adsabs/AstroCLIMB huggingface dataset:
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: Example of the effect of wavenumber griddings when band integrating spectra. Left: 0.025, 0.1, 0.25, and 1.0 cm−1 griddings. Right: 0.025 and 0.1 cm−1 griddings from the left plot. All spectra are computed using identical setups except for the wavenumber gridding. The gridding of the spectra computed with a maximum wavelength of 11 μm is offset by ∼0.09 cm−1 compared to the spectra with a maximum wavelength of 10 μm. Note the model spread in the 2.5–3.5 μm and >4.5 μm regions of the left panel. By comparison, the right panel shows little spread in the band-integrated spectra.
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 retrieved posteriors for the three indicated Barstow et al. (2020) model 0 spectra at two different wavenumber-grid resolutions. While the retrieved temperatures and radii are generally unaffected, the molecular abundances are more sensitive to the grid resolution.
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 retrieved posteriors for HD 189733b at two different wavenumber-grid resolutions. In general, the posteriors match; only CO and CH4 show minor differences, though they are not significant enough to affect conclusions drawn from the posterior.
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: Summary of retrieval results for the s05hjcloudisoBarstowEtal test, which retrieve on the spectra of Barstow et al. (2020) Model 1 cases with 60 ppm uncertainties. Best-fit spectra (left column) and marginalized posteriors (right column) for the NEMESIS (top row), CHIMERA (middle row), and TAU-REX (bottom row) data sets.
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: Summary of retrieval results for the s04hjclearisoBarstowEtal test, which retrieve on the spectra of Barstow et al. (2020) Model 0 cases with 60 ppm uncertainties. Best-fit spectra (left column) and marginalized posteriors (right column) for the NEMESIS (top row), CHIMERA (middle row), and TAU-REX (bottom row) data sets.
Paper: Titan Stratospheric Haze Bands Observed in Cassini VIMS as Tracers of Meridional Circulation
Authors: N. W. Kutsop, A. G. Hayes, P. M. Corlies, S. Le Mouélic, J. I. Lunine, C. A. Nixon, P. Rannou, S. Rodriguez, M. T. Roman, C. Sotin, T. Tokano
Figure caption: The average latitude of the observed primary and secondary annuli. The black regions are all the locations in time that were at a viewing geometry shared by the majority (95%) of our detections of the annuli (incidence angle < ∼ 90° and emission < ∼ 60°). The red circle at ∼750 latitude and L  S  = ∼40° is a direct detection of the NPA in flyby T85.
Paper: Titan Stratospheric Haze Bands Observed in Cassini VIMS as Tracers of Meridional Circulation
Authors: N. W. Kutsop, A. G. Hayes, P. M. Corlies, S. Le Mouélic, J. I. Lunine, C. A. Nixon, P. Rannou, S. Rodriguez, M. T. Roman, C. Sotin, T. Tokano
Figure caption: Top: T061, 2009-08-25, L  S  = 0.°49; bottom: T096, 2013-12-01, LS  = 51.°2. (A) 494 nm mosaic with manifold correction. (B) 1155 nm mosaic with manifold correction. (C) ISS NAC observations taken during the same respective flyby. Both are taken with filters CL1 and CB3 with an effective wavelength of 938.03 nm (Knowles 2016). Image names are N1630071434_1 (top) and N1764434226_1 (bottom).
Paper: Titan Stratospheric Haze Bands Observed in Cassini VIMS as Tracers of Meridional Circulation
Authors: N. W. Kutsop, A. G. Hayes, P. M. Corlies, S. Le Mouélic, J. I. Lunine, C. A. Nixon, P. Rannou, S. Rodriguez, M. T. Roman, C. Sotin, T. Tokano
Figure caption: Transect of pixels from mosaic of T61 flyby [2009-08-25] (see Figure 2). The deviation in each of the three curves is attributed to the EQA. The inflection point of each deviation is attributed to the center of the annulus, and the Gaussian tail on either side of the inflection point is the uncertainty in locating the annulus. The north–south asymmetry appears as the smooth parabolic curve between the hemispheres. The EQA adds a sharp deviation in the curve, without which the north–south asymmetry would appear as a gradient between the hemispheres, rather than the asymmetry we see.
Paper: Titan Stratospheric Haze Bands Observed in Cassini VIMS as Tracers of Meridional Circulation
Authors: N. W. Kutsop, A. G. Hayes, P. M. Corlies, S. Le Mouélic, J. I. Lunine, C. A. Nixon, P. Rannou, S. Rodriguez, M. T. Roman, C. Sotin, T. Tokano
Figure caption: Orthographic mosaics of T096, 2013-12-01, L S = 51.°2. (A) 1155 nm mosaic. (B) 1155 nm mosaic with manifold correction. (C) Context using VIMS-ISS map (Seignovert et al. 2019).
