adsabs/AstroCLIMB huggingface dataset:
Paper: Shape Models of Lucy Targets (3548) Eurybates and (21900) Orus from Disk-integrated Photometry
Authors: Stefano Mottola, Stephan Hellmich, Marc W. Buie, Amanda M. Zangari, Robert D. Stephens, Mario Di Martino, Gerrit Proffe, Simone Marchi, Catherine B. Olkin, Harold F. Levison
Figure caption: Sphere-integrated phase curve for Orus. The blue squares represent the geometry-corrected individual data points for the subset of the observations for which a reliable transformation to the Johnson V band could be determined.
Paper: Shape Models of Lucy Targets (3548) Eurybates and (21900) Orus from Disk-integrated Photometry
Authors: Stefano Mottola, Stephan Hellmich, Marc W. Buie, Amanda M. Zangari, Robert D. Stephens, Mario Di Martino, Gerrit Proffe, Simone Marchi, Catherine B. Olkin, Harold F. Levison
Figure caption: Same as Figure 5, but for Orus.
Paper: Shape Models of Lucy Targets (3548) Eurybates and (21900) Orus from Disk-integrated Photometry
Authors: Stefano Mottola, Stephan Hellmich, Marc W. Buie, Amanda M. Zangari, Robert D. Stephens, Mario Di Martino, Gerrit Proffe, Simone Marchi, Catherine B. Olkin, Harold F. Levison
Figure caption: Three orthographic views of the Orus convex shape model.
Paper: Spectral Analysis of Clay-bearing Outcrops in Northern Xanthe Terra, Mars: Comparison with Oxia Planum, the Landing Site for the ExoMars Rover Mission
Authors: Jeremy Brossier, Francesca Altieri, Maria Cristina De Sanctis, Alessandro Frigeri, Marco Ferrari, Simone De Angelis, Andrea Apuzzo
Figure caption: (a) Spectra of the CRISM denoised reflectance, normalized and offset for clarity. Unusable data at (1) 1.65 μm is associated with intermittent spikes from a detector filter boundary, and (2) 1.90–2.10 μm is due to an instrumental artifact resulting from the atmospheric removal pipeline (Murchie et al. 2009 Leask et al. 2018). Spectra are smoothed by averaging hundreds to thousands of pixels (Table 2). (b) We also include three spectra recently obtained from clay outcrops in Oxia Planum (Brossier et al. 2022a). (c) Laboratory spectra of main candidate Fe,Mg-rich clays: nontronite, saponite, Fe-rich saponite (e.g., Griffithite) and vermiculite ores (vermiculite and hydrobiotite components; see references in Section 4). All major absorptions are shown with vertical lines at 1.41, 1.92, and 2.30 μm, as well as 2.40 and 2.53 μm. Lab spectra for pure vermiculite and hydrobiotite are truncated at 2.5 μm, while other spectra go up to 2.6 μm. These two lab spectra are available through a spectral library (i.e., Swayze et al. 2018), whose samples have been verified and identified as such (see also Brossier et al. 2022a). The only spectra displayed in the literature so far and available in the RELAB repository (e.g., Carter et al. 2013; Krzesińska et al. 2021; Mandon et al. 2021) are not considered as pure, but are rather vermiculite-rich mixtures with biotite, hydrobiotite, and vermiculite components (Cloutis 2015).
Paper: Spectral Analysis of Clay-bearing Outcrops in Northern Xanthe Terra, Mars: Comparison with Oxia Planum, the Landing Site for the ExoMars Rover Mission
Authors: Jeremy Brossier, Francesca Altieri, Maria Cristina De Sanctis, Alessandro Frigeri, Marco Ferrari, Simone De Angelis, Andrea Apuzzo
Figure caption: (a) Localization of prominent regions in circum–Chryse Planitia (e.g., Mawrth Vallis, Oxia Planum, and Xanthe Terra) on MOLA global topographic map. (b, c) THEMIS (Fergason et al. 2006) infrared daytime maps of northern Xanthe Terra colorized by MOLA topography (lower elevations in teal, higher elevation areas in brown): (b) Sabrina and Hypanis valley systems (315.0° E, 11.2° N), and (c) near the Cantoura crater (308.4° E, 15.5° N). Color-coded footprints correspond to CRISM targeted cubes available in the infrared range (1–4 μm) and used in this work. Black footprints display cubes that are not selected for further analysis since we did not detect clays in those scenes. Red patches indicate previous detections of hydrated phases derived from OMEGA and CRISM multispectral data (Carter et al. 2015; Adler et al. 2019) and also shown in Favaro et al. (2022). MV = Mawrth Vallis; OP = Oxia Planum; XT = Xanthe Terra. Purple and pink circles indicate the locations of Viking 1 (1976) and Mars Pathfinder (1997) landing sites for reference, respectively.
