adsabs/AstroCLIMB huggingface dataset:
Paper: Emission from Multiple Molecular Isotopologues in a High-inclination Protoplanetary Disk
Authors: Colette Salyk, Klaus M. Pontoppidan, Andrea Banzatti, Edwin Bergin, Nicole Arulanantham, Joan Najita, Geoffrey A. Blake, John Carr, Ke Zhang, Chengyan Xie
Figure caption: Left: best-fit CO2 column density vs. temperature for published slab models. For 2MASS-J16053215-1933159, we show the “Component II” fits, which are consistent with the nondetection of 13CO2 in that source (B. Tabone et al. 2023), and for Sz 98, we show both reported models (D. Gasman et al. 2023), connected by a blue line. The sources with the three highest column densities are labeled. Center: best-fit HCN column density vs. temperature. Right: best-fit cold vs. hot water temperatures. The sources on the 1:1 line were fit with only a single water component. If more than two components were used in the fit, we show the warmest and coolest components. The slab model parameters shown in all three panels are collected from D. Gasman et al. (2023), B. Tabone et al. (2023), K. R. Schwarz et al. (2024), A. Banzatti et al. (2023), C. Xie et al. (2023), S. L. Grant et al. (2023, 2024), K. M. Pontoppidan et al. (2024), C. E. Muñoz-Romero et al. (2024), G. Perotti et al. (2023), and M. Temmink et al. (2024a, 2024b). The color bar shows the stellar mass in solar masses.
Paper: Emission from Multiple Molecular Isotopologues in a High-inclination Protoplanetary Disk
Authors: Colette Salyk, Klaus M. Pontoppidan, Andrea Banzatti, Edwin Bergin, Nicole Arulanantham, Joan Najita, Geoffrey A. Blake, John Carr, Ke Zhang, Chengyan Xie
Figure caption: Left: oxygen isotope fractionation relative to ISM ratios—following standard cosmochemistry notation, heavier O is to the upper right of the plot. δ17O﹩{}^{{\prime} }﹩ is defined as 103 ln (17Ri/17RLocalISM), δ18O﹩{}^{{\prime} }﹩ = 103 ln (18Ri/18RLocalISM), and Ri is the atomic ratio, while 17RLocalISM and 18RLocalISM are the local ISM atomic ratios 18O/16O and 17O/16O, i.e., the inverse of those used in the rest of the text—see also Table 1. The dotted and dashed lines have slopes of 0.5 and 1, as expected for mass-independent and mass-dependent fractionation, respectively. The green star and orange square mark our values derived from CO2 emission from MY Lup, as described in Section 4.2. Right: carbon isotope ratios derived from MY Lup’s CO2 emission (assuming a fixed oxygen ratio, as described in Section 4.2), compared to values from R. L. Smith et al. (2015), the local ISM, and the solar system (S. N. Milam et al. 2005 and references therein). The points are offset on the x-axis for clarity.
Paper: Emission from Multiple Molecular Isotopologues in a High-inclination Protoplanetary Disk
Authors: Colette Salyk, Klaus M. Pontoppidan, Andrea Banzatti, Edwin Bergin, Nicole Arulanantham, Joan Najita, Geoffrey A. Blake, John Carr, Ke Zhang, Chengyan Xie
Figure caption: (a) χ2 contours for a fit to HCN only. Here and in panel (b), a white star marks the best-fit model; the white circles mark additional models explored in panel (c). The white contours mark 1σ, 2σ, and 3σ confidence intervals, assuming the minimum ﹩{\chi }_{{\rm{red}}}^{2}=1﹩. (b) χ2 contours for a combined fit to HCN and H13CN, with 12C/13C fixed to the ISM ratio. (c) Three models (with parameters marked in panel (a)) with differing 12C/13C ratios but only subtle changes in the quality of the model fit. (d) Best-fit model for HCN and H13CN combined (﹩{N}_{{\rm{HCN}}}=1.4\times 1{0}^{19}\,{{\rm{cm}}}^{-2}﹩, ﹩{N}_{{{\rm{H}}}^{13}{\rm{CN}}}=2.0\times 1{0}^{17}\,{{\rm{cm}}}^{-2}﹩, T = 250 K, and R = 0.61 au), with 12C/13C fixed to the ISM ratio, corresponding to the star in panel (b). A pink triangle marks a tentative detection of HC15N, and the brown curve shows a C2H2 model with T = 250 K, R = 0.61 au, and N = 1016 cm−2.
