adsabs/AstroCLIMB huggingface dataset:
Paper: The Power of High-precision Broadband Photometry: Tracing the Milky Way Density Profile with Blue Horizontal Branch Stars in the Dark Energy Survey
Authors: Fengqing Yu, 枫青 余, Ting S. Li, Joshua S. Speagle, 佳士 沈, Gustavo E. Medina, Sergey E. Koposov, Joss Bland-Hawthorn, Lara R. Cullinane, Gwendolyn M. Eadie, Denis Erkal, Geraint F. Lewis, Guilherme Limberg, Daniel B. Zucker
Figure caption: Same as the bottom right panel of Figure 4, but with a more complex parametric form of the BHB ratio. Shown is the predicted probability of a source in the BHB group, the BS group, and the outlier group, parameterized by equations defined in Appendix A. Our model generates physically sensible magnitude and color dependencies across each subgroup.
Paper: Retrieval of Thermally Resolved Water Vapor Distributions in Disks Observed with JWST-MIRI
Authors: Carlos E. Romero-Mirza, Andrea Banzatti, Karin I. Öberg, Klaus M. Pontoppidan, Colette Salyk, Joan Najita, Geoffrey A. Blake, Sebastiaan Krijt, Nicole Arulanantham, Paola Pinilla, Feng Long, Giovanni Rosotti, Sean M. Andrews, David J. Wilner, Jenny Calahan
Figure caption: Same as Figure 3, but for the compact disk of FZ Tau.
Paper: Retrieval of Thermally Resolved Water Vapor Distributions in Disks Observed with JWST-MIRI
Authors: Carlos E. Romero-Mirza, Andrea Banzatti, Karin I. Öberg, Klaus M. Pontoppidan, Colette Salyk, Joan Najita, Geoffrey A. Blake, Sebastiaan Krijt, Nicole Arulanantham, Paola Pinilla, Feng Long, Giovanni Rosotti, Sean M. Andrews, David J. Wilner, Jenny Calahan
Figure caption: Same as Figure 3, but for the extended disk of AS 209.
Paper: Retrieval of Thermally Resolved Water Vapor Distributions in Disks Observed with JWST-MIRI
Authors: Carlos E. Romero-Mirza, Andrea Banzatti, Karin I. Öberg, Klaus M. Pontoppidan, Colette Salyk, Joan Najita, Geoffrey A. Blake, Sebastiaan Krijt, Nicole Arulanantham, Paola Pinilla, Feng Long, Giovanni Rosotti, Sean M. Andrews, David J. Wilner, Jenny Calahan
Figure caption: Same as Figure 7, but for GK Tau.
Paper: Retrieval of Thermally Resolved Water Vapor Distributions in Disks Observed with JWST-MIRI
Authors: Carlos E. Romero-Mirza, Andrea Banzatti, Karin I. Öberg, Klaus M. Pontoppidan, Colette Salyk, Joan Najita, Geoffrey A. Blake, Sebastiaan Krijt, Nicole Arulanantham, Paola Pinilla, Feng Long, Giovanni Rosotti, Sean M. Andrews, David J. Wilner, Jenny Calahan
Figure caption: Same as Figure 3, but for the extended disk of IQ Tau.
Paper: Retrieval of Thermally Resolved Water Vapor Distributions in Disks Observed with JWST-MIRI
Authors: Carlos E. Romero-Mirza, Andrea Banzatti, Karin I. Öberg, Klaus M. Pontoppidan, Colette Salyk, Joan Najita, Geoffrey A. Blake, Sebastiaan Krijt, Nicole Arulanantham, Paola Pinilla, Feng Long, Giovanni Rosotti, Sean M. Andrews, David J. Wilner, Jenny Calahan
Figure caption: Same as Figure 3, but for the compact disk of GK Tau.
Paper: Retrieval of Thermally Resolved Water Vapor Distributions in Disks Observed with JWST-MIRI
Authors: Carlos E. Romero-Mirza, Andrea Banzatti, Karin I. Öberg, Klaus M. Pontoppidan, Colette Salyk, Joan Najita, Geoffrey A. Blake, Sebastiaan Krijt, Nicole Arulanantham, Paola Pinilla, Feng Long, Giovanni Rosotti, Sean M. Andrews, David J. Wilner, Jenny Calahan
Figure caption: Same as Figure 3, but for the compact disk of HP Tau.