Paper: Spectral Analysis of Clay-bearing Outcrops in Northern Xanthe Terra, Mars: Comparison with Oxia Planum, the Landing Site for the ExoMars Rover Mission
Authors: Jeremy Brossier, Francesca Altieri, Maria Cristina De Sanctis, Alessandro Frigeri, Marco Ferrari, Simone De Angelis, Andrea Apuzzo
Figure caption: Maps of clay-bearing outcrops for (unprojected) CRISM cubes selected in three sites of interest: FRT0A605 targeting an isolated outcrop in eastern Xanthe Terra (317.5° E, 10.0° N; top), FRS37E48 targeting outcrops at the Magong crater, near the Sabrina fan delta (313.6° E, 12.0° N; middle), and FRS3D053 targeting outcrops close to the Cantoura crater (308.0° E, 15.9° N; bottom). Left: ROIs are automatically determined for all pixels with strong absorptions at 1.9 and 2.3 μm (BD1900R2 and D2300). They are overlapping a CRISM band near 1.3 μm (R1330) to display the infrared albedo and correlate with the morphology (Pelkey et al. 2007; Viviano-Beck et al. 2014). Right: maps displaying the spectral criterion “D2300” indicative of narrow absorption at 2.3 μm.
Paper: Spectral Analysis of Clay-bearing Outcrops in Northern Xanthe Terra, Mars: Comparison with Oxia Planum, the Landing Site for the ExoMars Rover Mission
Authors: Jeremy Brossier, Francesca Altieri, Maria Cristina De Sanctis, Alessandro Frigeri, Marco Ferrari, Simone De Angelis, Andrea Apuzzo
Figure caption: (a) Simplified geologic map of Magong crater and surroundings (313.4° E, 12.1° N). Morphological units are defined from CTX imagery (Platz et al. 2014 Knade et al. 2017; see also Adler et al. 2022): Sabrina Vallis (in blue), fan delta (in green), dark deposits (in black), small craters (in yellow), isolated mounds (in white), lowland and highland materials (in light and dark brown, respectively). White footprints indicate the CRISM targeted data used to map the clay-bearing outcrops (in red). Pink patches correspond to possible detection of clays at the fan delta reported in past studies (not studied here). (b–e) Close-up views of key geologic units identified within Magong crater in HiRISE images: (b) fan delta with subhorizontally layered sediments, (c) polygonal cracks near the delta, and (d–e) dark rough deposits forming patches and also fill-in ancient small craters.
Paper: Spectral Analysis of Clay-bearing Outcrops in Northern Xanthe Terra, Mars: Comparison with Oxia Planum, the Landing Site for the ExoMars Rover Mission
Authors: Jeremy Brossier, Francesca Altieri, Maria Cristina De Sanctis, Alessandro Frigeri, Marco Ferrari, Simone De Angelis, Andrea Apuzzo
Figure caption: Left: maps displaying the distribution of the diverse band centers in the windows centered at 2.4 and 2.5 μm, for the FRT0A605 cube (Figure 3(b)). Right: histograms reporting the normalized counts (bins: 2.5 μm). Red vertical lines indicate the five CRISM spectral channels centered in the windows. (a) Band centers near 2.4 μm (2.36–2.44 μm) subdivided into three classes: (1) below 2.39 μm, (2) between 2.39 and 2.40 μm, and (3) above 2.40 μm. (b) Band centers near 2.5 μm (2.49–2.57 μm) subdivided into three classes: (1) below 2.52 μm, (2) between 2.52 and 2.54 μm, and (3) above 2.54 μm.
