adsabs/AstroCLIMB huggingface dataset:
Paper: The History of Eruptions at Acala Fluctus, Io: Source of Multiple Outbursts
Authors: Julie A. Rathbun, Madeline Pettine, Moses Milazzo, Christian Tate
Figure caption: Summary of observations that we interpret to be from Acala including nondetections from major campaigns. The same information is presented in Table 1. Outbursts are indicated by red diamonds and other observations by blue circles. Filled shapes indicate observations originally identified as Acala, and open shapes indicate observations originally identified as a source other than Acala but that we propose may be from Acala. Nondetections are indicated by a horizontal line. The y-axis breaks up observations into near-infrared (NIR), short mid-infrared (short MIR), longer-wavelength mid-infrared (long MIR), and far-infrared (FIR).
Paper: Comparative Mid-infrared Spectroscopy of Dark, Primitive Asteroids: Does Shared Taxonomic Class Indicate Shared Silicate Composition?
Authors: Oriel A. Humes, Audrey C. Martin, Cristina A. Thomas, Joshua P. Emery
Figure caption: Comparison of the NEATM predictions to the measured fluxes of 87 Sylvia as observed using the Spitzer Space Telescope (left) and SOFIA (right). For SOFIA observations, spectra are scaled using a multiplicative factor to match the photometric measurements of the asteroid obtained on the same flight (see Section 2.2 of the text for details). The analogous scaling procedure for the Spitzer data is described in Section 2.1 of the text, but the unaligned Spitzer data are excluded from the figure, as the difference between the aligned and unaligned fluxes is not visible on the scale of the figure.
Paper: Comparative Mid-infrared Spectroscopy of Dark, Primitive Asteroids: Does Shared Taxonomic Class Indicate Shared Silicate Composition?
Authors: Oriel A. Humes, Audrey C. Martin, Cristina A. Thomas, Joshua P. Emery
Figure caption: Mid-infrared spectra of asteroids 65 Cybele, 87 Sylvia, 140 Siwa, 267 Tirza, 269 Justitia, 336 Lacadiera, 386 Haidea, 944 Hidalgo, 1268 Libya, and 1702 Kalahari from 6 to 14 μm as observed by the Spitzer IRS instrument in SL mode. For 87 Sylvia and 140 Siwa, we also overplot the SOFIA FORCAST G111 observations scaled to the same average emissivity for comparison. See also Licandro et al. (2011), Marchis et al. (2012), Vernazza et al. (2013), and Lowry et al. (2022) for their analyses of the same Spitzer IRS spectra of 65 Cybele, 87 Sylvia, 386 Haidea, and 944 Hidalgo, respectively.
Paper: Comparative Mid-infrared Spectroscopy of Dark, Primitive Asteroids: Does Shared Taxonomic Class Indicate Shared Silicate Composition?
Authors: Oriel A. Humes, Audrey C. Martin, Cristina A. Thomas, Joshua P. Emery
Figure caption: Mid-infrared spectra of asteroids 267 Tirza, 386 Haidea, 944 Hidalgo, 1268 Libya, 1702 Kalahari, and 3552 Don Quixote from 14 to 40 μm as observed by the Spitzer IRS instrument in LL mode. See also Vernazza et al. (2013), Mommert et al. (2014), and Lowry et al. (2022) for their analyses of the same Spitzer IRS spectra of 368 Haidea, 944 Hidalgo, and 3552 Don Quixote, respectively.
Paper: Comparative Mid-infrared Spectroscopy of Dark, Primitive Asteroids: Does Shared Taxonomic Class Indicate Shared Silicate Composition?
Authors: Oriel A. Humes, Audrey C. Martin, Cristina A. Thomas, Joshua P. Emery
Figure caption: Mid-infrared spectra of asteroids 46 Hestia, 87 Sylvia, 140 Siwa, and 190 Ismene as observed by the SOFIA FORCAST instrument using the G111 (panel (a)) and G227 (panel (b)) grisms. Note that we do not display data points for which atmospheric transparency is low (<0.9).
