adsabs/AstroCLIMB huggingface dataset:
Paper: Interstellar Comets from Post-main-sequence Systems as Tracers of Extrasolar Oort Clouds
Authors: W. Garrett Levine, Aster G. Taylor, Darryl Z. Seligman, Devin J. Hoover, Robert Jedicke, Jennifer B. Bergner, Gregory P. Laughlin
Figure caption: Residual of the thermal model presented in this paper with regards to a similar model constructed in Mathematica.
Paper: Spatial Distribution of Glycine and Aspartic Acid in Rapidly Frozen Brines Relevant to Enceladus
Authors: Tuan H. Vu, Robert Hodyss, Paul V. Johnson, Morgan L. Cable
Figure caption: Raman spectrum of an analog Enceladus brine containing glycine (composition listed in Table 1) upon flash freezing at 110 K (top) and upon annealing at 220 K (bottom). The spectra are offset for clarity. The inset shows an expanded view of the 800–1800 cm−1 region. The colored boxes denote the spectral ranges used for mapping the individual component in Figure 2 (yellow for glycine, red for natron, orange for hydrohalite, and blue for water ice).
Paper: Spatial Distribution of Glycine and Aspartic Acid in Rapidly Frozen Brines Relevant to Enceladus
Authors: Tuan H. Vu, Robert Hodyss, Paul V. Johnson, Morgan L. Cable
Figure caption: Raman spectrum of the analog Enceladus brine containing aspartic acid (composition given in Table 1) upon flash freezing at 110 K (top) and after annealing at 220 K (bottom). The spectra are offset for clarity. The inset shows an expanded view of the 800–1800 cm−1 region, where the labeled peaks denote the vibrational signatures of aspartic acid. The symmetric stretch of the carboxylate side chain (the colored box) is used for mapping the distribution of aspartic acid in Figure 5.
Paper: Spatial Distribution of Glycine and Aspartic Acid in Rapidly Frozen Brines Relevant to Enceladus
Authors: Tuan H. Vu, Robert Hodyss, Paul V. Johnson, Morgan L. Cable
Figure caption: Pairwise correlation plots for various components in the frozen glycine–brine system, constructed from the Raman maps shown in Figure 2. The yellow line in each panel represents a linear fit of the displayed data, included as a guide to the eye. The p-values for all correlation pairs (i.e., the probability of observing these distributions if there is no correlation) are less than 0.00015, indicating sufficient statistical significance.
Paper: Spatial Distribution of Glycine and Aspartic Acid in Rapidly Frozen Brines Relevant to Enceladus
Authors: Tuan H. Vu, Robert Hodyss, Paul V. Johnson, Morgan L. Cable
Figure caption: Raman maps obtained at 220 K showing the distribution of aspartic acid (green), natron (red), hydrohalite (orange), and water ice (blue) in the annealed frozen brine system. In each panel, the concentration of the individual components increases with pixel brightness.
Paper: Spatial Distribution of Glycine and Aspartic Acid in Rapidly Frozen Brines Relevant to Enceladus
Authors: Tuan H. Vu, Robert Hodyss, Paul V. Johnson, Morgan L. Cable
Figure caption: Raman maps obtained at 220 K showing the distribution of glycine (yellow), natron (red), hydrohalite (orange), and water ice (blue) in the annealed frozen brine sample. In each panel, the concentration of the individual components increases with pixel brightness.
Paper: Col-OSSOS: Evidence for a Compositional Gradient Inherited from the Protoplanetary Disk?
Authors: Michaël Marsset, Wesley C. Fraser, Megan E. Schwamb, Laura E. Buchanan, Rosemary E. Pike, Kathryn Volk, Nuno Peixinho, Susan Benecchi, Michele T. Bannister, Nicole J. Tan, J. J. Kavelaars
Figure caption: Final inclination distribution of test particles in the dynamical simulations of Kaib & Sheppard (2016, blue and black lines) and Nesvorný & Vokrouhlický (2016, red line), as a function of their initial semimajor axis (bin average with 0.5 au steps). The left and right panels correspond to smooth and grainy migration scenarios, respectively. The continuous and dashed lines represent scenarios of fast and slow migrations, respectively, with exponential e-folding timescales (τ) as indicated in the legend. When two τ values are provided, the first one corresponds to the value before Neptune’s jump in semimajor axis, and the second one to the value after the jump. Colored regions correspond to the 1σ dispersion of inclination values at the final stage of the simulations. Despite the very large scatter in inclination values, the same trend of decreasing final inclinations as a function of increasing initial semimajor axis is observed in every simulation. Combining all data sets, test particles have an average 1° decrease in final inclinations per 1 au increase in initial semimajor axis.