Paper: Spectral Analysis of Clay-bearing Outcrops in Northern Xanthe Terra, Mars: Comparison with Oxia Planum, the Landing Site for the ExoMars Rover Mission
Authors: Jeremy Brossier, Francesca Altieri, Maria Cristina De Sanctis, Alessandro Frigeri, Marco Ferrari, Simone De Angelis, Andrea Apuzzo
Figure caption: Top: scatterplots of 2.3 μm vs. 1.4 μm band centers for the clay-bearing outcrops detected in Xanthe Terra (color-coded circles; see Figure 4) and compared with values obtained at Oxia Planum (black star; Brossier et al. 2022a), as well as candidate clays: nontronite and saponite (Clark et al. 1990 Bishop et al. 2013), Fe-rich saponite (e.g., Treiman et al. 2014; Chemtob et al. 2015), and vermiculite ores (including pure vermiculite and hydrobiotite components separately; Swayze et al. 2018). Bottom: scatterplots of 2.3 μm vs. 2.4 μm band centers. Since absorptions near 2.4 μm are barely recognized in most defined outcrops (i.e., FRS cubes), we only plot the values for FRT0A605 cube. Dashed outlines indicate the error areas for the candidate minerals (lab sampling at 2.5 nm).
Paper: Spectral Analysis of Clay-bearing Outcrops in Northern Xanthe Terra, Mars: Comparison with Oxia Planum, the Landing Site for the ExoMars Rover Mission
Authors: Jeremy Brossier, Francesca Altieri, Maria Cristina De Sanctis, Alessandro Frigeri, Marco Ferrari, Simone De Angelis, Andrea Apuzzo
Figure caption: CTX mosaic tiles of sites of interest in northern Xanthe Terra colorized by HRSC DEM (if available) or MOLA topography. Similarly to Figure 1, lower elevations are in teal and higher elevation areas are in brown. Footprints for CRISM data used in this study are color-coded and labeled for clarity.
Paper: Spectral Analysis of Clay-bearing Outcrops in Northern Xanthe Terra, Mars: Comparison with Oxia Planum, the Landing Site for the ExoMars Rover Mission
Authors: Jeremy Brossier, Francesca Altieri, Maria Cristina De Sanctis, Alessandro Frigeri, Marco Ferrari, Simone De Angelis, Andrea Apuzzo
Figure caption: Left: maps displaying the distribution of the diverse band centers in the windows centered at 1.4, 1.9, and 2.3 μm, for the FRT0A605 cube (Figure 2). Right: histograms reporting the normalized counts (bins: 2.5 μm). Red vertical lines indicate the five CRISM spectral channels centered in the windows. (a) Band centers near 1.4 μm (1.37–1.45 μm) subdivided into three classes: (1) below 1.40 μm, (2) between 1.40 and 1.41 μm, and (3) above 1.41 μm. (b) Band centers near 1.9 μm (1.88–1.96 μm) subdivided into three classes: (1) below 1.92 μm, (2) between 1.92 and 1.93 μm, and (3) above 1.93 μm. (c) Band centers near 2.3 μm (2.26–2.34 μm) subdivided into three classes: (1) below 2.30 μm, (2) between 2.30 and 2.31 μm, and (3) above 2.31 μm.
Paper: Spectral Analysis of Clay-bearing Outcrops in Northern Xanthe Terra, Mars: Comparison with Oxia Planum, the Landing Site for the ExoMars Rover Mission
Authors: Jeremy Brossier, Francesca Altieri, Maria Cristina De Sanctis, Alessandro Frigeri, Marco Ferrari, Simone De Angelis, Andrea Apuzzo
Figure caption: All sites of interest in CTX mosaic tiles, where all clay-bearing outcrops identified in this study are mapped in red. White footprints indicate the CRISM targeted data with the clay-bearing outcrops. Pink patches correspond to possible Fe,Mg-rich clays at Sabrina’s fan delta (not studied here) and reported in past studies (e.g., Platz et al. 2014; Knade et al. 2017).
Paper: Spectral Analysis of Clay-bearing Outcrops in Northern Xanthe Terra, Mars: Comparison with Oxia Planum, the Landing Site for the ExoMars Rover Mission
Authors: Jeremy Brossier, Francesca Altieri, Maria Cristina De Sanctis, Alessandro Frigeri, Marco Ferrari, Simone De Angelis, Andrea Apuzzo
Figure caption: (a–b) Close-up views of sites of interest in CTX mosaic tiles, where clay-bearing outcrops overlap with HiRISE imagery (same annotations as in Figure 8). (c–g) Outcrops shown in HiRISE images.