Paper: Increasing the Usability and Accessibility of Voyager 2 Images of Triton
Authors: Michael T. Bland, Emily S. Martin, Alex Patthoff
Figure caption: Comparison of the existing Triton mosaic with available high-resolution data. (a) A portion of the 1998 USGS global color mosaic in orthographic projection. This region is covered by image c1139350 at a scale of 1262 m pixel−1, which has been up-sampled to the 600 m pixel−1 scale of the mosaic. (b) The same region as shown in panel (a), but as seen in image c1139627 at 343 m pixel−1, which was not included in the 1998 USGS mosaic and was previously only available as an uncontrolled image (unaligned to the lower-resolution images) from the PDS. This image has a resolution twice that of the underlying data and was acquired at very high phase (115°; Table 1). Tie pointing is therefore challenging, and the image is still slightly misaligned. The image is centered at 349° E and 12° N (north is up) and uses the same projection as Figure 5.
Paper: Increasing the Usability and Accessibility of Voyager 2 Images of Triton
Authors: Michael T. Bland, Emily S. Martin, Alex Patthoff
Figure caption: Example of the improvement in image locations provided by our photogrammetric solution. The images are the same as those shown in Figure 2. The red and white arrows indicate features that were misaligned when using the default reconstructed SPICE information (same features as in Figure 2) but have now been brought into alignment. The region shown is roughly 1300 km east to west and is centered at approximately 343° E and 12° S (north is up). The projection is identical to that used in Figure 5.
Paper: Increasing the Usability and Accessibility of Voyager 2 Images of Triton
Authors: Michael T. Bland, Emily S. Martin, Alex Patthoff
Figure caption: The new Triton mosaic. The mosaic uses an orthographic projection centered on 15° E and 18° N (the 15° E meridian is vertical with north up) and at a scale of 600 m pixel−1. The images have been high-pass filtered with a 51 × 51 pixel window and 100% albedo add-back (i.e., a sharpening filter) to accentuate surface features. No photometric correction has been applied. Images included in this mosaic are listed in Table 2.
Paper: Increasing the Usability and Accessibility of Voyager 2 Images of Triton
Authors: Michael T. Bland, Emily S. Martin, Alex Patthoff
Figure caption: Visualizations of the tie point locations used in the (a) preliminary network and (b) final control network. Blue polygons show image footprints, and green crosses show tie point locations. The orientation is identical to that shown in Figure 5 below.
Paper: Increasing the Usability and Accessibility of Voyager 2 Images of Triton
Authors: Michael T. Bland, Emily S. Martin, Alex Patthoff
Figure caption: Example of Voyager 2 Triton images with incorrect location and orientation. These images (image numbers as shown) were downloaded from the PDS Imaging and Cartography Node, had default NAIF SPICE kernels (i.e., position and pointing) attached, and warped to a common projection and pixel scale (image reseaux were also removed to aid visualization). The red arrows highlight the same crater appearing in c1139503 and c1139445, which is misaligned by 200 km. The white arrows highlight a sinuous ridge in c1139509 and c1139445, which is misaligned by 130 km. Such misalignment is the “rule” rather than the exception for Triton data.
Paper: Increasing the Usability and Accessibility of Voyager 2 Images of Triton
Authors: Michael T. Bland, Emily S. Martin, Alex Patthoff
Figure caption: Sequence of six high-resolution images overlaid on our new mosaic. The high-resolution images are c1139619, c1139621, c1139623, c1139625, c1139627, and c1139529, all at pixel scale < 367 m pixel−1. This mosaic is a screenshot from a GIS in which the individual images have simply been added as layers on top of the underlying mosaic (orthographic projection at 600 m pixel−1).
