adsabs/AstroCLIMB huggingface dataset:
Paper: Predictions for the Dynamical States of the Didymos System before and after the Planned DART Impact
Authors: Derek C. Richardson, Harrison F. Agrusa, Brent Barbee, William F. Bottke, Andrew F. Cheng, Siegfried Eggl, Fabio Ferrari, Masatoshi Hirabayashi, Özgür Karatekin, Jay McMahon, Stephen R. Schwartz, Ronald-Louis Ballouz, Adriano Campo Bagatin, Elisabetta Dotto, Eugene G. Fahnestock, Oscar Fuentes-Muñoz, Ioannis Gkolias, Douglas P. Hamilton, Seth A. Jacobson, Martin Jutzi, Josh Lyzhoft, Rahil Makadia, Alex J. Meyer, Patrick Michel, Ryota Nakano, Guillaume Noiset, Sabina D. Raducan, Nicolas Rambaux, Alessandro Rossi, Paul Sánchez, Daniel J. Scheeres, Stefania Soldini, Angela M. Stickle, Paolo Tanga, Kleomenis Tsiganis, Yun Zhang
Figure caption: Comparisons of the attitude of Dimorphos resulting from (a) an idealized planar impact versus (b) the expected impact geometry for the current DART trajectory. Since the nonplanar components of DART’s velocity vector are relatively small, the realistic impact geometry closely matches the idealized planar case.
Paper: Predictions for the Dynamical States of the Didymos System before and after the Planned DART Impact
Authors: Derek C. Richardson, Harrison F. Agrusa, Brent Barbee, William F. Bottke, Andrew F. Cheng, Siegfried Eggl, Fabio Ferrari, Masatoshi Hirabayashi, Özgür Karatekin, Jay McMahon, Stephen R. Schwartz, Ronald-Louis Ballouz, Adriano Campo Bagatin, Elisabetta Dotto, Eugene G. Fahnestock, Oscar Fuentes-Muñoz, Ioannis Gkolias, Douglas P. Hamilton, Seth A. Jacobson, Martin Jutzi, Josh Lyzhoft, Rahil Makadia, Alex J. Meyer, Patrick Michel, Ryota Nakano, Guillaume Noiset, Sabina D. Raducan, Nicolas Rambaux, Alessandro Rossi, Paul Sánchez, Daniel J. Scheeres, Stefania Soldini, Angela M. Stickle, Paolo Tanga, Kleomenis Tsiganis, Yun Zhang
Figure caption: Top-down views of the rubble-pile models of Dimorphos in PKDGRAV. (a) is the stable case, with a/b = 1.2 and b/c = 1.1, while (b) is the unstable case, with a/b = 1.3 and b/c = 1.2. Despite the small apparent difference in their respective shapes, the resulting spin evolutions of these two rubble piles will differ significantly. Didymos is not included in this visualization, since it is just a point mass in these simulations.
Paper: An Open-source Bayesian Atmospheric Radiative Transfer (BART) Code. I. Design, Tests, and Application to Exoplanet HD 189733b
Authors: Joseph Harrington, Michael D. Himes, Patricio E. Cubillos, Jasmina Blecic, Patricio M. Rojo, Ryan C. Challener, Nate B. Lust, M. Oliver Bowman, Sarah D. Blumenthal, Ian Dobbs-Dixon, Andrew S. D. Foster, Austin J. Foster, M. R. Green, Thomas J. Loredo, Kathleen J. McIntyre, Madison M. Stemm, David C. Wright
Figure caption: Comparison between input and retrieved T(p) profiles (left column), the normalized contribution functions (middle column, BART3), and best-fit molecular abundances (right column) for the isothermal (top row), noninverted (middle row), and inverted (bottom row) emission cases of the s01hjcleariso, s02hjclearnoinv, and s03hjclearinv tests. Dark- and light-blue shadings in T(p) profile plots designate the 68.27% and 95.45% credible regions, respectively. These regions and the median derive from all the fits on a per-pressure-level basis. They do not follow the functional form of the individual profiles. Few, if any, individual T(p) profiles, including the best fit, stay confined to these regions, especially where the contribution functions indicate low sensitivity. BART accurately retrieves the T(p) profile and abundances wherever they contribute to the spectra. However, isothermal, nonscattering emission spectra are blackbodies, insensitive to abundances. Most MCMC-proposed spectra in those cases are not isothermal. Those with detectable structure (high abundances) are rarely accepted, creating the artificially low upper limits. This affects all Monte Carlo Bayesian retrievals.