Paper: Spectral Analysis of Clay-bearing Outcrops in Northern Xanthe Terra, Mars: Comparison with Oxia Planum, the Landing Site for the ExoMars Rover Mission
Authors: Jeremy Brossier, Francesca Altieri, Maria Cristina De Sanctis, Alessandro Frigeri, Marco Ferrari, Simone De Angelis, Andrea Apuzzo
Figure caption: Maps of all clay-bearing outcrops for the (unprojected) CRISM cubes selected for this work. Left: ROIs are automatically determined for all pixels with strong absorptions at 1.9 and 2.3 μm (BD1900R2 and D2300); they are overlapping the CRISM band near 1.3 μm (R1330) to display the infrared albedo and correlate with the morphology (Pelkey et al. 2007; Viviano-Beck et al. 2014). Right: maps displaying the spectral criterion “D2300” indicative of narrow absorption at 2.3 μm.
Paper: Spectral Analysis of Clay-bearing Outcrops in Northern Xanthe Terra, Mars: Comparison with Oxia Planum, the Landing Site for the ExoMars Rover Mission
Authors: Jeremy Brossier, Francesca Altieri, Maria Cristina De Sanctis, Alessandro Frigeri, Marco Ferrari, Simone De Angelis, Andrea Apuzzo
Figure caption: Left: maps displaying the distribution of the diverse band centers in the windows centered near (a) 1.4 μm [1.37–1.45 μm], (b) 1.9 μm [1.88–1.96 μm] and (c) 2.3 μm [2.26–2.34 μm], for the FRS37E48 and FRS3D053 cubes (Figure 2). Right: histograms reporting the normalized counts (bins: 2.5 μm). Red vertical lines indicate the five CRISM spectral channels centered in the windows.
Paper: Spectral Analysis of Clay-bearing Outcrops in Northern Xanthe Terra, Mars: Comparison with Oxia Planum, the Landing Site for the ExoMars Rover Mission
Authors: Jeremy Brossier, Francesca Altieri, Maria Cristina De Sanctis, Alessandro Frigeri, Marco Ferrari, Simone De Angelis, Andrea Apuzzo
Figure caption: Spectra of the CRISM denoised reflectance, normalized and offset for clarity, extracted from clay-bearing outcrops in northern Xanthe Terra (FRT0A605 in red) and Oxia Planum (FRT09A16 and FRT0810D in orange and yellow, respectively). Xanthe’s outcrops generally show weaker signatures relative to most outcrops in Oxia Planum, perhaps due to a higher dust cover in northern Xanthe Terra attenuating the clay spectral signatures.
Paper: Spectral Analysis of Clay-bearing Outcrops in Northern Xanthe Terra, Mars: Comparison with Oxia Planum, the Landing Site for the ExoMars Rover Mission
Authors: Jeremy Brossier, Francesca Altieri, Maria Cristina De Sanctis, Alessandro Frigeri, Marco Ferrari, Simone De Angelis, Andrea Apuzzo
Figure caption: All sites of interest in CTX mosaic tiles with color-coded footprints corresponding to HiRISE “RED” images georeferenced during our investigation, targeting clay-bearing outcrops and major morphological units (light green).
Paper: Fitting the Light Curve of 1I/‘Oumuamua with a Nonprincipal Axis Rotational Model and Outgassing Torques
Authors: Aster G. Taylor, Darryl Z. Seligman, Olivier R. Hainaut, Karen J. Meech
Figure caption: Best-fit synthetic light curves (red lines) and photometric data (gray points). The data shown are those taken in 2017 October only. The first row shows the CO84 model (Equation (18)), and the second shows the ML15 model (Equation (23)). The parameters for each model are given in Table 1. The third row shows the instantaneous normalized angular momentum magnitude L of both models over the same time period. It is important to note that the modulation in the angular momentum magnitude L over the course of the observations is a result of the continuous application of outgassing torques, because it is constant in the absence of torques. The time is shown in days, with a zero point at 58,000 MJD.
