adsabs/AstroCLIMB huggingface dataset:
Paper: A Complex Systems Approach to Exoplanet Atmospheric Chemistry: New Prospects for Ruling Out the Possibility of Alien Life As We Know It
Authors: Theresa Fisher, Estelle Janin, Sara Imari Walker
Figure caption: Ranked edge weights of each species in the biotic model, calculated by taking the average of edge weights for each node and then averaging that value over the entire ensemble. The black dashed line is the average of these values for all nodes when the fictitious species are present, and the red dashed line is the average of these values for all nodes without the fictitious species. The inclusion of the fictitious species H4 and H4CO2 (outlined by the red box) minimally affects average network statistics computed from edge weights.
Paper: A Complex Systems Approach to Exoplanet Atmospheric Chemistry: New Prospects for Ruling Out the Possibility of Alien Life As We Know It
Authors: Theresa Fisher, Estelle Janin, Sara Imari Walker
Figure caption: Number of edges for each species. The black dashed line is the average of these values for all nodes when the fictitious species are present, and the red dashed line is the average of these values for all nodes without the fictitious species. H4 and H4CO2 (outlined by the red boxes) both have comparatively few edges, and their presence or absence does not affect average values.
Paper: A Complex Systems Approach to Exoplanet Atmospheric Chemistry: New Prospects for Ruling Out the Possibility of Alien Life As We Know It
Authors: Theresa Fisher, Estelle Janin, Sara Imari Walker
Figure caption: Top: abundance of important atmospheric species as a function of scale height for each modeled scenario. Bottom: the temperature profile as a function of scale height. All the Archean Earth model scenarios are characterized by the same temperature–pressure profile from G. Arney et al. (2016)—here, output of the converged atmos simulations.
Paper: A Complex Systems Approach to Exoplanet Atmospheric Chemistry: New Prospects for Ruling Out the Possibility of Alien Life As We Know It
Authors: Theresa Fisher, Estelle Janin, Sara Imari Walker
Figure caption: P(observation) of given values of CH4 abundance in log ppm.
Paper: A Complex Systems Approach to Exoplanet Atmospheric Chemistry: New Prospects for Ruling Out the Possibility of Alien Life As We Know It
Authors: Theresa Fisher, Estelle Janin, Sara Imari Walker
Figure caption: P(observation) of given values of log average clustering coefficient.
Paper: A Complex Systems Approach to Exoplanet Atmospheric Chemistry: New Prospects for Ruling Out the Possibility of Alien Life As We Know It
Authors: Theresa Fisher, Estelle Janin, Sara Imari Walker
Figure caption: P(observation) of given values of log average shortest path length.
Paper: A Complex Systems Approach to Exoplanet Atmospheric Chemistry: New Prospects for Ruling Out the Possibility of Alien Life As We Know It
Authors: Theresa Fisher, Estelle Janin, Sara Imari Walker
Figure caption: P(observation) of given values of log mean degree.
Paper: A Complex Systems Approach to Exoplanet Atmospheric Chemistry: New Prospects for Ruling Out the Possibility of Alien Life As We Know It
Authors: Theresa Fisher, Estelle Janin, Sara Imari Walker
Figure caption: Bayesian analysis of the posterior likelihood of life, P(life|observation), assuming an observed value for network metrics and methane gas abundance, probed at 1 mbar. Given that the probability for life to exist on an exoplanet is unknown, we assess the posterior likelihood over a range of prior probabilities for life, P(life). Gray regions highlight metric values that are associated with a zero probability of life and are therefore antibiosignatures for the sets of models compared herein. In general, the subset of network metrics studied here can provide greater constraints on the probability of life given a set of observations than CH4 abundance alone, allowing distinguishing cases where Earth-like methanogenesis can be ruled out even when CH4 abundance alone is not conclusive.
