adsabs/AstroCLIMB huggingface dataset:
Paper: The First Detection of Molecular Activity in the Largest Known Oort Cloud Comet: ALMA Imaging of C/2014 UN271 (Bernardinelli–Bernstein) at 16.6 au from the Sun
Authors: Nathan X. Roth, Stefanie N. Milam, Martin A. Cordiner, Dominique Bockelée-Morvan, Nicolas Biver, Michael S. P. Kelley, Anthony J. Remijan, Steven B. Charnley, Carrie E. Holt, Kiernan D. Foster, Joseph Chatelain, Edward Gomez, Sarah Greenstreet, Tim Lister, Helen Usher
Figure caption: (A)–(C) Spectrally integrated flux maps for CO on 2024 March 17, with traces and labels as in Figure 1. Contour intervals in each map are in 1σ increments of the rms noise, with the lowest contour being 3σ. Panel (A) is at the native angular resolution, whereas panel (B) shows the same map with a 2″ Gaussian uv taper. Panel (C) compares the integrated red and blue components of the CO line against the continuum (heatmap) as in Figure 1B. (D) Comparison of autocorrelation and interferometric CO spectra on March 8 and 17. The solid blue, dashed red, and solid red vertical lines correspond to speeds of −0.38 km s−1, 0.066 km s−1, and 0.21 km s−1, respectively, highlighting the consistency of the blue CO component and variation in the red components.
Paper: The First Detection of Molecular Activity in the Largest Known Oort Cloud Comet: ALMA Imaging of C/2014 UN271 (Bernardinelli–Bernstein) at 16.6 au from the Sun
Authors: Nathan X. Roth, Stefanie N. Milam, Martin A. Cordiner, Dominique Bockelée-Morvan, Nicolas Biver, Michael S. P. Kelley, Anthony J. Remijan, Steven B. Charnley, Carrie E. Holt, Kiernan D. Foster, Joseph Chatelain, Edward Gomez, Sarah Greenstreet, Tim Lister, Helen Usher
Figure caption: (A) CO spectrum in UN271 on March 8 (black), with each panel representing spectra extracted from differing baseline ranges (angular scales). The spectra are displayed with a frequency resolution of 61 kHz (velocity resolution 0.08 km s−1). The best-fit model is overplotted in red. (B) Real part of the observed visibility amplitude as a function of projected baseline length for CO on March 8. The upper limit daughter model, as well as a parent model, are overplotted for comparison. The uv distance has been plotted in units of kλ. (C)–(D) Plots for March 17 with traces and labels as in panels (A)–(B).
Paper: The First Detection of Molecular Activity in the Largest Known Oort Cloud Comet: ALMA Imaging of C/2014 UN271 (Bernardinelli–Bernstein) at 16.6 au from the Sun
Authors: Nathan X. Roth, Stefanie N. Milam, Martin A. Cordiner, Dominique Bockelée-Morvan, Nicolas Biver, Michael S. P. Kelley, Anthony J. Remijan, Steven B. Charnley, Carrie E. Holt, Kiernan D. Foster, Joseph Chatelain, Edward Gomez, Sarah Greenstreet, Tim Lister, Helen Usher
Figure caption: Optical lightcurve of comet UN271 vs. time from 2024 February 29.0 (UTC) based on g-band photometry (circles) and r-band photometry (squares). The g-band data have been scaled by the color of the comet (–0.46 mag) to match the r-band photometry. Vertical dashed lines mark the times of the ALMA observations.
Paper: The First Detection of Molecular Activity in the Largest Known Oort Cloud Comet: ALMA Imaging of C/2014 UN271 (Bernardinelli–Bernstein) at 16.6 au from the Sun
Authors: Nathan X. Roth, Stefanie N. Milam, Martin A. Cordiner, Dominique Bockelée-Morvan, Nicolas Biver, Michael S. P. Kelley, Anthony J. Remijan, Steven B. Charnley, Carrie E. Holt, Kiernan D. Foster, Joseph Chatelain, Edward Gomez, Sarah Greenstreet, Tim Lister, Helen Usher
Figure caption: (A)–(B) Continuum visibilities on March 8 and March 17, with various nucleus and coma models overplotted. The uv distance has been plotted in units of kλ.