Paper: Fitting the Light Curve of 1I/‘Oumuamua with a Nonprincipal Axis Rotational Model and Outgassing Torques
Authors: Aster G. Taylor, Darryl Z. Seligman, Olivier R. Hainaut, Karen J. Meech
Figure caption: The ratio of the non-normal outgassing torque (Equation (12)) to the tidal torque (Equation (4)), assuming that a = 115 m and r  H  = 0.256 au. Panel A assumes that the aspect ratio ϵ is equal to 1/6, as is characteristic for ‘Oumuamua. Panel B assumes that ﹩\epsilon =1/\sqrt{2}﹩, which is typical for most small bodies. Contours are plotted at 104, 105, and 106 for both subplots.
Paper: Fitting the Light Curve of 1I/‘Oumuamua with a Nonprincipal Axis Rotational Model and Outgassing Torques
Authors: Aster G. Taylor, Darryl Z. Seligman, Olivier R. Hainaut, Karen J. Meech
Figure caption: Idealized models of an elongated ellipsoidal object. Panel A shows the ellipsoidal object, with the inertial (unprimed, black) coordinate system and the corotating (primed, blue) coordinate system. The object and the corotating axes are rotated by an angle β. Panel B shows the “dumbbell” model characterized by two masses m 1 and m 2 at a distance D, again rotated by an angle β. Only the inertial coordinate system is shown.
Paper: Fitting the Light Curve of 1I/‘Oumuamua with a Nonprincipal Axis Rotational Model and Outgassing Torques
Authors: Aster G. Taylor, Darryl Z. Seligman, Olivier R. Hainaut, Karen J. Meech
Figure caption: Diagram showing the structure and defined angles of a non-normal outgassing jet. The thick blue arrow indicates the outgassing jet direction, which is offset from the ellipsoid normal direction (the thick black arrow, given by Equation (6)) by the angle ϕ jet. The corotating frame (thin blue arrows) is rotated with respect to the inertial frame (thin black arrows) by the angle β.
Paper: Fitting the Light Curve of 1I/‘Oumuamua with a Nonprincipal Axis Rotational Model and Outgassing Torques
Authors: Aster G. Taylor, Darryl Z. Seligman, Olivier R. Hainaut, Karen J. Meech
Figure caption: The ratio of outgassing to tidal torques for ‘Oumuamua, which is given by Equation (10). The ratio is plotted for a range of heliocentric distances and the rotation state of the body, which reflects the angle between the body’s primary axis and the Sun. The contours are plotted every 100.25, and are shown on the colorbar.
Paper: Discovery of Seven Volcanic Outbursts on Io from an Infrared Telescope Facility Observation Campaign, 2016–2022
Authors: Christian D. Tate, Julie A. Rathbun, Alexander G. Hayes, John R. Spencer, Madeline Pettine
Figure caption: Effective temperature and area constraints for the 201905A (top), 201906A (middle), and 202010A (bottom) outburst events. The red curves in the left panels are the blackbody fits of the noncorrected photometric intensity measurements: Lp, Kcont, and CH4_l band (when available). The occultation light curve is the Lprime-band brightness of Io's observable (nonoccluded) surface vs. occultation phase, which is the rescaled time, with zero being the start and 1 being the finish of the occultation. The shaded regions in the left panels indicate the in-band wavelength range, and those in the right panels indicate the transitional phase range of the outbursts.
Paper: Discovery of Seven Volcanic Outbursts on Io from an Infrared Telescope Facility Observation Campaign, 2016–2022
Authors: Christian D. Tate, Julie A. Rathbun, Alexander G. Hayes, John R. Spencer, Madeline Pettine
Figure caption: Sunlit IRTF images of Io on several nights that show clear hot spots. The square shift-and-add images are used to constrain the spot location and project each pixel onto the map of Io that is to the right of each image. The heatmap scale is the same for all images. The bottom two rows show Lp (left) and M (right) images from August when both bands are imaged. All circled hot spots are outbursts, except for the upper left panel for 2017 March 31, in which Loki is a mini-outburst.
