adsabs/AstroCLIMB huggingface dataset:
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: Both panels show the results of the χ 2 minimization routine to determine the change in parameters of the NPA. Model A was constructed using flybys T094–T098, and Model B was constructed with flybys T101–T105. (A) Semimajor axis of the NPA as a function of L  S . The curves are Gaussian fits, with (B) median altitude of the NPA vs. L  S . The change in altitude is a product of the change in semimajor axis.
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) Latitudinal transect of the mosaic for the T100 flyby [2014-04-07, L  S  = 55.°17]. One primary (the NPA) and two secondaries are shown. The nomenclature is consistent with Figure 7. The annuli are highlighted at 1155 nm, where a deviation in the otherwise smooth curve is found. Similar convex deviations are found in the 894 nm transect, and concave deviations are found in the 498 nm transect. (B) 1155 nm mosaic with manifold correction. The colored lines identify the annuli and are consistent with panel (A). (C) Context using VIMS-ISS map (Seignovert et al. 2019).
Paper: Benzene Vapor Pressures at Titan Temperatures: First Microbalance Results
Authors: Reggie L. Hudson, Yukiko Y. Yarnall, Perry A. Gerakines
Figure caption: Vapor pressures of crystalline benzene in this work compared to literature results. The temperatures for the points (red squares) for the present work are the same as those used by Dubois et al. (2021).
Paper: Benzene Vapor Pressures at Titan Temperatures: First Microbalance Results
Authors: Reggie L. Hudson, Yukiko Y. Yarnall, Perry A. Gerakines
Figure caption: Vapor pressures of crystalline benzene.
Paper: Benzene Vapor Pressures at Titan Temperatures: First Microbalance Results
Authors: Reggie L. Hudson, Yukiko Y. Yarnall, Perry A. Gerakines
Figure caption: Vapor pressures of crystalline cyclohexane. The dashed and solid lines are extrapolations from ∼220 K using the equations of Ha et al. (1976) and Jackowski (1974), respectively. The five points (red squares) are from our lab measurements.
Paper: Benzene Vapor Pressures at Titan Temperatures: First Microbalance Results
Authors: Reggie L. Hudson, Yukiko Y. Yarnall, Perry A. Gerakines
Figure caption: Vapor pressures of crystalline H2O ice. The temperatures for the points (red squares) of the present work are the same as those used by Bryson et al. (1974).
Paper: Benzene Vapor Pressures at Titan Temperatures: First Microbalance Results
Authors: Reggie L. Hudson, Yukiko Y. Yarnall, Perry A. Gerakines
Figure caption: The data of Figure 3, but with the temperatures used to plot the points of Dubois et al. (2021) increased by 8 K. See the text for details.
Paper: Benzene Vapor Pressures at Titan Temperatures: First Microbalance Results
Authors: Reggie L. Hudson, Yukiko Y. Yarnall, Perry A. Gerakines
Figure caption: The low-temperature benzene data of this work (from Figure 3), the higher-temperature data reported by Růžička et al. (2014), and a curve fit of the combined data using the Cox equation. See the text for details.
Paper: Variability in Titan’s Mesospheric HCN and Temperature Structure as Observed by ALMA
Authors: Alexander E. Thelen, Conor A. Nixon, Richard G. Cosentino, Martin A. Cordiner, Nicholas A. Teanby, Claire E. Newman, Patrick G. J. Irwin, Steven B. Charnley
Figure caption: Plots of normalized functional derivatives calculated by NEMESIS for HCN (J = 4−3) spectra as a function of frequency and altitude with respect to HCN VMR (left column) and temperature (right column) in nadir and limb viewing geometries (top and bottom row, respectively). Contours increase with relative contribution.
Paper: Variability in Titan’s Mesospheric HCN and Temperature Structure as Observed by ALMA
Authors: Alexander E. Thelen, Conor A. Nixon, Richard G. Cosentino, Martin A. Cordiner, Nicholas A. Teanby, Claire E. Newman, Patrick G. J. Irwin, Steven B. Charnley
Figure caption: A priori vertical profiles used for radiative transfer modeling. (Left) Temperature a priori profiles from Thelen et al. (2018, 2019a) retrieved from ALMA CO spectra (100–550 km) and Cassini Radio Science data (<100 km) in 2012 (blue), 2014 (cyan), 2015 (green), and 2017 (purple). (Right) HCN VMR profiles retrieved from ALMA H13CN and HC15N spectra in 2012, 2014, and 2015 from Thelen et al. (2019b). A simple vertical gradient (black) was used to test the sensitivity of retrievals to vertical structure.