Paper: A Complex Systems Approach to Exoplanet Atmospheric Chemistry: New Prospects for Ruling Out the Possibility of Alien Life As We Know It
Authors: Theresa Fisher, Estelle Janin, Sara Imari Walker
Figure caption: Distributions of the probability (y-axis) of a simulated atmosphere yielding the given network metric value, species abundance variance, or CH4 abundance in log ppm (x-axis) over each of the sampled Archean Earth data sets, probed at 1 mbar. Brown represents models where methane is modeled as an abiotic surface flux. Green represents models where methane is modeled as a biotic surface flux, with the methanogenesis pathway explicitly included in the CRN. Purple represents models where methane was modeled as originating from a surface flux of undetermined origin (“anomalous surface flux”). Yellow represents models where methane is modeled as an anomalous steady-state component of the planet’s atmosphere with an unknown source.
Paper: A Complex Systems Approach to Exoplanet Atmospheric Chemistry: New Prospects for Ruling Out the Possibility of Alien Life As We Know It
Authors: Theresa Fisher, Estelle Janin, Sara Imari Walker
Figure caption: P(observation) of given values of log average neighbor degree.
Paper: A Complex Systems Approach to Exoplanet Atmospheric Chemistry: New Prospects for Ruling Out the Possibility of Alien Life As We Know It
Authors: Theresa Fisher, Estelle Janin, Sara Imari Walker
Figure caption: Anderson scores of the biotic flux scenario as compared to the three control models (abiotic flux, anomalous surface flux, and anomalous steady state) for CRN outputs probed at 0.2 mbar and 1 mbar (see legend). Each bar indicates the performance of the corresponding metric in distinguishing between different modeled scenarios. The black horizontal dotted line indicates the critical value for distinguishability between model scenarios at a 0.1% significance level, and the blue vertical dotted line separates the network metrics from CH4 abundance and global species abundance variance.
Paper: A Complex Systems Approach to Exoplanet Atmospheric Chemistry: New Prospects for Ruling Out the Possibility of Alien Life As We Know It
Authors: Theresa Fisher, Estelle Janin, Sara Imari Walker
Figure caption: The temperature profile as a function of scale height, input for the modern Earth simulations, adopted from the NASA Frontiers Development Lab. All modern Earth model scenarios use the same temperature–pressure profile in this study.
Paper: A Complex Systems Approach to Exoplanet Atmospheric Chemistry: New Prospects for Ruling Out the Possibility of Alien Life As We Know It
Authors: Theresa Fisher, Estelle Janin, Sara Imari Walker
Figure caption: P(observation) of given values of log edge betweenness centrality.
Paper: A Complex Systems Approach to Exoplanet Atmospheric Chemistry: New Prospects for Ruling Out the Possibility of Alien Life As We Know It
Authors: Theresa Fisher, Estelle Janin, Sara Imari Walker
Figure caption: P(observation) of given values of log node betweenness centrality.
Paper: The Spin Zone: Synchronously and Asynchronously Rotating Land Planets Have Spectral Differences in Transmission
Authors: Nicholas Scarsdale, C. E. Harman, Thomas J. Fauchez
Figure caption: The spectra of each instantiation of our simulation with the optical and spectral effects of clouds removed. As in Figure 4, each box shows the synchronous and 1 day rotator cases for different instellation values, which are printed in the legend. Despite the absence of clouds, visible (though smaller) differences persist in the spectra of less-irradiated models.
Paper: The Spin Zone: Synchronously and Asynchronously Rotating Land Planets Have Spectral Differences in Transmission
Authors: Nicholas Scarsdale, C. E. Harman, Thomas J. Fauchez
Figure caption: The standard deviation of the transit depth in the 1.8 μm bandpass for monthly cadence simulations over 2 yr.
