adsabs/AstroCLIMB huggingface dataset:
Paper: Evolution of Mercury’s Volatile-bearing Crust within Raditladi Basin
Authors: Deborah L. Domingue, John R. Weirich, J. Alexis P. Rodriguez, Samuel W. Courville, Frank C. Chuang, Matthew D. Richardson, Bryan J. Travis, Eric E. Palmer, Mario Zarroca
Figure caption: Example images from area III. Top left is NAC image N1025680666M. The top center image is a synthetic image of the image on the left based on the Hapke model parameters shown in Figure A8. The top right is a ratio of the observed image (left) to the model image (center). Bottom left is WAC image W0231179208G. The bottom center image is a synthetic image of the image on the left based on the Hapke model parameters shown in Figure A8. The bottom right is a ratio of the observed image (left) to the model image (center). The observed and synthetic images in the top row are displayed on a gray scale of 0–0.13, and those on the bottom row are displayed on a gray scale of 0–0.12. Both ratio images are displayed on a gray scale of 0–2.5. The black areas in the ratio image are regions in shadow in the observed image based on the SPC shape model. The pixelation in the synthetic images (center) is due to the 10 × 10 pixel binning of the original data set.
Paper: Evolution of Mercury’s Volatile-bearing Crust within Raditladi Basin
Authors: Deborah L. Domingue, John R. Weirich, J. Alexis P. Rodriguez, Samuel W. Courville, Frank C. Chuang, Matthew D. Richardson, Bryan J. Travis, Eric E. Palmer, Mario Zarroca
Figure caption: Example images from area I. Top left is NAC image N1046021872M. The top center image is a synthetic image of the image on the left based on the Hapke model parameters shown in Figure A6. The top right is a ratio of the observed image (left) to the model image (center). Bottom left is WAC image W0231179208G. The bottom center image is a synthetic image of the image on the left based on the Hapke model parameters shown in Figure A6. The bottom right is a ratio of the observed image (left) to the model image (center). The observed and synthetic images in the top row are displayed on a gray scale of 0–0.152, and those on the bottom row are displayed on a gray scale of 0–0.134. Both ratio images are displayed on a gray scale of 0–2.5. The black areas in the ratio image are regions in shadow in the observed image based on the SPC shape model.
Paper: Improved Constraints on the Vertical Profile of CH4 at Jupiter’s Mid- to High Latitudes, Using IRTF-TEXES and SOFIA-EXES Spectroscopy
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, Matthew Richter, Maisie Rashman, Curtis de Witt, Julianne Moses, Vincent Hue, Pablo Rodríguez-Ovalle, Thierry Fouchet, Ananyo Bhattacharya, Bilal Benmahi, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Top panel: retrieved temperature profiles (solid colored lines) and uncertainty (dotted colored lines) using the non-auroral-mean spectra at 62.5∘N for IRTF-TEXES results and 60∘N for SOFIA-EXES results. Results are colored according to the pressure level, as indicated by the legend on the left. The bottom left panel shows similar results for temperatures retrieved from auroral-mean spectra (poleward of the MAE) at 60∘N–62.5∘N. The bottom right panel shows retrieved profiles of CH3, which was allowed to vary in fitting the auroral-mean spectra. Only the 1 μbar results are shown where there is sensitivity to CH3 (see Figure 7).
Paper: Improved Constraints on the Vertical Profile of CH4 at Jupiter’s Mid- to High Latitudes, Using IRTF-TEXES and SOFIA-EXES Spectroscopy
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, Matthew Richter, Maisie Rashman, Curtis de Witt, Julianne Moses, Vincent Hue, Pablo Rodríguez-Ovalle, Thierry Fouchet, Ananyo Bhattacharya, Bilal Benmahi, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: The vertical contribution functions of the spectral settings/instruments analyzed in this work, which describe the relative contribution of each atmospheric level to the total radiance observed at the top of the atmosphere. Panels (a) and (b) show the contribution functions over a subset of the 606 cm−1 spectral setting, which captures CH3 emission, for IRTF-TEXES and SOFIA-EXES, respectively. Panels (c) and (d) show the contribution functions of IRTF-TEXES at 1248 cm−1 and SOFIA-EXES at 1299 cm−1, respectively. Panel (e) compares the mean contribution function for each spectral setting/instrument.