Paper: Emission from Multiple Molecular Isotopologues in a High-inclination Protoplanetary Disk
Authors: Colette Salyk, Klaus M. Pontoppidan, Andrea Banzatti, Edwin Bergin, Nicole Arulanantham, Joan Najita, Geoffrey A. Blake, John Carr, Ke Zhang, Chengyan Xie
Figure caption: Analysis with C ratios fixed to ISM values. (a) χ2 diagram for combined 13CO2 and 12CO2 fit. The white star shows the best-fit model, while the white circles show models highlighted in panel (b). The white solid and yellow dashed lines have the same meaning as in Figure 7(a). (b) 13CO2 Q branch overplotted with the best-fit model and two additional models at the edges of the 2σ χ2 contour. The legend labels show the values of ﹩{{N}_{\mathrm{CO}}}_{2}﹩ and T for these models. (c) C18O16O Q branch overplotted with models assuming the best-fit 16O/18O ratio and those representing the best fit ±1σ. (d) C17O16O Q branch overplotted with a model with the best-fit 16O/17O as well as one representing the best fit −1σ.
Paper: Emission from Multiple Molecular Isotopologues in a High-inclination Protoplanetary Disk
Authors: Colette Salyk, Klaus M. Pontoppidan, Andrea Banzatti, Edwin Bergin, Nicole Arulanantham, Joan Najita, Geoffrey A. Blake, John Carr, Ke Zhang, Chengyan Xie
Figure caption: Continuum- and water-subtracted MIRI-MRS spectrum of MY Lup (black) compared with three slab models (colors). Residuals (with regions contaminated by isotopologues or atomic emission removed) are shown below. The middle panels highlight two regions with significant differences between the residuals. The bottom panel highlights a CO2 feature in the HCN-emitting region, which was not included in the calculation of χ2.
Paper: Emission from Multiple Molecular Isotopologues in a High-inclination Protoplanetary Disk
Authors: Colette Salyk, Klaus M. Pontoppidan, Andrea Banzatti, Edwin Bergin, Nicole Arulanantham, Joan Najita, Geoffrey A. Blake, John Carr, Ke Zhang, Chengyan Xie
Figure caption: Analysis with the 16O/18O ratio fixed to the ISM value. (a) χ2 diagram for combined C18O16O and CO2 fit. The white star shows the best-fit model, while the white circles show the models highlighted in panel (b). The white solid and yellow dashed lines have the same meaning as in Figure 9(a). (b) C18O16O Q branch overplotted with the best-fit model and two additional models at the edges of the 2σ χ2 contour. The legend labels show the values of ﹩{N{}_{{\rm{CO}}}}_{2}﹩ and T for these models. (c) 13CO2 Q branch overplotted with models assuming the best-fit 13CO2 ratio and those representing the best fit ±1σ. (d) C17O16O Q branch overplotted with a model with the best-fit 16O/17O as well as one representing the best fit −1σ.
Paper: Emission from Multiple Molecular Isotopologues in a High-inclination Protoplanetary Disk
Authors: Colette Salyk, Klaus M. Pontoppidan, Andrea Banzatti, Edwin Bergin, Nicole Arulanantham, Joan Najita, Geoffrey A. Blake, John Carr, Ke Zhang, Chengyan Xie
Figure caption: Schematic demonstrating how an edge-on line of sight can increase the optical path through the disk atmosphere as compared to a face-on line of sight.
Paper: Emission from Multiple Molecular Isotopologues in a High-inclination Protoplanetary Disk
Authors: Colette Salyk, Klaus M. Pontoppidan, Andrea Banzatti, Edwin Bergin, Nicole Arulanantham, Joan Najita, Geoffrey A. Blake, John Carr, Ke Zhang, Chengyan Xie
Figure caption: Close-up of selected H I transitions. Upper and lower electronic levels are shown in the upper right of each panel.