Paper: Increasing the Usability and Accessibility of Voyager 2 Images of Triton
Authors: Michael T. Bland, Emily S. Martin, Alex Patthoff
Figure caption: Examples of ARD released for Triton. (a) An individual level 2 (calibrated and projected) photogrammetrically controlled Voyager 2 image (c1139445). (b) A partially processed version of the image shown in panel (a) that is calibrated and projected but still includes reseaux and corner marks. This region of Triton (identical to that shown in Figure 1(b)) has numerous small plume deposits (Hansen et al. 1990; Hofgartner et al. 2022; Martin et al. 2023), and distinguishing real features from reseau marks is critical.
Paper: Increasing the Usability and Accessibility of Voyager 2 Images of Triton
Authors: Michael T. Bland, Emily S. Martin, Alex Patthoff
Figure caption: Location of impact crater (circled in red) proposed to define Triton’s longitude system. The crater is located precisely at 40.°0 E (1.°1 S) in our mosaic and is readily identifiable in 5 (of 41) Voyager 2 images. A name for the crater is pending IAU approval.
Paper: Increasing the Usability and Accessibility of Voyager 2 Images of Triton
Authors: Michael T. Bland, Emily S. Martin, Alex Patthoff
Figure caption: Example of our processing of “level 1” (unprojected) images including reseau removal. (a) The raw image after ingestion into ISIS. (b) Reseaux have been replaced by null pixels. (c) Null pixels, corner marks, and dropped lines are filled in with a low-pass filter. The unprojected cube shown is c1139527.
Paper: The Sensitivity of NEO Surveyor to Low-perihelion Asteroids
Authors: Joseph R. Masiero, Yuna G. Kwon, Dar W. Dahlen, Frank J. Masci, Amy K. Mainzer
Figure caption: Comparison of the currently known population of near-Sun asteroids (orange) to the synthetic population used for our completeness determinations (blue). Histograms of orbital parameters (top left: perihelion distance; top middle: eccentricity; top right: aphelion distance; middle left: orbital inclination; center: argument of perihelion; middle right: longitude of the ascending node) and scatterplots of orbital elements (bottom left: perihelion distance vs. eccentricity; bottom middle: perihelion distance vs. inclination; bottom right: eccentricity vs. inclination) demonstrate that the synthesized population sufficiently samples the phase space occupied by the real objects.
Paper: The Sensitivity of NEO Surveyor to Low-perihelion Asteroids
Authors: Joseph R. Masiero, Yuna G. Kwon, Dar W. Dahlen, Frank J. Masci, Amy K. Mainzer
Figure caption: Fraction of synthetic objects recovered by NEO Surveyor after 5 yr (color bar) as a function of orbital elements assuming all objects have diameters of D = 150 m. Eccentricity vs. perihelion distance (left) shows a strong correlation with recovery fraction; inclination vs. perihelion distance (middle) shows only a weak trend; inclination vs. eccentricity (right) shows that eccentricity dominates the recoverability.
Paper: The Sensitivity of NEO Surveyor to Low-perihelion Asteroids
Authors: Joseph R. Masiero, Yuna G. Kwon, Dar W. Dahlen, Frank J. Masci, Amy K. Mainzer
Figure caption: Fraction of synthetic objects recovered by NEO Surveyor after 5 yr as a function of object size. Green points show all synthetic objects, magenta shows those objects with Earth MOIDs less that 0.05 au, and black shows a subset of objects close in orbital space to (3200) Phaethon. The lines for each color show the best fit to the calculated completeness points using Equation (1).
