adsabs/AstroCLIMB huggingface dataset:
Paper: JWST-TST DREAMS: The Nightside Emission and Chemistry of WASP-17b
Authors: Jacob Lustig-Yaeger, Kristin S. Sotzen, Kevin B. Stevenson, Shang-Min Tsai, Ryan C. Challener, Jayesh Goyal, Nikole K. Lewis, Dana R. Louie, L. C. Mayorga, Daniel Valentine, Hannah R. Wakeford, Lili Alderson, Natalie H. Allen, Thomas J. Fauchez, Ana Glidden, Amélie Gressier, Sarah M. Hörst, Jingcheng Huang, Zifan Lin, Avi M. Mandell, Elijah Mullens, Sarah Peacock, Edward W. Schwieterman, Jeff A. Valenti, C. Matt Mountain, Marshall Perrin, Roeland P. van der Marel
Figure caption: PIE spectra from the dayside (orange and red points) and nightside (blue and cyan points) of WASP-17b. Dayside and Nightside 1 and 2 represent the pre-ingress and post-egress baseline spectra, respectively. The secondary eclipse dayside spectrum extracted using traditional methods is shown in black. Simple blackbody curves show the expected planet flux near the equilibrium temperature of WASP-17b (1700 K; pink line) and at 1000 K (navy blue line), for reference.
Paper: JWST-TST DREAMS: The Nightside Emission and Chemistry of WASP-17b
Authors: Jacob Lustig-Yaeger, Kristin S. Sotzen, Kevin B. Stevenson, Shang-Min Tsai, Ryan C. Challener, Jayesh Goyal, Nikole K. Lewis, Dana R. Louie, L. C. Mayorga, Daniel Valentine, Hannah R. Wakeford, Lili Alderson, Natalie H. Allen, Thomas J. Fauchez, Ana Glidden, Amélie Gressier, Sarah M. Hörst, Jingcheng Huang, Zifan Lin, Avi M. Mandell, Elijah Mullens, Sarah Peacock, Edward W. Schwieterman, Jeff A. Valenti, C. Matt Mountain, Marshall Perrin, Roeland P. van der Marel
Figure caption: PHOENIX stellar model fit (blue points) to the calibrated stellar spectrum of WASP-17A observed with NIRSpec G395H using the NRS1 detector (black points). The relative residuals between the data and model are scattered around zero, with a standard deviation of ∼1.3%. The thermal emission from the planet must exceed this data–model noise floor for extraction of the PIE signal. In this case, WASP-17b’s average dayside planet-to-star flux ratio in NRS1 is measured at 0.133% (indicated in the lower panel), approximately 10 times below our model-derived limit.
Paper: The Hubble Tension Resolved by the DESI Baryon Acoustic Oscillations Measurements
Authors: X. D. Jia, J. P. Hu, D. H. Gao, S. X. Yi, F. Y. Wang
Figure caption: Fitting results of the equation of state w(z) of dark energy with the nonparametric method using BAO and SNe Ia. (a) The black points represent the best-fit values of w(z) with 1σ confidence level (red bar) at different redshift bins using the DESI DR2 BAO measurements and Pantheon plus SNe Ia sample. The black dashed line represents the standard ΛCDM model with w(z) = −1. The redshift intervals of the bins are shown in the blue bars. A descending trend of w(z) is found. It crosses w = −1, suggesting quintom-like behavior. (b) Same as panel (a), but for the DESI DR2 BAO measurements and DESY5 SNe Ia sample. The w(z) values in panels (a) and (b) are consistent within 1σ confidence level.
Paper: The Hubble Tension Resolved by the DESI Baryon Acoustic Oscillations Measurements
Authors: X. D. Jia, J. P. Hu, D. H. Gao, S. X. Yi, F. Y. Wang
Figure caption: Fitting results of the equation of state w(z) of dark energy with the nonparametric method. (a) The black points represent the best-fit values of w(z) with 1σ confidence level (red bar) at different redshift bins using the DESI DR2 BAO measurements. The black dashed line represents the standard ΛCDM model with w(z) = −1. The redshift intervals of the bins are shown as the blue bars. A descending trend of w(z) is found. (b) Same as panel (a), but for the Pantheon plus SNe Ia sample. The w(z) values from BAO and SNe Ia are consistent within 1σ confidence level.
