adsabs/AstroCLIMB huggingface dataset:
Paper: Thermal Oxidation Reaction between NH3 and O3: Low-temperature Formation of an ﹩{\mathrm{NH}}_{4}^{+}﹩-bearing Salt
Authors: Patrick D. Tribbett, Mark J. Loeffler
Figure caption: IR spectra of a H2O + NH3 + O3 sample (25:70:5) during warming and annealing at 90.6 K. Note after 8 min the sample reached 90.6 K.
Paper: Thermal Oxidation Reaction between NH3 and O3: Low-temperature Formation of an ﹩{\mathrm{NH}}_{4}^{+}﹩-bearing Salt
Authors: Patrick D. Tribbett, Mark J. Loeffler
Figure caption: IR spectra of a H2O + NH3 + O3 sample (25:70:5) during warming at a rate of 0.1 K minute−1. Spectra are vertically offset for clarity.
Paper: Thermal Oxidation Reaction between NH3 and O3: Low-temperature Formation of an ﹩{\mathrm{NH}}_{4}^{+}﹩-bearing Salt
Authors: Patrick D. Tribbett, Mark J. Loeffler
Figure caption: IR spectra of the O3 fundamental absorption feature in a H2O + NH3 + O3 sample (20:75:5) warmed at a rate of 0.1 K minute−1.
Paper: JWST Spectrophotometry of the Small Satellites of Uranus and Neptune
Authors: Matthew Belyakov, M. Ryleigh Davis, Zachariah Milby, Ian Wong, Michael E. Brown
Figure caption: Left panel: comparison of the normalized reflectance of Phoebe from Cassini VIMS data (Clark et al. 2019) and Jupiter Trojan Eurybates (Wong et al. 2024) to Uranian inner satellites Juliet, Belinda, and Puck. Eurybates, while having a similarly low albedo to the Uranian inner satellites, has a significantly different IR spectrum, with a much weaker 3.0 μm feature. Phoebe’s albedo is similar to the very dark Uranian satellites and seems to have a similarly deep 3.0 μm feature, with a similar upturn between 1.4 and 2.1 μm. Right panel: comparison of the normalized reflectance of Ceres (from Raponi et al. 2021) and Iapetus from VIMS to Neptunian inner satellites Despina, Galatea, and Proteus. Ceres’s 3.0 μm ammonia feature is shallow and does not match any ice-giant inner satellite. The dark part of Iapetus has a spectrum that is compatible with that of Despina but not Proteus or Galatea.
Paper: JWST Spectrophotometry of the Small Satellites of Uranus and Neptune
Authors: Matthew Belyakov, M. Ryleigh Davis, Zachariah Milby, Ian Wong, Michael E. Brown
Figure caption: Left panel: albedos of the r > 40 km satellites of Uranus (Cressida, Juliet, Portia, Belinda, and Puck). Right panel: albedos of four inner Neptunian satellites (Despina, Galatea, Larissa, and Proteus) for the four wavelengths observed. Each moon’s observations have a slight horizontal offset from the filter’s central wavelength to assist readability. Both diagrams share the same vertical axis for easier comparison. All of the satellites show a clear 3 μm absorption feature, and most have an upward slope between 1.4 and 2.1 μm. The Uranian satellites are on average lower albedo than the Neptunian ones and seem to have a somewhat smaller F300M–F460M slope.
Paper: JWST Spectrophotometry of the Small Satellites of Uranus and Neptune
Authors: Matthew Belyakov, M. Ryleigh Davis, Zachariah Milby, Ian Wong, Michael E. Brown
Figure caption: JWST NIRCam albedos of Proteus and Puck compared to the spectra of 2004 EW95 (Plutino) and 2007 VL305 (Neptune Trojan) from JWST Programs 2418 and 2550, respectively. Also shown are Voyager-derived visual geometric albedos, with the Puck albedo selected to be at the same phase angle as the JWST observations (see Figure 6 of Karkoschka 2001 and Table 2 of Karkoschka 2003). The spectrophotometry for Proteus and Puck closely matches the shape and albedo for the selected objects, both of which have less red/neutral spectral slopes, and perihelia also near 30 au. Higher-resolution spectra for Puck and Proteus are needed to reveal surface composition.