Paper: An Open-source Bayesian Atmospheric Radiative Transfer (BART) Code. I. Design, Tests, and Application to Exoplanet HD 189733b
Authors: Joseph Harrington, Michael D. Himes, Patricio E. Cubillos, Jasmina Blecic, Patricio M. Rojo, Ryan C. Challener, Nate B. Lust, M. Oliver Bowman, Sarah D. Blumenthal, Ian Dobbs-Dixon, Andrew S. D. Foster, Austin J. Foster, M. R. Green, Thomas J. Loredo, Kathleen J. McIntyre, Madison M. Stemm, David C. Wright
Figure caption: The BART Chart. In the main optimization loop (thick white arrows in the upper right), the statistics package (MC3, aqua box, top) feeds sets of free parameters to the RT machinery (BART2 and BART3; green boxes are code modules; white boxes name the information being transferred). Blue boxes are initialization and support (BART3). Straight bottoms indicate routines, while wavy bottoms indicate input from static data sources (files). The black silhouetted space telescope represents the observations. See Section 3.
Paper: An Open-source Bayesian Atmospheric Radiative Transfer (BART) Code. I. Design, Tests, and Application to Exoplanet HD 189733b
Authors: Joseph Harrington, Michael D. Himes, Patricio E. Cubillos, Jasmina Blecic, Patricio M. Rojo, Ryan C. Challener, Nate B. Lust, M. Oliver Bowman, Sarah D. Blumenthal, Ian Dobbs-Dixon, Andrew S. D. Foster, Austin J. Foster, M. R. Green, Thomas J. Loredo, Kathleen J. McIntyre, Madison M. Stemm, David C. Wright
Figure caption: Best-fit spectra for the six synthetic retrieval tests of s01hjcleariso, s02hjclearnoinv, and s03hjclearinv: isothermal (top row), noninverted (middle row), and inverted (bottom row) atmospheres in transit (left column) and eclipse (right column) geometries. The transmission data look similar for all three cases, as they only differ in thermal profiles, to which transit geometry is generally insensitive.
Paper: An Open-source Bayesian Atmospheric Radiative Transfer (BART) Code. I. Design, Tests, and Application to Exoplanet HD 189733b
Authors: Joseph Harrington, Michael D. Himes, Patricio E. Cubillos, Jasmina Blecic, Patricio M. Rojo, Ryan C. Challener, Nate B. Lust, M. Oliver Bowman, Sarah D. Blumenthal, Ian Dobbs-Dixon, Andrew S. D. Foster, Austin J. Foster, M. R. Green, Thomas J. Loredo, Kathleen J. McIntyre, Madison M. Stemm, David C. Wright
Figure caption: Forward spectra for the c04hjclearisoBarstowEtal and c05hjcloudisoBarstowEtal tests: CO at 1500 K for 10−4 mixing ratio (top left) and 10−5 mixing ratio (top right), CO at 1000 K for 10−4 mixing ratio (middle left), the cloud-free HD 189733b-inspired Model 0 (middle right), and cloudy Model 1 (bottom left). The plotted residuals are computed based on the average of the NEMESIS, CHIMERA, and TAU-REX spectra, as in Barstow et al. (2020).
Paper: An Open-source Bayesian Atmospheric Radiative Transfer (BART) Code. I. Design, Tests, and Application to Exoplanet HD 189733b
Authors: Joseph Harrington, Michael D. Himes, Patricio E. Cubillos, Jasmina Blecic, Patricio M. Rojo, Ryan C. Challener, Nate B. Lust, M. Oliver Bowman, Sarah D. Blumenthal, Ian Dobbs-Dixon, Andrew S. D. Foster, Austin J. Foster, M. R. Green, Thomas J. Loredo, Kathleen J. McIntyre, Madison M. Stemm, David C. Wright
Figure caption: Isothermal, noninverted, and inverted T(p) profiles used for the RT model tests c01hjcleariso, c02hjclearnoinv, c03hjclearinv, and their associated retrieval tests (s01hjcleariso, s02hjclearnoinv, and s03hjclearinv). The inverted and noninverted profiles use the T(p) parameterization of Line et al. (2013). The profiles have effective temperatures generally around 1100 K, to resemble HD 189733b.