Paper: The Pale Blue Dot: Using the Planetary Spectrum Generator to Simulate Signals from Hyperrealistic Exo-Earths
Authors: Vincent Kofman, Geronimo Luis Villanueva, Thomas J. Fauchez, Avi M. Mandell, Ted M. Johnson, Allison Payne, Natasha Latouf, Soumil Kelkar
Figure caption: Top panel: simulations (1a) and DSCOVR/EPIC observations of Earth (1b) at spring equinox in 2022. UTC times of the simulations and observations are indicated above the figures. Second panel: simulations (2a) and Himawari-8 observations (2b) of the Earth from geostationary orbit (longitude 140.7). Third panel (3): in order of appearance, 3D simulation of the Earth at the time and orientation of the Voyager 1 spacecraft, which is subsequently modified by a Gaussian convolution. At a distance of 40 au, the pixel size of 5.3e-4 degree corresponds to approximately 6 times the Earth’s diameter. This is unresolved by Voyagers 1's cameras and results in the blurry image on the right. The discussion section elaborates on the generation of color from spectral radiance.
Paper: The Pale Blue Dot: Using the Planetary Spectrum Generator to Simulate Signals from Hyperrealistic Exo-Earths
Authors: Vincent Kofman, Geronimo Luis Villanueva, Thomas J. Fauchez, Avi M. Mandell, Ted M. Johnson, Allison Payne, Natasha Latouf, Soumil Kelkar
Figure caption: Progression of the simulations, combining the cloud-free simulations (first panel) with the fully cloudy simulations (second panel) to yield the simulations using the cloud fraction map (third panel). The last panel shows the DSCOVR/EPIC observation that is being reproduced. Observations and synthetic images show very similar dynamic range, absolute flux calibration, and coloring. No special or arbitrary scaling or calibrations were applied to the model or the data.
Paper: The Pale Blue Dot: Using the Planetary Spectrum Generator to Simulate Signals from Hyperrealistic Exo-Earths
Authors: Vincent Kofman, Geronimo Luis Villanueva, Thomas J. Fauchez, Avi M. Mandell, Ted M. Johnson, Allison Payne, Natasha Latouf, Soumil Kelkar
Figure caption: Comparison of the spectra obtained from this study with the calibrated DSCOVR/EPIC bands in units of spectral radiance (left) and albedo (right). The values for the albedo of the EPIC observations are obtained directly from their calibrations, whereas spectral radiance values are obtained by multiplying these values with the spectral radiance of the Sun at the top of the atmosphere. In the figure on the left, the solar spectrum and the 5777 K blackbody spectrum are shown, scaled by a factor of 0.1.
Paper: The Pale Blue Dot: Using the Planetary Spectrum Generator to Simulate Signals from Hyperrealistic Exo-Earths
Authors: Vincent Kofman, Geronimo Luis Villanueva, Thomas J. Fauchez, Avi M. Mandell, Ted M. Johnson, Allison Payne, Natasha Latouf, Soumil Kelkar
Figure caption: Definitions of the different orbital phases used in this work, as adopted from the descriptions of the PSG. This is by no means the only work that describes these phases as such, but in the interest of clarity, it is included here.
Paper: The Pale Blue Dot: Using the Planetary Spectrum Generator to Simulate Signals from Hyperrealistic Exo-Earths
Authors: Vincent Kofman, Geronimo Luis Villanueva, Thomas J. Fauchez, Avi M. Mandell, Ted M. Johnson, Allison Payne, Natasha Latouf, Soumil Kelkar
Figure caption: Simulations of the albedo of Earth during the summer solstice in 2022, calculated using ∼6500 subcalculations at a resolving power of 70. On the left, spectra of the calculations without clouds are shown, and the combined cloudless and cloudy simulations are shown on the right (see text for more information). The images at the top are generated from the spectra in units of spectral radiance, which is subsequently converted to albedo for the middle panels. The intensity of the molecular bands is integrated into equivalent width, which is shown as a function of UTC in the bottom plots.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Enhancement of the Cerean Exosphere by Sublimation from Complex Craters
Authors: Patrick O'Brien, Jennifer E. C. Scully, Margaret E. Landis, Norbert Schörghofer, Paul O. Hayne
Figure caption:                         Gray scale with geomorphic map (left) and photometrically corrected color (right) images of Haulani, Kupalo, Aristaeus, Azacca, Heneb, and Ikapati craters from the Dawn Framing Camera. In the geomorphic maps, the boundary of the crater wall/terraces is shown by a red line, fractures are dark blue lines, localized bright floor deposits are outlined in cyan, central structures are outlined in pale blue, and the approximate original area of the crater floor faculae is shaded in green. White dots are bright craters, and black dots are dark craters (see Figure 10 for a high-resolution version and Figure 5 for more information).