Paper: Discovery of Seven Volcanic Outbursts on Io from an Infrared Telescope Facility Observation Campaign, 2016–2022
Authors: Christian D. Tate, Julie A. Rathbun, Alexander G. Hayes, John R. Spencer, Madeline Pettine
Figure caption: Time series of the subobserver (e.g., central meridian) longitude +/− 90° for each of our eclipsed and sunlit observations. The black dots are the subobserver longitudes at the time of each outburst event. The panel on the right is the histogram of the observations divided into 15° sub-Earth longitude bins. The gray shaded regions show the periods of Jupiter's solar conjunction. The eclipsed observations are clustered around the sub-Jovian point at 0° west. The sunlit observations are scattered semi-evenly around Io, with the dashed line showing the average of three sunlit observations per 15° bin (or approximately one per 5° longitude). Note that while we have more observations of the leading hemisphere (centered on 90°W longitude), outbursts favor the trailing hemisphere (centered on 270°W longitude).
Paper: Discovery of Seven Volcanic Outbursts on Io from an Infrared Telescope Facility Observation Campaign, 2016–2022
Authors: Christian D. Tate, Julie A. Rathbun, Alexander G. Hayes, John R. Spencer, Madeline Pettine
Figure caption: Phase angles of Io's total brightness values for the sunlit observations. Of the full range from 0° to 12°, there are 12 sunlit observations with phase angles below 2°. These low phase angle observations in reflected sunlight may have a significant brightness contribution from the opposition surge effect.
Paper: Discovery of Seven Volcanic Outbursts on Io from an Infrared Telescope Facility Observation Campaign, 2016–2022
Authors: Christian D. Tate, Julie A. Rathbun, Alexander G. Hayes, John R. Spencer, Madeline Pettine
Figure caption: Images of Io and Jupiter from the IRTF SpeX camera during the outburst event of 2019 May 8. Io is in eclipse. The images are the infrared photometric filters (a) narrowband Kcont 2.3 μm, (b) broadband Lprime 3.8 μm, and (c) broadband 4.5–5.1 μm M band (see Table 2). The double effect in the images is due to the subtraction of A and B frames when the telescope nods by 5″ in the north–south direction to remove the telescope's and atmosphere's first-order thermal effects. The frames are 30″ across. Notice the other Jovian moons visible in the contK-band image that disappear in the longer-wavelength images. The Lprime is used for the occultations both because of its sensitivity to thermal anomalies on Io and because Jupiter itself is less bright due to its methane absorption. The signal-to-noise ratio is noticeably lower for the M-band images.
Paper: Discovery of Seven Volcanic Outbursts on Io from an Infrared Telescope Facility Observation Campaign, 2016–2022
Authors: Christian D. Tate, Julie A. Rathbun, Alexander G. Hayes, John R. Spencer, Madeline Pettine
Figure caption: Time series of Io's eclipsed disk-integrated sub-Jovian intensity for 2016–2022 in three bands. The three outbursts in this plot stand out in the contK band, which is near the peak of the spectral emissions for these volcanic events. The gray shaded regions show the periods of time when Jupiter is in solar conjunction.
Paper: Discovery of Seven Volcanic Outbursts on Io from an Infrared Telescope Facility Observation Campaign, 2016–2022
Authors: Christian D. Tate, Julie A. Rathbun, Alexander G. Hayes, John R. Spencer, Madeline Pettine
Figure caption: Localization constraints of the 201905A and 201906A outbursts at Acala Fluctus. The image in panel (b) is the IRTF SpeX direct image of Io on 2010 June 25.
Paper: Discovery of Seven Volcanic Outbursts on Io from an Infrared Telescope Facility Observation Campaign, 2016–2022
Authors: Christian D. Tate, Julie A. Rathbun, Alexander G. Hayes, John R. Spencer, Madeline Pettine
Figure caption: Time series of Io's total 3.8 μm endogenic brightness values for both eclipse and sunlit observations (where the estimated contribution from reflected sunlight has been subtracted). The outburst events are the points above 150 GW sr−1 μm−1. Despite the larger uncertainty in the sunlit observations, the events in 2018 May and 2021 August stand out. The gray shaded regions show the periods of Jupiter's solar conjunction when Io is not visible from Earth.
Paper: Discovery of Seven Volcanic Outbursts on Io from an Infrared Telescope Facility Observation Campaign, 2016–2022
Authors: Christian D. Tate, Julie A. Rathbun, Alexander G. Hayes, John R. Spencer, Madeline Pettine
Figure caption: Map showing the constrained locations of the outbursts characterized in this paper. The green lines are the occultation detections, and the outburst can be anywhere along the line. The purple squares show the outbursts discovered in sunlight; the black lines are their localization uncertainties.