Paper: Activity of Halley-type Comets 12P/Pons–Brooks and 13P/Olbers from SOHO/SWAN Observations
Authors: M. R. Combi, T. Mäkinen, J.-L. Bertaux, E. Quémerais, S. Ferron
Figure caption: Water production rate of comet 12P as a function of time from perihelion in days deconvolved to the production time of water at the nucleus. The triangles give the water production rate per second. The error bars give the 1σ fitting errors for each value, which are much larger because of the deconvolution procedure. There is also an overall ∼30% uncertainty from the model parameters and calibration. The peaks of eight individual outbursts, determined to the nearest day, are noted. The durations of the outbursts are given in Table 3. The filled squares are values from IR observations by E. Gibb et al. (2025, private communication), and the filled diamond is from ALMA observations by M. Cordiner et al. (2025, private communication). The crosses are from J. Li et al. (2025). The filled circles are from E. Jehin et al. (2024a, 2024b). The filled triangles are from L. Ferellec et al. (2024).
Paper: Activity of Halley-type Comets 12P/Pons–Brooks and 13P/Olbers from SOHO/SWAN Observations
Authors: M. R. Combi, T. Mäkinen, J.-L. Bertaux, E. Quémerais, S. Ferron
Figure caption: Active area of comet 12P as a function of time in days from perihelion. The water production rate gives the active area in square kilometers assuming the fast rotator model of J. J. Cowan & M. F. A’Hearn (1979). The short vertical lines show the peak times of the numbered outbursts shown in Figure 3 and given in Table 3. The lower solid horizontal line is the active area for a nucleus with a radius of 1.26 km, which would correspond to the smallest possible 100% active nucleus radius. The upper horizontal line corresponds to a 100% active nucleus of 5.6 km radius (D. Jewitt & J. Luu 2025). The middle solid horizontal line gives the calculated active area for a 100% active nucleus of radius 2.2 km from the early preperihelion activity given as the minimum possible size by J. Li et al. (2025).
Paper: Activity of Halley-type Comets 12P/Pons–Brooks and 13P/Olbers from SOHO/SWAN Observations
Authors: M. R. Combi, T. Mäkinen, J.-L. Bertaux, E. Quémerais, S. Ferron
Figure caption: Water production rate of comet 12P as a function of time from perihelion. The open symbols give the water production rate per second from single images, where diamonds are preperihelion and squares are postperihelion. The error bars give the 1σ formal random fitting errors for each value. There is a potential ∼30% uncertainty from the model parameters and calibration not included in the plotted error bars.
Paper: Activity of Halley-type Comets 12P/Pons–Brooks and 13P/Olbers from SOHO/SWAN Observations
Authors: M. R. Combi, T. Mäkinen, J.-L. Bertaux, E. Quémerais, S. Ferron
Figure caption: Water production rate in comet 12P as a function of heliocentric distance, with preperihelion to the left and postperihelion to the right. Crosses give the water production rate per second from single images. The error bars give the 1σ formal random fitting errors for each value. There is an additional ∼30% uncertainty from the model parameters and calibration. The solid lines give the best-fit power laws with slopes of −2.5 and −2.9 pre- and postperihelion, respectively.
Paper: Activity of Halley-type Comets 12P/Pons–Brooks and 13P/Olbers from SOHO/SWAN Observations
Authors: M. R. Combi, T. Mäkinen, J.-L. Bertaux, E. Quémerais, S. Ferron
Figure caption: Water production rate of comet 13P as a function of heliocentric distance (au). The diamonds give the water production rates before perihelion, and the squares give the values after perihelion. Although the power-law fits are not very meaningful, the dashed line gives the fit of a slope of +0.1 before perihelion and the dashed–dotted line a slope of –0.7 after to show the trends. See the caption in Figure 5 for the uncertainties and the text for discussion.
Paper: Activity of Halley-type Comets 12P/Pons–Brooks and 13P/Olbers from SOHO/SWAN Observations
Authors: M. R. Combi, T. Mäkinen, J.-L. Bertaux, E. Quémerais, S. Ferron
Figure caption: Water production rate of comet 13P as a function of time from perihelion. The diamonds give the water production rate per second from single images. The error bars give the 1σ formal random fitting errors for each value. There is a potential ∼30% uncertainty from the model parameters and calibration.
