adsabs/AstroCLIMB huggingface dataset:
Paper: Juno’s JunoCam Images of Europa
Authors: C. J. Hansen, M. A. Ravine, P. M. Schenk, G. C. Collins, E. J. Leonard, C. B. Phillips, M. A. Caplinger, F. Tosi, S. J. Bolton, Björn Jónsson
Figure caption: Difference images between Galileo (1997) and JunoCam (2022) imaging of Europa. The map is a simple cylindrical map projection centered at 40°E longitude. Left: Galileo G2 observation to JunoCam observation 4; right: Galileo C10 observation to JunoCam 4. White arrows highlight linear ridges or belts with dark difference signatures due to increased emission angles in the JunoCam observation. Black arrow highlights unusual but unresolved features with brightness difference attributed to different photometric phase functions.
Paper: Juno’s JunoCam Images of Europa
Authors: C. J. Hansen, M. A. Ravine, P. M. Schenk, G. C. Collins, E. J. Leonard, C. B. Phillips, M. A. Caplinger, F. Tosi, S. J. Bolton, Björn Jónsson
Figure caption: The image on the left shows the Galileo coverage while the image on the right was taken by JunoCam. The Galileo image shows the band of much less differentiated terrain, filled in by the JunoCam image on the right. While some of the differences in the two geologic maps arise from an improved mapping scale, others are due to the improved resolution, less radiation noise, and different lighting conditions of the two basemaps. The 1:15M geologic map based on the Galileo data is shown on the bottom left (Leonard et al. 2018, 2024), with a more detailed version allowed by the JunoCam imagery (∼1:10M) shown on the bottom right.
Paper: Juno’s JunoCam Images of Europa
Authors: C. J. Hansen, M. A. Ravine, P. M. Schenk, G. C. Collins, E. J. Leonard, C. B. Phillips, M. A. Caplinger, F. Tosi, S. J. Bolton, Björn Jónsson
Figure caption: The image on the left shows two northeast-trending bright bands emerging from the terminator of the color JunoCam image at 19°N and 39°N. The image on the right shows the locations of the bright bands Corick and Pasiphae in cyan. Interpreted tail-crack structures emanating from their eastern termini are mapped as dashed magenta lines. Simple cylindrical projection; background grayscale image is the global Voyager-Galileo image mosaic. The background mosaic is downloadable from the USGS online: https://astrogeology.usgs.gov/search/map/Ganymede/Voyager-Galileo/Ganymede_Voyager_GalileoSSI_global_mosaic_1km.
Paper: Juno’s JunoCam Images of Europa
Authors: C. J. Hansen, M. A. Ravine, P. M. Schenk, G. C. Collins, E. J. Leonard, C. B. Phillips, M. A. Caplinger, F. Tosi, S. J. Bolton, Björn Jónsson
Figure caption: A portion of JunoCam observation 2, green filter, as compared to Galileo clear image 6439 from orbit I25, has been coregistered and masked to include overlap areas only, and their ratio (right). The difference in terminator position between the two images (the terminator is just off to the right side of the Galileo image) reveals details of two large vertical troughs, and Midir crater is visible near the upper right. Differences between the two images can be attributed to differences in lighting and viewing geometry; no surface changes attributed to geologic activity are visible.
Paper: Juno’s JunoCam Images of Europa
Authors: C. J. Hansen, M. A. Ravine, P. M. Schenk, G. C. Collins, E. J. Leonard, C. B. Phillips, M. A. Caplinger, F. Tosi, S. J. Bolton, Björn Jónsson
Figure caption: Red/blue color ratio map of Europa from JunoCam observation 4. While the known reddish lineaments and irregular-shaped chaos patches are apparent, no diffuse patterns are evident to suggest ongoing plume deposition. The circular feature on the lower left is Callanish at −16.7/334.5W, identified as a large ringed feature with a diameter of 107.0 km.
Paper: Juno’s JunoCam Images of Europa
Authors: C. J. Hansen, M. A. Ravine, P. M. Schenk, G. C. Collins, E. J. Leonard, C. B. Phillips, M. A. Caplinger, F. Tosi, S. J. Bolton, Björn Jónsson
Figure caption: Midir crater in the Galileo basemap (left) and the JunoCam image (right). Both images were obtained at high incidence angles, but with opposite lighting directions. The Galileo image is lit from the left and the JunoCam image is lit from the right.
