adsabs/AstroCLIMB huggingface dataset:
Paper: The Next Generation Virgo Cluster Survey (NGVS). XL. The Morphological Classification of Virgo Cluster Galaxies
Authors: Max M. Kurzner, Patrick Côté, Laura Ferrarese, Kaixiang Wang, Eric W. Peng, Scott Wilkinson, Joel C. Roediger, Chelsea Spengler, Toby Brown, Chengze Liu, Sungsoon Lim, Rubén Sánchez-Janssen, Elisa Toloba, Puragra Guhathakurta, John P. Blakeslee, Patrick R. Durrell, Ariane Lançon, J. Christopher Mihos, Matthew A. Taylor, Tyrone E. Woods, Solveig Thompson, Lauren A. MacArthur
Figure caption: Same as the previous figure, except for the case of low-mass (M* ≤ 109M⊙) galaxies. The classification categories in terms of structural and star formation properties are applicable across the full range of stellar mass probed by the NGVS.
Paper: The Next Generation Virgo Cluster Survey (NGVS). XL. The Morphological Classification of Virgo Cluster Galaxies
Authors: Max M. Kurzner, Patrick Côté, Laura Ferrarese, Kaixiang Wang, Eric W. Peng, Scott Wilkinson, Joel C. Roediger, Chelsea Spengler, Toby Brown, Chengze Liu, Sungsoon Lim, Rubén Sánchez-Janssen, Elisa Toloba, Puragra Guhathakurta, John P. Blakeslee, Patrick R. Durrell, Ariane Lançon, J. Christopher Mihos, Matthew A. Taylor, Tyrone E. Woods, Solveig Thompson, Lauren A. MacArthur
Figure caption: Fractional confusion matrix comparing VCC and NGVS structural classifications. Each row corresponds to a VCC morphological class, and the color shading indicates the fraction of galaxies assigned to each NGVS structural category.
Paper: The Next Generation Virgo Cluster Survey (NGVS). XL. The Morphological Classification of Virgo Cluster Galaxies
Authors: Max M. Kurzner, Patrick Côté, Laura Ferrarese, Kaixiang Wang, Eric W. Peng, Scott Wilkinson, Joel C. Roediger, Chelsea Spengler, Toby Brown, Chengze Liu, Sungsoon Lim, Rubén Sánchez-Janssen, Elisa Toloba, Puragra Guhathakurta, John P. Blakeslee, Patrick R. Durrell, Ariane Lançon, J. Christopher Mihos, Matthew A. Taylor, Tyrone E. Woods, Solveig Thompson, Lauren A. MacArthur
Figure caption: Comparison of our morphological classifications to those from the Virgo Cluster Catalog of B. Binggeli et al. (1985). The pie charts show the breakdown of our NGVS classifications for each of six major morphological categories from the VCC: Es; S0s; dEs/dE, Ns; dS0s/dS0, Ns; spirals (Sa—Sm); and irregulars (Im).
Paper: The Next Generation Virgo Cluster Survey (NGVS). XL. The Morphological Classification of Virgo Cluster Galaxies
Authors: Max M. Kurzner, Patrick Côté, Laura Ferrarese, Kaixiang Wang, Eric W. Peng, Scott Wilkinson, Joel C. Roediger, Chelsea Spengler, Toby Brown, Chengze Liu, Sungsoon Lim, Rubén Sánchez-Janssen, Elisa Toloba, Puragra Guhathakurta, John P. Blakeslee, Patrick R. Durrell, Ariane Lançon, J. Christopher Mihos, Matthew A. Taylor, Tyrone E. Woods, Solveig Thompson, Lauren A. MacArthur
Figure caption: As in Figures 1 and 2, but highlighting transitional NGVS structural codes (ES, SI, and EI). Thumbnails are annotated (top to bottom) with the VCC identifier and VCC type from B. Binggeli et al. (1985), the compact NGVS code, and the stellar mass.
Paper: The Next Generation Virgo Cluster Survey (NGVS). XL. The Morphological Classification of Virgo Cluster Galaxies
Authors: Max M. Kurzner, Patrick Côté, Laura Ferrarese, Kaixiang Wang, Eric W. Peng, Scott Wilkinson, Joel C. Roediger, Chelsea Spengler, Toby Brown, Chengze Liu, Sungsoon Lim, Rubén Sánchez-Janssen, Elisa Toloba, Puragra Guhathakurta, John P. Blakeslee, Patrick R. Durrell, Ariane Lançon, J. Christopher Mihos, Matthew A. Taylor, Tyrone E. Woods, Solveig Thompson, Lauren A. MacArthur
Figure caption: Comparison of our morphological classifications to those from the EVCC of S. Kim et al. (2014). The pie charts show the breakdown of our NGVS classifications for each of four primary morphological categories in the EVCC: ellipticals, disk galaxies, irregulars, and early-type dwarfs.