Paper: The First Detection of Molecular Activity in the Largest Known Oort Cloud Comet: ALMA Imaging of C/2014 UN271 (Bernardinelli–Bernstein) at 16.6 au from the Sun
Authors: Nathan X. Roth, Stefanie N. Milam, Martin A. Cordiner, Dominique Bockelée-Morvan, Nicolas Biver, Michael S. P. Kelley, Anthony J. Remijan, Steven B. Charnley, Carrie E. Holt, Kiernan D. Foster, Joseph Chatelain, Edward Gomez, Sarah Greenstreet, Tim Lister, Helen Usher
Figure caption: (A)–(C) Measured and estimated fluxes for the quasar flux calibrators in this study, illustrating our estimation of the 233 GHz flux for J0538-4405 on March 8.
Paper: Evidence of Gaia Enceladus Experiencing at Least Two Passages around the Milky Way 
Authors: Ása Skúladóttir, Heitor Ernandes, Diane K. Feuillet, Alice Mori, Sofia Feltzing, Romain E. R. Lucchesi, Paola Di Matteo
Figure caption: Chemical abundances for the NS accreted stellar sample with low (pink circles) and high (green triangles) energies, as defined in Figure 2. For reference, the thick disk and high-α Milky Way populations created in situ are shown with small black crosses and blue circles, respectively. Representative error bars are shown in the bottom left corner of each panel.
Paper: NIRCam Yells at Cloud: JWST MIRI Imaging Can Directly Detect Exoplanets of the Same Temperature, Mass, Age, and Orbital Separation as Saturn and Jupiter
Authors: Rachel Bowens-Rubin, James Mang, Mary Anne Limbach, Aarynn L. Carter, Kevin B. Stevenson, Kevin Wagner, Giovanni Strampelli, Caroline V. Morley, Grant Kennedy, Elisabeth Matthews, Andrew Vanderburg, Maïssa Salama
Figure caption: Coldest planet detectable by distance to S/N = 3. To evaluate the trade space between F444W NIRCam coronagraphy and F2100W MIRI imaging, we compared the coldest planet detectable in the background-limited regime at S/N = 3 for both modes out to 70 pc. This plot was constructed using the measured background limits in apparent magnitude for EV Lac (M4V): F444W = 20.8 and F2100W = 15.75. The blue lines represent the detection limits for NIRCam F444W+MASK335, while the red lines indicate the limits for MIRI F2100W. These limits are shown for three atmospheric cases in equilibrium: clear, cloudy (fsed = 8), and maximally cloudy. Planets in the gray region fall below all detection limits and cannot be observed with either instrument mode. Planets in the green region are hot enough to be detected by both modes, regardless of their atmospheric properties. The red region marks planets that are always detectable with MIRI F2100W but only detectable with NIRCam F444W+MASK if they have a clear atmosphere. The light-blue region contains planets undetectable with MIRI F2100W but potentially detectable with NIRCam F444W+MASK if they have a clear atmosphere. The dark-blue region marks planets too faint for MIRI F2100W but bright enough to always be detected with NIRCam F444W+MASK, regardless of their atmospheric properties. MIRI F2100W provides a detection advantage that is independent of atmospheric conditions for systems within 20 pc. A Jupiter-temperature planet can be detected using MIRI F2100W within 7 pc, while a Saturn-temperature planet can be detected within 3 pc.
Paper: NIRCam Yells at Cloud: JWST MIRI Imaging Can Directly Detect Exoplanets of the Same Temperature, Mass, Age, and Orbital Separation as Saturn and Jupiter
Authors: Rachel Bowens-Rubin, James Mang, Mary Anne Limbach, Aarynn L. Carter, Kevin B. Stevenson, Kevin Wagner, Giovanni Strampelli, Caroline V. Morley, Grant Kennedy, Elisabeth Matthews, Andrew Vanderburg, Maïssa Salama
Figure caption: NIRCam F444W+MASK335R and MIRI F2100W contrast curves. The measured S/N = 3 (solid) and S/N = 5 (dotted) sensitivities for NIRCam F444W coronagraphy and MIRI F2100W imaging are shown for Wolf 359 (dark blue/red) and EV Lac (light blue/orange). In approximately 1 hr of integration, the NIRCam observations reached the S/N = 3 background-limited regime at a contrast of 6 × 10−7 by a separation of 2﹩\mathop{.}\limits^{\unicode{x02033}}﹩6. The MIRI imaging observations reached the S/N = 3 background-limited regime by a similar separation. Panels (e) and (f) show the NIRCam and MIRI sensitivity in units of absolute magnitude vs. au as compared to the absolute magnitude of Jupiter (green dotted line) and Saturn (purple dashed–dotted line) measured from their spectra. An exoplanet the same magnitude as the measured absolute magnitude of Saturn could be detected orbiting Wolf 359 using MIRI imaging but not NIRCam coronagraphy, highlighting the advantages of using MIRI imaging in this empirically bounded case.