Paper: Variability in Titan’s Mesospheric HCN and Temperature Structure as Observed by ALMA
Authors: Alexander E. Thelen, Conor A. Nixon, Richard G. Cosentino, Martin A. Cordiner, Nicholas A. Teanby, Claire E. Newman, Patrick G. J. Irwin, Steven B. Charnley
Figure caption: Titan HCN (J = 4−3) nadir spectra from ALMA observations in 2012 (blue), 2014 (cyan), 2015 (green), 2016 (red), and 2017 (purple). Spectra are vertically offset above or below the 2014 spectrum by subsequent multiples of 2 nW cm−2 sr−1/cm−1 for clarity and plotted in radiance units to account for the change in beam size between observations. The inset shows comparisons of absorption in the HCN line core, which sounds Titan’s mesopause, and the spectra have been shifted to compare absorption depths.
Paper: Variability in Titan’s Mesospheric HCN and Temperature Structure as Observed by ALMA
Authors: Alexander E. Thelen, Conor A. Nixon, Richard G. Cosentino, Martin A. Cordiner, Nicholas A. Teanby, Claire E. Newman, Patrick G. J. Irwin, Steven B. Charnley
Figure caption: Comparison of retrieved temperature profiles from 2015 after using perturbations of the a priori temperature and HCN profiles shown in Figure 2 to illustrate the stability of the retrieved mesopause and lower mesospheric inversion near 400 km (∼0.01 mbar). The best-fit vertical profile is shown in green.
Paper: Variability in Titan’s Mesospheric HCN and Temperature Structure as Observed by ALMA
Authors: Alexander E. Thelen, Conor A. Nixon, Richard G. Cosentino, Martin A. Cordiner, Nicholas A. Teanby, Claire E. Newman, Patrick G. J. Irwin, Steven B. Charnley
Figure caption: Weighting function distribution for nadir and limb viewing geometries for the 2017 observation. Beam locations were placed such that the top-of-atmosphere latitudes matched for both locations for each observation, taking into account Titan’s tilt. Weighting distributions are not coadded, as plotted, but calculated individually for each extraction region. Titan’s solid body radius (2575 km; dashed circle), top of atmosphere (1200 km above the surface; solid circle), and top-of-atmosphere latitudes are shown. The FWHM of the ALMA beam is denoted by the dashed ellipses.
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: Cratering efficiency (total ejecta mass (M) normalized by the impactor mass (m)) as a function of (a) the normalized crater volume (crater volume/impactor volume) and (b) the normalized density (density of the impactor/density of the target) for 1 g (stars) and 500 kg (squares) impactors. The open symbols identify impactors with impact velocities of 5 km s−1, and the filled symbols indicate impactors with impact velocities of 500 m s−1. The target cohesion strength varies from strong (dark green), to medium (blue), to weak (bright green). Note that two separate results for case 15 are plotted; the dark green square labeled case 15 represents the total normalized ejecta mass with the traditional ejecta plane defined (1% of the target thickness), and the dark green square labeled case 15* represents the total normalized ejecta mass resulting with a larger ejecta plane defined (2% of the target thickness).
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: Distribution of cumulative normalized ejecta mass (ejecta mass (m)/impactor mass (M)) as a function of normalized ejecta velocity (ejecta velocity (v)/impact velocity (U)) into (a) strong, (b) medium, and (c) weak target material. The 1 g impactors are plotted with lines and symbols, and the 500 kg impactors are plotted as lines (no symbols). The mass–velocity distributions represent 1 ms post impact for the 1 g impactors and 10 ms post impact for the 500 kg impactors because those time intervals reflect the completion of transient crater excavation. Impactors with impact velocities of 500 m s−1 and 5 km s−1 take the form of segmented (dashed or dotted) and solid lines, respectively.
