adsabs/AstroCLIMB huggingface dataset:
Paper: An Automated Occultation Network for Gravitational Mapping of the Trans-Neptunian Solar System
Authors: Daniel C. H. Gomes, Gary M. Bernstein
Figure caption: Summaries of the per-occultation measurement errors (left) and total information (right) for an occultation survey targeting TNOs. All curves have the same meaning as for the MBA case in Figure 3, except that the color scales and axis limits are changed. These plots assume N = 100 telescopes spaced D = 100 km apart, a much larger array than considered for MBAs and TNOs in order to obtain sufficient occultations per TNO. Further commentary is in Section 3.6.
Paper: An Automated Occultation Network for Gravitational Mapping of the Trans-Neptunian Solar System
Authors: Daniel C. H. Gomes, Gary M. Bernstein
Figure caption: Lower bound on the uncertainty σM for a point source at 400 au as a function of its location in the sky. We use the Mollweide projection and ecliptic coordinates with the vernal equinox at center.
Paper: Polycyclic Aromatic Hydrocarbons as an Extraterrestrial Atmospheric Technosignature
Authors: Dwaipayan Dubey, Ravi Kopparapu, Barbara Ercolano, Karan Molaverdikhani
Figure caption: (a) Contrast difference with and without PAHs in the reflected spectra for an Earth-like exoplanet around a Sun-like star for different levels of PAHs in the planet atmosphere (orange: current Earth; magenta: two times current Earth; green: five times current Earth; and blue: 10 times current Earth). This is calculated for the 8 m mirror of the HWO telescope. The circles represent the wavelength bin points of the spectra. The difference in 0.2–0.225 μm is due to Naphthalene and the difference in 0.3–0.38 μm is due to the cumulative effect of Anthracene and Pyrene. The different legends represent the different concentrations of PAHs, scaled by a factor, on Earth's atmosphere. (b) Calculated SNRs for different PAH concentrations as a function of wavelength. This is done for a future HWO-like telescope for an observation time of 10 hr and a planet 10 pc away from Earth. In the legend, the net SNR is calculated following Equation (5). Similar to Figure 3(a), the circles represent the wavelength bin points of the SNRs. (c) Measured net SNR values as a function of total observation time using an HWO-like telescope. With 10 times the current Earth concentration of Naphthalene, Anthracene, Phenanthrene, and Pyrene, achieving a significant SNR is unachievable with the current setup.
Paper: Polycyclic Aromatic Hydrocarbons as an Extraterrestrial Atmospheric Technosignature
Authors: Dwaipayan Dubey, Ravi Kopparapu, Barbara Ercolano, Karan Molaverdikhani
Figure caption: (a) Cross sections of four different PAHs in the UV region (0.2–0.4 μm). On average, Naphthalene, Anthracene, and Pyrene have stronger cross sections among all four considered. (b) Collective cross sections of PAHs and other molecules on Earth (taken from R. Kopparapu et al. 2021) for the wavelength coverage of a nominal 8 m class HWO (0.2–2 μm). PAHs have stronger features than other molecules in this region. The region between 0.3 and 0.4 μm serves as a promising window for detecting PAHs due to it having the least overlap with other molecular cross sections.
Paper: Polycyclic Aromatic Hydrocarbons as an Extraterrestrial Atmospheric Technosignature
Authors: Dwaipayan Dubey, Ravi Kopparapu, Barbara Ercolano, Karan Molaverdikhani
Figure caption: Contributions of different anthropogenic sources to the net global PAH emission, including four major PAH-producing countries, in the year 2007 (H. Shen et al. 2013). The pie charts illustrate the total emissions for each country as a whole. These countries exemplify the conditions found in both developed and developing regions globally. Firewood and crop residue burning, deforestation/wildfires, and motor vehicles are the dominating source profiles across the globe.
Paper: Polycyclic Aromatic Hydrocarbons as an Extraterrestrial Atmospheric Technosignature
Authors: Dwaipayan Dubey, Ravi Kopparapu, Barbara Ercolano, Karan Molaverdikhani
Figure caption: Complete spectra of an Earth-like exoplanet with different PAH concentrations around a Sun-like star using HWO. Left: 1 ppb concentration for all PAHs. Right: 10 ppb concentration for all PAHs. The wavelength coverage of HWO is divided into three different channels with different resolutions: blue band—UV (R ~  7); green band—visible (R ~  140); and red band—NIR (R ~  70). The differences between the spectra are only limited to the UV region (0.2–0.4 μm), due to the unavailability of PAH cross sections.