Paper: Emission from Multiple Molecular Isotopologues in a High-inclination Protoplanetary Disk
Authors: Colette Salyk, Klaus M. Pontoppidan, Andrea Banzatti, Edwin Bergin, Nicole Arulanantham, Joan Najita, Geoffrey A. Blake, John Carr, Ke Zhang, Chengyan Xie
Figure caption: Subtraction of CO2 model from water-model-subtracted data in the HCN-emitting region.
Paper: Searching for GEMS: Discovery and Characterization of Two Brown Dwarfs Around M Dwarfs 
Authors: Alexander Larsen, Tera N. Swaby, Henry A. Kobulnicky, Caleb I. Cañas, Shubham Kanodia, Jessica Libby-Roberts, Andrew Monson, Arvind F. Gupta, William Cochran, Suvrath Mahadevan, Chad Bender, Scott A. Diddams, Samuel Halverson, Andrea S. J. Lin, Maxwell Moe, Joe Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Gudmundur Stefansson
Figure caption: Host mass vs. companion mass for known transiting BDs. Black triangles denote transiting systems while gray dots denote nontransiting. The red dot denotes TOI-5389Ab and the blue × denotes TOI-5610b. The dashed lines mark the upper and lower mass limits for BDs at 80 and 13 MJ, respectively.
Paper: Searching for GEMS: Discovery and Characterization of Two Brown Dwarfs Around M Dwarfs 
Authors: Alexander Larsen, Tera N. Swaby, Henry A. Kobulnicky, Caleb I. Cañas, Shubham Kanodia, Jessica Libby-Roberts, Andrew Monson, Arvind F. Gupta, William Cochran, Suvrath Mahadevan, Chad Bender, Scott A. Diddams, Samuel Halverson, Andrea S. J. Lin, Maxwell Moe, Joe Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Gudmundur Stefansson
Figure caption: The Sonora–Bobcat models on a plot of companion radius vs. mass. The red lines represent isochrones of 0.1, 0.2, 0.4, 1, 3, and 10 Gyr (from light to dark), all at solar metallicity (﹩\left[{\rm{Fe}}/{\rm{H}}\right]=0.0﹩). The blue line shows the nearest model to TOI-5610b which is 1.5 Gyr at ﹩\left[{\rm{Fe}}/{\rm{H}}\right]=-0.5﹩. Only transiting systems are plotted. These models assume cloud-free atmospheres and solar C/O ratios.
Paper: Searching for GEMS: Discovery and Characterization of Two Brown Dwarfs Around M Dwarfs 
Authors: Alexander Larsen, Tera N. Swaby, Henry A. Kobulnicky, Caleb I. Cañas, Shubham Kanodia, Jessica Libby-Roberts, Andrew Monson, Arvind F. Gupta, William Cochran, Suvrath Mahadevan, Chad Bender, Scott A. Diddams, Samuel Halverson, Andrea S. J. Lin, Maxwell Moe, Joe Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Gudmundur Stefansson
Figure caption: Comparison plot of mass ratio vs. semimajor axis. Black triangles denote transiting systems while gray dots denote nontransiting. The red dot denotes TOI-5389Ab and the blue × denotes TOI-5610b. The histogram on the right shows the distribution in ﹩{\mathrm{log}}\,q﹩, transiting systems in black.
Paper: Searching for GEMS: Discovery and Characterization of Two Brown Dwarfs Around M Dwarfs 
Authors: Alexander Larsen, Tera N. Swaby, Henry A. Kobulnicky, Caleb I. Cañas, Shubham Kanodia, Jessica Libby-Roberts, Andrew Monson, Arvind F. Gupta, William Cochran, Suvrath Mahadevan, Chad Bender, Scott A. Diddams, Samuel Halverson, Andrea S. J. Lin, Maxwell Moe, Joe Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Gudmundur Stefansson
Figure caption: Cumulative distribution function for M-dwarf/BD systems divided into two populations via period. The light lines represent differing MCMC chains while the dark lines represent their averages.
Paper: Searching for GEMS: Discovery and Characterization of Two Brown Dwarfs Around M Dwarfs 
Authors: Alexander Larsen, Tera N. Swaby, Henry A. Kobulnicky, Caleb I. Cañas, Shubham Kanodia, Jessica Libby-Roberts, Andrew Monson, Arvind F. Gupta, William Cochran, Suvrath Mahadevan, Chad Bender, Scott A. Diddams, Samuel Halverson, Andrea S. J. Lin, Maxwell Moe, Joe Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Gudmundur Stefansson
Figure caption: Phased barycentric radial velocity curve and best-fit model for TOI-5389A. Residuals are plotted below. Systemic velocity γ is subtracted. Error bars are plotted but are too small to see.