Paper: Col-OSSOS: Evidence for a Compositional Gradient Inherited from the Protoplanetary Disk?
Authors: Michaël Marsset, Wesley C. Fraser, Megan E. Schwamb, Laura E. Buchanan, Rosemary E. Pike, Kathryn Volk, Nuno Peixinho, Susan Benecchi, Michele T. Bannister, Nicole J. Tan, J. J. Kavelaars
Figure caption: Comparison of optical spectral slopes of TNOs and Centaurs measured by different surveys. Top: measurements from H/WTSOSS and Col-OSSOS are compared to the data sets of MBOSS (left), Tegler, Romanishin and Consolmagno (TRC; middle), and Peixinho et al. (2015, right). The gray line indicates a 1:1 ratio, corresponding to perfect spectral slope equality between the surveys. Bottom: corresponding histograms of differences in spectral slopes between the surveys, fitted with a Gaussian curve represented by the black line. The mean (μ) and standard deviation (σ) of the histograms are indicated in each corresponding panel. We also indicate the average difference uncertainty between the two surveys.
Paper: Evidence for Nitrogen-bearing Species on Umbriel: Sourced from a Subsurface Ocean, Undifferentiated Crust, or Impactors?
Authors: Richard J. Cartwright, Riley A. DeColibus, Julie C. Castillo-Rogez, Chloe B. Beddingfield, William M. Grundy, Tom A. Nordheim
Figure caption: Seven reflectance spectra of Umbriel. All 15 spectra (A2, A3) were normalized to unity between 1.74 and 1.77 μm. These spectra were smoothed using the boxcar function described in the caption of Figure 1 (black), along with the 1σ uncertainties shown at their native resolutions (gray). The mid-observation subobserver longitude is listed in the top left corner of each plot. Relevant observing information for each spectrum is summarized in Table 1, organized by subobserver longitude. The greater point-to-point variation and lower S/N between 1.08 and 1.14 μm, 1.31 and 1.46 μm, 1.78 and 1.96 μm, and ≳2.35 μm results from increased telluric absorption in these wavelength regions. The sensitivities of SpeX (SXD mode) and TripleSpec are lower at wavelengths <1.4 μm and >2.3 μm, further reducing the S/N beyond these wavelengths. Additional structure at wavelengths <1.3 μm in some of the spectra results from scattered-light contributions from Uranus.
Paper: Origin-of-life Molecules in the Atmosphere after Big Impacts on the Early Earth
Authors: Nicholas F. Wogan, David C. Catling, Kevin J. Zahnle, Roxana Lupu
Figure caption: Postimpact H2 generation as a function of impactor mass under different modeling assumptions. Models 1A, 1B, 2, and 3B are identical to those described in Figure 1 of Itcovitz et al. (2022). The simulation’s preimpact volatile inventories, impact angle, and impact velocity are listed in Table 2. In model 1A, all iron delivered by an impact reacts with steam to produce H2. The resulting atmosphere does not equilibrate with an impact-generated melt pool. Model 1B assumes that a fraction (∼15%–30%) of the impactor iron reduces the steam atmosphere based on SPH simulations (Citron & Stewart 2022) and that the atmosphere is chemically isolated from a melt pool. Model 2 is like model 1A while also including postimpact equilibration with a melt pool with a redox state of ΔFMQ-2.3 to represent peridotite (Itcovitz et al. 2022). Model 3B assumes that a fraction (∼15%–30%) of the impactor iron reacts with the steam atmosphere based on SPH simulations and includes melt–atmosphere redox equilibration with a pool magma initially at ΔFMQ-2.3. As stated in Section 3.1, we nominally assume model 1A throughout the main text calculations. We also include simulations in the Appendix that instead adopt model 1B, which we consider to be a plausible lower bound for postimpact H2 generation.
