adsabs/AstroCLIMB huggingface dataset:
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 cumulative crater SFD for (a) all Dinkinesh craters and (b) only category 1 craters, with best-fit production functions that provide model crater ages (red lines). In panel (a), the solid red line is a fit to all craters >45 m diameter, and the dashed red line is a fit to all craters >110 m diameter. In panel (b), the red line is a fit to all craters ≥60 m diameter.
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: Polar views of Dinkinesh. Two images are projected on the shape model, lor_0752129617_03613 and lor_0752129707_03631. Panels (a) and (b) are the south pole and north pole, respectively. The dashed lines indicate the approximate boundaries of Sumak. In panel (b), the light-blue dotted lines indicate a depression that starts at the mid-latitudes and extends to the equatorial region, and it appears to be distinct from Sumak Fossa.
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: All Dinkinesh craters (black points) with the Selam craters (light-blue points) and the best-fit production function to the Selam 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: Dinkinesh interior strengths needed to prevent rotational failure for different rotation periods and body dimensions. The plot legends are in Pa. Note that these values reflect stresses created by rotation and are not the interior strength distribution. Panel labels are in the lower left corner. Panels (a)–(h) use the current body dimensions for Dinkinesh. Panels (i)–(l) use a hypothetical shape that has smaller equatorial dimensions and a larger vertical dimension, which simulates a potential configuration prior to mass shedding and flattening from YORP failure. The current Dinkinesh spin period is 3.7387 hr, panels (g) and (k). The red contour represents the 0 Pa boundary; inside the red contour, though, the body does not require any strength to maintain its shape at that spin rate.
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: Images of Selam and resolved surface features; north is approximately up in all images. (a) Image lor_0752129497_03589, taken during approach. Arrows identify Piękna Lobus and Lewa Lobus. Piękna Lobus is closest to Dinkinesh, which is to the left in this view. Lewa Lobus is almost completely shadowed by Piękna. (b) Portion of image lor_0752129590_03608. In this view Piękna Lobus is in the foreground and Lewa Lobus is in the background. (c) Portion of image lor_0752129617_03613, which is one of the last views of Selam before Selam leaves the L’LORRI FOV for a time around closest approach. The yellow arrows point to a broadening of the base of Uwoduhi Dorsum. The object in the lower right corner of this panel is Dinkinesh. (d) Portion of image lor_0752129947_03679, which is the first image after closest approach that fully contains Selam. (A short series of earlier images contain partial views of Selam.) Arrows identify Piękna Lobus and Lewa Lobus to clarify that the viewing geometry is “from the other side” compared with panel (a); in this view Dinkinesh is to the right. (e) A zoom-in of Selam from panel (d). Dotted purple lines note aspects of Piękna Lobus: the right-hand profile of Piękna is nearly planar, though slightly concave; near the contact with Lewa there is a linear feature. A white dotted “V”-shaped depression occupies roughly the middle third of Lewa Lobus. The white arrow points to a thin, approximately linear feature that marks the end of Lewa Lobus. This feature is approximately parallel to the Dinkinesh-facing edge of Piękna. (f) The same as panel (b), but with additional annotation. The green dashed line marks Uwoduhi Dorsum. The yellow dotted lines identify linear features on Piękna.
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: Examples of downslope movement on Dinkinesh. (a) Context view from lor_0752129557_03601; the white square outlines the region shown in panel (b). (b) A contrast stretch that enhances the visibility of two regions of downslope movement. The purple arrows point to a curvilinear feature on the flank of Fab Dorsum; the rust-colored arrows point to material that appears to be slumping from Bella Dorsum. (c) The Dinkinesh shape model colorized by geopotential elevation, with purple and rust-colored arrows pointing to approximately the same locations as in panel (b), illustrating that the location and apparent direction of material are consistent with moving in the local downhill direction. (d) Image lor_0752129722_03634. The white arrows point to apparent downslope movement inside Sumak Fossa. The light-green arrow points to a portion of the body that is just emerging into view during departure. (e) Image lor_0752129905_03671. The white and green arrows point to the same features as in panel (d). Though lower resolution, the feature identified by the green arrow is clearly separated from the foreground of the body by a depression.
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: Fab Dorsum height and width measurements, and examples of derived cross-sectional areas for Fab Dorsum. (a) Fab Dorsum height and width values across observed longitudes. (b–f) The profiles are a representative subset of the geometric profiles in Figure 12. The dashed and solid blue lines are the longitudinal profile and the Fab Dorsum portion, respectively. The black line connects the northern and southern boundaries of Fab Dorsum in each profile, and the light-blue shaded region is the cross-sectional area of Fab Dorsum for that profile.