Paper: A Catalogue of Interstellar Material Delivery from Nearby Debris Disks
Authors: Cole R. Gregg, Paul A. Wiegert
Figure caption: This is a zoomed-in version of the radiant plot in Figure 2, focusing on the direction in which 1I/’Oumuamua arrived. HD 38858 and HD 166 are the only systems plotted, to show the comparison in the radiant of their particles’ arrival directions. These particles are colored by their arrival velocity v∞.
Paper: A Catalogue of Interstellar Material Delivery from Nearby Debris Disks
Authors: Cole R. Gregg, Paul A. Wiegert
Figure caption: The top panel shows the expected current population of ≥100 m particles in the inner solar system. The bottom panel is the current flux of ≥200 μm particles at Earth.
Paper: The Geology of a Small Main-belt S-class Binary Asteroid System: Dinkinesh and Its Contact Binary Satellite Selam as Observed by the Lucy Mission
Authors: E. B. Bierhaus, S. Marchi, S. J. Robbins, S. Mottola, W. F. Bottke, K. Noll, J. F. Bell III, J. M. Sunshine, J. Spencer, D. Britt, H. Levison, F. Preusker, C. Howett, M. Hirabayshi
Figure caption: The phase angle α vs. pixel scale for L’LORRI images acquired from −1.83 hr through +1.99 hr relative to closest approach. Data are derived from the predicted trajectory. Arrows indicate the direction of the spacecraft relative to closest approach. The light-gray box identifies the parameter space for pixel scale ≤5 m pixel−1, and 40° ≤ α ≤ 90°, which is the preferred range for making measurements of surface features.
Paper: The Geology of a Small Main-belt S-class Binary Asteroid System: Dinkinesh and Its Contact Binary Satellite Selam as Observed by the Lucy Mission
Authors: E. B. Bierhaus, S. Marchi, S. J. Robbins, S. Mottola, W. F. Bottke, K. Noll, J. F. Bell III, J. M. Sunshine, J. Spencer, D. Britt, H. Levison, F. Preusker, C. Howett, M. Hirabayshi
Figure caption: The Dinkinesh shape model used in this paper. The lighter-gray region is the shape derived from Lucy images when the object was resolved, and the darker shade is the shape derived from other techniques (see text). The top row, from left to right, shows views from the +x-, +y-, and +z-directions. The bottom row, from left to right, shows views from the −x-, −y-, and −z-directions.
Paper: The Geology of a Small Main-belt S-class Binary Asteroid System: Dinkinesh and Its Contact Binary Satellite Selam as Observed by the Lucy Mission
Authors: E. B. Bierhaus, S. Marchi, S. J. Robbins, S. Mottola, W. F. Bottke, K. Noll, J. F. Bell III, J. M. Sunshine, J. Spencer, D. Britt, H. Levison, F. Preusker, C. Howett, M. Hirabayshi
Figure caption: Representative L’LORRI images of Dinkinesh and Selam. North is approximately up in both images. (a) L’LORRI image lor_0752129545_03599, taken 1.2 minutes before closest approach. Range is 528 km, pixel scale is 2.6 m pixel−1, and phase is 66°. The scale bar indicates approximately 100 m. (b) L’LORRI image lor_0752129617_03613, taken within a few seconds of closest approach. Range is 425 km, pixel scale is 2.1 m pixel−1, and phase is 29°. Dinkinesh is in the foreground, and Selam is in the background. The view of Selam is nearly parallel to the long axis of the bilobed body, meaning that Selam’s Dinkinesh-facing lobe almost entirely obscures the anti-Dinkinesh lobe.