Paper: Polycyclic Aromatic Hydrocarbons as an Extraterrestrial Atmospheric Technosignature
Authors: Dwaipayan Dubey, Ravi Kopparapu, Barbara Ercolano, Karan Molaverdikhani
Figure caption: (a) Contrast difference with and without PAHs. The circles represent the wavelength bin points of the spectra. (b) Net SNR as a function of observation time for different telescope architectures (orange—6 m; blue—8 m; and magenta—10 m). A larger diameter is suitable for reaching a higher SNR value with less observation time. However, with the current concentrations of Naphthalene, Anthracene, Phenanthrene, and Pyrene on Earth, none of the studied telescope diameters can resolve collective UV spectral features with a significant SNR value.
Paper: An Automated Occultation Network for Gravitational Mapping of the Trans-Neptunian Solar System
Authors: Daniel C. H. Gomes, Gary M. Bernstein
Figure caption: Light curves for the egress portion occultations of a point source by a spherical occulter of radius ρF,  where ﹩F=\sqrt{a\lambda /2}﹩ is the Fresnel scale. The horizontal axis can be considered either the distance from the geometric shadow edge (in units of F) or the time since the crossing of the geometric shadow edge (in units of tF = F/v⊥).
Paper: An Automated Occultation Network for Gravitational Mapping of the Trans-Neptunian Solar System
Authors: Daniel C. H. Gomes, Gary M. Bernstein
Figure caption: Fraction of the sky where the lower bound on σM lies below a given value. Dashed lines disregard the degeneracy of a Planet X tidal field with Kuiper Belt tidal-field uncertainties.
Paper: Saturnian Irregular Satellites as a Probe of Kuiper Belt Surface Evolution
Authors: Matthew Belyakov, Michael E. Brown
Figure caption: Top panel: comparison of the 3 μm feature on Phoebe (red), Siarnaq and Albiorix (orange), water-rich Centaurs (gray), and KBOs (blue) from Program 2418 (PI: N. Pinilla-Alonso). Phoebe’s 3 μm feature is similar to that of other water-rich KBO spectra, while Albiorix and Siarnaq are more similar to the most processed Centaurs, such as Okyrhoe. Bottom panel: comparison of the 3.0 μm feature across representative small bodies, Eurybates (green, +0.3 offset, from I. Wong et al. 2024), Themis (blue, +0.15 offset, from A. S. Rivkin & J. P. Emery 2010 and F. Usui et al. 2019), Siarnaq and Albiorix (orange), and the Neptune Trojan 2006 RJ103 (black, −0.2 offset, from L. Markwardt et al. 2023). The Jupiter Trojans and asteroid belt objects are distinct from the Saturnian irregulars, with significantly weaker 3.1 μm absorptions. The Neptune Trojan 2006 RJ103 has a deeper 3.0 μm band than the small Saturnian irregulars but also lacks water ice features at other wavelengths.
Paper: Saturnian Irregular Satellites as a Probe of Kuiper Belt Surface Evolution
Authors: Matthew Belyakov, Michael E. Brown
Figure caption: Relative reflectance spectra of the three largest Saturnian irregular satellites, Siarnaq, Albiorix, and Phoebe. The top panel shows the individual spectra of Albiorix and Siarnaq and their averaged spectrum, with Albiorix and Siarnaq offset down by 0.2 and 0.4, respectively. These two smaller, irregular satellites show a broad 3 μm absorption, a weak organic feature at 3.4 μm, and CO2 at 4.27 μm. The bottom panel shows the spectrum of Phoebe, combining the G235H and G395M exposures and binning down the G235H resolutions down by a factor of 3 to match the G395M resolution. Our spectrum matches results from Cassini VIMS with clear water ice and CO2 absorptions (R. N. Clark et al. 2005; W. C. Fraser & M. E. Brown 2018). The lack of evidence for water ice on the smaller Albiorix and Siarnaq distinguishes them from the water-rich Phoebe, indicating either the smaller irregular satellites were initially depleted of their water ice or that postcapture evolution removed the ice.