Paper: Juno’s JunoCam Images of Europa
Authors: C. J. Hansen, M. A. Ravine, P. M. Schenk, G. C. Collins, E. J. Leonard, C. B. Phillips, M. A. Caplinger, F. Tosi, S. J. Bolton, Björn Jónsson
Figure caption: A subtle change in color of the prominent north–south trending curved cycloid in the center is seen between the first and third images, possibly due to phase function effects. The relatively bluish tint might be interpreted as an indication of relatively youthful age.
Paper: Juno’s JunoCam Images of Europa
Authors: C. J. Hansen, M. A. Ravine, P. M. Schenk, G. C. Collins, E. J. Leonard, C. B. Phillips, M. A. Caplinger, F. Tosi, S. J. Bolton, Björn Jónsson
Figure caption: Gwern “crater” in the Galileo basemap (left) is shown to be a set of intersecting ridges in the JunoCam images (right).
Paper: Rotational Study of 5:3 and 7:4 Resonant Objects within the Main Classical Trans-Neptunian Belt
Authors: Audrey Thirouin, Scott S. Sheppard
Figure caption: The amplitude distributions for the 5:3 and 7:4 resonances are plotted (plots (a) and (b)). Due to the ambiguous dynamical class of 2003 SP317, it is color-coded differently and added to the distribution of the 7:4 being the closest in semimajor axis. Only ∼23% have a flat lightcurve. Similarly, as for the cold classicals, there is a trend between amplitude and period (plot (c); Thirouin & Sheppard 2019a).
Paper: Rotational Study of 5:3 and 7:4 Resonant Objects within the Main Classical Trans-Neptunian Belt
Authors: Audrey Thirouin, Scott S. Sheppard
Figure caption: We overplot a Maxwellian distribution to fit the rotational frequency distribution of several subpopulations, such as the cold classicals, the contact binaries across the trans-Neptunian belt, the other TNOs including all the objects except for the cold classicals and the resolved binaries, and the TNOs discussed in this paper. All the subpopulations follow a Maxwellian distribution, and we infer that the mean rotational periods of the cold classicals and TNOs from this paper are similar.
Paper: Rotational Study of 5:3 and 7:4 Resonant Objects within the Main Classical Trans-Neptunian Belt
Authors: Audrey Thirouin, Scott S. Sheppard
Figure caption: The periodogram’s tallest peak is at 5.56 cycles day−1, but as the lightcurve of 2001 QF331 is asymmetric and has a large amplitude, the double-peaked period of 8.63 hr is the adequate solution. The lightcurve is fitted with a second-order Fourier series (black curve) suggesting that this object is elongated.
Paper: Rotational Study of 5:3 and 7:4 Resonant Objects within the Main Classical Trans-Neptunian Belt
Authors: Audrey Thirouin, Scott S. Sheppard
Figure caption: We infer that the lightcurve of 2015 FP345 is double-peaked with ﹩{P}_{\mathrm{rotational}}^{\mathrm{double}}﹩ = 8.47 ± 0.02 hr. This lightcurve is fitted by a Fourier series demonstrating that this object is elongated and likely has spot(s) on its surface.
Paper: Rotational Study of 5:3 and 7:4 Resonant Objects within the Main Classical Trans-Neptunian Belt
Authors: Audrey Thirouin, Scott S. Sheppard
Figure caption: The periodicity of 2006 CJ69 is ﹩{P}_{\mathrm{rotational}}^{\mathrm{double}}﹩ = 23.39 ± 0.07 hr (with the periodogram tallest peak at f = 2.05 cycles day−1; plot (a)). 2006 CJ69 is a likely contact binary, as shown by its variability and nonsinusoidal lightcurve. The χ 2 of the Fourier series fit is 1.19.
Paper: Rotational Study of 5:3 and 7:4 Resonant Objects within the Main Classical Trans-Neptunian Belt
Authors: Audrey Thirouin, Scott S. Sheppard
Figure caption: The partial lightcurve of 2004 VE131 using only the 2021 December data from the LDT displays a large amplitude and gives us a hint that the lightcurve of this object is asymmetric. 2004 VE131 is a potential contact binary.
Paper: Rotational Study of 5:3 and 7:4 Resonant Objects within the Main Classical Trans-Neptunian Belt
Authors: Audrey Thirouin, Scott S. Sheppard
Figure caption: We suggest that 2004 SC60 has a double-peaked rotation of 58.09 ± 0.08 hr and Δm = 0.44 ± 0.04 mag. The lightcurve morphology is best interpreted if 2004 SC60 is a likely contact binary. The χ 2 of the Fourier series fit is 1.65.