Paper: JWST Spectrophotometry of the Small Satellites of Uranus and Neptune
Authors: Matthew Belyakov, M. Ryleigh Davis, Zachariah Milby, Ian Wong, Michael E. Brown
Figure caption: Background subtraction for an F140M (top) and an F300M (bottom) image of Neptune’s moon Despina. Despina is situated adjacent to the Le Verrier ring, which has a significant contribution to the flux around the moon. The left panels show the data after stage 2 pipeline reduction, which produces absolute flux-calibrated images. The middle panels show the composite background made by combining a model for the rings with a second-degree polynomial surface that characterizes the scattered-light background from Neptune The background-subtracted data are on the right, showing effective subtraction of the scattered-light gradient and the ring contribution. Note that while each image is 30 × 30 pixels, the pixel scale in the F300M image is twice that of the F140M image, which accounts for the difference in the apparent shape of the rings and the masking of Neptune in the F300M data.
Paper: JWST Spectrophotometry of the Small Satellites of Uranus and Neptune
Authors: Matthew Belyakov, M. Ryleigh Davis, Zachariah Milby, Ian Wong, Michael E. Brown
Figure caption: Representative JWST NIRCam images (brightness is square-root scale) of the Neptunian and Uranian systems in the F140M and F300M filters.
Paper: Observations of Titan’s Stratosphere during Northern Summer: Temperatures, CH3CN and CH3D Abundances
Authors: Alexander E. Thelen, Conor A. Nixon, Martin A. Cordiner, Emmanuel Lellouch, Sandrine Vinatier, Nicholas A. Teanby, Bryan Butler, Steven B. Charnley, Richard G. Cosentino, Katherine de Kleer, Patrick G. J. Irwin, Mark A. Gurwell, Zbigniew Kisiel, Raphael Moreno
Figure caption: Integrated emission (or “moment zero”) maps of Titan’s CH3D (A), CH3CN (B), and continuum (C) spectra. Panels (A) and (B) correspond to the emission integrated over the spectral transitions shown in Figure 1. The synthesized ALMA beam size (FWHM of the ALMA point-spread function) is shown as the hatched ellipse in the lower left; Titan’s solid surface, latitude, and longitudes are shown (solid and dashed blue lines). Contours are in increments of 1σ (A) and 10σ (B). Spectra were extracted for radiative transfer modeling at 20° latitude bins as displayed on the continuum emission map in panel (C) (yellow squares), and the corresponding area representing the ALMA beam footprint used to generate synthetic spectra from these individual regions on Titan’s limb is shown (yellow ellipses). Altitudes of 150 km and 1200 km above Titan’s surface are denoted by dotted and dashed blue circles, respectively, on the continuum map.
Paper: Observations of Titan’s Stratosphere during Northern Summer: Temperatures, CH3CN and CH3D Abundances
Authors: Alexander E. Thelen, Conor A. Nixon, Martin A. Cordiner, Emmanuel Lellouch, Sandrine Vinatier, Nicholas A. Teanby, Bryan Butler, Steven B. Charnley, Richard G. Cosentino, Katherine de Kleer, Patrick G. J. Irwin, Mark A. Gurwell, Zbigniew Kisiel, Raphael Moreno
Figure caption: (A) The resulting latitudinally resolved profiles of CH3CN abundance (solid lines) retrieved from ALMA CH3CN (J = 38–37) spectra. The retrievals are shown in a similar altitude range as the retrieved temperature profiles (Figure 4), though the CH3CN spectra are not sensitive to abundance variations below ∼160 km and above ∼450 km. The a priori CH3CN profile, constructed from the observations by Marten et al. (2002) and photochemical model predictions by Loison et al. (2015), is shown (dashed black line). (B) The fractional VMR error profiles corresponding to the vertical profiles in panel (A). (C) Temporal comparison of the CH3CN vertical profile retrieved at 40°N (solid red line and error envelope) to ALMA observations in 2015 (dashed orange profile and dotted errors) from Thelen et al. (2019b). (D) Comparison of an average of southern hemisphere profiles derived here (solid blue line and error envelope) to the vertical profile representing low southern latitudes in 2015 (purple dashed profile and dotted errors) from Thelen et al. (2019b).