Paper: The Hubble Tension Resolved by the DESI Baryon Acoustic Oscillations Measurements
Authors: X. D. Jia, J. P. Hu, D. H. Gao, S. X. Yi, F. Y. Wang
Figure caption: Corner plot of wi from the DESI DR2 BAO + Pantheon plus sample. The panels on the diagonal show the 1D histogram for each parameter obtained by marginalizing over the other parameters. The off-diagonal panels show two-dimensional projections of the posterior probability distributions for each pair of parameters, with contours to indicate 1σ–3σ confidence levels.
Paper: The Hubble Tension Resolved by the DESI Baryon Acoustic Oscillations Measurements
Authors: X. D. Jia, J. P. Hu, D. H. Gao, S. X. Yi, F. Y. Wang
Figure caption: Same as Figure 3, but for the DESI DR2 BAO + DESY5 SNe Ia sample.
Paper: The Pre-outburst Properties of the FU Ori Object HBC 722
Authors: Gregory J. Herczeg, 雷歌 沈, Bo Reipurth
Figure caption: Left: contour plot of the acceptable parameters of veiling and extinction for synthetic photometry fit to SDSS photometry. The best fit (purple asterisk) is shown in Figure 2. The yellow and blue contours correspond to the acceptable fit range, with ﹩{\chi }_{{\rm{red}}}^{2}=1.0﹩ and 1.5. The broader region shows the χ2 contours for fits to griz and excluding the u band, with acceptable parameters that extend to high veiling. Those values are ruled out because the synthetic spectrum with higher veiling and extinction produces a u-band brightness that is brighter than detected (red contours for u  = 21.0, the 1σ limit, and 20.5, which is 0.5 mag brighter than observed). Right: contours of ﹩{\chi }_{{\rm{red}}}^{2}=1.0﹩ for spectral types of M2.5 (purple), M3 (Sz 67, dark blue), M3.25 (TWA 7+TWA 15B, thick light blue), M3.5 (TWA 15B, orange), and Sz 121 (red dotted line indicating ﹩{\chi }_{\mathrm{red}}^{2}=1.7﹩, since no solutions were within ﹩{\chi }_{\mathrm{red}}^{2}=1.3﹩). In general the extinction and veiling both decrease to later spectral type, but no solutions reach AV > 2.
Paper: The Pre-outburst Properties of the FU Ori Object HBC 722
Authors: Gregory J. Herczeg, 雷歌 沈, Bo Reipurth
Figure caption: The synthetic photometry (red circles, calculated from the synthetic spectrum) that best reproduces the SDSS griz, 2MASS JHKS, and UKIRT JHK photometry of HBC 722 (blue asterisks). The synthetic spectrum (black line with red circles for photometry) consists of an M3.25 photosphere plus selected emission lines (green line), an accretion continuum (purple line), and a dust continuum emission (red line).
Paper: The Pre-outburst Properties of the FU Ori Object HBC 722
Authors: Gregory J. Herczeg, 雷歌 沈, Bo Reipurth
Figure caption: The WFGS2 red spectrum of HBC 722 (black lines, repeated with offsets) compared with spectra of nonaccreting X-Shooter templates from R. A. B. Claes et al. (2024). The templates all have veiling and extinction tailored to best match the observed spectrum of HBC 722. The spectrum also includes Hα and Ca II infrared triplet lines, indicating accretion.
Paper: The Pre-outburst Properties of the FU Ori Object HBC 722
Authors: Gregory J. Herczeg, 雷歌 沈, Bo Reipurth
Figure caption: BVRI color–magnitude diagrams from the Semkov photometry, compared with synthetic photometry from our fit to SDSS spectra, varying only the accretion continuum (dashed blue line). The red stars show the photometry from our best-fit SDSS model. Each panel also includes an extinction vector for AV = 0.5 mag. The purple square is single-epoch BVI photometry from S. Guieu et al. (2009).
Paper: The Pre-outburst Properties of the FU Ori Object HBC 722
Authors: Gregory J. Herczeg, 雷歌 沈, Bo Reipurth
Figure caption: The pre-outburst BVRI light curve of HBC 722 from E. H. Semkov et al. (2012), with vertical dashed lines showing the epoch of the SDSS photometry and the WFGS2 spectrum. The outlier B-band point is excluded from this figure and Figure 5.