Paper: An Open-source Bayesian Atmospheric Radiative Transfer (BART) Code. I. Design, Tests, and Application to Exoplanet HD 189733b
Authors: Joseph Harrington, Michael D. Himes, Patricio E. Cubillos, Jasmina Blecic, Patricio M. Rojo, Ryan C. Challener, Nate B. Lust, M. Oliver Bowman, Sarah D. Blumenthal, Ian Dobbs-Dixon, Andrew S. D. Foster, Austin J. Foster, M. R. Green, Thomas J. Loredo, Kathleen J. McIntyre, Madison M. Stemm, David C. Wright
Figure caption: Same as Figure 8, but for transmission cases of the s01hjcleariso, s02hjclearnoinv, and s03hjclearinv tests. (Recall that low-resolution transmission spectra are relatively insensitive to temperature structure.)
Paper: An Open-source Bayesian Atmospheric Radiative Transfer (BART) Code. I. Design, Tests, and Application to Exoplanet HD 189733b
Authors: Joseph Harrington, Michael D. Himes, Patricio E. Cubillos, Jasmina Blecic, Patricio M. Rojo, Ryan C. Challener, Nate B. Lust, M. Oliver Bowman, Sarah D. Blumenthal, Ian Dobbs-Dixon, Andrew S. D. Foster, Austin J. Foster, M. R. Green, Thomas J. Loredo, Kathleen J. McIntyre, Madison M. Stemm, David C. Wright
Figure caption: Spectra produced by transit for the 11 cases in the f05abundance test: the reference spectrum with no line, and the 10 spectra with 0.01%–0.1% LG1 in steps of 0.01%. Here and throughout, the axes (horizontal, in this case) may state a constant offset, for clarity.
Paper: An Open-source Bayesian Atmospheric Radiative Transfer (BART) Code. I. Design, Tests, and Application to Exoplanet HD 189733b
Authors: Joseph Harrington, Michael D. Himes, Patricio E. Cubillos, Jasmina Blecic, Patricio M. Rojo, Ryan C. Challener, Nate B. Lust, M. Oliver Bowman, Sarah D. Blumenthal, Ian Dobbs-Dixon, Andrew S. D. Foster, Austin J. Foster, M. R. Green, Thomas J. Loredo, Kathleen J. McIntyre, Madison M. Stemm, David C. Wright
Figure caption:  Transit's result for an isothermal atmosphere with theoretical Planck function overplotted (test f08isothermal).
Paper: An Open-source Bayesian Atmospheric Radiative Transfer (BART) Code. I. Design, Tests, and Application to Exoplanet HD 189733b
Authors: Joseph Harrington, Michael D. Himes, Patricio E. Cubillos, Jasmina Blecic, Patricio M. Rojo, Ryan C. Challener, Nate B. Lust, M. Oliver Bowman, Sarah D. Blumenthal, Ian Dobbs-Dixon, Andrew S. D. Foster, Austin J. Foster, M. R. Green, Thomas J. Loredo, Kathleen J. McIntyre, Madison M. Stemm, David C. Wright
Figure caption: Comparison of transit line shape to miniRT's Faddeeva function for that case (test f04broadening).
Paper: Dark-flight Estimates of Meteorite Fall Positions: Issues and a Case Study Using the Murrili Meteorite Fall
Authors: M. C. Towner, T. Jansen-Sturgeon, M. Cupak, E. K. Sansom, H. A. R. Devillepoix, P. A. Bland, R. M. Howie, J. P. Paxman, G. K. Benedix, B. A. D. Hartig
Figure caption: Plot showing the effects of density and shape on final position of a hypothetical 1 kg object. Shapes plotted are sphere, cylinder, and brick (as defined in the text). Density of the object is constrained to 2700, 3500, and 7500 kg m−3. For comparison we include the fall line based on the 2015-11-27 00:00 UTC wind snapshot (3500 kg m−3 sphere, varying mass) and the impact point from Figure 4.
Paper: Dark-flight Estimates of Meteorite Fall Positions: Issues and a Case Study Using the Murrili Meteorite Fall
Authors: M. C. Towner, T. Jansen-Sturgeon, M. Cupak, E. K. Sansom, H. A. R. Devillepoix, P. A. Bland, R. M. Howie, J. P. Paxman, G. K. Benedix, B. A. D. Hartig
Figure caption: Plot of wind profiles from each WRF model run for comparison. Dominating westerly winds at altitudes 10–15 km are typical for the subtropical jet stream in the area of the fall. The individual profiles are products of WRF runs starting from the snapshot 2015-11-26 18:00 UTC, 2015-11-27 00:00 UTC, and 2015-11-27 06:00 UTC.