Paper: Searching for GEMS: Discovery and Characterization of Two Brown Dwarfs Around M Dwarfs 
Authors: Alexander Larsen, Tera N. Swaby, Henry A. Kobulnicky, Caleb I. Cañas, Shubham Kanodia, Jessica Libby-Roberts, Andrew Monson, Arvind F. Gupta, William Cochran, Suvrath Mahadevan, Chad Bender, Scott A. Diddams, Samuel Halverson, Andrea S. J. Lin, Maxwell Moe, Joe Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Gudmundur Stefansson
Figure caption: Phased barycentric radial velocity curve and best-fit model for TOI-5610. Residuals are plotted below. Systemic velocity γ is subtracted. Error bars are plotted but are too small to see.
Paper: JWST-TST DREAMS: A Precise Water Abundance for Hot Jupiter WASP-17b from the NIRISS SOSS Transmission Spectrum
Authors: Dana R. Louie, Elijah Mullens, Lili Alderson, Ana Glidden, Nikole K. Lewis, Hannah R. Wakeford, Natasha E. Batalha, Knicole D. Colón, Amélie Gressier, Douglas Long, Michael Radica, Néstor Espinoza, Jayesh Goyal, Ryan J. MacDonald, Erin M. May, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, David Grant, Jingcheng Huang, Zifan Lin, Daniel Valentine, Mark Clampin, Marshall Perrin, Laurent Pueyo, Roeland P. van der Marel, C. Matt Mountain
Figure caption: Atmospheric retrievals with POSEIDON and pRT on HST + Spitzer data (L. Alderson et al. 2022), SOSS order 1 and 2 data (Ahsoka reduction, this work), and MIRI LRS data (D. Grant et al. 2023). Top and middle: median retrieved spectra (solid lines), with 1σ and 2σ confidence intervals (dark and light shaded regions) for POSEIDON retrievals on the full data set (top) and pRT retrieval on the full data set (middle). Retrievals displayed are those using the chemical inventory of model B (Appendix Table 4), with and without H−, and the retrievals from D. Grant et al. (2023) for comparison. Bottom panels: retrieved posteriors for isothermal atmospheric temperature and gas-phase volume mixing ratios (columns one and two) and cloud properties from POSEIDON (column three) and pRT (column four).
Paper: JWST-TST DREAMS: A Precise Water Abundance for Hot Jupiter WASP-17b from the NIRISS SOSS Transmission Spectrum
Authors: Dana R. Louie, Elijah Mullens, Lili Alderson, Ana Glidden, Nikole K. Lewis, Hannah R. Wakeford, Natasha E. Batalha, Knicole D. Colón, Amélie Gressier, Douglas Long, Michael Radica, Néstor Espinoza, Jayesh Goyal, Ryan J. MacDonald, Erin M. May, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, David Grant, Jingcheng Huang, Zifan Lin, Daniel Valentine, Mark Clampin, Marshall Perrin, Laurent Pueyo, Roeland P. van der Marel, C. Matt Mountain
Figure caption: Examination of three different LD treatments on the Ahsoka WASP-17b NIRISS SOSS R = 100 transmission spectrum. The top panel presents the three versions of the transmission spectrum. The second (middle top) and third (middle bottom) panels show the differences between two earlier LD treatments and our final Ahsoka analysis, where we fit LD at the pixel level, and then binned our results to R = 100. The second panel illustrates this difference with our original analysis, where we fixed LD at the pixel level, then binned to R = 100. The third panel displays this difference with an analysis where the pixel-level data were binned to R = 100 and then fit for LD. The two middle panels reveal that LD treatments have a progressively higher impact at longer wavelengths. The bottom panel compares our two earlier LD treatments, where we see a general agreement to within 1σ across most of the NIRISS SOSS bandpass. Note that all spectra are affected by field star contamination in the region just beyond 2 μm (see Figure 5), resulting in a region of lower transit depths. See Section 3.8 for detailed discussion.