Paper: Rotational Study of 5:3 and 7:4 Resonant Objects within the Main Classical Trans-Neptunian Belt
Authors: Audrey Thirouin, Scott S. Sheppard
Figure caption: A double-peaked lightcurve with ﹩{P}_{\mathrm{rotational}}^{\mathrm{double}}﹩ = 18.22 ± 0.04 hr and Δm = 0.40 ± 0.04 mag is favored for 2013 BN82. The fit is not perfect for our data (χ 2 = 1.53), inferring that 2013 BN82 is a likely contact binary.
Paper: Rotational Study of 5:3 and 7:4 Resonant Objects within the Main Classical Trans-Neptunian Belt
Authors: Audrey Thirouin, Scott S. Sheppard
Figure caption: The rotation of 2014 DK143 is ﹩{P}_{\mathrm{rotational}}^{\mathrm{double}}﹩ = 8.99 ± 0.03 hr. The asymmetric lightcurve with Δm = 0.21 ± 0.03 mag is well fitted by a Fourier series demonstrating that this object is elongated and has spot(s) on its surface.
Paper: Rotational Study of 5:3 and 7:4 Resonant Objects within the Main Classical Trans-Neptunian Belt
Authors: Audrey Thirouin, Scott S. Sheppard
Figure caption: Surface colors of small bodies trapped in the 5:3 (circles) and 7:4 (squares) resonances are color-coded such as orange for moderately red, red for very red, and brown for ultrared surfaces (plots (a) and (b)). The limit at an inclination of 10◦ separating the cold from the hot classical component is the dotted line (Sheppard 2012). Contact binaries (filled stars for most likely and likely, open stars for potential) and elongated objects (diamonds) are ultrared objects, except Manwë–Thorondor (plot (c)). In plot (d), cyan and teal circles are for 7:4 and 5:3 resonants (respectively) with a full lightcurve, whereas the triangles indicate a lower limit for the lightcurve amplitude. The ﹩i^{\prime} ﹩-band magnitude of 2003 SP317 (brown triangle in plots (a) and (b)) is unknown; therefore, this object is not included in plot (d), and only the ﹩g^{\prime} -r^{\prime} ﹩ is taken into account in plot (a).
Paper: Rotational Study of 5:3 and 7:4 Resonant Objects within the Main Classical Trans-Neptunian Belt
Authors: Audrey Thirouin, Scott S. Sheppard
Figure caption: We compare the rotational properties of the 2:1, 3:2, 7:4, 5:3, and cold classical (CC) TNOs (plots (a), (b), and (c)). The legend is the same for all plots. Running means show that small objects are more deformed in all subpopulations (plot (a)). Regions A, B, and C are defined in Sheppard & Jewitt (2004) and described in Section 3. Most TNOs are in region C, and only a handful of them have an amplitude larger than 0.9 mag (plot (c)). For clarity, error bars are not plotted.
Paper: Expanding Mars’s Climate Modeling: Interpretable Machine Learning for Modeling Mars Science Laboratory Relative Humidity
Authors: Nour Abdelmoneim, Dattaraj B. Dhuri, Dimitra Atri, Germán Martínez
Figure caption: RH observations by REMS. The left panel shows 5 yr of REMS RH. The corresponding data that are used for training (MY 31–MY 34), validation (MY 35), and testing (MY 36) are indicated. Seasonal variation is shown in the middle panel. Diurnal variation is shown in the right panel.
Paper: Rotational Study of 5:3 and 7:4 Resonant Objects within the Main Classical Trans-Neptunian Belt
Authors: Audrey Thirouin, Scott S. Sheppard
Figure caption: Objects in the 5:3 mean-motion resonance with Neptune.
Paper: Rotational Study of 5:3 and 7:4 Resonant Objects within the Main Classical Trans-Neptunian Belt
Authors: Audrey Thirouin, Scott S. Sheppard
Figure caption: Objects in the 7:4 mean-motion resonance with Neptune.
Paper: Challenges in Identifying Artificial Objects in the Near-Earth Object Population: Spectral Characterization of 2020 SO
Authors: Adam Battle, Vishnu Reddy, Juan A. Sanchez, Benjamin Sharkey, Tanner Campbell, Paul Chodas, Al Conrad, Daniel P. Engelhart, James Frith, Roberto Furfaro, Davide Farnocchia, Olga Kuhn, Neil Pearson, Barry Rothberg, Christian Veillet, Richard Wainscoat
Figure caption: Visible spectra of 2020 SO and several Centaur-D R/Bs overlaid on the NIR spectrum of 2020 SO, showing overall agreement in the visible wavelengths. The average Bus-DeMeo D-type asteroid visible-NIR spectrum from DeMeo et al. (2009a) is also shown for comparison. All of the spectra are normalized at 0.7 μm.