Paper: Speed-dependent Threshold for Electron Injection into Diffusive Shock Acceleration
Authors: Siddhartha Gupta, Damiano Caprioli, Anatoly Spitkovsky
Figure caption: Trajectories of a few transmitted (red) and reflected (cyan) electrons in a prescribed shock test, where we have taken vpt = 0.1 c, θBn = 45∘, ﹩{{ \mathcal M }}_{{\rm{s}},{\rm{e}}}=2﹩, Lsh = 1di, ﹩{{ \mathcal R }}_{{\rm{B}}}=4﹩, and proton-to-electron mass ratio mR = 100.
Paper: Speed-dependent Threshold for Electron Injection into Diffusive Shock Acceleration
Authors: Siddhartha Gupta, Damiano Caprioli, Anatoly Spitkovsky
Figure caption: Quantification of the electron reflection fraction (ηr) using prescribed shock simulations. Panels (a) and (b) show that ηr drops sharply for ﹩{{ \mathcal M }}_{{\rm{s}},{\rm{e}}}\gt 3﹩ and at higher inclinations. Panel (c) indicates that varying the shock thickness—either by adjusting Lsh (bottom axis, circles) or the mass ratio (top axis, stars)—has little effect on ηr. Panel (d) suggests a mild dependence on ﹩{{ \mathcal M }}_{{\rm{A}}}﹩. Notably, in all cases, the mean velocity of reflected electrons in the upstream frame is 1–4 vsh (see top color bar), consistent with our full PIC simulations.
Paper: Speed-dependent Threshold for Electron Injection into Diffusive Shock Acceleration
Authors: Siddhartha Gupta, Damiano Caprioli, Anatoly Spitkovsky
Figure caption: A method for finding De for ﹩{{ \mathcal M }}_{{\rm{A}}}=20﹩ shock using a snapshot of the fields at ﹩t=135{\omega }_{{\rm{ci}}}^{-1}﹩. Panel (a) shows Equation (B1) at eight different locations relative to the shock, while panel (b) presents the corresponding asymptotic values of De.
Paper: Speed-dependent Threshold for Electron Injection into Diffusive Shock Acceleration
Authors: Siddhartha Gupta, Damiano Caprioli, Anatoly Spitkovsky
Figure caption: Demonstrating a method for calculating Δp/p in PIC simulation. Descriptions are similar to Figure 1, with the background color representing the plasma x-velocity used to identify the instantaneous shock locations (the dashed white curve). The fractional momentum change, Δp/p, aligns with Equation (1).
Paper: Speed-dependent Threshold for Electron Injection into Diffusive Shock Acceleration
Authors: Siddhartha Gupta, Damiano Caprioli, Anatoly Spitkovsky
Figure caption: Same as Figure 4, but using mR = 1836.
Paper: Stellar Obliquities of Young Systems, Atmospheres Undergoing Contraction and Escape (SOYSAUCE): A Likely Aligned Orbit for the 3 Myr Planet TIDYE-1 b
Authors: Madyson G. Barber, Andrew W. Mann, Marshall C. Johnson, Mayuko Mori, John Livingston, Daniel M. Krolikowski, Norio Narita, Akihiko Fukui, Teruyuki Hirano, Andrew Vanderburg, Adam L. Kraus, Benjamin M. Tofflemire, Sydney Vach, Sarah Blunt, Lissa Haskell
Figure caption: Distribution of sky-projected obliquity angles (∣λ∣) for transiting planets across system ages (J. Southworth 2011; https://www.astro.keele.ac.uk/jkt/tepcat/obliquity.html). This only considers planets with masses below 10 MJ (or no measured mass), Teff < 6250 K, σλ < 25°, and those with literature ages (taken from the NASA Exoplanet archive; J. L. Christiansen et al. 2025). All points are colored by the planet radius. Young systems tend to be aligned but the difference is not significant. TIDYE-1 b (IRAS 04125+2902b; star) is consistent with the few other <0.1 Gyr systems. The background shading represents rough approximations of the timescales for processes of interest for the SOYSAUCE survey.