Paper: Dark-flight Estimates of Meteorite Fall Positions: Issues and a Case Study Using the Murrili Meteorite Fall
Authors: M. C. Towner, T. Jansen-Sturgeon, M. Cupak, E. K. Sansom, H. A. R. Devillepoix, P. A. Bland, R. M. Howie, J. P. Paxman, G. K. Benedix, B. A. D. Hartig
Figure caption: Fall line predictions from the Murrili bright-flight endpoint, assuming a chondritic sphere and brick, using the wind model 06:00 snapshot as described in the following section. The actual recovered fall position is marked with a black triangle.
Paper: Dark-flight Estimates of Meteorite Fall Positions: Issues and a Case Study Using the Murrili Meteorite Fall
Authors: M. C. Towner, T. Jansen-Sturgeon, M. Cupak, E. K. Sansom, H. A. R. Devillepoix, P. A. Bland, R. M. Howie, J. P. Paxman, G. K. Benedix, B. A. D. Hartig
Figure caption: Top: Monte Carlo results of 1.5–2.3 kg chondritic meteorite, 1000 runs, allowing initial shape to vary from sphere to rounded brick. Bottom: same as the top panel, but with wind variation of 5% allowed in direction and magnitude of the 00:00 snapshot-based wind profile provided by WRF. The simulations also allow variation in the initial vector from the end of bright-flight triangulation, using the uncertainties in Table 2.
Paper: Dark-flight Estimates of Meteorite Fall Positions: Issues and a Case Study Using the Murrili Meteorite Fall
Authors: M. C. Towner, T. Jansen-Sturgeon, M. Cupak, E. K. Sansom, H. A. R. Devillepoix, P. A. Bland, R. M. Howie, J. P. Paxman, G. K. Benedix, B. A. D. Hartig
Figure caption: Flow schematic of dark-flight modeling.
Paper: Dark-flight Estimates of Meteorite Fall Positions: Issues and a Case Study Using the Murrili Meteorite Fall
Authors: M. C. Towner, T. Jansen-Sturgeon, M. Cupak, E. K. Sansom, H. A. R. Devillepoix, P. A. Bland, R. M. Howie, J. P. Paxman, G. K. Benedix, B. A. D. Hartig
Figure caption: Modeled trajectories of chondritic spheres for different masses in longitude and latitude, showing the influence of winds and atmosphere during descent, from Murrili bright-flight endpoint.
Paper: Dark-flight Estimates of Meteorite Fall Positions: Issues and a Case Study Using the Murrili Meteorite Fall
Authors: M. C. Towner, T. Jansen-Sturgeon, M. Cupak, E. K. Sansom, H. A. R. Devillepoix, P. A. Bland, R. M. Howie, J. P. Paxman, G. K. Benedix, B. A. D. Hartig
Figure caption: Variation in fall line predictions for chondritic spheres due to variations in WRF wind model data, with the model snapshot shown in the legend. Numbers along the line indicate the mass on the ground. Some numbers are omitted for clarity on some lines, but the points shown correspond to matching mass markers on the lowermost curve. The final recovered meteorite fall position (1.68 kg) is also shown with a filled triangle.
Paper: Dark-flight Estimates of Meteorite Fall Positions: Issues and a Case Study Using the Murrili Meteorite Fall
Authors: M. C. Towner, T. Jansen-Sturgeon, M. Cupak, E. K. Sansom, H. A. R. Devillepoix, P. A. Bland, R. M. Howie, J. P. Paxman, G. K. Benedix, B. A. D. Hartig
Figure caption: Modeled Murrili fall speed, and drag coefficient as a function of altitude.