Paper: NIRCam Yells at Cloud: JWST MIRI Imaging Can Directly Detect Exoplanets of the Same Temperature, Mass, Age, and Orbital Separation as Saturn and Jupiter
Authors: Rachel Bowens-Rubin, James Mang, Mary Anne Limbach, Aarynn L. Carter, Kevin B. Stevenson, Kevin Wagner, Giovanni Strampelli, Caroline V. Morley, Grant Kennedy, Elisabeth Matthews, Andrew Vanderburg, Maïssa Salama
Figure caption: Comparison of Jupiter/Saturn measured spectra with clear and cloudy equilibrium models. The measured spectra of Jupiter and Saturn were scaled to the distance of Wolf 359 (2.4 pc) for comparison with clear and cloudy models. The horizontal lines represent detection limits for various JWST instrument modes: NIRCam F444W coronagraphy (blue), MIRI F2100W imaging (red), MIRI coronagraphy (gold), and MIRI imaging (black). When the spectra exceed the instrument limit, the flux can be detected using that mode. Most JWST modes could detect a true Jupiter analog orbiting Wolf 359 at separations in the background-limited region of the contrast curve. However, when considering the case of a true Saturn analog, NIRCam F444W coronagraphy is only capable of detecting a Saturn-temperature exoplanet if the planet has a clear atmosphere.
Paper: NIRCam Yells at Cloud: JWST MIRI Imaging Can Directly Detect Exoplanets of the Same Temperature, Mass, Age, and Orbital Separation as Saturn and Jupiter
Authors: Rachel Bowens-Rubin, James Mang, Mary Anne Limbach, Aarynn L. Carter, Kevin B. Stevenson, Kevin Wagner, Giovanni Strampelli, Caroline V. Morley, Grant Kennedy, Elisabeth Matthews, Andrew Vanderburg, Maïssa Salama
Figure caption: GO 6122 sensitivity to cold planets assuming three varying atmospheric conditions. We converted our measured S/N = 3 (solid) and S/N = 5 (dotted) contrast curves into estimates of the effective temperatures of a potentially detectable exoplanet. We adopt three atmosphere cases: clear (left), cloudy equilibrium with fsed = 8 (middle), and maximum cloud (right). While the limits for MIRI F2100W imaging and NIRCam F444W coronagraphy are similar assuming a planet with a clear atmosphere, MIRI F2100W imaging can be more sensitive to cold planets by more than 100 K if the planet has a cloudy atmosphere. We caution that the fsed = 8 cloudy equilibrium model set is only mildly cloudy—both Saturn and TWA 7b are significantly cloudier (fsed = 3–4; A. M. Lagrange et al. 2025). As a result, the middle panel may be overly optimistic for NIRCam and not fully representative of typical cloudiness levels on cold planets.
Paper: NIRCam Yells at Cloud: JWST MIRI Imaging Can Directly Detect Exoplanets of the Same Temperature, Mass, Age, and Orbital Separation as Saturn and Jupiter
Authors: Rachel Bowens-Rubin, James Mang, Mary Anne Limbach, Aarynn L. Carter, Kevin B. Stevenson, Kevin Wagner, Giovanni Strampelli, Caroline V. Morley, Grant Kennedy, Elisabeth Matthews, Andrew Vanderburg, Maïssa Salama
Figure caption: Wolf 359 images from NIRCam (blue) and MIRI (red) before and after PSF subtraction. PSF subtraction was performed in order to improve the sensitivity to finding faint astrophysical sources near the star. The white circle represents an angular separation of 15 au for the Wolf 359 system. The dark spots in the background of the PSF-subtracted frames are due to positive sources in the reference-star frames; this issue is expected to be mitigated in future analysis when additional reference stars are available. In the MIRI F2100W frames, an image artifact is present approximately 75 pixels above the center of the star. Future proper motion follow-up observations are needed to identify whether uncataloged point sources are comoving companions.