Paper: Stellar Obliquities of Young Systems, Atmospheres Undergoing Contraction and Escape (SOYSAUCE): A Likely Aligned Orbit for the 3 Myr Planet TIDYE-1 b
Authors: Madyson G. Barber, Andrew W. Mann, Marshall C. Johnson, Mayuko Mori, John Livingston, Daniel M. Krolikowski, Norio Narita, Akihiko Fukui, Teruyuki Hirano, Andrew Vanderburg, Adam L. Kraus, Benjamin M. Tofflemire, Sydney Vach, Sarah Blunt, Lissa Haskell
Figure caption: MAROON-X relative radial velocities from the red (red squares; top) and blue (blue circles; middle) channels. The best-fit RM and stellar RV trend models for each channel are shown as the opaque dotted red and solid blue lines, with 50 random sample fits pulled from the posterior shown as the translucent dotted red and solid blue lines. The bottom plot shows the residuals compared to the best-fit model for each channel, with a 5 minute shift applied to the blue channel RVs for clarity. The red and blue channel fits agree with one another, with the blue RV trend line showing a slightly steeper slope, as expected.
Paper: Stellar Obliquities of Young Systems, Atmospheres Undergoing Contraction and Escape (SOYSAUCE): A Likely Aligned Orbit for the 3 Myr Planet TIDYE-1 b
Authors: Madyson G. Barber, Andrew W. Mann, Marshall C. Johnson, Mayuko Mori, John Livingston, Daniel M. Krolikowski, Norio Narita, Akihiko Fukui, Teruyuki Hirano, Andrew Vanderburg, Adam L. Kraus, Benjamin M. Tofflemire, Sydney Vach, Sarah Blunt, Lissa Haskell
Figure caption: Simultaneous photometric observations of the transit of IRAS 04125+2902b in TESS (top), LCOGT (left), and MuSCAT3 (right). In all observations, the 15 minute binned data are shown in purple with the raw data shown as the background colored points. The best-fit transit and stellar variability model is shown as the brown line in every filter.
Paper: Stellar Obliquities of Young Systems, Atmospheres Undergoing Contraction and Escape (SOYSAUCE): A Likely Aligned Orbit for the 3 Myr Planet TIDYE-1 b
Authors: Madyson G. Barber, Andrew W. Mann, Marshall C. Johnson, Mayuko Mori, John Livingston, Daniel M. Krolikowski, Norio Narita, Akihiko Fukui, Teruyuki Hirano, Andrew Vanderburg, Adam L. Kraus, Benjamin M. Tofflemire, Sydney Vach, Sarah Blunt, Lissa Haskell
Figure caption: Corner plot of a subset of the RM parameters. The contours show the 1, 2, and 3σ levels. Only 99% of the distribution is shown for clarity. The sky-projected obliquity angle (λ) is correlated with the impact parameter (b) but seems to be minimally impacted by the the RV trend line parameters (γ and ﹩\dot{\gamma }﹩), with the exemption of the largest λ values (with a near-flat RM signal near egress) corresponding to a tighter RV trend line solution. Remaining, unshown parameters are similarly Gaussian distributed with little correlation between parameters.
Paper: Prediscovery TESS Observations of Interstellar Object 3I/ATLAS
Authors: Jorge Martinez-Palomera, Amy Tuson, Christina Hedges, Jessie Dotson, Thomas Barclay, Brian Powell
Figure caption: Full image stack of 3I/ATLAS, using all frames available from TESS sector 92 after quality filtering. Data from camera 2 CCD 3 (left) and camera 1 CCD 2 (right) are stacked separately to preserve instrument characteristics. The pixels with SNR > 3 are highlighted in red; these are used for aperture photometry (see Section 2.5).
Paper: Prediscovery TESS Observations of Interstellar Object 3I/ATLAS
Authors: Jorge Martinez-Palomera, Amy Tuson, Christina Hedges, Jessie Dotson, Thomas Barclay, Brian Powell
Figure caption: Stacked images of 3I/ATLAS from TESS sector 92. We stacked 901 (∼2.1 days) and 520 (∼1.2 days) frames from camera 2 CCD 3 (first row) and camera 1 CCD 2 (second and third row), respectively. The aperture masks used for photometry are plotted in red; the masks are different for each camera to account for instrument characteristics. Due to the stacking procedure, the row and column pixel values do not represent the location in the original TESS FFI and are only shown for reference. The images are aligned so that the target is always centered. See Section 2.4 for details on the stacking procedure and Section 2.5 for details on the photometry.