Paper: Improved Constraints on the Vertical Profile of CH4 at Jupiter’s Mid- to High Latitudes, Using IRTF-TEXES and SOFIA-EXES Spectroscopy
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, Matthew Richter, Maisie Rashman, Curtis de Witt, Julianne Moses, Vincent Hue, Pablo Rodríguez-Ovalle, Thierry Fouchet, Ananyo Bhattacharya, Bilal Benmahi, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: The family of photochemical models adopted in this work. Panel (a) shows the vertical profiles of the eddy diffusion coefficient (solid, colored lines) and the molecular diffusion coefficient profile (black, dotted). Panels (b) and (c) show the corresponding vertical profiles of CH4 and CH3, respectively. The homopause pressure levels and the eddy diffusion coefficient at the homopause of each model are shown in the legend.
Paper: Improved Constraints on the Vertical Profile of CH4 at Jupiter’s Mid- to High Latitudes, Using IRTF-TEXES and SOFIA-EXES Spectroscopy
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, Matthew Richter, Maisie Rashman, Curtis de Witt, Julianne Moses, Vincent Hue, Pablo Rodríguez-Ovalle, Thierry Fouchet, Ananyo Bhattacharya, Bilal Benmahi, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Observed SOFIA-EXES auroral-mean spectra (points with error bars) at 68∘N of the CH3 (top panel) and CH4 (middle panel) emission on 2021 June 10. The best-fitting model spectrum is included as the solid red line. The bottom panel shows the corresponding retrieved profiles (solid red lines) and uncertainty (dotted red lines) of temperature (according to the lower x-axis) and CH3 volume mixing ratio (according to the upper x-axis). The vertical profile of CH3 is from Model 10b, which is the best-fitting model at this latitude/date.
Paper: Improved Constraints on the Vertical Profile of CH4 at Jupiter’s Mid- to High Latitudes, Using IRTF-TEXES and SOFIA-EXES Spectroscopy
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, Matthew Richter, Maisie Rashman, Curtis de Witt, Julianne Moses, Vincent Hue, Pablo Rodríguez-Ovalle, Thierry Fouchet, Ananyo Bhattacharya, Bilal Benmahi, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: The location of the CH4 homopause as a function of latitude at mid- to high southern latitudes, as derived from IRTF-TEXES observations on 2021 June 28–29 (top row), 2021 November 8 (second row), 2022 June 24–25 (third row), 2022 July 5–6 (fourth row), and 2023 July 20 (fifth row). Results are shown in both pressure space (left column) and altitude space (right column). Black results denote a longitudinal mean where all sampled longitudes were coadded into a single spectrum. Red results sample longitudes poleward of the southern MAE. Results where only an upper error bar in altitude or a lower error bar in pressure is shown indicate that only an upper or lower limit could be derived. Vertical dashed lines mark the lowest-latitude extent of the southern MAE (B. Bonfond et al. 2017).
Paper: Improved Constraints on the Vertical Profile of CH4 at Jupiter’s Mid- to High Latitudes, Using IRTF-TEXES and SOFIA-EXES Spectroscopy
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, Matthew Richter, Maisie Rashman, Curtis de Witt, Julianne Moses, Vincent Hue, Pablo Rodríguez-Ovalle, Thierry Fouchet, Ananyo Bhattacharya, Bilal Benmahi, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: The location of the CH4 homopause as a function of latitude at mid- to high northern latitudes, as derived from IRTF-TEXES observations on 2019 April 16 (top row) and 2019 August 20 (second row) and SOFIA-EXES observations on 2021 June 10–11 (third row) and 2021 June 17–18 (fourth row). Results are shown in both pressure space (left column) and altitude space (right column). Black results denote a longitudinal mean, blue results denote the nonauroral mean, and red results denote an auroral mean using—see Figure 1 for further details. Results where only an upper error bar in altitude or a lower error bar in pressure is shown indicate that only an upper or lower limit could be derived. Vertical dashed lines mark the lowest-latitude extent of the northern MAE (B. Bonfond et al. 2017).