Paper: Retrieval of Thermally Resolved Water Vapor Distributions in Disks Observed with JWST-MIRI
Authors: Carlos E. Romero-Mirza, Andrea Banzatti, Karin I. Öberg, Klaus M. Pontoppidan, Colette Salyk, Joan Najita, Geoffrey A. Blake, Sebastiaan Krijt, Nicole Arulanantham, Paola Pinilla, Feng Long, Giovanni Rosotti, Sean M. Andrews, David J. Wilner, Jenny Calahan
Figure caption: Same as Figure 7, but for GQ Lup.
Paper: Retrieval of Thermally Resolved Water Vapor Distributions in Disks Observed with JWST-MIRI
Authors: Carlos E. Romero-Mirza, Andrea Banzatti, Karin I. Öberg, Klaus M. Pontoppidan, Colette Salyk, Joan Najita, Geoffrey A. Blake, Sebastiaan Krijt, Nicole Arulanantham, Paola Pinilla, Feng Long, Giovanni Rosotti, Sean M. Andrews, David J. Wilner, Jenny Calahan
Figure caption: Same as Figure 7, but for IQ Tau.
Paper: Retrieval of Thermally Resolved Water Vapor Distributions in Disks Observed with JWST-MIRI
Authors: Carlos E. Romero-Mirza, Andrea Banzatti, Karin I. Öberg, Klaus M. Pontoppidan, Colette Salyk, Joan Najita, Geoffrey A. Blake, Sebastiaan Krijt, Nicole Arulanantham, Paola Pinilla, Feng Long, Giovanni Rosotti, Sean M. Andrews, David J. Wilner, Jenny Calahan
Figure caption: Same as Figure 7, but for HP Tau.
Paper: To High Redshift and Low Mass: Exploring the Emergence of Quenched Galaxies and Their Environments at 3 < z < 6 in the Ultra-deep JADES MIRI F770W Parallel
Authors: Stacey Alberts, Christina C. Williams, Jakob M. Helton, Katherine A. Suess, Zhiyuan Ji, Irene Shivaei, Jianwei Lyu, George Rieke, William M. Baker, Nina Bonaventura, Andrew J. Bunker, Stefano Carniani, Stephane Charlot, Emma Curtis-Lake, Francesco D'Eugenio, Daniel J. Eisenstein, Anna de Graaff, Kevin N. Hainline, Ryan Hausen, Benjamin D. Johnson, Roberto Maiolino, Eleonora Parlanti, Marcia J. Rieke, Brant E. Robertson, Yang Sun, Sandro Tacchella, Christopher N. A. Willmer, Chris J. Willott
Figure caption: Photometric redshift and stellar mass distribution of the final, mass-selected sample, cut at log M ⋆/M ⊙ ≥ 8.5. The main panel shows the properties (green circles) derived from fitting including the F770W data point. The histograms show the distributions with (green solid) and without (gray hatched) the F770W flux density.
Paper: To High Redshift and Low Mass: Exploring the Emergence of Quenched Galaxies and Their Environments at 3 < z < 6 in the Ultra-deep JADES MIRI F770W Parallel
Authors: Stacey Alberts, Christina C. Williams, Jakob M. Helton, Katherine A. Suess, Zhiyuan Ji, Irene Shivaei, Jianwei Lyu, George Rieke, William M. Baker, Nina Bonaventura, Andrew J. Bunker, Stefano Carniani, Stephane Charlot, Emma Curtis-Lake, Francesco D'Eugenio, Daniel J. Eisenstein, Anna de Graaff, Kevin N. Hainline, Ryan Hausen, Benjamin D. Johnson, Roberto Maiolino, Eleonora Parlanti, Marcia J. Rieke, Brant E. Robertson, Yang Sun, Sandro Tacchella, Christopher N. A. Willmer, Chris J. Willott
Figure caption: Comparison of the stellar mass measurements down to log M ⋆/M ⊙ = 8.5 with and without the F770W data point. The color bar indicates A  V . The vast majority, save for a few at A  V  ≳ 2, are well fit by a linear relation (orange line) with a scatter of 0.07 dex.