Paper: Enhancement of the Cerean Exosphere by Sublimation from Complex Craters
Authors: Patrick O'Brien, Jennifer E. C. Scully, Margaret E. Landis, Norbert Schörghofer, Paul O. Hayne
Figure caption: Bright and dark craters used to estimate thickness of partially buried floor faculae for (a) Aristaeus, (b) Azacca, (c) Heneb, and (d) Ikapati craters. White numbers (>X m) indicate thicknesses derived from bright superposing craters that did not excavate all the way through the floor faculae. Black numbers (<X m) indicate thicknesses derived from dark superposing and adjacent craters that excavated deeper than the floor faculae. Yellow numbers (X m) are absolute thickness estimates derived from adjacent maximum and minimum thicknesses. When there is more than one absolute thickness estimate, the estimates are averaged. The green dashed line is the approximate original area of the crater floor faculae.
Paper: Enhancement of the Cerean Exosphere by Sublimation from Complex Craters
Authors: Patrick O'Brien, Jennifer E. C. Scully, Margaret E. Landis, Norbert Schörghofer, Paul O. Hayne
Figure caption: Depth to volatiles before (left) and after (right) a complex-crater-forming impact. Large impacts thin the dessicated lag layer and excavate ice-rich material from the subsurface, depositing it in the crater’s ejecta blanket and floor. Impact heating can also drive the later emplacement of bright faculae. Following the formation of a complex crater, volatiles are replenished in the near-surface environment, leading to enhanced sublimation relative to the preimpact ice table.
Paper: Enhancement of the Cerean Exosphere by Sublimation from Complex Craters
Authors: Patrick O'Brien, Jennifer E. C. Scully, Margaret E. Landis, Norbert Schörghofer, Paul O. Hayne
Figure caption: Area scaling laws for each of the three complex crater volatile reservoirs. Ejecta blankets (solid line) are a circular annulus extending 1.5 crater radii from the rim (Section 2.1). Lobate deposits (dashed–dotted line) are assumed to occupy 30% of the crater’s flat floor (Section 2.2). A novel faculae area scaling law (dashed line) was produced in this work by mapping a set of young complex craters (circles; Section 2.3).
Paper: Enhancement of the Cerean Exosphere by Sublimation from Complex Craters
Authors: Patrick O'Brien, Jennifer E. C. Scully, Margaret E. Landis, Norbert Schörghofer, Paul O. Hayne
Figure caption: (a) Global map showing locations of all type 1a, 1b, and 2 craters as defined in this work. Type 1 craters are labeled with white text and type 2 with black text. (b) Haulani crater: an example of a type 1a crater. (c) Ikapati crater: an example of a type 1b crater. (d) Dantu crater: an example of a type 2 crater.
Paper: The Pale Blue Dot: Using the Planetary Spectrum Generator to Simulate Signals from Hyperrealistic Exo-Earths
Authors: Vincent Kofman, Geronimo Luis Villanueva, Thomas J. Fauchez, Avi M. Mandell, Ted M. Johnson, Allison Payne, Natasha Latouf, Soumil Kelkar
Figure caption: Exposure time requirements to reach an S/N of 5 for the integrated band for Earth seen from 10 pc for the five different telescope concepts studied here. The full sets of parameters describing the concepts are given in Table 3. The y-axis shows the equivalent width at the times indicated in the figure. Both the cloudless simulations and simulations with cloud coverage are shown.