Paper: The Possible Formation of Jupiter from Supersolar Gas
Authors: Artyom Aguichine, Olivier Mousis, Jonathan I. Lunine
Figure caption: Top panels: water enrichment profiles ﹩{f}_{{{\rm{H}}}_{2}{\rm{O}},\phi }(r,t)﹩ as a function of heliocentric distance at t = 100, 200, 300, and 400 kyr of the PSN evolution, with ϕ = solid (solid lines) or vapor (dashed lines). Bottom panels: carbon monoxide enrichment profiles f CO,ϕ (r, t) as a function of heliocentric distance at the same epochs of the PSN evolution, with ϕ = solid (solid lines) or vapor (dashed lines). The blue bar corresponds to the H2O abundance relative to the protosolar O abundance derived from Juno measurements at a 1σ level (Li et al. 2020). Each column corresponds to a different value of α.
Paper: The Possible Formation of Jupiter from Supersolar Gas
Authors: Artyom Aguichine, Olivier Mousis, Jonathan I. Lunine
Figure caption: Time evolution of the trace species enrichments at the heliocentric distance of 4 au. Top panels: species in solid+vapor phase f X,total(4au, t). Middle panels: species in vapor phase f X,vapor(4au, t). Bottom panels: species in solid phase f X,solid(4au, t). The blue and green bars correspond to the H2O and NH3 abundances relative to the protosolar O and N abundances, respectively, derived from Juno measurements at a 1σ level (Li et al. 2020), respectively. The shaded bar corresponds to the range covered by S, C, P, Ar, Kr, and Xe enrichments derived from spacecraft measurements (Atreya et al. 2003; Mousis et al. 2018). Each column corresponds to a different value of α.
Paper: The Possible Formation of Jupiter from Supersolar Gas
Authors: Artyom Aguichine, Olivier Mousis, Jonathan I. Lunine
Figure caption: Same as Figure 3, but for elemental enrichments. When an element is assumed to be present in only one species (e.g., P in PH3, or noble gases), the enrichments are identical to those of Figure 3. As C, N, and O are distributed among several molecules, their enrichments exhibit several peaks. For example, when α ≤ 10−3, enrichment peaks of N in vapor+solid and vapor phases (top and middle rows) are due to NH3 at 150 kyr, and N2 at ∼1 Myr. When α ≥ 5 × 10−3, the iceline of CO2 moves below 4 au after 100 kyr of PSN evolution, which results in a decrease of the C and O abundances in the vapor phase (middle row) and an increase in the C and O abundances in the solid phase (bottom row).
Paper: The Possible Formation of Jupiter from Supersolar Gas
Authors: Artyom Aguichine, Olivier Mousis, Jonathan I. Lunine
Figure caption: Positions of the icelines during the PSN evolution, assuming α = 10−3. The relative positions of the icelines is not affected by the variation of the α value.
Paper: Titan Stratospheric Haze Bands Observed in Cassini VIMS as Tracers of Meridional Circulation
Authors: N. W. Kutsop, A. G. Hayes, P. M. Corlies, S. Le Mouélic, J. I. Lunine, C. A. Nixon, P. Rannou, S. Rodriguez, M. T. Roman, C. Sotin, T. Tokano
Figure caption: The R.A. and the decl. offset of the normal vector of the annuli from the solid-body rotation axis. Diamonds are data from the EQA, and circles are data from the NPA. The colors correspond to the time of observation.
Paper: Titan Stratospheric Haze Bands Observed in Cassini VIMS as Tracers of Meridional Circulation
Authors: N. W. Kutsop, A. G. Hayes, P. M. Corlies, S. Le Mouélic, J. I. Lunine, C. A. Nixon, P. Rannou, S. Rodriguez, M. T. Roman, C. Sotin, T. Tokano
Figure caption: Schematic showing the VIMS destriping routine described in Appendix A.
Paper: Titan Stratospheric Haze Bands Observed in Cassini VIMS as Tracers of Meridional Circulation
Authors: N. W. Kutsop, A. G. Hayes, P. M. Corlies, S. Le Mouélic, J. I. Lunine, C. A. Nixon, P. Rannou, S. Rodriguez, M. T. Roman, C. Sotin, T. Tokano
Figure caption: Zoom-in of the modeled atmospheric spectra and the modeled annulus spectra from Figure 3. The difference between the two spectra is less than the line width at certain wavelengths.