Paper: The Geology of a Small Main-belt S-class Binary Asteroid System: Dinkinesh and Its Contact Binary Satellite Selam as Observed by the Lucy Mission
Authors: E. B. Bierhaus, S. Marchi, S. J. Robbins, S. Mottola, W. F. Bottke, K. Noll, J. F. Bell III, J. M. Sunshine, J. Spencer, D. Britt, H. Levison, F. Preusker, C. Howett, M. Hirabayshi
Figure caption: Sumak Fossa, the major trough on Dinkinesh. In all panels, north is approximately up. (a) Image lor_ 0752129497_ 03589, taken during approach at ∼80° phase and 3.3 m pixel−1. This version is unannotated to show all features, including the “valley-like” morphology of Sumak Fossa at high southern latitudes. From this perspective the view looks nearly straight through the deep trough. (b) The same image as panel (a), with orange outlines to demark the boundaries of Sumak Fossa, which crosses the body at mid-latitudes in the north and close to the pole in the south. (c) Image lor_ 0752129617_ 03613, taken during approach at ∼28° phase and 2.1 m pixel−1. The image is rendered on the shape model to illustrate the relative locations of Sumak Fossa seen from the eastern (∼approach) hemisphere. The blue and yellow lines trace the approximate path of Sumak Fossa in the northern and southern hemispheres, respectively. (d) Image lor_ 0752129707_ 03631, taken during departure at ∼15° phase and 2.9 m pixel−1. This view provides among the highest-resolution views of the western side of Sumak Fossa. Here, too, the image is rendered on the shape model. In addition to the blue and yellow lines that trace the feature, the colored arrows point to transitions in the morphology of the feature as it arcs back toward the equator. The light-blue arrow points to the northern boundary of a depression that may be distinct from Sumak Fossa. The gold and light-yellow arrows point to the parts of southern Sumak Fossa that have different widths and depths. Panels (e) and (f) are images lor_ 0752129722_ 03634 and lor_ 0752129827_ 03655, departure images acquired at ∼19° phase and 3.2 m pixel−1 and at ∼37° phase and 5.1 m pixel−1, respectively. The arrows point to the same features as in panel (d).
Paper: The Geology of a Small Main-belt S-class Binary Asteroid System: Dinkinesh and Its Contact Binary Satellite Selam as Observed by the Lucy Mission
Authors: E. B. Bierhaus, S. Marchi, S. J. Robbins, S. Mottola, W. F. Bottke, K. Noll, J. F. Bell III, J. M. Sunshine, J. Spencer, D. Britt, H. Levison, F. Preusker, C. Howett, M. Hirabayshi
Figure caption: The measured Dinkinesh crater population. (a) The spatial distribution of the craters, colorized by category (see label in panel (b)). The light-gray regions are approximately the unilluminated surfaces not seen during the flyby. The actual dawn and dusk terminators are irregular owing to surface topography and span a range of ∼10°–15° longitude, depending on latitude. Panels (b), (c), and (d) are the cumulative, differential, and relative versions of the crater SFD, respectively. Error bars are Poisson sqrt-N. The black data are for all data, and the individual colors correspond to each category as noted by the figure legend in panel (b). Panels (e) and (f) are the Dinkinesh category 1–3 craters on the approach and departure hemispheres, respectively (compare with panel (a)), and rendered on the shape model. The two LORRI images used for these panels are lor_0752129617_03613 and lor_0752129707_03631. (g) The three category 1 craters on Selam, LORRI image lor_0752129590_03608.
Paper: The Geology of a Small Main-belt S-class Binary Asteroid System: Dinkinesh and Its Contact Binary Satellite Selam as Observed by the Lucy Mission
Authors: E. B. Bierhaus, S. Marchi, S. J. Robbins, S. Mottola, W. F. Bottke, K. Noll, J. F. Bell III, J. M. Sunshine, J. Spencer, D. Britt, H. Levison, F. Preusker, C. Howett, M. Hirabayshi
Figure caption: The measured Dinkinesh boulder population. (a) The spatial distribution of the category 1 boulder population. The light-gray regions are approximately the unilluminated surfaces not seen during the flyby. The actual dawn and dusk terminators are irregular owing to surface topography and span a range of ∼10°–15° longitude, depending on latitude. The red boulder is Totoka Saxum, the reference boulder that defines the prime meridian for the Dinkinesh coordinate system. Panels (b), (c), and (d) are the cumulative, differential, and relative versions of the boulder SFD, respectively. Error bars are Poisson sqrt-N. The black data are the unmerged combination of the two different datasets. The blue data are the merged category 1 population (plotted in panel (a)), and the orange data are category 2. The solid line in panel (c) is a weighted, least-squares fit to the category 1 data.