Paper: Improved Constraints on the Vertical Profile of CH4 at Jupiter’s Mid- to High Latitudes, Using IRTF-TEXES and SOFIA-EXES Spectroscopy
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, Matthew Richter, Maisie Rashman, Curtis de Witt, Julianne Moses, Vincent Hue, Pablo Rodríguez-Ovalle, Thierry Fouchet, Ananyo Bhattacharya, Bilal Benmahi, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Observed IRTF-TEXES spectra (points with error bars) of the southern auroral H2 S(1) (top panel), CH3 (second panel), and CH4 (third panel) emission as recorded by IRTF-TEXES on 2021 June 28. The best-fitted model spectrum is included as solid red. The bottom panel shows the corresponding retrieved profiles of temperature (according to the lower x-axis) and CH3 volume mixing ratio (according to the upper x-axis).
Paper: Improved Constraints on the Vertical Profile of CH4 at Jupiter’s Mid- to High Latitudes, Using IRTF-TEXES and SOFIA-EXES Spectroscopy
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, Matthew Richter, Maisie Rashman, Curtis de Witt, Julianne Moses, Vincent Hue, Pablo Rodríguez-Ovalle, Thierry Fouchet, Ananyo Bhattacharya, Bilal Benmahi, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Variations in the χ2 (Equation (1)) as a function of the model tested in inverting SOFIA-EXES spectra recorded on 2021 June 10–11. The top and bottom panels show the results at 60∘N using the auroral-mean spectra and non-auroral-mean spectra, respectively. In the left column, the upper x-axis shows the variation in χ2 with respect to homopause altitude; in the right column, the upper x-axis shows the variation with respect to homopause pressure. Vertical solid and dotted red lines indicate the best-fitting homopause location and 1σ confidence levels, respectively.
Paper: Improved Constraints on the Vertical Profile of CH4 at Jupiter’s Mid- to High Latitudes, Using IRTF-TEXES and SOFIA-EXES Spectroscopy
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, Matthew Richter, Maisie Rashman, Curtis de Witt, Julianne Moses, Vincent Hue, Pablo Rodríguez-Ovalle, Thierry Fouchet, Ananyo Bhattacharya, Bilal Benmahi, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Same as Figure 9, but using IRTF-TEXES observations recorded on 2021 June 28–29 (top row), 2021 November 8 (second row), 2022 June 24–25 (third row), 2022 5–6 July (fourth row), and 2023 July 20 (fifth row).
Paper: Occultation-based Size and Shape of (269) Justitia
Authors: Marc W. Buie, Hoor AlMazmi, حور المازمي, Paul Hayne, Anna Marciniak, Brian A. Keeney, Fahad Alawadhi, فهد العوضي, Alia Almansoori, علياء المنصوري, Noora Rashed Alsaeed, Amer Sarhan Alsawwafi, عامر سرحان الصوافي, Arvind Jayashankara Aradhya, Dahlia Baker, Samuel F. A. Cartwright, Elad David, Hugh M. Davidson, Ian Faber, Chelsea Ferrell, William Goodwyn Ferrell, Kai Getrost, Julian Hammerl, Parker Hinton, Jack L. Jewell, Roxanne L. Kamin, John Keller, Mykal Lefevre, Steve Messner, Vadim Nikitin, Heshani Pieris, Arunima Prakash, Julien Salmon, Abdullah Essa Sharif, Michael Skrutskie, Kya C. Sorli, Thibaud Teil, تيبو تيل, Anne J Verbiscer, Jacopo Villa
Figure caption: Limb profile for Justitia for the JU20230831 campaign. This diagram is shown in a sky-normal orientation (north and east are labeled). The origin (black X) denotes the ephemeris location of Justitia. Each line represents the path of the star relative to the object. Blue lines are for sites that recorded a positive occultation. Red lines are for sites that recorded data but did not see an occultation. Gray lines are for sites that were deployed but were unable to take any useful data. The direction of apparent motion of the star is given by the arrow in the upper-right corner of the plot. The orange dots show the location where the star either disappears or reappears. The cyan ellipse is the best-fitting ellipse to the limb points (unweighted) and the close dashed lines are fits to the systematic extremes given the uncertainties (−σ on the left and +σ on the right for the largest, reversed for the smallest). The solid limb curve is a function-free representation of a limb that is consistent with all of the data (see text for details). The red diamond shows the center of the fitted ellipse and the purple square is the center of the limb profile. Each point on this limb has a number to facilitate discussion, and extra control points are plotted small black triangles.