Paper: Neptune’s Moon Triton: Continuing Surface Seasonal Volatile Transport
Authors: Michael D. Hicks, Bonnie J. Buratti, David Dombroski
Figure caption: Adapted from Figure 10 in Buratti et al. (2011), showing the evolution of Triton’s peak-to-peak light-curve amplitude as a function of time, with the model extended into future epochs. All light curves were obtained in the V band or its equivalent, with the exception of the 1987 data point, which was obtained at 0.89 μm and is an upper limit only (Lark et al. 1989). Because the amplitude of Triton’s light curve is smaller at this wavelength (Buratti et al. 2011), it is expected to fall below the static frost model. The solid line represents a light-curve amplitude model (Hillier at al. 1991) which assumes a static albedo distribution on Triton’s surface as measured by Voyager 2. The light-curve amplitude in 2004 and 2017 shows measurements of the peak-to-peak amplitude and suggests that the frost distribution on Triton is changing with time. The Voyager 2 data point from 1989 was obtained at an average subspacecraft latitude of approximately −50°, which corresponds to the latitude on Triton as observed from Earth in 1999. Thus, the amplitude is even more accurately aligned with the model than is illustrated here.
Paper: Neptune’s Moon Triton: Continuing Surface Seasonal Volatile Transport
Authors: Michael D. Hicks, Bonnie J. Buratti, David Dombroski
Figure caption: A. Light curves of Triton through time, along with third-order polynomial fits, with the results from this paper on top. TMO is Table Mountain Observatory and MKO is Maunakea Observatory. The ground-based data were obtained in the V filter (0.55μ), while the Voyager 2 measurements were obtained in the green filter (0.56 μm); see Hillier et al. (1991) and Buratti et al. (2011). The light-curve amplitude between 1989 and 2010 shows a substantial increase, even when corrections are made for the viewing geometry (Buratti et al. 2011). B. The existing maps of Triton (with the Voyager 2 map on the bottom and the HST map on top) show substantial volatile transport (Bauer et al. 2010). The increases in albedo as indicated by our 2017 TMO light curve correspond to the increases at the same longitude in the HST map; we observe an additional increase at ∼0°.
Paper: Neptune’s Moon Triton: Continuing Surface Seasonal Volatile Transport
Authors: Michael D. Hicks, Bonnie J. Buratti, David Dombroski
Figure caption: The rotational light curve of Triton in the BVR filters in 2017. The data show observations from five observing runs (run C failed to yield any measurements due to weather and equipment issues). The data have been corrected to opposition using a phase coefficient of 0.015 mags/degree, as discussed in the text. The formal errors from the IRAF routines we used are reflected in the plotted symbols: they are about the size of the data points. These errors do not incorporate factors such as imperfect subtraction of scattered light from Neptune and nonphotometric conditions for which even on-chip standard stars could not correct. The more realistic error in this data is represented by the scatter in the data on each night. The dotted lines are the Fourier fits from Table 2.(The data used to create this figure are available.)
Paper: Neptune’s Moon Triton: Continuing Surface Seasonal Volatile Transport
Authors: Michael D. Hicks, Bonnie J. Buratti, David Dombroski
Figure caption: The V-band geometric albedo of Triton through time. The values are listed in Table 4. The dotted line is the subobserver latitude. The lower albedos correspond to Triton’s short-term reddening events, which are most likely lower because Triton’s reddish terrain is lower in albedo than the rest of the moon (McEwen 1990).
Paper: Neptune’s Moon Triton: Continuing Surface Seasonal Volatile Transport
Authors: Michael D. Hicks, Bonnie J. Buratti, David Dombroski
Figure caption: Removing Neptune’s scattered light in the images. As discussed in the text, ring-masking decomposes the flat-fielded image (A) into a radially antisymmetric (B) and a radially symmetric (C) image centered about Neptune. This method allows a more accurate determination of the sky level and flux values for each Triton frame.
Paper: Neptune’s Moon Triton: Continuing Surface Seasonal Volatile Transport
Authors: Michael D. Hicks, Bonnie J. Buratti, David Dombroski
Figure caption: Efficiency of ring-masking in removing scattered light from Neptune. Plotted are radial profiles centered about Triton both before (filled circle) and after (empty circle) ring-masking has been applied to the image. Also shown are typical object and sky apertures used in the analysis.
Paper: Neptune’s Moon Triton: Continuing Surface Seasonal Volatile Transport
Authors: Michael D. Hicks, Bonnie J. Buratti, David Dombroski
Figure caption: The published colors of Triton through time, which are listed in Table 5. These data do not have a temporal range as extensive as the albedo measurements.