Paper: The Geology of a Small Main-belt S-class Binary Asteroid System: Dinkinesh and Its Contact Binary Satellite Selam as Observed by the Lucy Mission
Authors: E. B. Bierhaus, S. Marchi, S. J. Robbins, S. Mottola, W. F. Bottke, K. Noll, J. F. Bell III, J. M. Sunshine, J. Spencer, D. Britt, H. Levison, F. Preusker, C. Howett, M. Hirabayshi
Figure caption: Sumak Fossa width and depth measurements. Panels (a)–(c) illustrate the locations of six profiles across Sumak Fossa. Each profile has a specific color that is consistent across the panels in this figure. The numbers are not sequential because we discarded some profiles owing to larger error. The unprimed and primed versions of the profile number indicate the profile direction (generally left to right) shown in subsequent panels. (a) Profiles 1–3 are in the northeastern hemisphere. (b) Profile 5 is in the southeastern hemisphere. (c) Profiles 6 and 7 are in the southwestern hemisphere. (d–i) The geometric height (hgeom) vs. distance for each profile after a linear detrending of the geometric height. The gray bands bounding each profile are the 1σ radial errors of the profile. (j) The profiles in panels (d)–(i) replotted with normalized distances, highlighting the unique depth of profile 7. (f) The depth/width ratio of each profile, labeled by profile number, and with colors consistent with panels (d)–(i). Error bars are derived from the propagation of errors for the depth and width measurements.
Paper: The Geology of a Small Main-belt S-class Binary Asteroid System: Dinkinesh and Its Contact Binary Satellite Selam as Observed by the Lucy Mission
Authors: E. B. Bierhaus, S. Marchi, S. J. Robbins, S. Mottola, W. F. Bottke, K. Noll, J. F. Bell III, J. M. Sunshine, J. Spencer, D. Britt, H. Levison, F. Preusker, C. Howett, M. Hirabayshi
Figure caption: Crater depth-to-diameter (d/D) ratios for three of the best-resolved craters. Panels (a)–(c) are profiles of geometric height; each panel is the same scale to visually preserve the relative differences in diameter and depth between craters. The height is the solid line, which is bounded by a gray band that represents the 1σ radial error for each shape model facet in the profile. (d) The d/D values for the three craters as a function of D. The colors correspond to the profile colors in panels (a)–(c). (e) The location of the profiles on the body. The crater number and the primed number indicate the direction of the profiles in panels (a)–(c).
Paper: The Geology of a Small Main-belt S-class Binary Asteroid System: Dinkinesh and Its Contact Binary Satellite Selam as Observed by the Lucy Mission
Authors: E. B. Bierhaus, S. Marchi, S. J. Robbins, S. Mottola, W. F. Bottke, K. Noll, J. F. Bell III, J. M. Sunshine, J. Spencer, D. Britt, H. Levison, F. Preusker, C. Howett, M. Hirabayshi
Figure caption: Views of Dinkinesh and Fab Dorsum, the equatorial ridge, throughout the encounter. The images selected are approximately 20° steps in phase angle, with some variation given the availability of images across the phase angles observed during the encounter, and to avoid saturated images. (For example, the images around 0° have significant saturation.) Blue and gold arrows point to the approximate northern and southern boundaries, respectively, of Fab Dorsum. Panels (a)–(d) are from the approach; panels (e) and (f) are from departure. Phase angles and pixel scales are derived from the predicted trajectory. (a) Image lor_ 0752129482_ 03586. (b) Image lor_ 0752129557_ 03601. (c) Image lor_ 0752129602_ 03610; Selam is visible in the upper right corner. (d) Image lor_ 0752129632_ 03616. (e) Image lor_ 0752129722_ 03634. (f) Image lor_ 0752129872_ 03664.