Paper: Retrieval of Thermally Resolved Water Vapor Distributions in Disks Observed with JWST-MIRI
Authors: Carlos E. Romero-Mirza, Andrea Banzatti, Karin I. Öberg, Klaus M. Pontoppidan, Colette Salyk, Joan Najita, Geoffrey A. Blake, Sebastiaan Krijt, Nicole Arulanantham, Paola Pinilla, Feng Long, Giovanni Rosotti, Sean M. Andrews, David J. Wilner, Jenny Calahan
Figure caption: Top: the average column density for cold (blue) and hot (orange) water vapor, extracted from the tapered column density profiles, as a function of mass accretion rate (left) and submillimeter dust disk radius (right). Bottom: same as the top panel, but for the total emitting area of hot and cold water vapor.
Paper: Retrieval of Thermally Resolved Water Vapor Distributions in Disks Observed with JWST-MIRI
Authors: Carlos E. Romero-Mirza, Andrea Banzatti, Karin I. Öberg, Klaus M. Pontoppidan, Colette Salyk, Joan Najita, Geoffrey A. Blake, Sebastiaan Krijt, Nicole Arulanantham, Paola Pinilla, Feng Long, Giovanni Rosotti, Sean M. Andrews, David J. Wilner, Jenny Calahan
Figure caption: Corner plot for the two-temperature fit to FZ Tau. Dashed lines indicate the 1σ percentiles. The 2D histogram contours correspond to the 0.5σ, 1.0σ, 1.5σ, and 2.0σ confidence levels. The histograms have been smoothed by a Gaussian kernel of width 0.02% of the prior span.
Paper: Retrieval of Thermally Resolved Water Vapor Distributions in Disks Observed with JWST-MIRI
Authors: Carlos E. Romero-Mirza, Andrea Banzatti, Karin I. Öberg, Klaus M. Pontoppidan, Colette Salyk, Joan Najita, Geoffrey A. Blake, Sebastiaan Krijt, Nicole Arulanantham, Paola Pinilla, Feng Long, Giovanni Rosotti, Sean M. Andrews, David J. Wilner, Jenny Calahan
Figure caption: Same as Figure 27, but for the exponentially tapered power-law column density fit.
Paper: Retrieval of Thermally Resolved Water Vapor Distributions in Disks Observed with JWST-MIRI
Authors: Carlos E. Romero-Mirza, Andrea Banzatti, Karin I. Öberg, Klaus M. Pontoppidan, Colette Salyk, Joan Najita, Geoffrey A. Blake, Sebastiaan Krijt, Nicole Arulanantham, Paola Pinilla, Feng Long, Giovanni Rosotti, Sean M. Andrews, David J. Wilner, Jenny Calahan
Figure caption: Same as Figure 27, but for the power-law column density fit.
Paper: Retrieval of Thermally Resolved Water Vapor Distributions in Disks Observed with JWST-MIRI
Authors: Carlos E. Romero-Mirza, Andrea Banzatti, Karin I. Öberg, Klaus M. Pontoppidan, Colette Salyk, Joan Najita, Geoffrey A. Blake, Sebastiaan Krijt, Nicole Arulanantham, Paola Pinilla, Feng Long, Giovanni Rosotti, Sean M. Andrews, David J. Wilner, Jenny Calahan
Figure caption: Same as Figure 7, but for CI Tau.
Paper: Retrieval of Thermally Resolved Water Vapor Distributions in Disks Observed with JWST-MIRI
Authors: Carlos E. Romero-Mirza, Andrea Banzatti, Karin I. Öberg, Klaus M. Pontoppidan, Colette Salyk, Joan Najita, Geoffrey A. Blake, Sebastiaan Krijt, Nicole Arulanantham, Paola Pinilla, Feng Long, Giovanni Rosotti, Sean M. Andrews, David J. Wilner, Jenny Calahan
Figure caption: Same as Figure 7, but for AS 209.
Paper: Filamentary Molecular Cloud Formation via Collision-induced Magnetic Reconnection in a Cold Neutral Medium
Authors: Shuo Kong (孔朔), Rowan J. Smith, David Whitworth, Erika T. Hamden
Figure caption: MRCOLA_CNM initial condition in two viewing angles. (a) A view in the x–y plane. Two spherical CNM clouds are in thermal pressure balance with the ambient WNM. They collide at the origin of the Cartesian coordinate system (red) in which the z-axis points toward us (red circle with point, right-hand rule). The colliding velocities are v 1,x  and v 2,x  for the two clouds, respectively. Magnetic fields point toward us (black circles with points) for x < 0 and away from us (black circles with crosses) for x > 0. The collision triggers the formation of the filament (orange) along the y-axis. Note that the filament is imaginary in this initial condition figure. It will form after the cloud collision. (b) A view in the z–x plane. In this view, magnetic fields are parallel to the plane of the sky. The y-axis points toward us (red circle with point), so we see the filament (orange) cross section (again imaginary). The green ellipse marks the location of the compression pancake if there are no magnetic fields. With CMR, the field reconnects at two edges of the pancake and forms a field loop (black dashed arrow curve inside the green ellipse) around the pancake. The magnetic tension squeezes the pancake to the central axis (y-axis), making it a filament. Outside the pancake, the reconnected field forms two half-loops and pulls gas away.