Paper: Observations of Titan’s Stratosphere during Northern Summer: Temperatures, CH3CN and CH3D Abundances
Authors: Alexander E. Thelen, Conor A. Nixon, Martin A. Cordiner, Emmanuel Lellouch, Sandrine Vinatier, Nicholas A. Teanby, Bryan Butler, Steven B. Charnley, Richard G. Cosentino, Katherine de Kleer, Patrick G. J. Irwin, Mark A. Gurwell, Zbigniew Kisiel, Raphael Moreno
Figure caption: (A) The resulting latitudinally resolved temperature profiles (solid lines) retrieved using the ALMA CO (J = 6–5) spectra. The input disk-averaged profile retrieved from previous ALMA observations (Thelen et al. 2020) is shown (dashed black line). (B) The retrieval errors corresponding to the vertical profiles in panel (A). Errors below ∼80 km are tapered to 0 K to hold the tropospheric temperature values to those derived from the Cassini Radio Science data (Schinder et al. 2020). (C) Comparison of the retrieved temperature profile from Thelen et al. (2018) over a range of northern latitudes (centered at ∼48°N; dashed orange profile and dotted errors) and the profile presented here at 40°N (solid red profile and error envelope). (D) Comparison of the retrieved temperature profile from Thelen et al. (2018) representing low southern latitudes (∼16°S; dashed purple profile and dotted errors) and an average of the profiles retrieved here from 20°S to 77°S (solid blue profile and error envelope). The pressure axis on all panels is approximate, represented by the pressures from equatorial latitudes.
Paper: Observations of Titan’s Stratosphere during Northern Summer: Temperatures, CH3CN and CH3D Abundances
Authors: Alexander E. Thelen, Conor A. Nixon, Martin A. Cordiner, Emmanuel Lellouch, Sandrine Vinatier, Nicholas A. Teanby, Bryan Butler, Steven B. Charnley, Richard G. Cosentino, Katherine de Kleer, Patrick G. J. Irwin, Mark A. Gurwell, Zbigniew Kisiel, Raphael Moreno
Figure caption: Converted CH4 abundances as a function of latitude from Figure 8 using the D/H derived in Thelen et al. (2019a) are shown in purple. The weighted average of the converted CH4 abundance is shown to the left. The shaded error envelopes illustrate the range of converted CH4 abundances after considering the D/H ratios from ALMA (=1.033 × 10−4; Thelen et al. 2019a) and CIRS (=1.36 × 10−4; Nixon et al. 2012 and references therein). The CH4 abundances found by the Huygens GCMS (Niemann et al. 2010) and DISR (Bézard 2014; Rey et al. 2018) are shown (red, black, and orange data points, respectively). Green squares show the average measurements of stratospheric CH4 derived from Cassini/CIRS by Lellouch et al. (2014). Abundances between ∼150 and 200 km from Cassini occultation measurements are shown by blue crosses (Rannou et al. 2021, 2022).
Paper: Observations of Titan’s Stratosphere during Northern Summer: Temperatures, CH3CN and CH3D Abundances
Authors: Alexander E. Thelen, Conor A. Nixon, Martin A. Cordiner, Emmanuel Lellouch, Sandrine Vinatier, Nicholas A. Teanby, Bryan Butler, Steven B. Charnley, Richard G. Cosentino, Katherine de Kleer, Patrick G. J. Irwin, Mark A. Gurwell, Zbigniew Kisiel, Raphael Moreno
Figure caption: Limb-averaged Titan spectrum, created by averaging nine separate 20◦ latitude bins from both the eastern and western hemispheres following the combination of both ALMA executions during 2022 June. The spectral resolution was 977 kHz. Spectra were extracted from ∼150 km above the surface. Data are shown following continuum subtraction. Transitions of the CH3CN (J = 38–37) band from the CDMS catalog, Doppler-shifted to Titan’s rest velocity, are shown in red for reference; the line marker amplitudes are arbitrary. The dotted box denotes the spectral range of the figure inset, which focuses on the CH3D (J = 3–2) triplet. The CH3D transitions from the CDMS catalog are again denoted in vertical purple lines in the inset. As a result of the continuum subtraction, the extent of the pressure-broadened CH3D band is evident, in comparison to the relatively narrow CH3CN emission lines.