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: Crater profile for (panels (a), (c), and (e)) 1 g impactors at 1 ms post impact and (panels (b), (d), and (f)) 500 kg impactors at 10 ms post impact from similar impactor geometries (ogive or solid cone) but varying impact velocities. Note that the transient crater is fully formed 1 and 10 ms postimpact for the 1 g and 500 kg impactors, respectively. The target material is brown, and the impactor material is gray. The top dark green panels, middle blue panels, and bottom bright green panels illustrate craters resulting from strong, medium, and weak target material, respectively. The following cases and impact velocities are plotted: (a) case 10: ogive, 500 m s−1; (b) case 1: solid cone, 5 km s−1; (c) case 17: solid cone, 500 m s−1; (d) case 11: ogive, 5 km s−1; (e) case 5: ogive, 5 km s−1; and (f) case 16: solid cone, 500 m s−1.
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: Crater volume as a function of impactor volume for (a) 1 g and (b) 500 kg impactors. The open symbols identify impactors with impact velocities of 5 km s−1, and the filled symbols indicate impactors with impact velocities of 500 m s−1. The target cohesion strength ranges from strong (dark green), to medium (blue), and to weak (bright green).
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: Transient crater profiles at 10 ms post impact from 500 kg impactors of differing geometry with impact velocities of 5 km s−1 into (panels (a) and (c)) strong and (panels (b) and (c)) medium strength target material. The following cases are plotted: (a) case 1: Al cone with solid nose; (b) case 7: Cu plate (note the gray ejecta plume consisting of target material); (c) case 8: Al ring; (d) case 11: Cu ogive.
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: Schematic representation of the (top) 2D axisymmetric impactor structures and (bottom) 3D impactor structures investigated in this work. The limiting dimensions for each shape are labeled as r for the radius and h for the height. Refer to Table A1 for a full description of the impactor dimensions and resolutions for each test case. The asterisk indicates that the hollow nose is created by removing a sphere of material from the cone, resulting in the nose of the cone having variable thickness.
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: (a) Crater volume as a function of impactor volume. (b) β as a function of normalized ejecta mass. (c) Normalized ejecta mass vs. normalized crater volume. (d) Normalized ejecta mass vs. normalized impactor density for all 1 g impactors with 500 km s−1 impact velocities, where the tensile strength was kept constant at −100 MPa, compared to case 2 (Cu sphere) rerun into strong, medium, and weak targets, where the tensile strength was varied from 1 to 90 MPa.
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: Schematic representation of the transient crater and resulting ejecta within CTH (case 2). The ejecta plane is shown as a green dotted line and placed above the impact plane at a distance of 1% of the target thickness. The witness plates are shown as black dashed lines and monitor the ejecta material leaving the grid.
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: Momentum enhancement factor (β) as a function of the normalized ejecta mass (total ejecta mass (M)/impactor mass (m)). The stars represent 1 g impactors and the squares 500 kg impactors; filled and open symbols represent impact velocities of 500 m s−1 and 5 km s−1, respectively.
Paper: Optical Constants of a Titan Haze Analog from 0.4 to 3.5 μm Determined Using Vacuum Spectroscopy
Authors: Chao He, Sarah M. Hörst, Michael Radke, Marcella Yant
Figure caption: Optical constants of our Titan tholin sample (red) from 0.4 to 3.5 μm. Top: extinction coefficient (k). Bottom: refractive index (n) obtained from two independent methods (solid red line from Equation (6) and dotted red line from Equation (9)). Our optical constants are available as the data behind the figure. The optical constants of the Titan tholins in this wavelength range from previous studies are also plotted for comparison (colors and symbols are labeled at the top).(The data used to create this figure are available.)
Paper: Optical Constants of a Titan Haze Analog from 0.4 to 3.5 μm Determined Using Vacuum Spectroscopy
Authors: Chao He, Sarah M. Hörst, Michael Radke, Marcella Yant
Figure caption: Transmittance (top) and reflectance (bottom) spectra of our Titan tholin film sample in the visible and near-IR region (25,000 to 2850 cm−1, or 0.4 to 3.5 μm). The spectra in red (2850–9000 cm−1) were acquired with the DLaTGS detector and KBr beam splitter, the spectra in blue (8000–12,000 cm−1) with the DLaTGS detector and quartz beam splitter, and the spectra in purple (9000–25,000 cm−1) with the silicon diode detector and quartz beam splitter. The interference fringes are observed in the original spectra, and the spectra after removing the interference fringes are shown by the black dashed lines.