Paper: Filamentary Molecular Cloud Formation via Collision-induced Magnetic Reconnection in a Cold Neutral Medium
Authors: Shuo Kong (孔朔), Rowan J. Smith, David Whitworth, Erika T. Hamden
Figure caption: MRCOLA_CNM density slice plots for the z = 0 plane. The linear color scale shows the total gas density in units of n H,tot. The magenta filled circles show the sinks. The circle size is proportional to the sink mass. The time step is shown at the top right in each panel. The arrows show the velocity vectors. The arrow color scales with the velocity magnitude (the bottom color bar). This slice corresponds to Figure 1(a).
Paper: Full Stokes-vector Inversion of the Solar Mg II h and k Lines
Authors: Hao Li, Tanausú del Pino Alemán, Javier Trujillo Bueno
Figure caption: In the top panels, intensity (in log scale and normalized to the maximum) and Stokes fractional polarization (Q/I, U/I, and V/I) profiles obtained by the CLASP2. The reference direction of the positive Stokes Q is parallel to the solar limb. In the bottom panels, slit-jaw images in the H I Lyα line recorded by CLASP2. The left and right columns correspond to the observations of the plage and limb targets, respectively. The regions delimited by green dashed lines in the top panels indicate the locations of the four spatially averaged profiles in Figures 2–5. The blue lines in the bottom panels indicate the position of the spectrograph’s slit.
Paper: Full Stokes-vector Inversion of the Solar Mg II h and k Lines
Authors: Hao Li, Tanausú del Pino Alemán, Javier Trujillo Bueno
Figure caption: Left column: From top to bottom, Stokes I, Q, U, and V profiles, respectively. The open circles correspond to the temporally and spatially averaged observed Stokes profiles. The solid black curves are the inversion fit. Right column: From top to bottom, horizontal component of the plasma velocity, magnetic field longitudinal component, magnetic field transversal component, and magnetic field azimuth in the plane perpendicular to the LOS, in solid black curves (left axis), respectively, and the real part of the Q = 1 tensor, the imaginary part of the Q = 1 tensor, the real part of the Q = 2 tensor, and the imaginary part of the Q = 2 tensor characterizing the lack of axial symmetry, in dashed red curves (right axis), respectively. The black solid curve in the velocity panel corresponds to the component in the plane containing the LOS and the local vertical (x component), while the blue solid curve corresponds to the component perpendicular to the same plane (y component). This case corresponds to Q-3, a region in the quiet Sun (μ = 0.417 in Figure 1).
Paper: Full Stokes-vector Inversion of the Solar Mg II h and k Lines
Authors: Hao Li, Tanausú del Pino Alemán, Javier Trujillo Bueno
Figure caption: Left column: From top to bottom, Stokes I, Q, U, and V profiles, respectively. The open circles correspond to the temporally and spatially averaged observed Stokes profiles. The dashed–dotted blue and solid black curves are the inversion fits from the first and the second magnetic cycles, respectively, while the dashed orange curves show the profile synthesized in the inverted atmosphere neglecting the magnetic field. Note that the k 1v minimum at around 279.57 nm is blended with a Mn I resonance line and that the corresponding wavelength points are not considered in the inversion, resulting in a straight line in the fit. Right column: From top to bottom, magnetic field strength, magnetic field longitudinal component, magnetic field transversal component, and magnetic field azimuth in the plane perpendicular to the LOS, in solid black (dashed–dotted blue) curves from the second (first) magnetic cycle (left axis), respectively, and the real part of the Q = 1 tensor, the imaginary part of the Q = 1 tensor, the real part of the Q = 2 tensor, and the imaginary part of the Q = 2 tensor characterizing the lack of axial symmetry, in dashed red curves (right axis), respectively. This case corresponds to P-1, a region at the edge of the plage (μ = 0.712 in Figure 1).
