
Paper: The Supersonic Project: Lighting Up the Faint End of the JWST UV Luminosity Function
Authors: Claire E. Williams, William Lake, Smadar Naoz, Blakesley Burkhart, Tommaso Treu, Federico Marinacci, Yurina Nakazato, Mark Vogelsberger, Naoki Yoshida, Gen Chiaki, Yeou S. Chiou, Avi Chen
Figure caption: Comparison of the projected density of gas and stars in the region of a highly star-forming object in our simulations at z = 12 between the 2σ bc run (left) and the 0σ bc (right) run. A bar is shown in each panel denoting a distance of 1 kpc. Both the left and right boxes are centered on a galaxy in 2σ bc, and a physical offset of the location of the galaxy is noticeable as the 0σ bc galaxy appears to the left of the box. This is due to the stream velocity, which points in the ﹩+\hat{x}﹩ direction (to the right). The galaxy at the center of the left two panels formed stars rapidly between z = 15 and 12, with an SFR of ﹩\dot{{M}_{* }}=0.176\,{M}_{\odot }﹩ yr−1, the fifth highest in our 2σ bc run. It has M * = 107.51 M ⊙ at z = 12. The stellar mass history of this object in the interval between z = 15 and 12 is shown in Figure 7 in Appendix B.
Paper: The Supersonic Project: Lighting Up the Faint End of the JWST UV Luminosity Function
Authors: Claire E. Williams, William Lake, Smadar Naoz, Blakesley Burkhart, Tommaso Treu, Federico Marinacci, Yurina Nakazato, Mark Vogelsberger, Naoki Yoshida, Gen Chiaki, Yeou S. Chiou, Avi Chen
Figure caption: Stellar mass (M *) vs. total halo mass (M  h ) for the two runs at z = 12 (top) and 15 (bottom). The data are binned along the y-axis and shown with error bars corresponding to one standard deviation. The 0σ bc run is given in blue (left points), and the 2σ bc run is in pink (right points). Underneath the binned data, the actual distributions are shown, with the 0σ bc runs shown in gray and the 2σ bc runs shown in pink.
Paper: Three-dimensional GRMHD Simulations of Neutron Star Jets
Authors: Pushpita Das, Oliver Porth
Figure caption: Inner magnetosphere for different rotation and magnetic axis inclinations at t = 12,000r  g /c. The upper panels show ﹩{\mathrm{log}}_{10}\rho ﹩, and the middle panels show ﹩{\mathrm{log}}_{10}\sigma ﹩ in the z–x plane. The lower panels show ﹩{\mathrm{log}}_{10}\beta ﹩ in the equatorial plane (x–y). The gray dashed lines show the corotation radius. The black lines in the lower panels show the β = 1 contour.
Paper: The Supersonic Project: Lighting Up the Faint End of the JWST UV Luminosity Function
Authors: Claire E. Williams, William Lake, Smadar Naoz, Blakesley Burkhart, Tommaso Treu, Federico Marinacci, Yurina Nakazato, Mark Vogelsberger, Naoki Yoshida, Gen Chiaki, Yeou S. Chiou, Avi Chen
Figure caption: Top panel: the number of halos greater than mass M for the standard value σ 8 = 0.8 (dark gray) and 1.7 (light gray) used in the simulations presented here. The halo mass function from Sheth & Tormen (2002) is used. Also shown are the numerical results from our simulations at a selection of redshifts (pink and blue dashed lines). Bottom panel: the ratio between n(>M) at σ 8 = 0.8 and 1.7 (f 1.7) as a function of halo mass. This ratio corresponds to the correction factor used to calibrate our UVLF.