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: Bella Dorsum from multiple views throughout the flyby; north is approximately up in all panels. The blue and gold arrows point to the northern and southern arcs, respectively. Each panel includes the phase angle and pixel scale of the image shown. The images are (a) lor_0752129572_03604; (b) lor_0752129590_03608; (c) lor_0752129617_03613, with Selam visible behind Dinkinesh; (d) lor_0752129647_03619; (e) lor_0752129722_03634; and (f) lor_0752129827_03655.
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: Detrended longitudinal profiles of Fab Dorsum. The blue line is the geometric height; the green circle marks the peak geometric height of the profile. The orange line is the geopotential height; the red circle marks the minimum geopotential height of the profile. Each panel includes the average geopotential slope (i.e., the slope of the orange line) between the latitudes spanned by the green and red circles.
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: Detrended geometric height profiles of Bella Dorsum. Panels (a)–(g) are profiles across the northern arc. (h) The location of the profiles using image lor_0752129617_03613 projected onto the shape model. Panel (a) notes the direction of the profiles relative to panel (h): all profiles start on the side closest to the limb and move inward.
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: YORP spin-up and collisional timescales. (a) The two blue curves correspond to the minimum and maximum YORP spin-up time for asteroids with the same bulk density and semimajor axis as Dinkinesh. (b) The red curve is the estimated asteroid collisional lifetime in the main belt, as a function of diameter. The collisional lifetime for Dinkinesh is ∼10 times greater than the YORP spin-up time, consistent with the expectation that Dinkinesh has had time to spin up to failure at least once, and potentially several times.
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 largest of the most recent troughs, Indah Fossa. Dinkinesh north is approximately up in both panels. (a) Multiple white arrows indicate the feature as seen in the unprojected L’LORRI image lor_0752129617_03613. (b) The same L’LORRI image projected onto the shape model; the thick white line is a mapping of the feature on the shape model using SBMT.
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: Plane fits to Dinkinesh structural features. (a) Separate fits to the northern and southern portions of Sumak Fossa, with Dinkinesh rendered at +45° in the (x, y)-plane, a view seen during approach. (b) The same as in panel (a), except rendered at −45° in the (x, y)-plane, a view seen during departure. (c) A view from above the north pole showing the plane fits for Sumak north and south, as well as the plane fit for Bella Dorsum. From this perspective the Bella Dorsum plane essentially appears as a line. The planes for north and south Sumak are cropped to keep all elements visible. (d) The Bella Dorsum plane fit alone, rendered at +45° in the (x, y)-plane. This illustrates that the plane of the feature is aligned at 45° to the (x, y) axes and is nearly parallel to the z-axis. (e) The Bella Dorsum plane fit, rendered at −45° in the (x, y)-plane. (f) Perspective view of Bella Dorsum illustrating the planar north–south symmetry of the feature. (g) View of the plane fit to Indah Fossa from the +x-axis. (h) Perspective view of the fit in panel (g).
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 time history of processes on Dinkinesh. We define T0 as the last major resetting event of the surface, likely YORP-driven failure that created Sumak Fossa and Fab Dorsum (and one or both lobes of Selam). Since that time, both Yarkovsky and YORP have acted continuously, affecting the semimajor axis evolution and body rotation. Though not continuous, impact cratering also spans from T0 to the current day. Bella Dorsum may be concurrent with the most recent YORP failure that created Sumak and Fab, or it may predate that time. Fab Dorsum superimposes Sumak Fossa, though it may have formed from the same YORP failure; thus, we tie the start of Fab to the end of Sumak. After the global restructuring from YORP failure, the surface includes evidence for more recent but smaller-scale activity: Indah Fossa, and possible cases of mass wasting from geopotential highs.
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: Maximum boulder sizes vs. representative asteroid diameter: dratio is the maximum boulder size on an asteroid normalized by a representative asteroid diameter. This plot uses the values from Table 6.
Paper: Modeling the Solar System. I. Characterization Limits from Analytic Timing Variations
Authors: Bethlee M. Lindor, Eric Agol
Figure caption: Posterior probability density functions of the ﹩{{ \mathcal H }}_{PPP}﹩ model, which includes the mass ratios, periods, and eccentricity vectors of each planet. In the panels along the diagonal, we bound the histograms by the 99.5% confidence interval of a given component. The off-diagonal panels show parameter correlations and the 0.5σ, 1σ, 1.5σ, and 2σ contours.
Paper: Modeling the Solar System. I. Characterization Limits from Analytic Timing Variations
Authors: Bethlee M. Lindor, Eric Agol
Figure caption: Same as Figure 15, but corresponding to the ﹩{{ \mathcal H }}_{PPPP}﹩ model.