Paper: The Next Generation Virgo Cluster Survey (NGVS). XL. The Morphological Classification of Virgo Cluster Galaxies
Authors: Max M. Kurzner, Patrick Côté, Laura Ferrarese, Kaixiang Wang, Eric W. Peng, Scott Wilkinson, Joel C. Roediger, Chelsea Spengler, Toby Brown, Chengze Liu, Sungsoon Lim, Rubén Sánchez-Janssen, Elisa Toloba, Puragra Guhathakurta, John P. Blakeslee, Patrick R. Durrell, Ariane Lançon, J. Christopher Mihos, Matthew A. Taylor, Tyrone E. Woods, Solveig Thompson, Lauren A. MacArthur
Figure caption: CMD for NGVS galaxies, along with several scatter plots using nonparametric statistics. Galaxies are labeled by their structural code (left) and star formation code (right) for the sample of 762 galaxies having statmorph measurements with Mg ≲ −13 as discussed in the text.
Paper: The Next Generation Virgo Cluster Survey (NGVS). XL. The Morphological Classification of Virgo Cluster Galaxies
Authors: Max M. Kurzner, Patrick Côté, Laura Ferrarese, Kaixiang Wang, Eric W. Peng, Scott Wilkinson, Joel C. Roediger, Chelsea Spengler, Toby Brown, Chengze Liu, Sungsoon Lim, Rubén Sánchez-Janssen, Elisa Toloba, Puragra Guhathakurta, John P. Blakeslee, Patrick R. Durrell, Ariane Lançon, J. Christopher Mihos, Matthew A. Taylor, Tyrone E. Woods, Solveig Thompson, Lauren A. MacArthur
Figure caption: Same as Figure 16 except with compact galaxies from Section 5.1.1 denoted by large squares. We note that compact galaxies bifurcate in the CMD as expected and that these galaxies are generally categorized as being more morphologically complex with higher values of C, G, and M20.
Paper: A Panchromatic Characterization of the Evening and Morning Atmosphere of WASP-107 b: Composition and Cloud Variations, and Insight into the Effect of Stellar Contamination
Authors: Matthew M. Murphy, Thomas G. Beatty, Everett Schlawin, Taylor J. Bell, Michael Radica, Thomas D. Kennedy, Nishil Mehta, Luis Welbanks, Michael R. Line, Vivien Parmentier, Thomas P. Greene, Sagnick Mukherjee, Jonathan J. Fortney, Kazumasa Ohno, Lindsey Wiser, Anastasia Triantafillides, Emily Rauscher, Isaac R. Edelman, Marcia J. Rieke
Figure caption: Comparing various model scenarios to our observed limb spectra of WASP-107 b. Panel (A) shows the best-fit models of M. M. Murphy et al. (2024b), whom initially inferred an evening–morning temperature difference based on the NIRCam F322W2 spectra, extended to our wider wavelength range. We reduced the opacity of the F444W and MIRI points to emphasize that these data were not used in M. M. Murphy et al. (2024b). Panel (B) shows the best-fit models of L. Welbanks et al. (2024a), recomputed for the differing evening- and morning-limb temperatures. We find evidence for evening–morning variation in the abundances of SO2 and CO2 as well as a heterogeneous cloud distribution. The solid line in panel (C) shows the result of including these asymmetries, while the dotted line includes just the molecular asymmetries.