Paper: The Supersonic Project: Lighting Up the Faint End of the JWST UV Luminosity Function
Authors: Claire E. Williams, William Lake, Smadar Naoz, Blakesley Burkhart, Tommaso Treu, Federico Marinacci, Yurina Nakazato, Mark Vogelsberger, Naoki Yoshida, Gen Chiaki, Yeou S. Chiou, Avi Chen
Figure caption: Box plot of stellar mass in the most massive 100 galaxies in the simulation between z = 15 and 12. The medians are shown as circles, and the boxes extend from the first to the third quartiles at each redshift. For clarity, the dashed blue boxes corresponding to the no stream velocity case have been offset along the x-axis by +3 Myr. Best-fit lines to the medians give ﹩{\mathrm{log}}_{10}\left({M}_{* }/{M}_{\odot }\right)=0.0043{\mathrm{log}}_{10}\left(t/\mathrm{Myr}\right)+5.78﹩ for the stream velocity run (solid line) and ﹩{\mathrm{log}}_{10}\left({M}_{* }/{M}_{\odot }\right)=0.0036{\mathrm{log}}_{10}\left(t/\mathrm{Myr}\right)+6.06﹩ for the no stream velocity run (dashed line). This panel highlights the difference between the large masses shown in Figure 3 as a function of redshift. Whiskers extend to the most distant data point within 1.5 times the interquartile range from the box.
Paper: The Supersonic Project: Lighting Up the Faint End of the JWST UV Luminosity Function
Authors: Claire E. Williams, William Lake, Smadar Naoz, Blakesley Burkhart, Tommaso Treu, Federico Marinacci, Yurina Nakazato, Mark Vogelsberger, Naoki Yoshida, Gen Chiaki, Yeou S. Chiou, Avi Chen
Figure caption: Stellar mass of massive objects between z = 12 and 15 with the stream velocity (pink) and the same object without the stream velocity (blue). An example object (the same object shown in the center of Figure 1) is shown in the thick dashed lines. In the simulation run with stream velocity (shown in pink), the object grows from 106.39 to 107.49 M ⊙, whereas without the stream velocity (blue), the object has already formed the bulk of its stellar mass by that time.
Paper: The Supersonic Project: Lighting Up the Faint End of the JWST UV Luminosity Function
Authors: Claire E. Williams, William Lake, Smadar Naoz, Blakesley Burkhart, Tommaso Treu, Federico Marinacci, Yurina Nakazato, Mark Vogelsberger, Naoki Yoshida, Gen Chiaki, Yeou S. Chiou, Avi Chen
Figure caption: GSMF with (pink lines) and without (blue lines) stream velocity at z = 12 (solid) and 15 (dashed).
Paper: A Fokker–Planck Framework for Studying the Variability of the Magnetic Field Direction in the Alfvénic Streams of the Solar Wind
Authors: N. H. Bian, Gang Li
Figure caption: Modeled time series of the pitch-angle cosine ﹩\mu (t)=\cos \theta (t)﹩ for the concentration parameter κ = 3. The value μ = 1 corresponds to Parker’s prediction.
Paper: A Fokker–Planck Framework for Studying the Variability of the Magnetic Field Direction in the Alfvénic Streams of the Solar Wind
Authors: N. H. Bian, Gang Li
Figure caption: Modeled time series of the pitch-angle cosine ﹩\mu (t)=\cos \theta (t)﹩ of the magnetic field vector, solution of Equation (13) for κ = 0. The concentration parameter is zero. It corresponds to Barnes's (1981) spherical diffusion model. Time is normalized by the inverse angular diffusivity of the magnetic field vector.
Paper: New Mass and Radius Constraints on the LHS 1140 Planets: LHS 1140 b Is either a Temperate Mini-Neptune or a Water World
Authors: Charles Cadieux, Mykhaylo Plotnykov, René Doyon, Diana Valencia, Farbod Jahandar, Lisa Dang, Martin Turbet, Thomas J. Fauchez, Ryan Cloutier, Collin Cherubim, Étienne Artigau, Neil J. Cook, Billy Edwards, Tim Hallatt, Benjamin Charnay, François Bouchy, Romain Allart, Lucile Mignon, Frédérique Baron, Susana C. C. Barros, Björn Benneke, B. L. Canto Martins, Nicolas B. Cowan, J. R. De Medeiros, Xavier Delfosse, Elisa Delgado-Mena, Xavier Dumusque, David Ehrenreich, Yolanda G. C. Frensch, J. I. González Hernández, Nathan C. Hara, David Lafrenière, Gaspare Lo Curto, Lison Malo, Claudio Melo, Dany Mounzer, Vera Maria Passeger, Francesco Pepe, Anne-Sophie Poulin-Girard, Nuno C. Santos, Danuta Sosnowska, Alejandro Suárez Mascareño, Simon Thibault, Valentina Vaulato, Gregg A. Wade, François Wildi
Figure caption: Fe/Mg distribution for LHS 1140 b according to different assumptions (no prior or stellar prior) for the bare-rock (red) and water-world (green and purple) models compared to the host star (black). We plot the kernel density estimate of the interior model posterior, which is normalized to have a mode of 1. We include the M dwarf distribution of Fe/Mg from the APOGEE DR16 (gray histogram, sample size of ∼1000; Majewski & APOGEE Team 2016; Ahumada et al. 2020) for comparison.