Paper: Infrared Spectra of Organic and Salt-bearing Ices under Titan Conditions: Constraints on Detection of Ocean Materials
Authors: Paul V. Johnson, Robert Hodyss, Michael J. Malaska
Figure caption: IR reflectance spectra of inorganic salts in water ice at 95 K before (solid line) and after (dotted line) annealing. Spectra have been offset for clarity as follows: ammonium sulfate (red: 100), sodium bicarbonate (green: 70), sodium carbonate (black: 35), and sodium sulfate (blue: 0). The spectra before and after annealing of a given species are at the same offset. Dark and light gray bars indicate 10% transmission windows from altitudes of 1500 km and 1 m, corresponding to observations from orbit and a lander, respectively (P. Corlies et al. 2021).
Paper: Infrared Spectra of Organic and Salt-bearing Ices under Titan Conditions: Constraints on Detection of Ocean Materials
Authors: Paul V. Johnson, Robert Hodyss, Michael J. Malaska
Figure caption: IR reflectance spectra of ammonium formate in water ice at 95 K over a range of concentrations. Spectra have been offset for clarity as follows: saturated (red: 58), 10 M (black: 43), 5 M (blue: 23), 1 M (green: 18), and 0.5 M (brown: 0). Dark and light gray bars indicate 10% transmission windows from altitudes of 1500 km and 1 m, corresponding to observations from orbit and a lander, respectively (P. Corlies et al. 2021).
Paper: Infrared Spectra of Organic and Salt-bearing Ices under Titan Conditions: Constraints on Detection of Ocean Materials
Authors: Paul V. Johnson, Robert Hodyss, Michael J. Malaska
Figure caption: IR reflectance spectra of urea in water ice at 95 K over a range of concentrations after annealing at 200 K. Spectra have been offset for clarity as follows: saturated (red: 55), 5 M (black: 26), 2.5 M (blue: 17), 2 M (green: 4), and 1 M (brown: 0). Dark and light gray bars indicate 10% transmission windows from altitudes of 1500 km and 1 m, corresponding to observations from orbit and a lander, respectively (P. Corlies et al. 2021).
Paper: Infrared Spectra of Organic and Salt-bearing Ices under Titan Conditions: Constraints on Detection of Ocean Materials
Authors: Paul V. Johnson, Robert Hodyss, Michael J. Malaska
Figure caption: IR reflectance spectra of acetonitrile in water ice at 95 K over a range of concentrations after annealing at 200 K. Spectra have been offset for clarity as follows: 100 wt% (red: 107), 10 wt% (black: 71), 5 wt% (blue: 59), 2.5 wt% (green: 36), and 0.5 wt% (brown: 0). Dark and light gray bars indicate 10% transmission window altitudes of 1500 km and 1 m, corresponding to observations from orbit and a lander, respectively (P. Corlies et al. 2021).
Paper: Infrared Spectra of Organic and Salt-bearing Ices under Titan Conditions: Constraints on Detection of Ocean Materials
Authors: Paul V. Johnson, Robert Hodyss, Michael J. Malaska
Figure caption: IR reflectance spectra of acetonitrile in water ice at 95 K over a range of concentrations. Spectra have been offset for clarity as follows: 100 wt% (red: 74), 10 wt% (black: 49), 5 wt% (blue: 39), 2.5 wt% (green: 23), and 0.5 wt% (brown: 0). Dark and light gray bars indicate 10% transmission windows from altitudes of 1500 km and 1 m, corresponding to observations from orbit and a lander, respectively (P. Corlies et al. 2021).
Paper: Infrared Spectra of Organic and Salt-bearing Ices under Titan Conditions: Constraints on Detection of Ocean Materials
Authors: Paul V. Johnson, Robert Hodyss, Michael J. Malaska
Figure caption: IR reflectance spectra of ammonium formate in water ice at 95 K over a range of concentrations after annealing at 200 K. Spectra have been offset for clarity as follows: saturated (red: 52), 10 M (black: 35), 5 M (blue: 16), 1 M (green: 9), and 0.5 M (brown: 0). Dark and light gray bars indicate 10% transmission windows from altitudes of 1500 km and 1 m, corresponding to observations from orbit and a lander, respectively (P. Corlies et al. 2021).