Paper: Prediscovery TESS Observations of Interstellar Object 3I/ATLAS
Authors: Jorge Martinez-Palomera, Amy Tuson, Christina Hedges, Jessie Dotson, Thomas Barclay, Brian Powell
Figure caption: Background modeling, as described in Section 2.2. The left/right panel shows an example of a cadence with/without strong scattered light (SL). We show the raw flux (top), our background model that accounts for scattered light and stars (middle), and the residuals (bottom). The “holes” in the residuals are pixels that were identified as outliers and rejected.
Paper: Prediscovery TESS Observations of Interstellar Object 3I/ATLAS
Authors: Jorge Martinez-Palomera, Amy Tuson, Christina Hedges, Jessie Dotson, Thomas Barclay, Brian Powell
Figure caption: Light curve of 3I/ATLAS from observatories with bandpasses similar to TESS, including the PRF photometry from this work (black diamonds). The TESS measurements from A. D. Feinstein et al. (2025) are shown for comparison (purple squares). The top axis shows the heliocentric distance covered by 3I/ATLAS during the observations. The gray shaded region represents the TESS sector 92 observing window. The vertical dashed line represents the date 3I/ATLAS was discovered (2025 July 1). The blue line shows the expected Tmag as reported by JPL Horizons (converted from Vmag using T. L. Farnham et al. 2021). The different colored markers represent photometric bandpasses similar to TESS (600–1000 nm): r, i, and z are equivalent to Sloan Digital Sky Survey riz bands; R represents the equivalent Johnson–Cousins R band (centered on 658 nm); and Ao is the ATLAS orange bandpass (560–820 nm). Data were collected from the MPC Explorer service on 2025 September 15 (B. T. Bolin et al. 2025; C. O. Chandler et al. 2025; A. Chernyshov et al. 2025; L. Pipeline et al. 2025; T. Santana-Ros et al. 2025; J. Tonry et al. 2025; Q. Ye et al. 2025).
Paper: Prediscovery TESS Observations of Interstellar Object 3I/ATLAS
Authors: Jorge Martinez-Palomera, Amy Tuson, Christina Hedges, Jessie Dotson, Thomas Barclay, Brian Powell
Figure caption: 3I/ATLAS light curves using aperture (top) and PRF (bottom) photometry in flux (left) and magnitude (right), measured from the stacked images. Data from camera 2 CCD 3 is shown in blue squares, while orange circles represent data from camera 1 CCD 2. Error bars in the time axis represent the window used for image stacking. The solid red line and shaded region represent the mean background flux and 1σ intervals. The horizontal dashed red line represents the 3σ average detection limit across all stacked images. The x-axis is defined with respect to the time of discovery 2025 July 1.
Paper: Prediscovery TESS Observations of Interstellar Object 3I/ATLAS
Authors: Jorge Martinez-Palomera, Amy Tuson, Christina Hedges, Jessie Dotson, Thomas Barclay, Brian Powell
Figure caption: Normalized flux for every pixel in the image cutout with respect to the expected position of 3I/ATLAS. Data correspond to observations from TESS sector 92 camera 2 CCD 3 (top row) and camera 1 CCD 2 (bottom row). The left panels show the original ephemeris from JPL Horizons (accessed on 2025 July 28), while the right panels show the corrected ephemeris as described in Section 2.3. A stronger signal is represented by redder points.
Paper: Prediscovery TESS Observations of Interstellar Object 3I/ATLAS
Authors: Jorge Martinez-Palomera, Amy Tuson, Christina Hedges, Jessie Dotson, Thomas Barclay, Brian Powell
Figure caption: Light curve of 3I/ATLAS in terms of the absolute visual magnitude. The error bars are dominated by the ±0.3 mag uncertainty in the Tmag to Vmag conversion, as reported in T. L. Farnham et al. (2021). The mean absolute magnitude (13.8; solid red horizontal line) and 1σ bounds (±0.4; dashed red horizontal lines) are included for reference. The top axis shows the heliocentric distance covered by 3I/ATLAS during the observations.
Paper: Prediscovery TESS Observations of Interstellar Object 3I/ATLAS
Authors: Jorge Martinez-Palomera, Amy Tuson, Christina Hedges, Jessie Dotson, Thomas Barclay, Brian Powell
Figure caption: Left: photometry using camera-specific apertures (black line) as defined by selecting pixels with SNR > 3 from the deep-stacked images per camera (as described in Section 2.5), largest fixed aperture from camera 1 CCD 2 (blue line), and fixed circular apertures with radius ranging from 1 to 3 pixels (gray lines). Right: aperture light curve using images with the position corrections (black) and without the corrections (red).