Paper: Occultation-based Size and Shape of (269) Justitia
Authors: Marc W. Buie, Hoor AlMazmi, حور المازمي, Paul Hayne, Anna Marciniak, Brian A. Keeney, Fahad Alawadhi, فهد العوضي, Alia Almansoori, علياء المنصوري, Noora Rashed Alsaeed, Amer Sarhan Alsawwafi, عامر سرحان الصوافي, Arvind Jayashankara Aradhya, Dahlia Baker, Samuel F. A. Cartwright, Elad David, Hugh M. Davidson, Ian Faber, Chelsea Ferrell, William Goodwyn Ferrell, Kai Getrost, Julian Hammerl, Parker Hinton, Jack L. Jewell, Roxanne L. Kamin, John Keller, Mykal Lefevre, Steve Messner, Vadim Nikitin, Heshani Pieris, Arunima Prakash, Julien Salmon, Abdullah Essa Sharif, Michael Skrutskie, Kya C. Sorli, Thibaud Teil, تيبو تيل, Anne J Verbiscer, Jacopo Villa
Figure caption: Lightcurve data for JU20230831, part 1. Normalized lightcurves are shown where unity is equal to the sum of the flux from the target star and Justitia. Each data set is labeled with the site ID, the cross-track offset, the predicted mid-time, the uncertainty per point (σ), and the time and spatial resolution of the data. Complete lightcurves are provided for Figures 2–4 as data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Occultation-based Size and Shape of (269) Justitia
Authors: Marc W. Buie, Hoor AlMazmi, حور المازمي, Paul Hayne, Anna Marciniak, Brian A. Keeney, Fahad Alawadhi, فهد العوضي, Alia Almansoori, علياء المنصوري, Noora Rashed Alsaeed, Amer Sarhan Alsawwafi, عامر سرحان الصوافي, Arvind Jayashankara Aradhya, Dahlia Baker, Samuel F. A. Cartwright, Elad David, Hugh M. Davidson, Ian Faber, Chelsea Ferrell, William Goodwyn Ferrell, Kai Getrost, Julian Hammerl, Parker Hinton, Jack L. Jewell, Roxanne L. Kamin, John Keller, Mykal Lefevre, Steve Messner, Vadim Nikitin, Heshani Pieris, Arunima Prakash, Julien Salmon, Abdullah Essa Sharif, Michael Skrutskie, Kya C. Sorli, Thibaud Teil, تيبو تيل, Anne J Verbiscer, Jacopo Villa
Figure caption: Deployment area for JU20230831. The prediction is denoted by the gray shaded area bounded by dashed lines for the anticipated 59 km diameter. The red shaded region bounded by the solid lines shows a 54.4 km-wide track that is consistent with the observations. The red diamonds denote sites with positive detections of an occultation. The blue circles indicate the locations of sites that had data ruling out an occultation. The gray squares are for deployed sites that were unable to collect useful data. Two sites (TM:failed and SM:negative) are not shown for clarity due to their distance from the main group.
Paper: Occultation-based Size and Shape of (269) Justitia
Authors: Marc W. Buie, Hoor AlMazmi, حور المازمي, Paul Hayne, Anna Marciniak, Brian A. Keeney, Fahad Alawadhi, فهد العوضي, Alia Almansoori, علياء المنصوري, Noora Rashed Alsaeed, Amer Sarhan Alsawwafi, عامر سرحان الصوافي, Arvind Jayashankara Aradhya, Dahlia Baker, Samuel F. A. Cartwright, Elad David, Hugh M. Davidson, Ian Faber, Chelsea Ferrell, William Goodwyn Ferrell, Kai Getrost, Julian Hammerl, Parker Hinton, Jack L. Jewell, Roxanne L. Kamin, John Keller, Mykal Lefevre, Steve Messner, Vadim Nikitin, Heshani Pieris, Arunima Prakash, Julien Salmon, Abdullah Essa Sharif, Michael Skrutskie, Kya C. Sorli, Thibaud Teil, تيبو تيل, Anne J Verbiscer, Jacopo Villa
Figure caption: Lightcurve correction from the mean to the time of occultation. This is a smooth curve representation of the Justitia lightcurve within a month of the occultation. The horizontal line is the mean of the displayed lightcurve set to the Fink/ZTF value. The dashed line shows the rotational phase during the pre-event calibration photometry. The solid vertical line marks the rotational phase at the time of the occultation.