Paper: New Mass and Radius Constraints on the LHS 1140 Planets: LHS 1140 b Is either a Temperate Mini-Neptune or a Water World
Authors: Charles Cadieux, Mykhaylo Plotnykov, René Doyon, Diana Valencia, Farbod Jahandar, Lisa Dang, Martin Turbet, Thomas J. Fauchez, Ryan Cloutier, Collin Cherubim, Étienne Artigau, Neil J. Cook, Billy Edwards, Tim Hallatt, Benjamin Charnay, François Bouchy, Romain Allart, Lucile Mignon, Frédérique Baron, Susana C. C. Barros, Björn Benneke, B. L. Canto Martins, Nicolas B. Cowan, J. R. De Medeiros, Xavier Delfosse, Elisa Delgado-Mena, Xavier Dumusque, David Ehrenreich, Yolanda G. C. Frensch, J. I. González Hernández, Nathan C. Hara, David Lafrenière, Gaspare Lo Curto, Lison Malo, Claudio Melo, Dany Mounzer, Vera Maria Passeger, Francesco Pepe, Anne-Sophie Poulin-Girard, Nuno C. Santos, Danuta Sosnowska, Alejandro Suárez Mascareño, Simon Thibault, Valentina Vaulato, Gregg A. Wade, François Wildi
Figure caption: Posterior distribution for LHS 1140 b interior parameters for the water-world scenario (WMF > 0) for different Fe/Mg assumptions: no prior (black), stellar prior (red), and Sun prior (blue). For the stellar and Sun prior cases, the log-probability function is modified to include the restriction posed by Fe/Mg and Mg/Si ratios measured on the host star or the Sun (Table C3). The red lines (and red cross) in Fe/Si and Fe/Mg space correspond to the stellar measurements. The vertical red dashed lines represent the 16th and 84th percentiles of the posterior for the stellar prior case. Note that the values in the parameter titles are for the stellar prior case only.
Paper: New Mass and Radius Constraints on the LHS 1140 Planets: LHS 1140 b Is either a Temperate Mini-Neptune or a Water World
Authors: Charles Cadieux, Mykhaylo Plotnykov, René Doyon, Diana Valencia, Farbod Jahandar, Lisa Dang, Martin Turbet, Thomas J. Fauchez, Ryan Cloutier, Collin Cherubim, Étienne Artigau, Neil J. Cook, Billy Edwards, Tim Hallatt, Benjamin Charnay, François Bouchy, Romain Allart, Lucile Mignon, Frédérique Baron, Susana C. C. Barros, Björn Benneke, B. L. Canto Martins, Nicolas B. Cowan, J. R. De Medeiros, Xavier Delfosse, Elisa Delgado-Mena, Xavier Dumusque, David Ehrenreich, Yolanda G. C. Frensch, J. I. González Hernández, Nathan C. Hara, David Lafrenière, Gaspare Lo Curto, Lison Malo, Claudio Melo, Dany Mounzer, Vera Maria Passeger, Francesco Pepe, Anne-Sophie Poulin-Girard, Nuno C. Santos, Danuta Sosnowska, Alejandro Suárez Mascareño, Simon Thibault, Valentina Vaulato, Gregg A. Wade, François Wildi
Figure caption: Individual Spitzer transits of LHS 1140 b (transits 1–4) and c (transit 4 only). The best-fit transit models of the planets are shown in blue, with the residual of the fit shown below.