Paper: Observations of Titan’s Stratosphere during Northern Summer: Temperatures, CH3CN and CH3D Abundances
Authors: Alexander E. Thelen, Conor A. Nixon, Martin A. Cordiner, Emmanuel Lellouch, Sandrine Vinatier, Nicholas A. Teanby, Bryan Butler, Steven B. Charnley, Richard G. Cosentino, Katherine de Kleer, Patrick G. J. Irwin, Mark A. Gurwell, Zbigniew Kisiel, Raphael Moreno
Figure caption: CH3D abundance in Titan’s stratosphere (between ∼100 and 300 km; ∼0.1–10 mbar). The retrieval error bars are shown for each data point. Each data point represents the averaged atmospheric CH3D VMR for latitudes spanning ∼±10° (low latitudes) to ∼±20° (high latitudes) due to the size of the ALMA beam and the subobserver latitude of Titan (∼12°), as shown in Figure 2(C). The weighted average of all observations is shown (leftmost data point).
Paper: Observations of Titan’s Stratosphere during Northern Summer: Temperatures, CH3CN and CH3D Abundances
Authors: Alexander E. Thelen, Conor A. Nixon, Martin A. Cordiner, Emmanuel Lellouch, Sandrine Vinatier, Nicholas A. Teanby, Bryan Butler, Steven B. Charnley, Richard G. Cosentino, Katherine de Kleer, Patrick G. J. Irwin, Mark A. Gurwell, Zbigniew Kisiel, Raphael Moreno
Figure caption: Top row: representative ALMA data (black) compared to synthetic spectra from the corresponding best-fit NEMESIS models at 60◦N (red), the equator (purple), and 60◦S (blue) for spectral ranges covering the CH3D (left column), CH3CN (middle column), and CO (right column) transitions. Spectra are offset by arbitrary, constant factors for clarity (0.2 Jy for CH3D; 0.5 Jy for CH3CN and CO). The interloping CH3CN (J = 386–376) transition at 697.804 GHz is denoted in the equatorial CH3D spectrum. Bottom row: residual (data–model) spectra corresponding to the data and models in the top row. Residual spectra are offset for clarity (0.12 Jy for CH3D; 0.2 for CH3CN; 0.3 for CO).
Paper: Observations of Titan’s Stratosphere during Northern Summer: Temperatures, CH3CN and CH3D Abundances
Authors: Alexander E. Thelen, Conor A. Nixon, Martin A. Cordiner, Emmanuel Lellouch, Sandrine Vinatier, Nicholas A. Teanby, Bryan Butler, Steven B. Charnley, Richard G. Cosentino, Katherine de Kleer, Patrick G. J. Irwin, Mark A. Gurwell, Zbigniew Kisiel, Raphael Moreno
Figure caption: Temperatures from Figure 4(A), shown as a map as a function of latitude and altitude over the vertical range where our ALMA observations are sensitive. The latitudes below 80°S are not shown due to Titan’s subobserver latitude at the time of these observations, which shrouds the south pole from view. Temperature contours are shown for reference, as is an approximate pressure grid from equatorial latitudes.
Paper: Observations of Titan’s Stratosphere during Northern Summer: Temperatures, CH3CN and CH3D Abundances
Authors: Alexander E. Thelen, Conor A. Nixon, Martin A. Cordiner, Emmanuel Lellouch, Sandrine Vinatier, Nicholas A. Teanby, Bryan Butler, Steven B. Charnley, Richard G. Cosentino, Katherine de Kleer, Patrick G. J. Irwin, Mark A. Gurwell, Zbigniew Kisiel, Raphael Moreno
Figure caption: Map of CH3CN abundances as a function of latitude and altitude. The pressure axis is approximate, represented by the pressures from equatorial latitudes.
Paper: Lunar North Polar Cold Traps Based on Diurnally and Seasonally Varying Temperatures
Authors: Norbert Schörghofer, Jean-Pierre Williams, Erwan Mazarico
Figure caption: (a) Maximum potential sublimation rate, ﹩{\max }_{t}(E)﹩, poleward of 80°N with logarithmic color scale. Black contours correspond to 100 kg m−2 Ga−1. (b) Long-term average of the potential sublimation rate, mean t (E). (c) Comparison of contours for a 100 kg m−2 Ga−1 sublimation rate for ﹩{\max }_{t}(E)﹩ and mean t (E). The red contours are plotted on top of the blue contours, and always enclose a smaller area than the blue contours. The background map is a shaded topographic relief. (d) Correlation of ﹩{\max }_{t}(E)﹩ with mean t (E) on logarithmic scales.