Paper: A Panchromatic Characterization of the Evening and Morning Atmosphere of WASP-107 b: Composition and Cloud Variations, and Insight into the Effect of Stellar Contamination
Authors: Matthew M. Murphy, Thomas G. Beatty, Everett Schlawin, Taylor J. Bell, Michael Radica, Thomas D. Kennedy, Nishil Mehta, Luis Welbanks, Michael R. Line, Vivien Parmentier, Thomas P. Greene, Sagnick Mukherjee, Jonathan J. Fortney, Kazumasa Ohno, Lindsey Wiser, Anastasia Triantafillides, Emily Rauscher, Isaac R. Edelman, Marcia J. Rieke
Figure caption: The evening- and morning-limb transmission spectra of WASP-107 b as observed by JWST NIRCam F322W2 (circles), NIRCam F444W (squares), and MIRI/LRS (triangles). The evening-limb spectrum is shown in orange, and the morning-limb spectrum in blue. The diagram in the lower left illustrates the orientation of each limb relative to WASP-107 b’s transit trajectory, but note that the bodies in the diagram are not to scale, they are not aligned to the true orbital geometry, and the exact shape of the colored slices do not accurately represent the true shape and scale of the limbs as probed in transmission. The NIRCam F322W2 portion of the spectrum shown here matches that first presented by M. M. Murphy et al. (2024b). In addition, while not shown, the combination of our morning and evening spectra are consistent with the panchromatic limb-combined spectrum of these instruments presented in L. Welbanks et al. (2024a).
Paper: A Panchromatic Characterization of the Evening and Morning Atmosphere of WASP-107 b: Composition and Cloud Variations, and Insight into the Effect of Stellar Contamination
Authors: Matthew M. Murphy, Thomas G. Beatty, Everett Schlawin, Taylor J. Bell, Michael Radica, Thomas D. Kennedy, Nishil Mehta, Luis Welbanks, Michael R. Line, Vivien Parmentier, Thomas P. Greene, Sagnick Mukherjee, Jonathan J. Fortney, Kazumasa Ohno, Lindsey Wiser, Anastasia Triantafillides, Emily Rauscher, Isaac R. Edelman, Marcia J. Rieke
Figure caption: Data–model residuals from fitting the broadband transit light curves of each instrument’s observation of WASP-107 b. Each time series is aligned relative to its local time of conjunction using the ephemeris of M. M. Murphy et al. (2024b). We binned the SOSS, F322W2, NRS1, F444W, NRS2, and MIRI light curves into 2.2, 3.4, 0.9, 7.0, 0.9, and 0.7 minute bins, respectively, so that all time series shown have similar scatter of ∼75 ppm. Binned data are in black, and the unbinned data are in gray. The vertical blue dashed lines mark the four approximate transit contact points for reference. We see potential starspot crossings, marked in red, during the NIRISS SOSS visit (panel (A)) and the NIRSpec G395H visit (panels (C) and (E), which are simultaneous observations in two bands). We do not see evidence for spot crossings during either of the NIRCam or MIRI visits.
Paper: A Panchromatic Characterization of the Evening and Morning Atmosphere of WASP-107 b: Composition and Cloud Variations, and Insight into the Effect of Stellar Contamination
Authors: Matthew M. Murphy, Thomas G. Beatty, Everett Schlawin, Taylor J. Bell, Michael Radica, Thomas D. Kennedy, Nishil Mehta, Luis Welbanks, Michael R. Line, Vivien Parmentier, Thomas P. Greene, Sagnick Mukherjee, Jonathan J. Fortney, Kazumasa Ohno, Lindsey Wiser, Anastasia Triantafillides, Emily Rauscher, Isaac R. Edelman, Marcia J. Rieke
Figure caption: Comparing the evening (orange) and morning (blue) limb transmission spectra observed with JWST/NIRISS SOSS (stars) and NIRSpec G395H (triangles) to those with JWST/NIRCam F322W2 and F444W (both circles). Panel (A) shows the nominal results for each instrument. Panel (B) shows the result of applying the correction we develop for contamination from starspot crossings to the NIRISS and NIRSpec spectra, discussed in Section 4.2.5. These corrections are +110 ppm and +20 ppm uniform offsets to the NIRISS evening- and morning-limb spectra, respectively, and −195 ppm and +240 ppm offsets to the NIRSpec evening- and morning-limb spectra, respectively.