Paper: New Mass and Radius Constraints on the LHS 1140 Planets: LHS 1140 b Is either a Temperate Mini-Neptune or a Water World
Authors: Charles Cadieux, Mykhaylo Plotnykov, René Doyon, Diana Valencia, Farbod Jahandar, Lisa Dang, Martin Turbet, Thomas J. Fauchez, Ryan Cloutier, Collin Cherubim, Étienne Artigau, Neil J. Cook, Billy Edwards, Tim Hallatt, Benjamin Charnay, François Bouchy, Romain Allart, Lucile Mignon, Frédérique Baron, Susana C. C. Barros, Björn Benneke, B. L. Canto Martins, Nicolas B. Cowan, J. R. De Medeiros, Xavier Delfosse, Elisa Delgado-Mena, Xavier Dumusque, David Ehrenreich, Yolanda G. C. Frensch, J. I. González Hernández, Nathan C. Hara, David Lafrenière, Gaspare Lo Curto, Lison Malo, Claudio Melo, Dany Mounzer, Vera Maria Passeger, Francesco Pepe, Anne-Sophie Poulin-Girard, Nuno C. Santos, Danuta Sosnowska, Alejandro Suárez Mascareño, Simon Thibault, Valentina Vaulato, Gregg A. Wade, François Wildi
Figure caption: Posterior distribution for LHS 1140 b interior parameters for the Hycean world scenario (icy planet with 250 km H2 atmosphere on top). Here, we use the same assumptions as the stellar prior water-world model. The red lines (and red cross) represent the stellar ratios, while the vertical black dashed lines are the 16th and 84th percentiles of the posterior. Note that the simulation radius is smaller (ΔR p ∼ 0.03 R ⊕) due to the H2 atmosphere, which is not included in our interior model.
Paper: New Mass and Radius Constraints on the LHS 1140 Planets: LHS 1140 b Is either a Temperate Mini-Neptune or a Water World
Authors: Charles Cadieux, Mykhaylo Plotnykov, René Doyon, Diana Valencia, Farbod Jahandar, Lisa Dang, Martin Turbet, Thomas J. Fauchez, Ryan Cloutier, Collin Cherubim, Étienne Artigau, Neil J. Cook, Billy Edwards, Tim Hallatt, Benjamin Charnay, François Bouchy, Romain Allart, Lucile Mignon, Frédérique Baron, Susana C. C. Barros, Björn Benneke, B. L. Canto Martins, Nicolas B. Cowan, J. R. De Medeiros, Xavier Delfosse, Elisa Delgado-Mena, Xavier Dumusque, David Ehrenreich, Yolanda G. C. Frensch, J. I. González Hernández, Nathan C. Hara, David Lafrenière, Gaspare Lo Curto, Lison Malo, Claudio Melo, Dany Mounzer, Vera Maria Passeger, Francesco Pepe, Anne-Sophie Poulin-Girard, Nuno C. Santos, Danuta Sosnowska, Alejandro Suárez Mascareño, Simon Thibault, Valentina Vaulato, Gregg A. Wade, François Wildi
Figure caption: Posterior distribution for LHS 1140 b interior parameters for the bare-rock scenario (WMF = 0). The chemical weight ratios Fe/Si and Fe/Mg are derived quantities. The red lines (and red cross) in Fe/Si and Fe/Mg space correspond to the stellar measurements. The vertical black dashed lines represent the 16th and 84th percentiles of the posterior.
Paper: New Mass and Radius Constraints on the LHS 1140 Planets: LHS 1140 b Is either a Temperate Mini-Neptune or a Water World
Authors: Charles Cadieux, Mykhaylo Plotnykov, René Doyon, Diana Valencia, Farbod Jahandar, Lisa Dang, Martin Turbet, Thomas J. Fauchez, Ryan Cloutier, Collin Cherubim, Étienne Artigau, Neil J. Cook, Billy Edwards, Tim Hallatt, Benjamin Charnay, François Bouchy, Romain Allart, Lucile Mignon, Frédérique Baron, Susana C. C. Barros, Björn Benneke, B. L. Canto Martins, Nicolas B. Cowan, J. R. De Medeiros, Xavier Delfosse, Elisa Delgado-Mena, Xavier Dumusque, David Ehrenreich, Yolanda G. C. Frensch, J. I. González Hernández, Nathan C. Hara, David Lafrenière, Gaspare Lo Curto, Lison Malo, Claudio Melo, Dany Mounzer, Vera Maria Passeger, Francesco Pepe, Anne-Sophie Poulin-Girard, Nuno C. Santos, Danuta Sosnowska, Alejandro Suárez Mascareño, Simon Thibault, Valentina Vaulato, Gregg A. Wade, François Wildi
Figure caption: Mass–radius diagram of transiting exoplanets around M dwarfs (gray points) with well-established mass and radius (relative uncertainty <30%) from the NASA Exoplanet Archive (Akeson et al. 2013). Various theoretical composition curves from Guillot & Morel (1995), Valencia et al. (2007, 2013), and Aguichine et al. (2021) are plotted with the water-rich models assuming an Earth-like interior (33% iron by mass). The synthetic population of terrestrials enveloped in H/He (0.1%–30% initial mass fraction) of Rogers et al. (2023) is highlighted in orange. This region also highlights interior model degeneracy where the nature (H/He- or water-rich) of sub-Neptunes cannot be reliably determined from mass and radius alone. The mass and radius posteriors (1σ and 2σ contours) of LHS 1140 b (green) and LHS 1140 c (purple) from our joint transit RV analysis are drawn. Published values from LB20 derived from HARPS+ESPRESSO and TESS (sector 3) are shown with open circles. The results of M19 from HARPS and MEarth+Spitzer are presented with open squares.