Paper: Origin-of-life Molecules in the Atmosphere after Big Impacts on the Early Earth
Authors: Nicholas F. Wogan, David C. Catling, Kevin J. Zahnle, Roxana Lupu
Figure caption: Three phases of atmospheric evolution after a large asteroid impact on the Hadean Earth. In phase 1, the impactor vaporizes the ocean and heats up the atmosphere. Iron delivered by the impactor reacts with hot steam to make H2. The H2 is also modulated by equilibration between the atmosphere and an impact-generated melt pond. In phase 2, as the steam-rich atmosphere cools for thousands of years, H2 reacts with CO2 to make atmospheric CH4. Ultimately, the steam condenses to an ocean. Finally, in phase 3, N2 and CH4 photochemistry generates HCN and other prebiotic nitriles. The H2-dominated atmosphere escapes to space over millions of years, causing the return of a more oxidizing N2 and CO2 atmosphere.
Paper: Origin-of-life Molecules in the Atmosphere after Big Impacts on the Early Earth
Authors: Nicholas F. Wogan, David C. Catling, Kevin J. Zahnle, Roxana Lupu
Figure caption: Kinetics-climate simulation of a cooling steam atmosphere caused by a 1.58 × 1021 kg impactor. The model uses the Table 2 nominal parameters. The top panel is surface temperature, and the bottom panel shows atmospheric composition.
Paper: Dual-band Fourier-transform Millimeter-wave Spectrometry for In Situ Gas Sensing
Authors: Brian J. Drouin, Deacon J. Nemchick, Ananda Nole, Adrian Tang, Chung-Tse Michael Wu, Neda Khiabani, Maria Alonso, Mau-Chung Frank Chang
Figure caption: Center: photograph of dual-slot W-band coupler (horizontal) and dual-patch differential G-band coupler (vertical) used for low-SWaP system, 1 mm scale bar given. Inset microphotos: (lower left) G-band CMOS R x , (upper left) W-band CMOS R x , (upper right) G-band waveguide probe, (lower right) W-band waveguide probe.
Paper: Dual-band Fourier-transform Millimeter-wave Spectrometry for In Situ Gas Sensing
Authors: Brian J. Drouin, Deacon J. Nemchick, Ananda Nole, Adrian Tang, Chung-Tse Michael Wu, Neda Khiabani, Maria Alonso, Mau-Chung Frank Chang
Figure caption: Schematic showing basic elements of semiconfocal millimeter-wave Fourier-transform molecular sensor embedded in a vacuum chamber side by side with basic elements for a tunable laser spectrometer and a quadrupole-ion-trap mass spectrometer.
Paper: Dual-band Fourier-transform Millimeter-wave Spectrometry for In Situ Gas Sensing
Authors: Brian J. Drouin, Deacon J. Nemchick, Ananda Nole, Adrian Tang, Chung-Tse Michael Wu, Neda Khiabani, Maria Alonso, Mau-Chung Frank Chang
Figure caption: Left: free-induction decay and Fourier-transform spectrum, with and without background subtraction, measured with the low-SWaP system. Leakage from the CMOS pulse switch and radio-frequency interference from the USART are well separated from the target measurement. Right: free-induction decay and Fourier-transform spectrum measured with the modular system over frozen ice sample.
Paper: Dual-band Fourier-transform Millimeter-wave Spectrometry for In Situ Gas Sensing
Authors: Brian J. Drouin, Deacon J. Nemchick, Ananda Nole, Adrian Tang, Chung-Tse Michael Wu, Neda Khiabani, Maria Alonso, Mau-Chung Frank Chang
Figure caption: Left: assembly of low-SWaP system on benchtop; heat straps not shown. Right: assembly of the modular system. The millimeter-wave transceivers are outlined in red; the central coupler plates in both systems are 2 × 2 cm2.
Paper: Dual-band Fourier-transform Millimeter-wave Spectrometry for In Situ Gas Sensing
Authors: Brian J. Drouin, Deacon J. Nemchick, Ananda Nole, Adrian Tang, Chung-Tse Michael Wu, Neda Khiabani, Maria Alonso, Mau-Chung Frank Chang
Figure caption: Measurements of minimal detection limits of carbonyl sulfide (OCS), and its isotopologues, provide a diagnostic tool to assess both the sensitivity and the bandwidth. OCS features in each isotopologue appear every ∼12 GHz; these measurements extend to the last measurable features on either side of the band. Error bars are based on isotopic abundance; labels indicate isotopologue; 622 ≡16O12C32S; values in parenthesis are ν 2 (bending mode) quanta.