Paper: NIRCam Yells at Cloud: JWST MIRI Imaging Can Directly Detect Exoplanets of the Same Temperature, Mass, Age, and Orbital Separation as Saturn and Jupiter
Authors: Rachel Bowens-Rubin, James Mang, Mary Anne Limbach, Aarynn L. Carter, Kevin B. Stevenson, Kevin Wagner, Giovanni Strampelli, Caroline V. Morley, Grant Kennedy, Elisabeth Matthews, Andrew Vanderburg, Maïssa Salama
Figure caption: Planet brightness estimates for clear and cloudy cold giant exoplanets using equilibrium models. The absolute magnitude estimates for a clear atmosphere (dashed line, open circle) and a cloudy atmosphere (solid line, filled symbols) are shown for NIRCam F444W coronagraphy (left in blue) and MIRI F2100W imaging (right in red). The absolute magnitudes were estimated using the custom cold giant planet models described in Section 4.1. The maximum-cloud model magnitudes (open circles) were computed using the SED of a blackbody. While the magnitude at F2100W is equally capable of detecting clear and cloudy planets, the F444W magnitude varies significantly depending on cloud conditions.
Paper: Evidence of Gaia Enceladus Experiencing at Least Two Passages around the Milky Way 
Authors: Ása Skúladóttir, Heitor Ernandes, Diane K. Feuillet, Alice Mori, Sofia Feltzing, Romain E. R. Lucchesi, Paola Di Matteo
Figure caption: Chemical abundances for the accreted stellar sample with low (pink circles) and high (green triangles) energies, as defined in Figure 2. The average values for [Al/Fe] are shown with a line, while the shaded area shows the error of the mean. For [Mg/Fe] and [Mg/Ba], trend lines are shown with 68% confidence interval. Other abundance ratios are shown in Appendix B. Top marginal plot shows the metallicity distribution of the accreted samples. For reference, the thick disk and high-α Milky Way populations created in situ are shown with small black crosses and blue circles, respectively. Representative error bar for individual measurements is shown in the bottom left corner.
Paper: Evidence of Gaia Enceladus Experiencing at Least Two Passages around the Milky Way 
Authors: Ása Skúladóttir, Heitor Ernandes, Diane K. Feuillet, Alice Mori, Sofia Feltzing, Romain E. R. Lucchesi, Paola Di Matteo
Figure caption: Simulation of Gaia Enceladus falling into the Milky Way (A. Mori et al. 2024). Top panels show the energy and angular momentum (E–Lz) relation for the accreted stars (small points) that are now residing in the Milky Way. Left panel shows all stars and the right panel those at a Sun-like distance from the Galactic center (7–9 kpc). Color-coding at a given point in (E–Lz) shows the average position of stars in Gaia Enceladus before the merger—the outskirts in green and the inner regions in pink, as shown by the bottom panels. Star symbols (white to blue) show how the barycenter of Gaia Enceladus loses energy and angular momentum with time and more passages through the Milky Way.
Paper: Evidence of Gaia Enceladus Experiencing at Least Two Passages around the Milky Way 
Authors: Ása Skúladóttir, Heitor Ernandes, Diane K. Feuillet, Alice Mori, Sofia Feltzing, Romain E. R. Lucchesi, Paola Di Matteo
Figure caption: Energy and angular momentum (E–Lz) relation of observed stars. Accreted stars (low α) are separated into high and low energies, shown with green triangles and pink circles, respectively. Thick disk stars are shown with black crosses; high-α stars are shown with blue circles. The point size increases with decreasing [Fe/H]. For comparison, Milky Way field stars from APOGEE Data Release 17 are shown with small gray dots (S. R. Majewski et al. 2017; Abdurro’uf et al. 2022), selected as described in S. Feltzing & D. Feuillet (2023).