Paper: Statistical Significance of Mission Parameters on the Deflection Efficiency of Kinetic Impacts: Applications for the Next-generation Kinetic Impactor
Authors: Mallory E. DeCoster, Emma S.G. Rainey, Thomas W. Rosch, Angela M. Stickle
Figure caption: Experimental results replotted from Ikeda et al. (2017). Lines represent a linear fit to the data points to show approximate trends. In total, Ikeda et al. showed that the impactor geometry does not affect the ejecta mass but does affect  β because impactors that promote large ejecta emission angles (α) result in a smaller β. The inset shows the crater formed in an exemplar CTH simulation and corresponding α.
Paper: Statistical Significance of Mission Parameters on the Deflection Efficiency of Kinetic Impacts: Applications for the Next-generation Kinetic Impactor
Authors: Mallory E. DeCoster, Emma S.G. Rainey, Thomas W. Rosch, Angela M. Stickle
Figure caption: Comparison of actual (black dots) vs. predicted (red line) values from the fit model for the ejecta mass (left) and momentum (right) constructed using the JMP statistical software. The red shaded area shows the 5%–95% confidence interval on the fit to the model. The fit model includes the following terms: impactor mass, impact velocity, impactor shape, target strength, and impactor composition. The black dots are the transformed ejecta mass values. The blue line represents the mean value of the y-axis points. Prior to fitting the distribution for crater depth and width, the values were transformed using a Box–Cox transformation with λ = −0.055 for the ejecta mass and λ = 0.041 for the ejecta momentum to make the values more normally distributed.
Paper: Statistical Significance of Mission Parameters on the Deflection Efficiency of Kinetic Impacts: Applications for the Next-generation Kinetic Impactor
Authors: Mallory E. DeCoster, Emma S.G. Rainey, Thomas W. Rosch, Angela M. Stickle
Figure caption: Comparison of actual (black dots) vs. predicted (red line) values from the fit model for crater depth (left) and width (right) using the JMP statistical software. The red shaded area shows the 5%–95% confidence interval on the fit to the model. The fit model includes the following terms: impactor mass, impact velocity, impactor shape, target strength, and impactor composition. The blue line represents the mean value of the y-axis points. Prior to fitting the distribution for crater depth and width, the CTH-derived values were transformed using a Box–Cox transformation with λ = 0.08 (left; depth) and λ = −0.101 (right; width) to make the values more normally distributed. The black dots are the transformed crater size values.
Paper: Statistical Significance of Mission Parameters on the Deflection Efficiency of Kinetic Impacts: Applications for the Next-generation Kinetic Impactor
Authors: Mallory E. DeCoster, Emma S.G. Rainey, Thomas W. Rosch, Angela M. Stickle
Figure caption: Comparison of actual (black dots) vs. predicted (red line) values from the fit model for momentum enhancement,  β, constructed using the JMP statistical software. The red shaded area shows the 5%–95% confidence interval on the fit to the model. The fit model includes the following terms: impactor mass, impact velocity, impactor shape, target strength, and impactor composition. The black dots are the transformed  β values. The blue line represents the mean value of the y-axis points. Prior to fitting the distribution for crater depth and width, the values for  β were transformed using a Box–Cox transformation with λ = −2 to make the values more normally distributed.
Paper: NEOWISE Observations of the Potentially Hazardous Asteroid (99942) Apophis
Authors: Akash Satpathy, Amy Mainzer, Joseph R. Masiero, Tyler Linder, Roc M. Cutri, Edward L. Wright, Jana Pittichová, Tommy Grav, Emily Kramer
Figure caption: Plots highlighting the TPM results with (99942) Apophis modeled as a triaxial ellipsoid. Clockwise from top left: average flux density during the two epochs along with the span of the bandpasses (the average flux was 95.37 μJy in W1 and 385.73 μJy in W2 during the first epoch and 621.31 μJy in W1 and 3496.75 μJy in W2 during the second epoch), histogram of the diameter results with the 68% (dashed lines) and 95% (dotted lines) confidence interval ranges, histogram of the thermal inertia results with the 68% (dashed lines) confidence interval range (the 95% confidence interval values lie outside the x-axis range), and histogram of the visual albedo results with the 68% (dashed lines) and 95% (dotted lines) confidence interval ranges. The fainter histograms in the top right, bottom left, and bottom right panels show the distribution without the LCDB pole solution constraint.