Paper: Optical Constants of a Titan Haze Analog from 0.4 to 3.5 μm Determined Using Vacuum Spectroscopy
Authors: Chao He, Sarah M. Hörst, Michael Radke, Marcella Yant
Figure caption: Transmittance (top) and reflectance (bottom) spectra of our Titan tholin film sample as a function of wavelength after removing the interference fringes. The reflectance from 0.4 to 0.7 μm is shown as a dashed line with a shaded gray area for the uncertainty due to the uncalibrated gold mirror.
Paper: Optical Constants of a Titan Haze Analog from 0.4 to 3.5 μm Determined Using Vacuum Spectroscopy
Authors: Chao He, Sarah M. Hörst, Michael Radke, Marcella Yant
Figure caption: Schematic of the experimental setup for tholin film sample production and FTIR measurement.
Paper: Optical Constants of a Titan Haze Analog from 0.4 to 3.5 μm Determined Using Vacuum Spectroscopy
Authors: Chao He, Sarah M. Hörst, Michael Radke, Marcella Yant
Figure caption: Extinction coefficients (k) retrieved from observational data (Lavvas et al. 2010; Rannou et al. 2010) and derived from laboratory-measured data (this study; Khare et al. 1984; Tran et al. 2003; Imanaka et al. 2012).
Paper: Mid-ultraviolet Hubble Observations of Europa and the Global Surface Distribution of SO2 
Authors: Tracy M. Becker, Samantha K. Trumbo, Philippa M. Molyneux, Kurt D. Retherford, Amanda R. Hendrix, Lorenz Roth, Ujjwal Raut, Juan Alday, Melissa A. McGrath
Figure caption: Mid-UV reflectance of Europa’s leading, trailing, sub-Jovian, and anti-Jovian hemispheres. We bin the 10 centermost STIS spatial pixels and average the reflectance from the two slit positions on each hemisphere, producing one spectrum near the apex of each hemisphere. The spectra are also smoothed by 20 data points. We use the SORCE/SOLSTICE to remove the solar signal for the mid-UV assessment. The dashed line represents a linear fit to the data. The narrower bumps in the spectra, including those near 280 nm, are due to the incomplete removal of solar features. The broad 280 nm feature of interest for this work, which spans 253–305 nm, is indicated by the light purple region. The very broad 230 nm feature observed only in the leading hemisphere spectra extends from ∼200 to 260 nm.
Paper: Mid-ultraviolet Hubble Observations of Europa and the Global Surface Distribution of SO2 
Authors: Tracy M. Becker, Samantha K. Trumbo, Philippa M. Molyneux, Kurt D. Retherford, Amanda R. Hendrix, Lorenz Roth, Ujjwal Raut, Juan Alday, Melissa A. McGrath
Figure caption: The central pixel from the sub-Jovian hemisphere shows an example of how the normalized spectrum appears when both the 280 and 230 nm features are present and overlapping. Pixels with this much overlap are flagged to indicate a likely overestimate of the band area of the 280 nm feature due to the additional absorption from the 230 nm feature. In these cases, we force the band depth measurement to occur at 279.4 nm to avoid being affected by the overlapping feature.
Paper: Mid-ultraviolet Hubble Observations of Europa and the Global Surface Distribution of SO2 
Authors: Tracy M. Becker, Samantha K. Trumbo, Philippa M. Molyneux, Kurt D. Retherford, Amanda R. Hendrix, Lorenz Roth, Ujjwal Raut, Juan Alday, Melissa A. McGrath
Figure caption: Normalized, continuum-removed spectra from the leading, trailing, sub-Jovian, and anti-Jovian hemispheres. We include one spectrum from pixels near the top, center, and bottom of the slit for each hemisphere; the approximate corresponding west longitude of those pixels is listed for reference. These example spectra show a clear variation in the strength of the 280 nm absorption feature in each hemisphere and the presence of the 230 nm feature on the leading hemisphere.
Paper: Mid-ultraviolet Hubble Observations of Europa and the Global Surface Distribution of SO2 
Authors: Tracy M. Becker, Samantha K. Trumbo, Philippa M. Molyneux, Kurt D. Retherford, Amanda R. Hendrix, Lorenz Roth, Ujjwal Raut, Juan Alday, Melissa A. McGrath
Figure caption: (Left) Linear fit (blue) to the spectral continuum of the trailing hemisphere of Europa. Regions used in the linear fit are marked in red. (Right) Trailing hemisphere spectrum with the continuum removed and a parabolic fit to the absorption feature centered at 279.4 nm.