Paper: Saturnian Irregular Satellites as a Probe of Kuiper Belt Surface Evolution
Authors: Matthew Belyakov, Michael E. Brown
Figure caption: The left panels show the 3–4 μm spectra and polynomial continuum fits of Orus, Albiorix, Siarnaq, and Phoebe (from top to bottom). The red lines show the area ignored by the continuum fit, which is the same area used by I. Wong et al. (2024). The right panels show the continuum-subtracted spectrum, with Gaussian fits to the organic band. Both individually and in their average, the small Saturnian irregular satellites show organic bands that are consistent with what is seen on the Trojans but at slightly longer wavelength. Phoebe does not show strong evidence for an absorption in the 3.25–3.6 μm, obscured by the water-ice 3 μm feature, which makes determining a continuum difficult.
Paper: Saturnian Irregular Satellites as a Probe of Kuiper Belt Surface Evolution
Authors: Matthew Belyakov, Michael E. Brown
Figure caption: Continuum-removed CO2 feature on, from top to bottom, Jupiter Trojan Eurybates, Albiorix and Siarnaq, Phoebe, and the average spectrum of q < 25 au KBOs and Centaurs. The band center of the CO2 feature on Phoebe is similar to that of the Centaurs, indicating a common trapping mechanism, as pure CO2 ice is not stable at Saturnian temperatures. Both Phoebe and the KBOs have a shallower short-wavelength slope that is not present on the CO2 on the smaller irregular satellites. CO2 on Eurybates has a distinct 4.258 μm band center (I. Wong et al. 2024), possibly indicating that a different medium is trapping the CO2 on Eurybates or that the wavelengths are temperature dependent.
Paper: Saturnian Irregular Satellites as a Probe of Kuiper Belt Surface Evolution
Authors: Matthew Belyakov, Michael E. Brown
Figure caption: Comparison of the continuum-removed 2.0 μm feature on Phoebe (red), Siarnaq and Albiorix (orange), selected Centaurs and the Plutno 2004 EW95 from J. Licandro et al. (2024) and N. Pinilla-Alonso et al. (2025), and the Neptune Trojan 2006 RJ103 from L. Markwardt et al. (2023). Each spectrum below Phoebe is successively offset by 0.1 down in relative reflectance. All of the KBOs and Phoebe show 2.0 μm absorptions, ranging from 3.5% band depth on Okyrhoe to 9% on Chariklo. By contrast, Siarnaq and Albiorix, as well as 2006 RJ103, show no evidence for a 2.0 μm band, suggesting a lack of exposed water ice.
Paper: Saturnian Irregular Satellites as a Probe of Kuiper Belt Surface Evolution
Authors: Matthew Belyakov, Michael E. Brown
Figure caption: Average of Siarnaq and Albiorix spectra with a layer of 10 μm grain size crystalline water ice added using Hapke modeling (original dashed, with water in black). Adding water ice as a singular component to the irregular satellites in an areal mixture results in a spectrum that matches Okyrhoe (red), indicating the irregular satellites are consistent with having once had a water-ice-rich spectrum.
Paper: Equatorial CO2 Distribution Suggests Active CO2 Supply on Europa
Authors: Shintaro Kadoya, Yasuhito Sekine, Takanori Kodama
Figure caption: Probability of CO2’s location and state as a function of time. A hypothetical source of CO2 was set at 10°S, 75°W, and a threshold for latitude was arbitrarily set at 60°. Solid and dashed lines represent the probability that a CO2 molecule is located at latitudes of >60 ° and <60 °, respectively, while a dotted line represents the probability of photoionization and subsequent loss of CO2 molecules. Repeated sublimation gradually transported CO2 particles from low latitudes to high latitudes, as shown by a decrease in the dashed line and the complementary increase in the solid line. Subsequently, photoionization decreased the amount of CO2, as shown by a gradual increase in the dotted line. Since we conducted the MC sampling for more than 107 particles, the standard error for each line is smaller than the width of the line.