Paper: NEOWISE Observations of the Potentially Hazardous Asteroid (99942) Apophis
Authors: Akash Satpathy, Amy Mainzer, Joseph R. Masiero, Tyler Linder, Roc M. Cutri, Edward L. Wright, Jana Pittichová, Tommy Grav, Emily Kramer
Figure caption: Plots highlighting the TPM results with (99942) Apophis modeled as a sphere. Clockwise from top left: average flux density during the two epochs along with the span of the bandpasses (the average flux was 95.77 μJy in W1 and 381.13 μJy in W2 during the first epoch and 622.88 μJy in W1 and 3475.26 μJy in W2 during the second epoch), histogram of the diameter results with the 68% (dashed lines) and 95% (dotted lines) confidence interval ranges, histogram of the thermal inertia results with the 68% (dashed lines) confidence interval range (the 95% confidence interval values lie outside the x-axis range), and histogram of the visual albedo results with the 68% (dashed lines) and 95% (dotted lines) confidence interval ranges. The fainter histograms in the top right, bottom left, and bottom right panels signify the solutions without the LCDB pole solution constraint.
Paper: NEOWISE Observations of the Potentially Hazardous Asteroid (99942) Apophis
Authors: Akash Satpathy, Amy Mainzer, Joseph R. Masiero, Tyler Linder, Roc M. Cutri, Edward L. Wright, Jana Pittichová, Tommy Grav, Emily Kramer
Figure caption: Light curves from the first and second observing epochs (left and right, respectively). The W1-band data from the first epoch were omitted due to marginal detections. The large amplitude in the light curves suggests that the object has an elongated shape, as previously shown by Brozovic et al. (2018).
Paper: NEOWISE Observations of the Potentially Hazardous Asteroid (99942) Apophis
Authors: Akash Satpathy, Amy Mainzer, Joseph R. Masiero, Tyler Linder, Roc M. Cutri, Edward L. Wright, Jana Pittichová, Tommy Grav, Emily Kramer
Figure caption: The CTIO observations in B, V, r, and g, taken at nearly the same time as NEOWISE’s first epoch of observations.
Paper: NEOWISE Observations of the Potentially Hazardous Asteroid (99942) Apophis
Authors: Akash Satpathy, Amy Mainzer, Joseph R. Masiero, Tyler Linder, Roc M. Cutri, Edward L. Wright, Jana Pittichová, Tommy Grav, Emily Kramer
Figure caption: Spin pole position solution with an emissivity of 0.9 as constrained by the triaxial TPM plotted in celestial coordinates. The peak pole position was found at an R.A. of 50.°6 and a decl. of 0°. The color bar denotes the number of solutions in the bin.
Paper: Titan Stratospheric Haze Bands Observed in Cassini VIMS as Tracers of Meridional Circulation
Authors: N. W. Kutsop, A. G. Hayes, P. M. Corlies, S. Le Mouélic, J. I. Lunine, C. A. Nixon, P. Rannou, S. Rodriguez, M. T. Roman, C. Sotin, T. Tokano
Figure caption: The averaged differential spectra of the NPA (blue) and the EQA (orange) from L  S  = 55° to 65° and from L  S  = 345° to 15°, respectively. The purple line indicates the average median altitude of Model A and Model B from our triangulation efforts of the NPA (Section 2.4). The green curves show the modeled altitudes where the atmosphere is opaque when averaged over the different terms of the k-correlated description. Solid green curve: the altitudes where the average column opacity is equal to 1. Dashed green curve: the average altitude where the column opacity is 1. Yellow, gold, and brown are the 50th, 85th, and 98th percentile values of the difference between neighboring pixels across all flybys, respectively. Features in the differential spectra are significant if they are outside these bounds. The gray area shows the range of expected minimum altitudes based on the detection at ∼1.2 μm with > P 98% and the detection at ∼2.3 μm with ≈P 85%.
Paper: Titan Stratospheric Haze Bands Observed in Cassini VIMS as Tracers of Meridional Circulation
Authors: N. W. Kutsop, A. G. Hayes, P. M. Corlies, S. Le Mouélic, J. I. Lunine, C. A. Nixon, P. Rannou, S. Rodriguez, M. T. Roman, C. Sotin, T. Tokano
Figure caption: The colored solid lines in each figure are spline fits to the corresponding data with an R 2 ≈ 0.95. These curves are nonphysical and are intended to facilitate comprehension. The three vertical gray bars in each figure are located at 498, 894, and 1155 nm. These are the wavelengths used for our transects and mosaics. (A) The EQA differential spectra taken from three time periods of equal length centered about L  S  = 15° (the peak of the blue sinusoid in Figure 10(A)); blue is from flybys T028–T061, green from T061–T082, and red from T082–T105. (B) The NPA differential spectra taken from three time periods of equal length spanning the range of observable flybys; blue is from T088–T095, green from T098–T108, and red from T119–nT262. (C) Differential spectra produced by creating a modeled spectra where the haze abundance at a range of altitudes is increased by 10% and then subtracting a modeled spectrum with typical haze abundance.