Paper: Occultation-based Size and Shape of (269) Justitia
Authors: Marc W. Buie, Hoor AlMazmi, حور المازمي, Paul Hayne, Anna Marciniak, Brian A. Keeney, Fahad Alawadhi, فهد العوضي, Alia Almansoori, علياء المنصوري, Noora Rashed Alsaeed, Amer Sarhan Alsawwafi, عامر سرحان الصوافي, Arvind Jayashankara Aradhya, Dahlia Baker, Samuel F. A. Cartwright, Elad David, Hugh M. Davidson, Ian Faber, Chelsea Ferrell, William Goodwyn Ferrell, Kai Getrost, Julian Hammerl, Parker Hinton, Jack L. Jewell, Roxanne L. Kamin, John Keller, Mykal Lefevre, Steve Messner, Vadim Nikitin, Heshani Pieris, Arunima Prakash, Julien Salmon, Abdullah Essa Sharif, Michael Skrutskie, Kya C. Sorli, Thibaud Teil, تيبو تيل, Anne J Verbiscer, Jacopo Villa
Figure caption: Lightcurve data for JU20230831, part 3. Normalized lightcurves are shown where unity is equal to the sum of the flux from the target star and Justitia. Each data set is labeled with the site ID, the cross-track offset, the predicted mid-time, the uncertainty per point (σ), and the time and spatial resolution of the data.
Paper: Occultation-based Size and Shape of (269) Justitia
Authors: Marc W. Buie, Hoor AlMazmi, حور المازمي, Paul Hayne, Anna Marciniak, Brian A. Keeney, Fahad Alawadhi, فهد العوضي, Alia Almansoori, علياء المنصوري, Noora Rashed Alsaeed, Amer Sarhan Alsawwafi, عامر سرحان الصوافي, Arvind Jayashankara Aradhya, Dahlia Baker, Samuel F. A. Cartwright, Elad David, Hugh M. Davidson, Ian Faber, Chelsea Ferrell, William Goodwyn Ferrell, Kai Getrost, Julian Hammerl, Parker Hinton, Jack L. Jewell, Roxanne L. Kamin, John Keller, Mykal Lefevre, Steve Messner, Vadim Nikitin, Heshani Pieris, Arunima Prakash, Julien Salmon, Abdullah Essa Sharif, Michael Skrutskie, Kya C. Sorli, Thibaud Teil, تيبو تيل, Anne J Verbiscer, Jacopo Villa
Figure caption: Lightcurve data for JU20230831, part 2. Normalized lightcurves are shown where unity is equal to the sum of the flux from the target star and Justitia. Each data set is labeled with the site ID, the cross-track offset, the predicted mid-time, the uncertainty per point (σ), and the time and spatial resolution of the data.
Paper: Improved Constraints on the Vertical Profile of CH4 at Jupiter’s Mid- to High Latitudes, Using IRTF-TEXES and SOFIA-EXES Spectroscopy
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, Matthew Richter, Maisie Rashman, Curtis de Witt, Julianne Moses, Vincent Hue, Pablo Rodríguez-Ovalle, Thierry Fouchet, Ananyo Bhattacharya, Bilal Benmahi, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: The latitude and longitude ranges used for coaddition of individual IRTF-TEXES spectra. Areas shown in black, blue, and red are henceforth described as the “longitudinal-mean,” “non-auroral-mean,” and “auroral-mean” observations, respectively. A similar scheme is adopted for SOFIA-EXES observations, but with a coarser latitude spacing. Spectra are not coadded at latitudes higher than ±74∘, where diffraction blurs planet signal with dark sky.