Paper: A Panchromatic Characterization of the Evening and Morning Atmosphere of WASP-107 b: Composition and Cloud Variations, and Insight into the Effect of Stellar Contamination
Authors: Matthew M. Murphy, Thomas G. Beatty, Everett Schlawin, Taylor J. Bell, Michael Radica, Thomas D. Kennedy, Nishil Mehta, Luis Welbanks, Michael R. Line, Vivien Parmentier, Thomas P. Greene, Sagnick Mukherjee, Jonathan J. Fortney, Kazumasa Ohno, Lindsey Wiser, Anastasia Triantafillides, Emily Rauscher, Isaac R. Edelman, Marcia J. Rieke
Figure caption: Investigating the abundances of SO2 on WASP-107 b’s evening and morning limbs. We performed a χ2 comparison between our observed limb spectra and model spectra with varying SO2 abundance. Panel (A) shows the evening-limb spectrum from NIRCam F444W and MIRI LRS truncated to points within prominent SO2 features, with all models consistent within the 68% confidence level. Panel (B) shows the same for the morning-limb spectrum, with the points excluded from this calculation due to strong overlapping cloud absorption in MIRI plotted in gray. Panel (C) shows the full results of these tests, plotting the calculated χ2 value, relative to the minimum, as a function of the input SO2 abundance for the evening- (orange) and morning-limb (blue) cases. The corresponding confidence intervals based on J. V. Wall & C. R. Jenkins (2012) are plotted as horizontal lines. For reference, we also show SO2 abundances previously inferred from the limb-combined spectrum in the literature.
Paper: A Panchromatic Characterization of the Evening and Morning Atmosphere of WASP-107 b: Composition and Cloud Variations, and Insight into the Effect of Stellar Contamination
Authors: Matthew M. Murphy, Thomas G. Beatty, Everett Schlawin, Taylor J. Bell, Michael Radica, Thomas D. Kennedy, Nishil Mehta, Luis Welbanks, Michael R. Line, Vivien Parmentier, Thomas P. Greene, Sagnick Mukherjee, Jonathan J. Fortney, Kazumasa Ohno, Lindsey Wiser, Anastasia Triantafillides, Emily Rauscher, Isaac R. Edelman, Marcia J. Rieke
Figure caption: Investigating the abundances of CO2 on WASP-107 b’s evening and morning limbs. We performed a χ2 comparison between our observed limb spectra and model spectra with varying CO2 abundance, focusing on the ∼4.5 μm feature in NIRCam/F444W. Panel (A) shows the evening-limb spectrum with all models consistent within the 68% confidence level, and panel (B) shows the same for the morning-limb spectrum. Panel (C) shows the full results of these tests, plotting the χ2 value, relative to the minimum, as a function of the input CO2 abundance for both the evening- (orange) and morning-limb (blue) cases. The corresponding confidence intervals based on J. V. Wall & C. R. Jenkins (2012), are plotted as horizontal lines. For reference, we also show CO2 abundances previously inferred for WASP-107 b from the limb-combined spectrum in the literature.
Paper: A Panchromatic Characterization of the Evening and Morning Atmosphere of WASP-107 b: Composition and Cloud Variations, and Insight into the Effect of Stellar Contamination
Authors: Matthew M. Murphy, Thomas G. Beatty, Everett Schlawin, Taylor J. Bell, Michael Radica, Thomas D. Kennedy, Nishil Mehta, Luis Welbanks, Michael R. Line, Vivien Parmentier, Thomas P. Greene, Sagnick Mukherjee, Jonathan J. Fortney, Kazumasa Ohno, Lindsey Wiser, Anastasia Triantafillides, Emily Rauscher, Isaac R. Edelman, Marcia J. Rieke
Figure caption: Investigating the abundances of H2O on WASP-107 b’s evening and morning limbs. As in Sections 4.4 and 4.5, we performed a χ2 comparison between our observed limb spectra and model spectra with varying H2O abundance, focusing on NIRCam/F322W2. Panel (A) shows the evening-limb spectrum with all models consistent within the 68% confidence level, and panel (B) shows the same for the morning-limb spectrum. Panel (C) shows the full results of these tests, plotting the χ2 value, relative to the minimum, as a function of the input H2O abundance for both the evening- (orange) and morning-limb (blue) cases. The corresponding confidence intervals based on J. V. Wall & C. R. Jenkins (2012), are plotted as horizontal lines. For reference, we also show H2O abundances previously inferred for WASP-107 b from the limb-combined spectrum in the literature.