Paper: Dual-band Fourier-transform Millimeter-wave Spectrometry for In Situ Gas Sensing
Authors: Brian J. Drouin, Deacon J. Nemchick, Ananda Nole, Adrian Tang, Chung-Tse Michael Wu, Neda Khiabani, Maria Alonso, Mau-Chung Frank Chang
Figure caption: Artist rendition of a low-SWaP system deployed next to a drill affixed to the side of a Philae-like comet landing craft (Di Lizia et al. 2016). Immersion of the open cavity structure in the plume allows for instantaneous monitoring of lost volatiles during sampling.
Paper: Dual-band Fourier-transform Millimeter-wave Spectrometry for In Situ Gas Sensing
Authors: Brian J. Drouin, Deacon J. Nemchick, Ananda Nole, Adrian Tang, Chung-Tse Michael Wu, Neda Khiabani, Maria Alonso, Mau-Chung Frank Chang
Figure caption: Waveguide connected hybrid CMOS systems envisaged for flight mission efforts.
Paper: Dual-band Fourier-transform Millimeter-wave Spectrometry for In Situ Gas Sensing
Authors: Brian J. Drouin, Deacon J. Nemchick, Ananda Nole, Adrian Tang, Chung-Tse Michael Wu, Neda Khiabani, Maria Alonso, Mau-Chung Frank Chang
Figure caption: Curve of growth measurements for partially deuterated water, HDO; each spectrum is a Fourier-transform of 100,000 free-induction decays.
Paper: First Optical Constants of Laboratory-generated Organic Refractory Materials (Tholins) Produced in the NASA Ames COSmIC Facility from the Visible to the Near Infrared (0.4–1.6 μm): Application to Titan’s Aerosols
Authors: Ella Sciamma-O'Brien, Ted L. Roush, Pascal Rannou, David Dubois, Farid Salama
Figure caption: Left: Front view of the PDN showing the electrodes and gas expansion slit (top); side view of the PDN planar plasma expansion during deposition of solid samples onto three substrates (bottom). Right: Schematic of the PDN (side view; adapted from Broks et al. 2005 and Nuevo et al. 2022).
Paper: Interstellar Comets from Post-main-sequence Systems as Tracers of Extrasolar Oort Clouds
Authors: W. Garrett Levine, Aster G. Taylor, Darryl Z. Seligman, Devin J. Hoover, Robert Jedicke, Jennifer B. Bergner, Gregory P. Laughlin
Figure caption: Analytically determined probability (Equation (9)) of ejecting test particles in the nonadiabatic limit where Ψ → ∞. Equation (6) determines the total mass lost in the event as M MS − M WD. Results are plotted against the test particle’s eccentricity before the mass-loss event, e J,0.
Paper: Interstellar Comets from Post-main-sequence Systems as Tracers of Extrasolar Oort Clouds
Authors: W. Garrett Levine, Aster G. Taylor, Darryl Z. Seligman, Devin J. Hoover, Robert Jedicke, Jennifer B. Bergner, Gregory P. Laughlin
Figure caption: Adiabatic index Ψ (Equation (2)) for exo–Oort orbital dynamics at the beginning of the host star’s AGB. Results are displayed as a heatmap on a grid of main-sequence stellar mass vs. initial semimajor axis a J,0. Contours of Ψ = [1, 10, 100] are drawn along with astrocentric distances of interest: the inner exo–Oort Cloud boundary (Equation (4)), the post-main-sequence Hill sphere radius, and the main-sequence Hill sphere radius (Equation (5)).
Paper: Post-flight Evaluation of Lidar-based Digital Terrain Models for OSIRIS-REx Navigation at Bennu
Authors: Jason M. Leonard, Jeroen L. Geeraert, Leilah K. McCarthy, Coralie D. Adam, Peter G. Antreasian, Olivier S. Barnouin, Michael G. Daly, Jeffrey A. Seabrook, Dante S. Lauretta
Figure caption: OLA performance for Recon B (a, b) vs. Iota (a) and the off-nadir angles (b). The HELT mean and 1σ standard deviation is given in orange, while the LELT performance is given in green. Histograms of the data per bin are given in blue.