Paper: New Mass and Radius Constraints on the LHS 1140 Planets: LHS 1140 b Is either a Temperate Mini-Neptune or a Water World
Authors: Charles Cadieux, Mykhaylo Plotnykov, René Doyon, Diana Valencia, Farbod Jahandar, Lisa Dang, Martin Turbet, Thomas J. Fauchez, Ryan Cloutier, Collin Cherubim, Étienne Artigau, Neil J. Cook, Billy Edwards, Tim Hallatt, Benjamin Charnay, François Bouchy, Romain Allart, Lucile Mignon, Frédérique Baron, Susana C. C. Barros, Björn Benneke, B. L. Canto Martins, Nicolas B. Cowan, J. R. De Medeiros, Xavier Delfosse, Elisa Delgado-Mena, Xavier Dumusque, David Ehrenreich, Yolanda G. C. Frensch, J. I. González Hernández, Nathan C. Hara, David Lafrenière, Gaspare Lo Curto, Lison Malo, Claudio Melo, Dany Mounzer, Vera Maria Passeger, Francesco Pepe, Anne-Sophie Poulin-Girard, Nuno C. Santos, Danuta Sosnowska, Alejandro Suárez Mascareño, Simon Thibault, Valentina Vaulato, Gregg A. Wade, François Wildi
Figure caption: Results of Global Climate Model (GCM) simulations of LHS 1140 b assuming an Earth-like atmosphere (1 bar N2, 400 ppm CO2; panels (a), (c), (d), and (e)) and a thick CO2-dominated atmosphere (5 bars CO2; panels (b), (f), (g), and (h)). Panels (a) and (b): surface temperature maps of LHS 1140 b. The black line indicates the line of stability between liquid water and sea ice. The extent of the ice-free ocean strongly depends on the amount of CO2 in the atmosphere. Panels (c)–(h): vertical profiles of the atmospheric temperatures, water vapor, and cloud mixing ratios (both H2O and CO2 ice clouds). The thick solid lines indicate the global mean vertical profiles, and the dotted lines indicate the terminator vertical profiles (impacting transit spectra).
Paper: New Mass and Radius Constraints on the LHS 1140 Planets: LHS 1140 b Is either a Temperate Mini-Neptune or a Water World
Authors: Charles Cadieux, Mykhaylo Plotnykov, René Doyon, Diana Valencia, Farbod Jahandar, Lisa Dang, Martin Turbet, Thomas J. Fauchez, Ryan Cloutier, Collin Cherubim, Étienne Artigau, Neil J. Cook, Billy Edwards, Tim Hallatt, Benjamin Charnay, François Bouchy, Romain Allart, Lucile Mignon, Frédérique Baron, Susana C. C. Barros, Björn Benneke, B. L. Canto Martins, Nicolas B. Cowan, J. R. De Medeiros, Xavier Delfosse, Elisa Delgado-Mena, Xavier Dumusque, David Ehrenreich, Yolanda G. C. Frensch, J. I. González Hernández, Nathan C. Hara, David Lafrenière, Gaspare Lo Curto, Lison Malo, Claudio Melo, Dany Mounzer, Vera Maria Passeger, Francesco Pepe, Anne-Sophie Poulin-Girard, Nuno C. Santos, Danuta Sosnowska, Alejandro Suárez Mascareño, Simon Thibault, Valentina Vaulato, Gregg A. Wade, François Wildi
Figure caption: Phase-folded Keplerian signals of LHS 1140 b (top) and c (bottom) with ESPRESSO from RVs produced with the LBL method in blue and CCF in red (LB20). Open and filled data points represent pre- and post-fiber upgrade of ESPRESSO (2019 June). The best-fit circular orbital solutions (black curves) of LHS 1140 b (K b = 3.80 ± 0.11 m s−1) and c (K c = 2.42 ± 0.07 m s−1) are respectively improved by 50% and 70% compared with previous estimates with CCF. The residual rms is equivalent to 0.50 m s−1 for LBL and 1.28 m s−1 for CCF.