Paper: Equatorial CO2 Distribution Suggests Active CO2 Supply on Europa
Authors: Shintaro Kadoya, Yasuhito Sekine, Takanori Kodama
Figure caption: Latitudinal distribution of (a) diurnally averaged surface temperature, (b) initial speed, (c) transport angle, and (d) flight time (in blue) and residence time (in orange). In this study, residence time specifically refers to the duration between adsorption and subsequent sublimation, excluding ionization effects. In (a), the error bars show the minimum and maximum temperature observed by the Galileo spacecraft (J. A. Rathbun et al. 2010). In (b) and (d), the solid lines represent the averaged value, while the gray shaded regions represent 99.7% credible intervals. In (c), the solid line represents the average value, while the dashed line represents the 99.7th percentile. Also, the horizontal dashed line in (b) represents the escape velocity of Europa (∼2 km s−1).
Paper: Equatorial CO2 Distribution Suggests Active CO2 Supply on Europa
Authors: Shintaro Kadoya, Yasuhito Sekine, Takanori Kodama
Figure caption: Distribution of CO2 on Europa due to a continuous supply of CO2: (a) shows the steady-state distribution, while (b), (c), and (d) show the distribution after 1 day, 10 days, and 100 days of supply, respectively. A hypothetical source of CO2 was set at 10°S, 75°W, which is indicated by white diamonds. The subobserver point was set at 30°S, 90°W. See also Supplementary Figure 12.
Paper: Equatorial CO2 Distribution Suggests Active CO2 Supply on Europa
Authors: Shintaro Kadoya, Yasuhito Sekine, Takanori Kodama
Figure caption: Difference in CO2 distribution in a steady state with different loss rates or residence time. In (a) and (b), the CO2 loss rate (τphoto in Equation (27)) was assumed to be 100 times and 1000 times less than the case shown in Figure 4, respectively. On the other hand, in (c) and (d), the residence time of CO2 (τice,co2 in Equation (14)) was assumed to be 106 and 107 times larger than the case shown in Figure 4. See Figure 4 for further details. A shorter timescale of CO2 loss and/or a larger residence time of CO2 resulted in a higher concentration of CO2 around the hypothetical source of CO2, indicated by white diamonds (10°S, 75°W).
Paper: Equatorial CO2 Distribution Suggests Active CO2 Supply on Europa
Authors: Shintaro Kadoya, Yasuhito Sekine, Takanori Kodama
Figure caption: Effect of diurnal insolation change: (a) surface temperature and (b) sublimation rate of CO2 ice at a sub-Jupiter point as a function of time and (c) zonally averaged residence time as a function of latitude. Solid lines represent the cases where Dice (Equation (C3)) is 0.1 cm (dark blue), 1 cm (light blue), and 10 cm (orange). The black dotted line is an end-member case of Dice = 0. In contrast, the black dashed line corresponds to the diurnally averaged temperature (Equation (19)), representing another end-member case of Dice = ∞ (see also Figure 2). The black solid line represents the average flight time (see also Figure 2(d)). Due to the diurnal temperature change (a), the sublimation rate of CO2 ice (solid and dashed lines in (b)) tends to be several orders of magnitude higher than that for the averaged temperature case (dashed line in (b)). Accordingly, the effect of diurnal change decreases the average residence time of a CO2 molecule, as shown in (c).
Paper: Equatorial CO2 Distribution Suggests Active CO2 Supply on Europa
Authors: Shintaro Kadoya, Yasuhito Sekine, Takanori Kodama
Figure caption: Model of the observed distribution of CO2 based on our results shown in Figure 4. The resolution and the subobserver point are aligned with the JWST’s observation (2.7°N, 93°W; S. K. Trumbo & M. E. Brown 2023; G. Villanueva et al. 2023). Additionally, the cross section from the observer’s perspective is considered. As a result, the intensity around the north pole seems stronger than around the south pole (a). The regions surrounded by white lines are Tara Regio (∼10°S, 75°W) and Powys Regio (∼0°S, 150°W) (E. J. Leonard et al. 2024).
Paper: Equatorial CO2 Distribution Suggests Active CO2 Supply on Europa
Authors: Shintaro Kadoya, Yasuhito Sekine, Takanori Kodama
Figure caption: A CO2 molecule trapped in surface roughness. (a) Once a CO2 molecule is trapped in a pit, several sublimation events may be required before the particle escapes from the pit. (b) The average number of sublimation events before escaping from a pit as a function of the D/R ratio of a pit. Vertical lines represent the roughness observed by the Galileo spacecraft (G. Steinbrügge et al. 2020) and expected bladed roughness (D. E. Hobley et al. 2018). Considering the surface roughness, the residence time of CO2 could be roughly 10 times larger than our results shown in Figure 3.