Paper: Evidence of Gaia Enceladus Experiencing at Least Two Passages around the Milky Way 
Authors: Ása Skúladóttir, Heitor Ernandes, Diane K. Feuillet, Alice Mori, Sofia Feltzing, Romain E. R. Lucchesi, Paola Di Matteo
Figure caption: Same as Figure 3 but for different cuts in energy: Ecut = −3.5 × 104 km2 s−2 (left) and Ecut = −5.5 × 104 km2 s−2 (right). Chemical abundances for the accreted stellar sample with low (pink circles, E < Ecut) and high (green triangles, E > Ecut) energies. Lines in the [Al/Fe] panels show average values of the two subsamples, while shaded areas are the error of the mean. In the [Mg/Fe] and [Mg/Ba] panels, trend lines are shown with 68% confidence interval. Top marginal plot shows the metallicity distribution of the accreted samples. For reference, the thick disk and high-α Milky Way populations created in situ are shown with small black crosses and blue circles, respectively. Representative error bars for individual stars are shown in the bottom left corner.
Paper: Evidence of Gaia Enceladus Experiencing at Least Two Passages around the Milky Way 
Authors: Ása Skúladóttir, Heitor Ernandes, Diane K. Feuillet, Alice Mori, Sofia Feltzing, Romain E. R. Lucchesi, Paola Di Matteo
Figure caption: Schematic figure showing how Gaia Enceladus fell into the potential of the Milky Way. First to be accreted with high kinetic energies are the outermost stars of Gaia Enceladus (green), from regions with less efficient star formation. These stars can subsequently be recognized by their lower [Mg/Fe] ratios at a given [Fe/H]. Conversely, the stars that originally resided closer to the center of Gaia Enceladus (pink) are accreted in later passages, thus having lower orbital energies and the chemical signatures of more efficient star formation (e.g., higher [Mg/Fe] at high [Fe/H]).
Paper: 3D Simulations Demonstrate Propagating Thermohaline Convection for Polluted White Dwarfs
Authors: Imogen G. Cresswell, Adrian E. Fraser, Evan B. Bauer, Evan H. Anders, Benjamin P. Brown
Figure caption: Vertical profiles of composition (top left), reduced density ratio (top right), advective flux (bottom left), and ratio of advective to diffusive flux (bottom right) at different times for the same simulation as in Figure 2. Lighter colors correspond to later times, and the dashed line in the top left shows the initial profile. The thermohaline front propagates into the thermohaline-stable zone and mixes, partially relaxing the initial composition gradient. But due to the constant flux of high-metallicity material from the top boundary, the upper region remains unstable and drives more turbulent than diffusive flux.
Paper: 3D Simulations Demonstrate Propagating Thermohaline Convection for Polluted White Dwarfs
Authors: Imogen G. Cresswell, Adrian E. Fraser, Evan B. Bauer, Evan H. Anders, Benjamin P. Brown
Figure caption: Bulk reduced density ratio r (left) and front location zfront (right) over time for a set of simulations varying Pr and τ. After a brief period of rapid increase, r grows only very slowly and, importantly, remains below 1. Smaller Pr results in a smaller (more unstable) final r, with a similar trend in reducing τ. Smaller Pr also results in faster front propagation.
Paper: 3D Simulations Demonstrate Propagating Thermohaline Convection for Polluted White Dwarfs
Authors: Imogen G. Cresswell, Adrian E. Fraser, Evan B. Bauer, Evan H. Anders, Benjamin P. Brown
Figure caption: Horizontally averaged profiles of vertical velocity (top), turbulent composition flux (middle), and ratio of turbulent to diffusive flux (bottom) at different stages of front propagation for the same simulations as are shown in Figure 4. The black dashed line shows the location of the front, zfront, with insets focusing on this region. Vertical velocity and turbulent fluxes show an overshoot region with fluid motions extending past the stability boundary and driving additional flux beyond the diffusive flux.
Paper: 3D Simulations Demonstrate Propagating Thermohaline Convection for Polluted White Dwarfs
Authors: Imogen G. Cresswell, Adrian E. Fraser, Evan B. Bauer, Evan H. Anders, Benjamin P. Brown
Figure caption: Vertical velocity (pink) and turbulent composition fluxes (green) vs. R0 for simulation data (points) compared to BGS13 (solid) and Kippenhahn (dashed) model predictions.
Paper: The First Detection of Molecular Activity in the Largest Known Oort Cloud Comet: ALMA Imaging of C/2014 UN271 (Bernardinelli–Bernstein) at 16.6 au from the Sun
Authors: Nathan X. Roth, Stefanie N. Milam, Martin A. Cordiner, Dominique Bockelée-Morvan, Nicolas Biver, Michael S. P. Kelley, Anthony J. Remijan, Steven B. Charnley, Carrie E. Holt, Kiernan D. Foster, Joseph Chatelain, Edward Gomez, Sarah Greenstreet, Tim Lister, Helen Usher
Figure caption: (A)–(B) Continuum flux maps for UN271 on 2024 March 8 and 17, with traces and labels as in Figure 1. Contour intervals in each map are in 5σ increments of the rms noise, with the lowest contour being 5σ.