Paper: Review and Revision of the Lunar Cratering Chronology—Lunar Timescale Part 2
Authors: Stephanie C. Werner, Benjamin Bultel, Tobias Rolf
Figure caption: Crater statistics for the Apollo 16 landing area. (a) Our counting unit with craters. (b) Overview of all counting units. (c) The respective crater size–frequency distributions. (d) Apollo 16 in comparison to crater size–frequency distributions (Fassett et al. 2012) for those basins, which likely contributed ejecta to the local stratigraphic column (see Table 1).
Paper: Review and Revision of the Lunar Cratering Chronology—Lunar Timescale Part 2
Authors: Stephanie C. Werner, Benjamin Bultel, Tobias Rolf
Figure caption: Crater statistics for the Apollo 14 landing area. (a) Overview of the counting units (green, Werner et al., this work; black, Neukum et al. 1975; as used in Neukum 1983; blue, Robbins 2014). (b) Counting unit with craters. (c) The respective crater size–frequency distributions.
Paper: Review and Revision of the Lunar Cratering Chronology—Lunar Timescale Part 2
Authors: Stephanie C. Werner, Benjamin Bultel, Tobias Rolf
Figure caption: Crater Statistics related to the Apollo 15 landing site. (a) Overview of the counting units: Neukum et al. (1975; used in Neukum 1983) outlined in black, Robbins (2014) in blue, this work in green. (b) The spectrally defined count unit including the marked craters. (c) The resulting crater size–frequency distribution.
Paper: Review and Revision of the Lunar Cratering Chronology—Lunar Timescale Part 2
Authors: Stephanie C. Werner, Benjamin Bultel, Tobias Rolf
Figure caption: Crater statistics for the Apollo 11 landing area. (a) Overview of the counting units (green, Werner et al., this work; black, Neukum et al. 1975; as used in Neukum 1983; blue, Robbins 2014). (b) Counting unit with craters. (c) The respective crater size–frequency distributions.
Paper: Review and Revision of the Lunar Cratering Chronology—Lunar Timescale Part 2
Authors: Stephanie C. Werner, Benjamin Bultel, Tobias Rolf
Figure caption: Crater Statistics related to the Luna 16 landing site. (a) Overview of the counting units: Robbins (2014) in blue, Werner et al. (this work) in green. (b) Our spectrally defined count unit including the marked craters. (c) The resulting crater size–frequency distribution.
Paper: Review and Revision of the Lunar Cratering Chronology—Lunar Timescale Part 2
Authors: Stephanie C. Werner, Benjamin Bultel, Tobias Rolf
Figure caption: Crater statistics at the Apollo 12 site unit. (a) Comparison of various counting units (green, Werner et al. and this work; black, Neukum & König 1976; blue, Robbins 2014). (b) Counting unit with craters following. (c) The resulting crater size–frequency distributions.
Paper: Review and Revision of the Lunar Cratering Chronology—Lunar Timescale Part 2
Authors: Stephanie C. Werner, Benjamin Bultel, Tobias Rolf
Figure caption: Crater statistics for the Apollo 17 landing area. (a) Spectrally defined counting unit with craters. (b) Overview of counting units (green, Werner et al., this work; black, Neukum 1983; blue, Robbins 2014). (c) The respective crater size frequency distributions.
Paper: Review and Revision of the Lunar Cratering Chronology—Lunar Timescale Part 2
Authors: Stephanie C. Werner, Benjamin Bultel, Tobias Rolf
Figure caption: Crater statistics for the Luna 20 landing area. (a) Counting unit with craters. (b) The respective crater-size frequency distribution, and comparison to Crisium superposed crater frequency after Fassett et al. (2012).
Paper: Review and Revision of the Lunar Cratering Chronology—Lunar Timescale Part 2
Authors: Stephanie C. Werner, Benjamin Bultel, Tobias Rolf
Figure caption: Crater Statistics related to the Luna 24 landing site. (a) Overview of the counting units: Robbins (2014) in blue, this work in green. (b) Our spectrally defined unit including the marked craters. (c) The resulting crater size–frequency distribution.