Paper: Equatorial CO2 Distribution Suggests Active CO2 Supply on Europa
Authors: Shintaro Kadoya, Yasuhito Sekine, Takanori Kodama
Figure caption: Latitudinal distribution of CO2 molecules: (a) the 10 day case, (b) the 100 day case, and (c) the steady-state case correspond to Figures 4(c), (d), and (a), respectively. Black circles represent the estimated probability of a CO2 molecule being located at a latitude (θ) within a bin width of ﹩\Delta \sin \theta =0.002﹩. Gray shaded regions, which are so narrow that they are mostly overlapped by circles and dotted lines, indicate the 99.7% credible interval for each estimated probability. Vertical black dashed lines represent the specified timescales for each case.
Paper: Equatorial CO2 Distribution Suggests Active CO2 Supply on Europa
Authors: Shintaro Kadoya, Yasuhito Sekine, Takanori Kodama
Figure caption: Collision between molecules of CO2 and O2.
Paper: Improved Carbon and Nitrogen Isotopic Ratios for CH3CN in Titan’s Atmosphere Using ALMA
Authors: Jonathon Nosowitz, Martin A. Cordiner, Conor A. Nixon, Alexander E. Thelen, Zbigniew Kisiel, Nicholas A. Teanby, Patrick G. J. Irwin, Steven B. Charnley, Véronique Vuitton
Figure caption: Plot of the a priori (left) and corresponding retrieved profiles (right) to investigate the sensitivity of the retrieved CH3CN VMR to the shape of the a priori. The retrieved CH3CN VMR profile (black) is compared against retrievals using scaled versions of our default “Marten–Loison” profile (green and red profiles), the M. Dobrijevic & J. Loison (2018) model profile (cyan), and a log-linear gradient profile (magenta) from A. E. Thelen et al. (2019). The gray shaded region in the right panel is the error on the default CH3CN retrieved profile.
Paper: Improved Carbon and Nitrogen Isotopic Ratios for CH3CN in Titan’s Atmosphere Using ALMA
Authors: Jonathon Nosowitz, Martin A. Cordiner, Conor A. Nixon, Alexander E. Thelen, Zbigniew Kisiel, Nicholas A. Teanby, Patrick G. J. Irwin, Steven B. Charnley, Véronique Vuitton
Figure caption: Averaging kernels for the CH3CN major isotopologue, from our best-fitting NEMESIS model. The color bar shows the representative altitude applicable for each kernel. The altitudes with the largest values (∼150–300 km) indicate the region of highest sensitivity of our model.
Paper: A Direct Simulation Monte Carlo–Driven Photochemical Model of Callisto’s Ionosphere
Authors: Shane R. Carberry Mogan, Luke E. Moore, Lucas Liuzzo, Andrew R. Poppe
Figure caption: Results from photochemical models of Callisto’s ionosphere, with inputs taken from DSMC models of Callisto’s neutral atmosphere (Figure 3), which is ionized by interactions with photons and magnetospheric electrons with a number density of 1 cm−3 and a temperature of 40 eV at the top of the atmosphere. We also list the expected Juice C/A altitude (200 km) as well as the density and energy thresholds for its PEP/NIM instrument, ∼1 cm−3 and 10 eV, respectively.
Paper: A Direct Simulation Monte Carlo–Driven Photochemical Model of Callisto’s Ionosphere
Authors: Shane R. Carberry Mogan, Luke E. Moore, Lucas Liuzzo, Andrew R. Poppe
Figure caption: Results from our DSMC and photochemical models of Callisto’s atmosphere and ionosphere where only interactions with photons were considered at solar median and SZA = 0∘ (red) and 90∘ (blue) are compared to the results of the photochemical model of M.-C. Liang et al. (2005), “L05,” at solar maximum and SZA = 80∘ (green). Number density profiles are plotted for O2 (top left panel), CO2 (top center panel), O (top right panel), O﹩{}_{2}^{+}﹩ (bottom left panel), CO﹩{}_{2}^{+}﹩ (bottom center panel), and O+ (bottom right panel).