Paper: A Panchromatic Characterization of the Evening and Morning Atmosphere of WASP-107 b: Composition and Cloud Variations, and Insight into the Effect of Stellar Contamination
Authors: Matthew M. Murphy, Thomas G. Beatty, Everett Schlawin, Taylor J. Bell, Michael Radica, Thomas D. Kennedy, Nishil Mehta, Luis Welbanks, Michael R. Line, Vivien Parmentier, Thomas P. Greene, Sagnick Mukherjee, Jonathan J. Fortney, Kazumasa Ohno, Lindsey Wiser, Anastasia Triantafillides, Emily Rauscher, Isaac R. Edelman, Marcia J. Rieke
Figure caption: Results of time-averaging tests for each of our broadband fits (Figure 3). Top: plotting the rms of the data–model residuals, relative to the unbinned case, as a function of the number of integrations per bin N. The expected behavior of pure white noise is indicated by the dashed gray line, which falls off as ﹩1/\sqrt{N}﹩. Bottom: plotting the raw rms as a function of the actual temporal size of each bin. The expected white noise behaviors, different for each instrument, are plotted as dashed colored lines. Results for NIRISS are shown in blue, NIRCam F322W2 in black, NIRCam F444W in orange, NIRSpec NRS1 in purple, NIRSpec NRS2 in lime, and MIRI LRS in red. At the bottom, the small vertical lines indicate the length of transit ingress/egress for reference, either in units of each instrument’s integration time (top) or the actual time (bottom).
Paper: A Panchromatic Characterization of the Evening and Morning Atmosphere of WASP-107 b: Composition and Cloud Variations, and Insight into the Effect of Stellar Contamination
Authors: Matthew M. Murphy, Thomas G. Beatty, Everett Schlawin, Taylor J. Bell, Michael Radica, Thomas D. Kennedy, Nishil Mehta, Luis Welbanks, Michael R. Line, Vivien Parmentier, Thomas P. Greene, Sagnick Mukherjee, Jonathan J. Fortney, Kazumasa Ohno, Lindsey Wiser, Anastasia Triantafillides, Emily Rauscher, Isaac R. Edelman, Marcia J. Rieke
Figure caption: Results from our two GCM families of runs of WASP-107 b. The left column (panels (Ai) and (Aii)) show the results from RM-GCM and the right column (panels (Bi) and (Bii)) from SPARC/MITgcm. The top panels ((Ai) and (Bi)) show the evening (orange) and morning (blue) terminator temperature–pressure profiles in each model for both the cloudy (solid) and clear (dashed) atmosphere cases. For reference, the vertical dotted lines and shaded regions are the evening- and morning-limb temperatures and uncertainties determined from the observed limb spectra by M. M. Murphy et al. (2024b). We also plot the approximate condensation curves for relevant species (Na2S, ZnS, KCl, and MnS) following the equations of C. V. Morley et al. (2012) for 10 × solar metallicity, but note these are independent of the GCM. The bottom panels ((Aii) and (Bii)) show the evening–morning temperature difference as a function of pressure, compared to that inferred by M. M. Murphy et al. (2024b). For reference, in each panel, the gray bar indicates the approximate range of pressures that our observations probe based on A. Dyrek et al. (2024).
Paper: A Panchromatic Characterization of the Evening and Morning Atmosphere of WASP-107 b: Composition and Cloud Variations, and Insight into the Effect of Stellar Contamination
Authors: Matthew M. Murphy, Thomas G. Beatty, Everett Schlawin, Taylor J. Bell, Michael Radica, Thomas D. Kennedy, Nishil Mehta, Luis Welbanks, Michael R. Line, Vivien Parmentier, Thomas P. Greene, Sagnick Mukherjee, Jonathan J. Fortney, Kazumasa Ohno, Lindsey Wiser, Anastasia Triantafillides, Emily Rauscher, Isaac R. Edelman, Marcia J. Rieke
Figure caption: Gallery of light-curve residuals from our fits to the JWST/NIRSpec G395H spectroscopic light curves, with NRS1 data on the left and NRS2 on the right. Gray points are the light curve at native cadence, and black points are binned to ∼500 s cadence chosen to be consistent across all instruments (Figures B1–B5). Each channel’s residual time series is vertically offset for visual separation, and note the different offsets in each panel. The vertical blue lines demarcate the approximate four transit contacts to indicate ingress and egress.
Paper: A Panchromatic Characterization of the Evening and Morning Atmosphere of WASP-107 b: Composition and Cloud Variations, and Insight into the Effect of Stellar Contamination
Authors: Matthew M. Murphy, Thomas G. Beatty, Everett Schlawin, Taylor J. Bell, Michael Radica, Thomas D. Kennedy, Nishil Mehta, Luis Welbanks, Michael R. Line, Vivien Parmentier, Thomas P. Greene, Sagnick Mukherjee, Jonathan J. Fortney, Kazumasa Ohno, Lindsey Wiser, Anastasia Triantafillides, Emily Rauscher, Isaac R. Edelman, Marcia J. Rieke
Figure caption: Gallery of light-curve residuals from our fits to the JWST/NIRCam F322W2 spectroscopic light curves. Gray points are the light curve at native cadence, and black points are binned to ∼500 s cadence chosen to be consistent across all instruments (Figures B2–B5). Each channel’s residual time series is vertically offset for visual separation. The vertical blue lines demarcate the approximate four transit contacts to indicate ingress and egress.