Paper: Dark-flight Estimates of Meteorite Fall Positions: Issues and a Case Study Using the Murrili Meteorite Fall
Authors: M. C. Towner, T. Jansen-Sturgeon, M. Cupak, E. K. Sansom, H. A. R. Devillepoix, P. A. Bland, R. M. Howie, J. P. Paxman, G. K. Benedix, B. A. D. Hartig
Figure caption: Monte Carlo simulations of Murrili (fixed at 1.68 kg, 3500 kg m−3) falling at different orientations. Top: the scatter for falling in a high-drag orientation (horizontal orientation in Figure 9); bottom: in a low-drag orientation (vertical in Figure 9), as indicated by fall direction arrows in Figure 9. Percent line is described in the text.
Paper: Dark-flight Estimates of Meteorite Fall Positions: Issues and a Case Study Using the Murrili Meteorite Fall
Authors: M. C. Towner, T. Jansen-Sturgeon, M. Cupak, E. K. Sansom, H. A. R. Devillepoix, P. A. Bland, R. M. Howie, J. P. Paxman, G. K. Benedix, B. A. D. Hartig
Figure caption: Murrili meteorite dimensions and shape. In both images, the black scale bar is 50 mm. Compared to a sphere, the rock is flattened and heart shaped, but almost teardrop from the side view. An STL file representing this shape is available as data-behind-the-figure.(The data used to create this figure are available.)
Paper: An Open-source Bayesian Atmospheric Radiative Transfer (BART) Code. I. Design, Tests, and Application to Exoplanet HD 189733b
Authors: Joseph Harrington, Michael D. Himes, Patricio E. Cubillos, Jasmina Blecic, Patricio M. Rojo, Ryan C. Challener, Nate B. Lust, M. Oliver Bowman, Sarah D. Blumenthal, Ian Dobbs-Dixon, Andrew S. D. Foster, Austin J. Foster, M. R. Green, Thomas J. Loredo, Kathleen J. McIntyre, Madison M. Stemm, David C. Wright
Figure caption: Comparison of best-fit retrieved log abundances for HD 189733b: BART's retrieved 68% credible region, TAU-REX's Stage 1 result, CHIMERA's best fit and 68% interval, the best fit and possible fit range reported by Lee et al. (2012), and the range of values reported by Line et al. (2012), Madhusudhan & Seager (2009), and Swain et al. (2009).
Paper: An Open-source Bayesian Atmospheric Radiative Transfer (BART) Code. I. Design, Tests, and Application to Exoplanet HD 189733b
Authors: Joseph Harrington, Michael D. Himes, Patricio E. Cubillos, Jasmina Blecic, Patricio M. Rojo, Ryan C. Challener, Nate B. Lust, M. Oliver Bowman, Sarah D. Blumenthal, Ian Dobbs-Dixon, Andrew S. D. Foster, Austin J. Foster, M. R. Green, Thomas J. Loredo, Kathleen J. McIntyre, Madison M. Stemm, David C. Wright
Figure caption: Retrieval results for HD 189733b (r01hd189733b test). Top left: T(p) profiles explored by the MCMC (see Figure 8). Top right: Normalized contribution functions of filters (see Figure 8). Middle left: Best-fit spectrum. Middle right: Pairwise correlations (marginalized over posterior) for all model parameters. Values are in base-10 logarithm, except for α and β. Bottom: trace plots of explored model parameters. The 10 chains are concatenated.
Paper: An Open-source Bayesian Atmospheric Radiative Transfer (BART) Code. I. Design, Tests, and Application to Exoplanet HD 189733b
Authors: Joseph Harrington, Michael D. Himes, Patricio E. Cubillos, Jasmina Blecic, Patricio M. Rojo, Ryan C. Challener, Nate B. Lust, M. Oliver Bowman, Sarah D. Blumenthal, Ian Dobbs-Dixon, Andrew S. D. Foster, Austin J. Foster, M. R. Green, Thomas J. Loredo, Kathleen J. McIntyre, Madison M. Stemm, David C. Wright
Figure caption: Retrieved 1D marginalized posterior distributions for each molecule considered in the synthetic retrieval. The forward model was computed using a 0.1 cm−1 grid, while the retrieval models were computed using 0.1 (top left), 0.25 (top right), 0.5 (bottom left), and 1.0 (bottom right) cm−1 grids. Note that only the 0.1 cm−1 grid correctly retrieves the underlying parameters within 1σ; as the gridding becomes coarser, the accuracy decreases, with the 1.0 cm−1 gridding entirely missing four out of five of the parameters.