Paper: Titan Stratospheric Haze Bands Observed in Cassini VIMS as Tracers of Meridional Circulation
Authors: N. W. Kutsop, A. G. Hayes, P. M. Corlies, S. Le Mouélic, J. I. Lunine, C. A. Nixon, P. Rannou, S. Rodriguez, M. T. Roman, C. Sotin, T. Tokano
Figure caption: Top: western azimuthal offset of the normal vector of the annulus from the subsolar vector. The yellow squares are taken from Roman et al. (2009), Table 1, Column (6). The black crosses are taken from Tokano (2010), Figure 6(b). Bottom: magnitude of the polar offset of the normal vector of the annulus from the solid-body rotation axis (north pole). The red line is taken from Tokano (2010), Figure 5(a).
Paper: Titan Stratospheric Haze Bands Observed in Cassini VIMS as Tracers of Meridional Circulation
Authors: N. W. Kutsop, A. G. Hayes, P. M. Corlies, S. Le Mouélic, J. I. Lunine, C. A. Nixon, P. Rannou, S. Rodriguez, M. T. Roman, C. Sotin, T. Tokano
Figure caption: (A) Blue: maximum value of ΔI/F of the EQA differential spectrum. Orange: minimum value of ΔI/F of the EQA differential spectrum. Green: maximum value of ΔI/F of the NPA differential spectrum. Purple: minimum value of ΔI/F of the NPA differential spectrum. (B) Blue: the wavelength of the maximum ΔI/F of the EQA differential spectrum. Orange: the wavelength of the minimum ΔI/F of the EQA differential spectrum. Green: the wavelength of the maximum ΔI/F of the NPA differential spectrum. Purple: the wavelength of the minimum ΔI/F of the NPA differential spectrum. The opacity of the data points correlates to the relative weight of the data. Data are weighted according to the number of transect detections. For details on the curves, see Table 2.
Paper: Titan Stratospheric Haze Bands Observed in Cassini VIMS as Tracers of Meridional Circulation
Authors: N. W. Kutsop, A. G. Hayes, P. M. Corlies, S. Le Mouélic, J. I. Lunine, C. A. Nixon, P. Rannou, S. Rodriguez, M. T. Roman, C. Sotin, T. Tokano
Figure caption: Top: the R.A. offset of the normal vector of the annuli from the solid-body rotation axis in an inertial reference frame (ICRF). The R.A. of Titan's solid-body rotation axis is R. A. = 39.°48 (Stiles et al. 2008). The green sinusoid through the flyby has a goodness-of-fit metric of R 2 = 0.411. Bottom: the decl. offset of the normal vector of the annuli from the solid-body rotation axis in an inertial reference frame (ICRF). The decl. of Titan's solid-body rotation axis is R.A. = 83.°43 (Stiles et al. 2008).
Paper: Titan Stratospheric Haze Bands Observed in Cassini VIMS as Tracers of Meridional Circulation
Authors: N. W. Kutsop, A. G. Hayes, P. M. Corlies, S. Le Mouélic, J. I. Lunine, C. A. Nixon, P. Rannou, S. Rodriguez, M. T. Roman, C. Sotin, T. Tokano
Figure caption: Averaged differential spectrum of the EQA from L  S  = 345° to 15° (flybys T044–T072). The differential spectra shown with the cyan curve are produced from the difference between model spectra with typical haze abundance and model spectra where the haze abundance is increased at 100–130 km by 10%.
Paper: Titan Stratospheric Haze Bands Observed in Cassini VIMS as Tracers of Meridional Circulation
Authors: N. W. Kutsop, A. G. Hayes, P. M. Corlies, S. Le Mouélic, J. I. Lunine, C. A. Nixon, P. Rannou, S. Rodriguez, M. T. Roman, C. Sotin, T. Tokano
Figure caption: T095, 2013-10-14, L  S = 49.°7. (A) Our triangulated model of the NPA (orange) and the contemporaneous VIMS observation (black and white) projected onto Titan as seen from the side. (B) The projection of the modeled annulus onto Titan (orange) fitting our observation of the annulus (blue) in Lat–Lon space.