Paper: Equatorial Waves and Superrotation in the Stratosphere of a Titan General Circulation Model
Authors: Neil T. Lewis, Nicholas A. Lombardo, Peter L. Read, Juan M. Lora
Figure caption: Vertical profile of temperature T and buoyancy frequency N at the equator (solid) and 60°N (dashed) around northern hemisphere late summer (black) and late autumn (gray).
Paper: Equatorial Waves and Superrotation in the Stratosphere of a Titan General Circulation Model
Authors: Neil T. Lewis, Nicholas A. Lombardo, Peter L. Read, Juan M. Lora
Figure caption: Zonal-mean zonal wind ﹩\overline{u}﹩ and TEM stream function Ψ* for northern hemisphere late summer and late autumn. Six contour levels are shown for Ψ* at ±107, ±108, and ±109 kg s−1 (negative contours dashed). Positive Ψ* indicates clockwise overturning.
Paper: Evidence for Nitrogen-bearing Species on Umbriel: Sourced from a Subsurface Ocean, Undifferentiated Crust, or Impactors?
Authors: Richard J. Cartwright, Riley A. DeColibus, Julie C. Castillo-Rogez, Chloe B. Beddingfield, William M. Grundy, Tom A. Nordheim
Figure caption: Left: Nineteen Umbriel spectra (black, labeled a–s) and 1σ uncertainties (gray error bars) that display 2.14 μm (purple markers), 2.2 μm (blue markers), 2.22 μm (green markers), and/or 2.24 μm (red markers) absorption features with both band depths and areas >2σ (Tables A2–A5). The subobserver longitude for each spectrum is also listed (Table 1). All spectra were normalized to unity between 1.74 and 1.77 μm and offset vertically for clarity. To make spectral features easier to identify, the data have been lightly smoothed using boxcar functions ranging from 4 pixels wide (IRTF/SpeX PRISM mode spectra), 8 to 12 pixels wide (IRTF/SpeX SXD mode spectra), and 16 pixels wide (3.5 m/TripleSpec spectra). Right: Modified simple cylindrical map projection of the Voyager 2/Imaging Science System image mosaic of Umbriel (NASA/JPL/Caltech/USGS). The subobserver longitude and latitude for all 33 spectra are indicated with filled circles that represent the center of the target disk. These observations were disk integrated and averaged over an entire hemisphere. The 19 spectra on the left are represented by colored circles (labeled a–s), with colors and band centers defined below the map. Spectra that display two bands are represented by two-color semicircles, spectra that display three bands are represented by three-color wedges, and spectra without band depth and area measurements >2σ are shown as black circles. The white arrow points to the bright annulus of material mantling the floor of Wunda crater. The candidate constituents listed below the map are shown in Figure 4 and discussed in further detail in Sections 3.4 and 4.2.
Paper: Origin-of-life Molecules in the Atmosphere after Big Impacts on the Early Earth
Authors: Nicholas F. Wogan, David C. Catling, Kevin J. Zahnle, Roxana Lupu
Figure caption: The HCN production and precursor species after a (panel (a)) 6.3 × 1020 and (panel (b)) 2.5 × 1021 kg impactor. In both panels, (i) shows mixing ratios, while (ii) shows photolysis and reaction rates. Panel (b) contains haze aerosols that cause CH4 photolysis to be higher in the atmosphere compared to panel (a). High-altitude CH4 photolysis, closer to N2 photolysis, promotes HCN production because photolysis can more readily combine to make cyanides.
Paper: Origin-of-life Molecules in the Atmosphere after Big Impacts on the Early Earth
Authors: Nicholas F. Wogan, David C. Catling, Kevin J. Zahnle, Roxana Lupu
Figure caption: Earth and Titan photochemical model validation. Panels (a) and (b) show the Photochem model applied to Earth and Titan, respectively, compared to data from the literature (Ehhalt et al. 1975; Massie & Hunten 1981; Marten et al. 2002; Vuitton et al. 2006; Cui et al. 2009; Adriani et al. 2011).
Paper: Origin-of-life Molecules in the Atmosphere after Big Impacts on the Early Earth
Authors: Nicholas F. Wogan, David C. Catling, Kevin J. Zahnle, Roxana Lupu
Figure caption: Identical to Figure 7 in the main text but assumes postimpact H2 generation if governed by model 1B described in Figure 2.