Paper: Full Stokes-vector Inversion of the Solar Mg II h and k Lines
Authors: Hao Li, Tanausú del Pino Alemán, Javier Trujillo Bueno
Figure caption: From top to bottom (top three panels in the left column): Stokes Q, U, and V profiles, respectively. The open circles correspond to the temporally and spatially averaged observed Stokes profiles. From left to right and top to bottom (top three panels in the second and third columns): longitudinal component of the magnetic field, magnetic field strength, transversal component of the magnetic field, magnetic field inclination with respect to the local vertical, magnetic field azimuth in the plane perpendicular to the LOS, and magnetic field azimuth in the local vertical reference frame, respectively. From left to right (bottom row): the real part of the Q = 1 tensor, the imaginary part of the Q = 1 tensor, the real part of the Q = 2 tensor, and the imaginary part of the Q = 2 tensor characterizing the lack of axial symmetry, respectively. The solid black, and dashed blue, red, orange and pink curves correspond to the fit and inferred quantities from the inversion when including different combinations of horizontal inhomogeneity parameters as free parameters (see legend in the top-left panel and see text for the description of the labels). The inferred quantities for the orange and pink cases are not shown because they do not fit the observations. This case corresponds to a region at the edge of the plage (μ = 0.712 in Figure 1).
Paper: Full Stokes-vector Inversion of the Solar Mg II h and k Lines
Authors: Hao Li, Tanausú del Pino Alemán, Javier Trujillo Bueno
Figure caption: Left column: From top to bottom, Stokes I, Q, U, and V profiles, respectively. The open circles correspond to the temporally and spatially averaged observed Stokes profiles. The solid black (blue) curves are the inversion fits when accounting for (neglecting) the parameters for the horizontal inhomogeneity. Right column: From top to bottom, magnetic field strength, magnetic field longitudinal component, magnetic field transversal component, and magnetic field azimuth in the plane perpendicular to the LOS, in solid black (blue) curves for the inversion accounting for (neglecting) the parameters for the horizontal inhomogeneity (left axis), respectively, and the real part of the Q = 1 tensor, the imaginary part of the Q = 1 tensor, the real part of the Q = 2 tensor, and the imaginary part of the Q = 2 tensor characterizing the lack of axial symmetry, in dashed red curves (right axis), respectively. This case corresponds to Q-1, a region in the quiet Sun (μ = 0.563 in Figure 1).
Paper: Full Stokes-vector Inversion of the Solar Mg II h and k Lines
Authors: Hao Li, Tanausú del Pino Alemán, Javier Trujillo Bueno
Figure caption: From top to bottom (top three panels in the left column): Stokes Q, U, and V profiles, respectively. The open circles correspond to the temporally and spatially averaged observed Stokes profiles. From left to right and top to bottom (top three panels in the second and third columns): longitudinal component of the magnetic field, magnetic field strength, transversal component of the magnetic field, magnetic field inclination with respect to the local vertical, magnetic field azimuth in the plane perpendicular to the LOS, and magnetic field azimuth in the local vertical reference frame, respectively. From left to right (bottom row): horizontal component of the plasma velocity in the plane containing the LOS and the local vertical, horizontal component of the plasma velocity perpendicular to the same plane and the vertical, the real part of the Q = 1 tensor, and the imaginary part of the Q = 2 tensor characterizing the lack of axial symmetry, respectively. The solid black, and dashed blue, red, orange and pink curves correspond to the fit and inferred quantities from the inversion when including different combinations of horizontal inhomogeneity parameters in the inversion (see legend in the top-left panel and see text for the description of the labels). This case corresponds to a region in the quiet Sun (μ = 0.417 in Figure 1).
Paper: Full Stokes-vector Inversion of the Solar Mg II h and k Lines
Authors: Hao Li, Tanausú del Pino Alemán, Javier Trujillo Bueno
Figure caption: Same as Figure 3, but for Q-2, the region in the quiet Sun with μ = 0.101 (see Figure 1).
Paper: Full Stokes-vector Inversion of the Solar Mg II h and k Lines
Authors: Hao Li, Tanausú del Pino Alemán, Javier Trujillo Bueno
Figure caption: From top to bottom, the intensity I and Stokes Q, U, and V profiles for the spatial average at μ = 0.712 (dashed black curve; see Figure 2). The colored solid curves show the profiles for the individual pixels included in the average. The y-axis units are the same as those in Figure 2.