Paper: Infrared Spectra of Organic and Salt-bearing Ices under Titan Conditions: Constraints on Detection of Ocean Materials
Authors: Paul V. Johnson, Robert Hodyss, Michael J. Malaska
Figure caption: IR reflectance spectra of organics in water ice at 95 K before (solid line) and after (dotted line) annealing. Spectra have been offset for clarity as follows: acetonitrile (red: 114), ammonium formate (brown: 70), urea (blue: 50), indole (cyan: 40), sodium acetate (black: 0), glycine (green: 5), and uracil (purple: 1). The spectra before and after annealing of a given species are at the same offset. Dark and light gray bars indicate 10% transmission windows from altitudes of 1500 km and 1 m, corresponding to observations from orbit and a lander, respectively (P. Corlies et al. 2021).
Paper: Infrared Spectra of Organic and Salt-bearing Ices under Titan Conditions: Constraints on Detection of Ocean Materials
Authors: Paul V. Johnson, Robert Hodyss, Michael J. Malaska
Figure caption: IR reflectance spectra of urea in water ice at 95 K over a range of concentrations. Spectra have been offset for clarity as follows: saturated (red: 63), 5 M (black: 44), 2.5 M (blue: 28), 2 M (green: 9), and 1 M (brown: 0). Dark and light gray bars indicate 10% transmission windows from altitudes of 1500 km and 1 m, corresponding to observations from orbit and a lander, respectively (P. Corlies et al. 2021).
Paper: Using SOFIA’s EXES to Search for C6H2 and C4N2 in Titan’s Atmosphere
Authors: Zachary C. McQueen, Conor A. Nixon, Curtis de Witt, Véronique Vuitton, Panayotis Lavvas, Juan Alday, Nicholas A. Teanby, Joseph Penn, Antoine Jolly, Patrick G. J. Irwin
Figure caption: The 3σ upper limits found for this study (gray squares) for C6H2 (A) and C4N2 (B), along with previous studies of the upper limits. Also included are the photochemical model vertical profiles of each species (red and blue traces), the uniform profiles used for the upper limits (gray solid trace), and the scaling factor for the V. Vuitton et al. (2019) C6H2 profile (gray dashed trace). The gray dotted line in panel (B) is the saturation altitude calculated using the V. Vuitton et al. (2019) temperature profile and equation for the saturation vapor pressures in N. Fray & B. Schmitt (2009).
Paper: Using SOFIA’s EXES to Search for C6H2 and C4N2 in Titan’s Atmosphere
Authors: Zachary C. McQueen, Conor A. Nixon, Curtis de Witt, Véronique Vuitton, Panayotis Lavvas, Juan Alday, Nicholas A. Teanby, Joseph Penn, Antoine Jolly, Patrick G. J. Irwin
Figure caption: (A) The Δχ2 plotted as a function of the VMR for the uniform profile of C6H2 and (B) the corresponding simulated spectra for the 1σ, 2σ, and 3σ upper limits with C6H2 peaks indicated by the black triangle markers. (C)–(D) The Δχ2 and corresponding spectra for the upper limits of C4N2. All emission features in panel (D) are due to C4N2.
Paper: Using SOFIA’s EXES to Search for C6H2 and C4N2 in Titan’s Atmosphere
Authors: Zachary C. McQueen, Conor A. Nixon, Curtis de Witt, Véronique Vuitton, Panayotis Lavvas, Juan Alday, Nicholas A. Teanby, Joseph Penn, Antoine Jolly, Patrick G. J. Irwin
Figure caption: Retrieved stratospheric profiles (colored trace) of C4H2 (A) and C3H4 (B) and the photochemical model predictions from V. Vuitton et al. (2019; solid black trace) and J. Loison et al. (2015; dot-dotted–dashed trace). The scaled profile from V. Vuitton et al. (2019), used as the a priori reference profile, is shown in the solid gray trace. The retrieved profile from S. Vinatier et al. (2007) is also shown for comparison (gray points and dotted–dashed trace). Each panel also shows the Jacobian at ﹩{\bar{\nu }}_{\max }﹩ for each molecule to indicate the altitude range the model is sensitive to.
Paper: Using SOFIA’s EXES to Search for C6H2 and C4N2 in Titan’s Atmosphere
Authors: Zachary C. McQueen, Conor A. Nixon, Curtis de Witt, Véronique Vuitton, Panayotis Lavvas, Juan Alday, Nicholas A. Teanby, Joseph Penn, Antoine Jolly, Patrick G. J. Irwin
Figure caption: Model fit (red trace) to the measured spectrum (gray trace) for the 621 cm−1 (A) and 472 cm−1 (B) spectral settings. Bottom panels show the residual of the model fit to the measured spectra and a 1σ estimation of the instrument uncertainty in the blue shaded regions. Emission features from C4H2 and C3H4 are indicated by the respective markers in panel (A). There are no known emission features in the 472 cm−1 spectral setting, and only the haze and CIA continuum levels were fit in the retrieval.