Paper: A Direct Simulation Monte Carlo–Driven Photochemical Model of Callisto’s Ionosphere
Authors: Shane R. Carberry Mogan, Luke E. Moore, Lucas Liuzzo, Andrew R. Poppe
Figure caption: Maxwellian energy distributions for magnetospheric electrons with upstream temperatures of 40 eV (top) and 400 eV (bottom), calculated as a function of radial altitude above Callisto’s surface based on the energy deposited in the atmosphere.
Paper: A Direct Simulation Monte Carlo–Driven Photochemical Model of Callisto’s Ionosphere
Authors: Shane R. Carberry Mogan, Luke E. Moore, Lucas Liuzzo, Andrew R. Poppe
Figure caption: Electron-impact ionization cross sections (y-axis) for H (red) and O (blue) as a function of energy (x-axis). These electron-impact cross sections are taken from S. R. Carberry Mogan et al. (2023a).
Paper: A Direct Simulation Monte Carlo–Driven Photochemical Model of Callisto’s Ionosphere
Authors: Shane R. Carberry Mogan, Luke E. Moore, Lucas Liuzzo, Andrew R. Poppe
Figure caption: The ratio of the number density of electrons that reach the surface without depositing all of their energy compared to the number density of electrons at the top of the atmosphere according to an initial temperature of 40 eV (red) and 400 eV (blue).
Paper: A Direct Simulation Monte Carlo–Driven Photochemical Model of Callisto’s Ionosphere
Authors: Shane R. Carberry Mogan, Luke E. Moore, Lucas Liuzzo, Andrew R. Poppe
Figure caption: Collision cross sections for electrons impacting CO2 (y-axis) as a function of energy (x-axis). These electron-impact cross sections are taken from Y. Itikawa (2002).
Paper: A Direct Simulation Monte Carlo–Driven Photochemical Model of Callisto’s Ionosphere
Authors: Shane R. Carberry Mogan, Luke E. Moore, Lucas Liuzzo, Andrew R. Poppe
Figure caption: Collision cross sections for electrons impacting H2 (y-axis) as a function of energy (x-axis). These electron-impact cross sections are taken from the following references: S. R. Carberry Mogan et al. (2023a) for e + H2 →  H﹩{}_{2}^{+}﹩ + 2e, L. H. Scarlett et al. (2018) for e + H2 →  2H + e, and H. C. Straub et al. (1996) for e + H2 →  H + H+ + 2e.
Paper: A Direct Simulation Monte Carlo–Driven Photochemical Model of Callisto’s Ionosphere
Authors: Shane R. Carberry Mogan, Luke E. Moore, Lucas Liuzzo, Andrew R. Poppe
Figure caption: Collision cross sections for electrons impacting O2 (y-axis) as a function of energy (x-axis). These electron-impact cross sections are taken from the following references: S. R. Carberry Mogan et al. (2023a) for e + O2 →  O﹩{}_{2}^{+}﹩ + 2e, H. C. Straub et al. (1996) for e + O2 →  O + O+ + 2e, and P. C. Cosby (1993) for e + O2 →  2O + e.
Paper: A Direct Simulation Monte Carlo–Driven Photochemical Model of Callisto’s Ionosphere
Authors: Shane R. Carberry Mogan, Luke E. Moore, Lucas Liuzzo, Andrew R. Poppe
Figure caption: Collision cross sections for electrons impacting CO (y-axis) as a function of energy (x-axis). These electron-impact cross sections are taken from Y. Itikawa (2015).
Paper: A Direct Simulation Monte Carlo–Driven Photochemical Model of Callisto’s Ionosphere
Authors: Shane R. Carberry Mogan, Luke E. Moore, Lucas Liuzzo, Andrew R. Poppe
Figure caption: Results from photochemical models of Callisto’s ionosphere, with inputs taken from DSMC models of Callisto’s neutral atmosphere (Figure 3), which is ionized by interactions with photons and magnetospheric electrons with a number density of 1 cm−3 and a temperature of 400 eV at the top of the atmosphere. We also list the expected Juice C/A altitude (200 km) as well as the density and energy thresholds for its PEP/NIM instrument, ∼1 cm−3 and 10 eV, respectively.