Paper: Probing Cold-to-temperate Exoplanetary Atmospheres: The Role of Water Condensation on Surface Identification with JWST
Authors: Ziyu Huang, 子钰 黄, Xinting Yu, 馨婷 余, Shang-Min Tsai, Julianne I. Moses, Kazumasa Ohno, Joshua Krissansen-Totton, Xi Zhang, Jonathan J. Fortney
Figure caption: Simulated VMR profiles for the main chemical species for K2-18 b with A b = 0.56 (T eq = 227 K) for the shallow case and deep case, with and without water condensation (solid and dashed lines); the black dashed–dotted line shows the saturation vapor mixing ratio of water.
Paper: Probing Cold-to-temperate Exoplanetary Atmospheres: The Role of Water Condensation on Surface Identification with JWST
Authors: Ziyu Huang, 子钰 黄, Xinting Yu, 馨婷 余, Shang-Min Tsai, Julianne I. Moses, Kazumasa Ohno, Joshua Krissansen-Totton, Xi Zhang, Jonathan J. Fortney
Figure caption: Simulated VMR profiles for the main chemical species for LHS 1140 b with A b = 0.3 (T eq = 214 K) for the shallow and deep cases, with and without water condensation. The notations are the same as in Figure 2.
Paper: The BANANA Project. VII. High Eccentricity Predicts Spin–Orbit Misalignment in Binaries
Authors: Marcus L. Marcussen, Simon H. Albrecht, Joshua N. Winn, Yubo Su, Mia S. Lundkvist, Kevin C. Schlaufman
Figure caption: High obliquities are associated with high orbital eccentricity. The results for the spin–orbit alignment of our binary star sample are shown as a function of eccentricity in five bins. The eccentricity ranges are indicated by horizontal bars and vertical bars represent the one-sigma confidence intervals for 〈ψ〉. Pink, green and black signify edge-on, face-on, and combined results, respectively. The green error bars were displaced slightly to the right to avoid overlapping with the pink error bars.
Paper: The BANANA Project. VII. High Eccentricity Predicts Spin–Orbit Misalignment in Binaries
Authors: Marcus L. Marcussen, Simon H. Albrecht, Joshua N. Winn, Yubo Su, Mia S. Lundkvist, Kevin C. Schlaufman
Figure caption: Biases due to secondary stars. The distribution and means (dashed lines) of the normalized vbroad, ﹩\widehat{{\mathtt{vbroad}}}﹩, are shown in the left column, and those of the vbroad uncertainty in the right column. Our sample is split into edge-on and face-on systems in the top row, split into low and high eccentricities in the middle row and split into low and high orbital periods in the bottom row. These results suggest that spin–orbit alignment is the primary cause of the observed difference in vbroad and that light from secondary companions causes at most a minimal bias.
Paper: The BANANA Project. VII. High Eccentricity Predicts Spin–Orbit Misalignment in Binaries
Authors: Marcus L. Marcussen, Simon H. Albrecht, Joshua N. Winn, Yubo Su, Mia S. Lundkvist, Kevin C. Schlaufman
Figure caption: Edge- and face-on alignment. Top two panels: Each colored distribution shows the probability of making a certain measurement of ﹩\langle \widehat{{\mathtt{vbroad}}}\rangle ﹩, given an assumed degree of spin–orbit alignment (quantified by 〈ψ〉). Vertical lines mark the observed values of ﹩\langle \widehat{{\mathtt{vbroad}}}\rangle ﹩ across all eccentricities, for the edge-on sample (top) and the face-on sample (middle). Bottom panel: The posterior PDF of 〈ψ〉 derived from the edge-on (pink) and face-on (green) samples, as well as their combination (black). The gray shading shows 1σ  uncertainties. The results of analyzing the two subsets are compatible, and the face-on sample gives tighter constraints.
Paper: Probing Cold-to-temperate Exoplanetary Atmospheres: The Role of Water Condensation on Surface Identification with JWST
Authors: Ziyu Huang, 子钰 黄, Xinting Yu, 馨婷 余, Shang-Min Tsai, Julianne I. Moses, Kazumasa Ohno, Joshua Krissansen-Totton, Xi Zhang, Jonathan J. Fortney
Figure caption:  P–T profiles of K2-18 b (top) and LHS 1140 b (bottom) with albedo from 0 to 0.75. Dashed lines are condensation curves of H2O (purple for sublimation and brown for vaporization) following Equations (1) and (2). These condensation curves are constructed by using e s /XH2O, where we assumed the mixing ratio of water, XH2O = 0.1.