Paper: Lunar North Polar Cold Traps Based on Diurnally and Seasonally Varying Temperatures
Authors: Norbert Schörghofer, Jean-Pierre Williams, Erwan Mazarico
Figure caption: Cold trap area poleward of 80°N latitude as a function of sublimation rate threshold and for various methods. The total PSR area based on a 240 m px−1 LOLA map is also shown.
Paper: Lunar North Polar Cold Traps Based on Diurnally and Seasonally Varying Temperatures
Authors: Norbert Schörghofer, Jean-Pierre Williams, Erwan Mazarico
Figure caption: Time coverage of available data for 2009 July to 2024 January poleward of 80°N, defined as the percentage of the 96 × 2 = 192 temporal bins populated with Diviner data measurements.
Paper: Lunar North Polar Cold Traps Based on Diurnally and Seasonally Varying Temperatures
Authors: Norbert Schörghofer, Jean-Pierre Williams, Erwan Mazarico
Figure caption: Mean surface temperature poleward of 80°N averaged over diurnal and seasonal cycles.
Paper: Lunar North Polar Cold Traps Based on Diurnally and Seasonally Varying Temperatures
Authors: Norbert Schörghofer, Jean-Pierre Williams, Erwan Mazarico
Figure caption: (a)–(c) Time series for the year 2019 at stereographic coordinates (−150 km, +62 km), the location indicated by a black star in panel (e) in Lenard Crater. This location briefly receives direct sunlight three times during the year, when the Sun partially rises above the horizon. (c) Radiative equilibrium temperatures are calculated based on the direct irradiance, assuming an albedo of 0.11 and an emissivity of 0.99, and compared with channel 9 Diviner measurements. (d) Elevation of the horizon and the Sun. Dots are spaced by 1 hr. The azimuth is measured clockwise relative to the right-pointing horizontal axis in map (e) and part of solar disk emerges above the horizon near summer solstice at sunrise. (e) Topography of the area relative to sphere. Contours are spaced 250 m, and the elevation varies between −3500 m and +1504 m within the region shown. The lowest horizon elevations, as viewed from the study location (black star), are on the far side of Hermite Crater (azimuths ∼30–80°), beyond the area shown.
Paper: Lunar North Polar Cold Traps Based on Diurnally and Seasonally Varying Temperatures
Authors: Norbert Schörghofer, Jean-Pierre Williams, Erwan Mazarico
Figure caption: (a) Comparison of PSRs and cold traps in a portion of the north polar region. Occasionally, Diviner-based cold traps extend beyond the PSR. The background map is a shaded topographic relief, and the north pole is at the lower right corner. (b) Fraction of diurnal–seasonal bins occupied with Diviner data. Contours are the same cold traps as in (a). (c) Maximum direct irradiance over the year 2025.
Paper: Lunar North Polar Cold Traps Based on Diurnally and Seasonally Varying Temperatures
Authors: Norbert Schörghofer, Jean-Pierre Williams, Erwan Mazarico
Figure caption: Pumping differential in the north polar region for a supply rate of 1 m Ga−1, overlaid on a shaded topographic relief. Subsurface cold trapping is expected in the colored regions.
Paper: Lunar North Polar Cold Traps Based on Diurnally and Seasonally Varying Temperatures
Authors: Norbert Schörghofer, Jean-Pierre Williams, Erwan Mazarico
Figure caption: Depth to loss rates of 1 kg m−2 Ga−1 poleward of 80°N. White indicates ice is stable at depths larger than 20 cm or not stable at any depth.