Paper: Mid-ultraviolet Hubble Observations of Europa and the Global Surface Distribution of SO2 
Authors: Tracy M. Becker, Samantha K. Trumbo, Philippa M. Molyneux, Kurt D. Retherford, Amanda R. Hendrix, Lorenz Roth, Ujjwal Raut, Juan Alday, Melissa A. McGrath
Figure caption: (Top) Comparison of the modeled IR spectrum of pure water ice and the intraparticle model parameters used to reproduce the SO2 feature in the UV (Figure 8), offset for clarity. The inset shows the difference between the two models; the addition of the impurities changes the ice reflectance by only a few thousandths of a percentage point. (Bottom) A significant increase in SO2 concentration is required to alter the ice optical constants enough to introduce a detectable 4.07 μm feature. Therefore, the inclusion of small concentrations of SO2 is capable of producing the strong feature in the UV without creating a notable 4.07 μm SO2 feature, consistent with observations of Europa’s surface.
Paper: Mid-ultraviolet Hubble Observations of Europa and the Global Surface Distribution of SO2 
Authors: Tracy M. Becker, Samantha K. Trumbo, Philippa M. Molyneux, Kurt D. Retherford, Amanda R. Hendrix, Lorenz Roth, Ujjwal Raut, Juan Alday, Melissa A. McGrath
Figure caption: The SO2 band area as a function of the cosine of the angle from the apex of the trailing hemisphere. This reveals that the band area falls roughly as a cosine away from the apex (0°N, 270°W), similar to the pattern expected for sulfur plasma implantation (Pospieszalska & Johnson 1989). The spread in band strength reflects latitudinal and longitudinal variability away from a perfect cosine dependence that may reflect factors other than sulfur implantation or could be indicative of how ion energies or Europa’s position in the magnetic sheet may affect implantation and/or subsequent evolution of the species (Section 6.2).
Paper: Mid-ultraviolet Hubble Observations of Europa and the Global Surface Distribution of SO2 
Authors: Tracy M. Becker, Samantha K. Trumbo, Philippa M. Molyneux, Kurt D. Retherford, Amanda R. Hendrix, Lorenz Roth, Ujjwal Raut, Juan Alday, Melissa A. McGrath
Figure caption: Map of SO2 (a) band depth and (b) band area for all four HST visits. We leave off pixels with more than one corner off the limb of Europa and average the band strengths in regions of overlap. These plots are two representations of essentially the same information, the strength and overall area of the absorption feature, and therefore unsurprisingly agree qualitatively. In agreement with past results, we find that the SO2 is constrained to the trailing hemisphere (between ∼180°W and 360°W), with preferential concentration toward the apex (0°N, 270°W). Europa base image courtesy of NASA/JPL/Bjorn Jonsson.
Paper: Mid-ultraviolet Hubble Observations of Europa and the Global Surface Distribution of SO2 
Authors: Tracy M. Becker, Samantha K. Trumbo, Philippa M. Molyneux, Kurt D. Retherford, Amanda R. Hendrix, Lorenz Roth, Ujjwal Raut, Juan Alday, Melissa A. McGrath
Figure caption: Intraparticle models of small inclusions within water ice. Including both a UV-absorbing tholin and the SO2 inclusions reproduce the overall shape and strength of the 280 nm absorption feature  for regions observed at the apex of Europa’s trailing hemisphere.
Paper: Mid-ultraviolet Hubble Observations of Europa and the Global Surface Distribution of SO2 
Authors: Tracy M. Becker, Samantha K. Trumbo, Philippa M. Molyneux, Kurt D. Retherford, Amanda R. Hendrix, Lorenz Roth, Ujjwal Raut, Juan Alday, Melissa A. McGrath
Figure caption: The SO2 feature band depth as a function of surface reflectance averaged over 290–300 nm. Filled circles represent the most reliable measurements, while squares represent pixels that had overlapping 280 and 230 nm features and therefore produce a less reliable measurement. We note that band depths of <5% are within the noise and likely indicate a nondetection of the 280 nm feature.