Paper: New Mass and Radius Constraints on the LHS 1140 Planets: LHS 1140 b Is either a Temperate Mini-Neptune or a Water World
Authors: Charles Cadieux, Mykhaylo Plotnykov, René Doyon, Diana Valencia, Farbod Jahandar, Lisa Dang, Martin Turbet, Thomas J. Fauchez, Ryan Cloutier, Collin Cherubim, Étienne Artigau, Neil J. Cook, Billy Edwards, Tim Hallatt, Benjamin Charnay, François Bouchy, Romain Allart, Lucile Mignon, Frédérique Baron, Susana C. C. Barros, Björn Benneke, B. L. Canto Martins, Nicolas B. Cowan, J. R. De Medeiros, Xavier Delfosse, Elisa Delgado-Mena, Xavier Dumusque, David Ehrenreich, Yolanda G. C. Frensch, J. I. González Hernández, Nathan C. Hara, David Lafrenière, Gaspare Lo Curto, Lison Malo, Claudio Melo, Dany Mounzer, Vera Maria Passeger, Francesco Pepe, Anne-Sophie Poulin-Girard, Nuno C. Santos, Danuta Sosnowska, Alejandro Suárez Mascareño, Simon Thibault, Valentina Vaulato, Gregg A. Wade, François Wildi
Figure caption: Phase-folded transit of LHS 1140 b observed with the Spitzer Infrared Array Camera (at 4.5 μm). The transit of LHS 1140 c from transit 4 is masked (see Figure A1 for individual transits). The open circles represent 8 minute binned photometry, and the blue curve depicts the best-fit transit model. The residuals of this fit are shown below.
Paper: New Mass and Radius Constraints on the LHS 1140 Planets: LHS 1140 b Is either a Temperate Mini-Neptune or a Water World
Authors: Charles Cadieux, Mykhaylo Plotnykov, René Doyon, Diana Valencia, Farbod Jahandar, Lisa Dang, Martin Turbet, Thomas J. Fauchez, Ryan Cloutier, Collin Cherubim, Étienne Artigau, Neil J. Cook, Billy Edwards, Tim Hallatt, Benjamin Charnay, François Bouchy, Romain Allart, Lucile Mignon, Frédérique Baron, Susana C. C. Barros, Björn Benneke, B. L. Canto Martins, Nicolas B. Cowan, J. R. De Medeiros, Xavier Delfosse, Elisa Delgado-Mena, Xavier Dumusque, David Ehrenreich, Yolanda G. C. Frensch, J. I. González Hernández, Nathan C. Hara, David Lafrenière, Gaspare Lo Curto, Lison Malo, Claudio Melo, Dany Mounzer, Vera Maria Passeger, Francesco Pepe, Anne-Sophie Poulin-Girard, Nuno C. Santos, Danuta Sosnowska, Alejandro Suárez Mascareño, Simon Thibault, Valentina Vaulato, Gregg A. Wade, François Wildi
Figure caption: Primordial H/He atmosphere photoevaporation simulation of LHS 1140 b. Each curve corresponds to different initial envelope mass fractions f atm,0. These simulations model thermal contraction, EUV-driven atmospheric escape, and core-powered mass loss using the methodology of Cherubim et al. (2023). f atm,0 = 0.1%–0.2% is consistent with the observed radius given the age of the system (>5 Gyr).