Paper: JWST-TST DREAMS: A Precise Water Abundance for Hot Jupiter WASP-17b from the NIRISS SOSS Transmission Spectrum
Authors: Dana R. Louie, Elijah Mullens, Lili Alderson, Ana Glidden, Nikole K. Lewis, Hannah R. Wakeford, Natasha E. Batalha, Knicole D. Colón, Amélie Gressier, Douglas Long, Michael Radica, Néstor Espinoza, Jayesh Goyal, Ryan J. MacDonald, Erin M. May, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, David Grant, Jingcheng Huang, Zifan Lin, Daniel Valentine, Mark Clampin, Marshall Perrin, Laurent Pueyo, Roeland P. van der Marel, C. Matt Mountain
Figure caption: Examination of order 0 field star contaminant. Here, we construct the median of our time series of extracted 1D stellar spectra. The order 0 field star contaminant visible in Figure 4 between columns 768 (2.050 μm) and 791 (2.073 μm) manifests as excess flux in order 1 over the corresponding wavelength range. We depict the contamination region using gray shading. Field star contaminants dilute the transmission spectrum at wavelengths where the contamination occurs. A field star contaminant is also visible near 1.0 μm in order 2, but we do not extract order 2 wavelengths beyond 0.95 μm (indicated by the dotted line), since the S/N for order 1 is much higher in this wavelength regime.
Paper: JWST-TST DREAMS: A Precise Water Abundance for Hot Jupiter WASP-17b from the NIRISS SOSS Transmission Spectrum
Authors: Dana R. Louie, Elijah Mullens, Lili Alderson, Ana Glidden, Nikole K. Lewis, Hannah R. Wakeford, Natasha E. Batalha, Knicole D. Colón, Amélie Gressier, Douglas Long, Michael Radica, Néstor Espinoza, Jayesh Goyal, Ryan J. MacDonald, Erin M. May, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, David Grant, Jingcheng Huang, Zifan Lin, Daniel Valentine, Mark Clampin, Marshall Perrin, Laurent Pueyo, Roeland P. van der Marel, C. Matt Mountain
Figure caption: WASP-17b transmission spectrum with the best-fit PICASO + Virga forward model and pressure–temperature profile, compared to forward model fits from D. Grant et al. 2023. Left: forward models presented by D. Grant et al. (2023) fit to HST + Spitzer + MIRI spectra are shown in pink (ATMO) and yellow (PICASO + Virga) with the fit offsets for the HST data (light gray). The best-fit PICASO + Virga forward model applied to this work (STIS + SOSS + MIRI) is shown in dark blue with the offsets applied to the HST STIS data (dark gray). Both PICASO + Virga models show similar properties in the infrared (IR) but diverge in the optical where the STIS data are allowed to “float” (with a fit offset) to match the higher precision JWST data. Right: pressure–temperature profiles for each of the models along with the condensation curve for SiO2(s) at 1× and 50 × solar metallicity. The shaded region denotes the pressures probed in transmission over the full wavelength range.
Paper: JWST-TST DREAMS: A Precise Water Abundance for Hot Jupiter WASP-17b from the NIRISS SOSS Transmission Spectrum
Authors: Dana R. Louie, Elijah Mullens, Lili Alderson, Ana Glidden, Nikole K. Lewis, Hannah R. Wakeford, Natasha E. Batalha, Knicole D. Colón, Amélie Gressier, Douglas Long, Michael Radica, Néstor Espinoza, Jayesh Goyal, Ryan J. MacDonald, Erin M. May, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, David Grant, Jingcheng Huang, Zifan Lin, Daniel Valentine, Mark Clampin, Marshall Perrin, Laurent Pueyo, Roeland P. van der Marel, C. Matt Mountain
Figure caption: WASP-17b NIRISS SOSS F277W exposure following application of Ahsoka Stages 1 and 2. The PASTASOSS-derived spectral traces and optimized spectral extraction widths are shown for reference. The F277W exposure reveals bright chevron-shaped order 0 field star contaminants, which dilute the transmission spectrum at those wavelengths corresponding to regions where they overlap the order 1 and order 2 spectral extraction regions. Through examination of the spatial cross sections of the order 0 field star contaminants, we determined the most significant contaminant lies between columns 768 and 791 of order 1. See Figure 5 for details.