Paper: Improved Constraints on the Vertical Profile of CH4 at Jupiter’s Mid- to High Latitudes, Using IRTF-TEXES and SOFIA-EXES Spectroscopy
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, Matthew Richter, Maisie Rashman, Curtis de Witt, Julianne Moses, Vincent Hue, Pablo Rodríguez-Ovalle, Thierry Fouchet, Ananyo Bhattacharya, Bilal Benmahi, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Spectra recorded by IRTF-TEXES on 2021 June 28 in the 587 cm−1, (top panel), 606 cm−1 (middle panel), and 1248 cm−1 (bottom panel) spectral settings, which respectively capture emission features of the H2 S(1) quadrupole line, CH3, and CH4. Black spectra are a longitudinal mean at 50∘N, blue spectra are a nonauroral mean at 67.5∘N, and red spectra are an auroral mean at 67.5∘N (see Figure 1/Section 2 for further details on the spatial coaddition). Only a subset of the spectral ranges measured are shown for clarity.
Paper: Improved Constraints on the Vertical Profile of CH4 at Jupiter’s Mid- to High Latitudes, Using IRTF-TEXES and SOFIA-EXES Spectroscopy
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, Matthew Richter, Maisie Rashman, Curtis de Witt, Julianne Moses, Vincent Hue, Pablo Rodríguez-Ovalle, Thierry Fouchet, Ananyo Bhattacharya, Bilal Benmahi, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Spectra recorded by SOFIA-EXES on 2021 June 10–11 in the 606 cm–1 (top panel) and 1248 cm−1 (bottom panel) spectral settings, which respectively capture emission features of CH3 and CH4. Black spectra are a longitudinal mean at 52∘N, blue spectra are a nonauroral mean at 64∘N, and red spectra are an auroral mean at 64∘N (see Figure 1/Section 2 for further details on the spatial coaddition). Only a subset of the spectral ranges measured are shown for clarity.
Paper: Improved Constraints on the Vertical Profile of CH4 at Jupiter’s Mid- to High Latitudes, Using IRTF-TEXES and SOFIA-EXES Spectroscopy
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, Matthew Richter, Maisie Rashman, Curtis de Witt, Julianne Moses, Vincent Hue, Pablo Rodríguez-Ovalle, Thierry Fouchet, Ananyo Bhattacharya, Bilal Benmahi, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Mean radiances calculated over the ~1299 cm−1 bandpass for SOFIA-EXES observations recorded on 2021 June 10–11 (gray circles) and June 17–18 (black circles). Error bars on mean observed radiances are included but are too small to be seen on the range of the plot. Forward-modeled (“FM”) radiances of IRTF-TEXES results derived from observations on 2021 June 28 are shown as red circles.
Paper: Improved Constraints on the Vertical Profile of CH4 at Jupiter’s Mid- to High Latitudes, Using IRTF-TEXES and SOFIA-EXES Spectroscopy
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, Matthew Richter, Maisie Rashman, Curtis de Witt, Julianne Moses, Vincent Hue, Pablo Rodríguez-Ovalle, Thierry Fouchet, Ananyo Bhattacharya, Bilal Benmahi, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: The longitudinal-mean radiance averaged between 606.96 and 607.01 cm−1, which captures tropospheric continuum, using IRTF-TEXES measurements on 2021 June 28 (red) and SOFIA-EXES measurements on 2021 June 10/11 (green) and 2021 June 17/18 (dark purple). IRTF-TEXES results have been convolved in latitude such that they are at a similar spatial resolution to the SOFIA-EXES results.
Paper: Resolved Convection in Hydrogen-rich Atmospheres
Authors: Jacob T. Seeley, Robin D. Wordsworth
Figure caption: Results from the DeepBL experiment for μa =  4, 6, and 14 g mol−1. (Left) Temperature profiles, with the altitude at which qv = qcrit marked with a solid circle. The p = 0.1 bar altitude for each simulation is marked with a triangle. (Middle) Specific humidity profiles; the profiles of qcrit are indicated by the dashed lines. (Right) Cloud fraction profiles.