Paper: JWST-TST DREAMS: The Nightside Emission and Chemistry of WASP-17b
Authors: Jacob Lustig-Yaeger, Kristin S. Sotzen, Kevin B. Stevenson, Shang-Min Tsai, Ryan C. Challener, Jayesh Goyal, Nikole K. Lewis, Dana R. Louie, L. C. Mayorga, Daniel Valentine, Hannah R. Wakeford, Lili Alderson, Natalie H. Allen, Thomas J. Fauchez, Ana Glidden, Amélie Gressier, Sarah M. Hörst, Jingcheng Huang, Zifan Lin, Avi M. Mandell, Elijah Mullens, Sarah Peacock, Edward W. Schwieterman, Jeff A. Valenti, C. Matt Mountain, Marshall Perrin, Roeland P. van der Marel
Figure caption: Summary of retrieval results for the dayside (orange) and nightside (purple) emission spectra of WASP-17b for retrievals using error inflation. Top left: emission spectra measurements fitted with the median retrieved model spectrum with envelopes for the 1σ and 2σ posterior credible intervals. The error bars shown are inflated using Equation (6) with the median retrieved value of b. Top right: retrieved PT profile constraints. Bottom row: histograms showing the 1D posterior probability density for a subset of retrieved parameters. The subplot titles list the 1σ posterior constraints.
Paper: JWST-TST DREAMS: The Nightside Emission and Chemistry of WASP-17b
Authors: Jacob Lustig-Yaeger, Kristin S. Sotzen, Kevin B. Stevenson, Shang-Min Tsai, Ryan C. Challener, Jayesh Goyal, Nikole K. Lewis, Dana R. Louie, L. C. Mayorga, Daniel Valentine, Hannah R. Wakeford, Lili Alderson, Natalie H. Allen, Thomas J. Fauchez, Ana Glidden, Amélie Gressier, Sarah M. Hörst, Jingcheng Huang, Zifan Lin, Avi M. Mandell, Elijah Mullens, Sarah Peacock, Edward W. Schwieterman, Jeff A. Valenti, C. Matt Mountain, Marshall Perrin, Roeland P. van der Marel
Figure caption: Our WASP-17b dayside and nightside temperature measurements constrain the heat redistribution (f) and bond albedo (AB). The orange (blue) contours show possible dayside (nightside) equilibrium temperatures as a function of heat redistribution (y-axis) and bond albedo (x-axis). The thick contours show the median retrieved temperatures bounded by ±1σ uncertainties. The black contours show the joint constraints on f and AB from our temperature measurements (e.g., see Figure 1 of N. B. Cowan & E. Agol 2011 for an analogous example scenario). Our nightside constraints agree with expectations based on the measured heat redistribution from the MIRI LRS eclipse map (D. Valentine et al. 2024).
Paper: JWST-TST DREAMS: The Nightside Emission and Chemistry of WASP-17b
Authors: Jacob Lustig-Yaeger, Kristin S. Sotzen, Kevin B. Stevenson, Shang-Min Tsai, Ryan C. Challener, Jayesh Goyal, Nikole K. Lewis, Dana R. Louie, L. C. Mayorga, Daniel Valentine, Hannah R. Wakeford, Lili Alderson, Natalie H. Allen, Thomas J. Fauchez, Ana Glidden, Amélie Gressier, Sarah M. Hörst, Jingcheng Huang, Zifan Lin, Avi M. Mandell, Elijah Mullens, Sarah Peacock, Edward W. Schwieterman, Jeff A. Valenti, C. Matt Mountain, Marshall Perrin, Roeland P. van der Marel
Figure caption: The dayside (orange) and nightside (purple) abundance profiles of SO2 from our two-column VULCAN grids with 10 times solar metallicity. The solid lines assume Kzz = 1011 cm2 s−1, whereas the dashed lines assume Kzz = 107 cm2 s−1, showing the strongest and weakest vertical mixing cases in our model grid, respectively. The light to dark shades of each color represent zonal wind speeds of 100, 200, 500, 1000, 3000, and 5000 m s−1. The dotted lines are those without including zonal wind (vertical mixing only). The error bars show the 1σ retrieved constraints, with their vertical positions chosen to be near the peak of the contribution function.