Paper: Uranus’s Influence on Neptune’s Exterior Mean-motion Resonances
Authors: Severance Graham, Kathryn Volk
Figure caption: Test particle period ratio with Neptune vs. ψ in the phase space from Neptune's 2:1 to 28:1 resonances (∼50−280 au) for four different N:U period ratios. In each simulation, particles are initialized with the equivalent of q = 33 au for present-day Neptune’s orbit. Dark blue test particles indicate a longer normalized residence time, which is defined as a function of its change in semimajor axis (Δa) across multiple small time intervals (see the Appendix). Lighter yellow test particles indicate a shorter normalized residence time. Particles assigned a residence time of 0 (i.e., particles that scatter for the entire simulation) are plotted in light gray for clarity to separate them from the resonant-interacting particles. Uranus is included as a full perturber in all but the leftmost plot; in the limited Uranus effects simulation, Uranus interacts with the other massive bodies but not directly with the test particles. Notice the dramatic destabilization of Neptune’s external resonances when Neptune is set to be in the 2:1 resonance with Uranus. We discuss in Section 3 how the stability of Neptune’s external resonances depends on the the mutual period ratio between Uranus and Neptune. In the leftmost plot, note that the destabilization remains when Uranus perturbs Neptune but is not included in the force calculations for the test particles.
Paper: Dimorphos’s Orbit Period Change and Attitude Perturbation due to Its Reshaping after the DART Impact
Authors: Ryota Nakano, Masatoshi Hirabayashi, Sabina D. Raducan, Petr Pravec, Shantanu P. Naidu, Harrison F. Agrusa, Steven Chesley, Fabio Ferrari, Martin Jutzi, Colby C. Merrill, Alex J. Meyer, Patrick Michel, Derek C. Richardson, Paul Sánchez, Peter Scheirich, Stephen R. Schwartz, Yun Zhang, Adriano Campo Bagatin, Po-Yen Liu, Andrew F. Cheng
Figure caption: Reshaping-induced orbit period change, ΔP reshaping, as a function of a  s /b  s  and b  s /c  s . Reshaping is assumed to occur along the principal axes, and the post-impact shape is symmetrical about the Y-axis, as shown in Figure 2. The current estimates of the axis ratios a  s /b  s  and b  s /c  s  are indicated by the horizontal and vertical error bars, respectively (i.e., 1.1 ≤ a  s /b  s  ≤ 1.4 from Pravec et al., in review; a  s /b  s  = 1.300 ± 0.010 and b  s /c  s  = 1.3 ± 0.2 from Naidu et al. 2024). The dashed line indicates b  s /c  s  = 1.0, below which the attitude becomes unstable. The red contour line indicates ΔP reshaping = 0 s, which would extend toward the pre-impact axis ratios, a  s /b  s  ≈ 1.06 and b  s /c  s  ≈ 1.47 (Daly et al. 2024).
Paper: Dimorphos’s Orbit Period Change and Attitude Perturbation due to Its Reshaping after the DART Impact
Authors: Ryota Nakano, Masatoshi Hirabayashi, Sabina D. Raducan, Petr Pravec, Shantanu P. Naidu, Harrison F. Agrusa, Steven Chesley, Fabio Ferrari, Martin Jutzi, Colby C. Merrill, Alex J. Meyer, Patrick Michel, Derek C. Richardson, Paul Sánchez, Peter Scheirich, Stephen R. Schwartz, Yun Zhang, Adriano Campo Bagatin, Po-Yen Liu, Andrew F. Cheng
Figure caption: Synthetic shape model of reshaped Dimorphos (left) top-down view and (right) side view. The original shape model of Dimorphos is illustrated in gray. The red arrow indicates the DART impact condition. The change in the negative semi-intermediate axis length is denoted as Δ− Y. Although they are not shown, the changes in the semimajor and semiminor axes lengths (i.e., Δ± X and Δ± Z) are also defined in a similar way.
Paper: Dimorphos’s Orbit Period Change and Attitude Perturbation due to Its Reshaping after the DART Impact
Authors: Ryota Nakano, Masatoshi Hirabayashi, Sabina D. Raducan, Petr Pravec, Shantanu P. Naidu, Harrison F. Agrusa, Steven Chesley, Fabio Ferrari, Martin Jutzi, Colby C. Merrill, Alex J. Meyer, Patrick Michel, Derek C. Richardson, Paul Sánchez, Peter Scheirich, Stephen R. Schwartz, Yun Zhang, Adriano Campo Bagatin, Po-Yen Liu, Andrew F. Cheng
Figure caption: Post-impact shape model of Dimorphos based on smoothed particle hydrodynamics (SPH) impact simulation results: (left) top-down view and (right) side view. The DART spacecraft approached approximately along Dimorphos’s intermediate axis (i.e., Y-axis in the figure) from negative to positive direction and impacted near the center of figure of the body.