Paper: The First Detection of Molecular Activity in the Largest Known Oort Cloud Comet: ALMA Imaging of C/2014 UN271 (Bernardinelli–Bernstein) at 16.6 au from the Sun
Authors: Nathan X. Roth, Stefanie N. Milam, Martin A. Cordiner, Dominique Bockelée-Morvan, Nicolas Biver, Michael S. P. Kelley, Anthony J. Remijan, Steven B. Charnley, Carrie E. Holt, Kiernan D. Foster, Joseph Chatelain, Edward Gomez, Sarah Greenstreet, Tim Lister, Helen Usher
Figure caption: (A)–(B) Δχ2 analysis for the CO Lp in UN271 on March 8 and 17.
Paper: On the Origins of Coronal Alfvénic Waves
Authors: Richard J. Morton, Roberto Soler
Figure caption: Results of fit to enhancement only. The information is identical in both plots, with the only difference being the scaling of the vertical axes. The measured power spectra from the Doppler velocities (minus the estimated power law and data noise) are shown as the gray circles with uncertainties. The posterior mean model of the power enhancement from Equation (5) is shown as the solid blue line, and the 94% highest-density interval is indicated by the shaded blue region. The contribution of upwardly propagating Alfvénic waves excited in the photosphere is indicated by the purple dashed–dotted curve. The pink dashed curve indicates a coarse estimate for the contribution from mode conversion of p-modes to the coronal Alfvénic waves.
Paper: On the Origins of Coronal Alfvénic Waves
Authors: Richard J. Morton, Roberto Soler
Figure caption: The coronal power spectrum. The measured power spectra from the Doppler velocities are shown as the gray circles with uncertainties. The posterior mean model of Equation (5) is shown as the solid blue line, and the 94% highest-density interval is indicated by the shaded blue region. In addition to this, we display the posterior mean estimates for the power-law component (yellow dashed), the data noise (gray dashed), and the component of the power from the upwardly propagating, photospheric-driven Alfvénic waves (purple dashed–dotted line).
Paper: On the Origins of Coronal Alfvénic Waves
Authors: Richard J. Morton, Roberto Soler
Figure caption: Sketch of Alfvénic wave arising from interchange reconnection between chromospheric loops in the internetwork field and the network field.
Paper: On the Origins of Coronal Alfvénic Waves
Authors: Richard J. Morton, Roberto Soler
Figure caption: Posterior distributions for the fraction of the coronal Doppler velocity power spectrum provided by each source. Purple corresponds to the photospheric-driven Alfvénic waves, fuchsia corresponds to the p-modes, and light blue corresponds to the unknown source.
Paper: The Sulfur Plume in the Horsehead Nebula: New Detections of S2H, SH+, and CO+
Authors: A. Fuente, G. Esplugues, P. Rivière-Marichalar, D. Navarro-Almaida, R. Martín-Doménech, G. M. Muñoz-Caro, A. Sánchez-Monge, A. Taillard, H. Carrascosa, J. J. Miranzo-Pastor, A. Tasa-Chaveli, P. Fernández-Ruiz, V. V. Guzmán, J. R. Goicoechea, M. Gerin, J. Pety
Figure caption: Rotational diagram of S2H based on 30 m data from A. Fuente et al. (2017; black squares) and the ALMA TP data presented in this work (red squares) assuming a beam-filling factor of 1. It should be noticed that the assumed beam-filling factor is not relevant for the calculation of Trot since the observations were performed with similar angular resolution (HPBW ∼24″–29″).
Paper: Potential-driven Metal Cycling: JADES Census of Gas-phase Metallicity for Galaxies at 1 < z < 7
Authors: Cheng Jia, Enci Wang, Cheqiu Lyu, Chengyu Ma, Jie Song, Yangyao Chen, Kai Wang, Haoran Yu, Zeyu Chen, Jinyang Wang, Yifan Wang, Xu Kong
Figure caption: Similar to Figure 3, but for galaxies z > 3.