Paper: JWST-TST DREAMS: A Precise Water Abundance for Hot Jupiter WASP-17b from the NIRISS SOSS Transmission Spectrum
Authors: Dana R. Louie, Elijah Mullens, Lili Alderson, Ana Glidden, Nikole K. Lewis, Hannah R. Wakeford, Natasha E. Batalha, Knicole D. Colón, Amélie Gressier, Douglas Long, Michael Radica, Néstor Espinoza, Jayesh Goyal, Ryan J. MacDonald, Erin M. May, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, David Grant, Jingcheng Huang, Zifan Lin, Daniel Valentine, Mark Clampin, Marshall Perrin, Laurent Pueyo, Roeland P. van der Marel, C. Matt Mountain
Figure caption: Eureka! (T. J. Bell et al. 2022) Stage 5 white light curve emcee (D. Foreman-Mackey et al. 2013) fits to the Ahsoka data reduction for order 1 (left ) and order 2 (right ). The top panels depict the data corrected with our polynomial systematics model (colored points), and overplotted with the best-fit transit model (black curves). The center panels show residuals, with rms scatter indicated in black text. In the top and center plots, mean error bars are 145 ppm for order 1 and 209 ppm for order 2. The bottom panels show histogram distributions of residuals in terms of the number of standard deviations σ. We overplot Gaussian curves matching the values of mean and standard deviation for the residuals of each order. The alignment of our distributions with a Gaussian trend indicates the systematics are well handled. See Table 1 for our white light curve prior and best-fit parameter values.
Paper: JWST-TST DREAMS: A Precise Water Abundance for Hot Jupiter WASP-17b from the NIRISS SOSS Transmission Spectrum
Authors: Dana R. Louie, Elijah Mullens, Lili Alderson, Ana Glidden, Nikole K. Lewis, Hannah R. Wakeford, Natasha E. Batalha, Knicole D. Colón, Amélie Gressier, Douglas Long, Michael Radica, Néstor Espinoza, Jayesh Goyal, Ryan J. MacDonald, Erin M. May, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, David Grant, Jingcheng Huang, Zifan Lin, Daniel Valentine, Mark Clampin, Marshall Perrin, Laurent Pueyo, Roeland P. van der Marel, C. Matt Mountain
Figure caption: WASP-17b NIRISS SOSS transmission spectra from our three independent pipelines, presented at R = 100. Top: order 1 and order 2 reductions from each pipeline. Bottom three panels: we plot the differences in transit depths between pipelines. In the wavelength region where we have transit depths for both order 1 and order 2, we compare only the values for order 1. Additionally, we make no comparisons for points where we do not have transit depth values for all three pipelines. (For example, the Ahsoka analysis does not include data short-ward of 0.63 μm, so we make no comparisons at those shorter wavelengths.) See text for a discussion of similarities and differences between the results of the three pipelines.
Paper: JWST-TST DREAMS: A Precise Water Abundance for Hot Jupiter WASP-17b from the NIRISS SOSS Transmission Spectrum
Authors: Dana R. Louie, Elijah Mullens, Lili Alderson, Ana Glidden, Nikole K. Lewis, Hannah R. Wakeford, Natasha E. Batalha, Knicole D. Colón, Amélie Gressier, Douglas Long, Michael Radica, Néstor Espinoza, Jayesh Goyal, Ryan J. MacDonald, Erin M. May, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, David Grant, Jingcheng Huang, Zifan Lin, Daniel Valentine, Mark Clampin, Marshall Perrin, Laurent Pueyo, Roeland P. van der Marel, C. Matt Mountain
Figure caption: Examples of our Eureka! (T. J. Bell et al. 2022) Stage 5 spectroscopic light curve emcee (D. Foreman-Mackey et al. 2013) pixel-level fits to the Ahsoka data reduction for orders 1 and 2. Plots on the left show the pixel-level data corrected with polynomial systematics models (colored points), and overplotted with the best-fit transit models (black curves). The wavelengths for each spectral channel are shown above the corresponding transit light curve. The panels on the right show the residuals for the corresponding data, with rms scatter indicated in black text. Data and best-fit transit curves are offset for each spectral channel for clarity. See Section 3.4.2 for further details.