Paper: A Panchromatic Characterization of the Evening and Morning Atmosphere of WASP-107 b: Composition and Cloud Variations, and Insight into the Effect of Stellar Contamination
Authors: Matthew M. Murphy, Thomas G. Beatty, Everett Schlawin, Taylor J. Bell, Michael Radica, Thomas D. Kennedy, Nishil Mehta, Luis Welbanks, Michael R. Line, Vivien Parmentier, Thomas P. Greene, Sagnick Mukherjee, Jonathan J. Fortney, Kazumasa Ohno, Lindsey Wiser, Anastasia Triantafillides, Emily Rauscher, Isaac R. Edelman, Marcia J. Rieke
Figure caption: Comparing the relative limb transit depths of WASP-107 b to WASP-39 b (N. Espinoza et al. 2024). Panel (A) shows the evening-limb spectra for each planet, relative to the depth at 4.15 μm and scaled to each planet’s scale height. Panel (B) shows the same for the morning-limb spectra, and panel (C) shows the relative evening- and morning-limb spectra just for WASP-107 b.
Paper: A Panchromatic Characterization of the Evening and Morning Atmosphere of WASP-107 b: Composition and Cloud Variations, and Insight into the Effect of Stellar Contamination
Authors: Matthew M. Murphy, Thomas G. Beatty, Everett Schlawin, Taylor J. Bell, Michael Radica, Thomas D. Kennedy, Nishil Mehta, Luis Welbanks, Michael R. Line, Vivien Parmentier, Thomas P. Greene, Sagnick Mukherjee, Jonathan J. Fortney, Kazumasa Ohno, Lindsey Wiser, Anastasia Triantafillides, Emily Rauscher, Isaac R. Edelman, Marcia J. Rieke
Figure caption: Relative changes in the best-fit evening- (top panel) and morning-limb (bottom panel) transmission spectra when unfixing certain orbital parameters during the fit. The effects of unfixing the period are shown as circles, semimajor axis as squares, inclination as triangles, and eccentricity as stars. We compare these changes to the relative 1σ uncertainty obtained on the limb depths, shown by the black dashed lines.
Paper: A Panchromatic Characterization of the Evening and Morning Atmosphere of WASP-107 b: Composition and Cloud Variations, and Insight into the Effect of Stellar Contamination
Authors: Matthew M. Murphy, Thomas G. Beatty, Everett Schlawin, Taylor J. Bell, Michael Radica, Thomas D. Kennedy, Nishil Mehta, Luis Welbanks, Michael R. Line, Vivien Parmentier, Thomas P. Greene, Sagnick Mukherjee, Jonathan J. Fortney, Kazumasa Ohno, Lindsey Wiser, Anastasia Triantafillides, Emily Rauscher, Isaac R. Edelman, Marcia J. Rieke
Figure caption: Spatial distributions of MnS (left) and Na2S (right) clouds as a function of longitude, averaged over all latitudes, and pressure in our cloudy SPARC/MITgcm model. The color mapping represents the mass mixing ratio of the cloud particle, with the same scaling in each panel.
Paper: A Panchromatic Characterization of the Evening and Morning Atmosphere of WASP-107 b: Composition and Cloud Variations, and Insight into the Effect of Stellar Contamination
Authors: Matthew M. Murphy, Thomas G. Beatty, Everett Schlawin, Taylor J. Bell, Michael Radica, Thomas D. Kennedy, Nishil Mehta, Luis Welbanks, Michael R. Line, Vivien Parmentier, Thomas P. Greene, Sagnick Mukherjee, Jonathan J. Fortney, Kazumasa Ohno, Lindsey Wiser, Anastasia Triantafillides, Emily Rauscher, Isaac R. Edelman, Marcia J. Rieke
Figure caption: Gallery of light-curve residuals from our fits to the JWST/NIRCam F444W spectroscopic light curves. Gray points are the light curve at native cadence, and black points are binned to ∼500 s cadence chosen to be consistent across all instruments (Figures B1–B5). Each channel’s residual time series is vertically offset for visual separation. The vertical blue lines demarcate the approximate four transit contacts to indicate ingress and egress.