Paper: The Pale Blue Dot: Using the Planetary Spectrum Generator to Simulate Signals from Hyperrealistic Exo-Earths
Authors: Vincent Kofman, Geronimo Luis Villanueva, Thomas J. Fauchez, Avi M. Mandell, Ted M. Johnson, Allison Payne, Natasha Latouf, Soumil Kelkar
Figure caption: Simulations with different phenomena enabled to study the relative contribution of ocean glint to the total albedo. For these simulations, the Himawari-8 observations were adapted (fourth image in the middle panel of Figure 2).
Paper: Enhancement of the Cerean Exosphere by Sublimation from Complex Craters
Authors: Patrick O'Brien, Jennifer E. C. Scully, Margaret E. Landis, Norbert Schörghofer, Paul O. Hayne
Figure caption: (Left) Time-dependent sublimation rates at Occator crater. (right) Variance-based sensitivity analysis of model parameters (Table 2) applied to Occator. Nearly all the variance (characterized by the total order Sobol’ index) in the output emission rate can be attributed to inputs characterizing the ejecta blanket, like the ejecta radius, η  ej , and the weight fraction of water ice in the ejecta blanket, w  ej .
Paper: Enhancement of the Cerean Exosphere by Sublimation from Complex Craters
Authors: Patrick O'Brien, Jennifer E. C. Scully, Margaret E. Landis, Norbert Schörghofer, Paul O. Hayne
Figure caption: Water vapor emission rate from all complex craters on Ceres as a function of the ejecta blanket radius in units of crater radii, η  ej , and the H2O weight fraction of ice-rich ejecta, w  ej , for the “low” thermal inertia case (Section 2.4). The dotted contour line denotes the emission rate of the global ice table (Prettyman et al. 2017). The black dot represents the average ejecta radius of craters with fluidized-appearing ejecta (Hughson et al. 2019) and the inferred water-ice fraction of Occator ejecta (Prettyman et al. 2021). If Cerean ejecta blankets extend on average more than approximately one crater radius beyond and contain more than a few weight percent H2O, then outgassing from ejecta deposits is predicted to exceed that of the global ice table.
Paper: Enhancement of the Cerean Exosphere by Sublimation from Complex Craters
Authors: Patrick O'Brien, Jennifer E. C. Scully, Margaret E. Landis, Norbert Schörghofer, Paul O. Hayne
Figure caption: Cumulative water vapor emission rate for all complex craters on Ceres. The solid black line shows the median of 1000 Monte Carlo runs, and colors indicate the contribution from the three volatile reservoirs. The dotted red line is the emission rate inferred from sublimation of the global ice table (Prettyman et al. 2017). Craters with known ages form within a fixed interval for each Monte Carlo run, hence the spike at ∼20 Ma due to Occator.
Paper: Enhancement of the Cerean Exosphere by Sublimation from Complex Craters
Authors: Patrick O'Brien, Jennifer E. C. Scully, Margaret E. Landis, Norbert Schörghofer, Paul O. Hayne
Figure caption: Time-dependent sublimation rates for seven young complex craters. Dashed lines indicate craters with uncertain ages, which have been randomly sampled within a range of probable formation ages.
Paper: Enhancement of the Cerean Exosphere by Sublimation from Complex Craters
Authors: Patrick O'Brien, Jennifer E. C. Scully, Margaret E. Landis, Norbert Schörghofer, Paul O. Hayne
Figure caption: Time-dependent sublimation curves and variance-based sensitivity analysis for Haulani, Kupalo, Aristaeus, Azacca, Heneb, and Ikapati craters.
Paper: Enhancement of the Cerean Exosphere by Sublimation from Complex Craters
Authors: Patrick O'Brien, Jennifer E. C. Scully, Margaret E. Landis, Norbert Schörghofer, Paul O. Hayne
Figure caption: Faculae mapping for Haulani, Kupalo, Aristaeus, Azacca, Heneb, and Ikapati craters.