Paper: Challenges in Identifying Artificial Objects in the Near-Earth Object Population: Spectral Characterization of 2020 SO
Authors: Adam Battle, Vishnu Reddy, Juan A. Sanchez, Benjamin Sharkey, Tanner Campbell, Paul Chodas, Al Conrad, Daniel P. Engelhart, James Frith, Roberto Furfaro, Davide Farnocchia, Olga Kuhn, Neil Pearson, Barry Rothberg, Christian Veillet, Richard Wainscoat
Figure caption: Photometric color spectrum of 2020 SO taken with the LBT compared to the average visible spectrum for S- and D-type asteroids in the Bus–DeMeo taxonomy. Error bars represent 1σ uncertainties and all spectra are normalized at 0.7 μm.
Paper: Challenges in Identifying Artificial Objects in the Near-Earth Object Population: Spectral Characterization of 2020 SO
Authors: Adam Battle, Vishnu Reddy, Juan A. Sanchez, Benjamin Sharkey, Tanner Campbell, Paul Chodas, Al Conrad, Daniel P. Engelhart, James Frith, Roberto Furfaro, Davide Farnocchia, Olga Kuhn, Neil Pearson, Barry Rothberg, Christian Veillet, Richard Wainscoat
Figure caption: Near-infrared spectra of 2020 SO taken during its approach and normalized at 1.5 μm. The phase angle (PA) during observations is indicated in the legend. Vertical arrows point to the approximate location of observed absorption bands.
Paper: Challenges in Identifying Artificial Objects in the Near-Earth Object Population: Spectral Characterization of 2020 SO
Authors: Adam Battle, Vishnu Reddy, Juan A. Sanchez, Benjamin Sharkey, Tanner Campbell, Paul Chodas, Al Conrad, Daniel P. Engelhart, James Frith, Roberto Furfaro, Davide Farnocchia, Olga Kuhn, Neil Pearson, Barry Rothberg, Christian Veillet, Richard Wainscoat
Figure caption: Phase angle (top) and brightness (bottom) of 2020 SO over time with UTC dates of campaign observations marked by vertical lines that span both subplots. The brightness axis is inverted so that brighter magnitudes (smaller numbers) appear higher. Data were retrieved from JPL Horizons prior to the object’s removal as an NEO from their database.
Paper: Challenges in Identifying Artificial Objects in the Near-Earth Object Population: Spectral Characterization of 2020 SO
Authors: Adam Battle, Vishnu Reddy, Juan A. Sanchez, Benjamin Sharkey, Tanner Campbell, Paul Chodas, Al Conrad, Daniel P. Engelhart, James Frith, Roberto Furfaro, Davide Farnocchia, Olga Kuhn, Neil Pearson, Barry Rothberg, Christian Veillet, Richard Wainscoat
Figure caption: Visible spectra of 2020 SO compared to several Centaur-D R/Bs, normalized at 0.7 μm. Variations in the slope of the Centaur spectra are likely due to phase angle variations between observations.
Paper: Challenges in Identifying Artificial Objects in the Near-Earth Object Population: Spectral Characterization of 2020 SO
Authors: Adam Battle, Vishnu Reddy, Juan A. Sanchez, Benjamin Sharkey, Tanner Campbell, Paul Chodas, Al Conrad, Daniel P. Engelhart, James Frith, Roberto Furfaro, Davide Farnocchia, Olga Kuhn, Neil Pearson, Barry Rothberg, Christian Veillet, Richard Wainscoat
Figure caption: End-member spectra for two materials found on Centaur-D R/Bs. Stainless steel (left) from Jorgensen (2000) and Jorgensen et al. (2001) shows a red spectral slope with a broad, subtle 1 μm feature. The double peak near 1.3–1.4 μm is due to detector dynamic range limitations and is not a real feature of stainless steel. PVF (right) shows a blue spectral slope after 0.5 μm with strong absorption bands near 1.7 and 2.3 μm plus fainter bands near 1.2 and 1.4 μm. Both spectra are normalized at 1.5 μm. Band parameters for the three deeper PVF bands are given in Table 2.
Paper: Challenges in Identifying Artificial Objects in the Near-Earth Object Population: Spectral Characterization of 2020 SO
Authors: Adam Battle, Vishnu Reddy, Juan A. Sanchez, Benjamin Sharkey, Tanner Campbell, Paul Chodas, Al Conrad, Daniel P. Engelhart, James Frith, Roberto Furfaro, Davide Farnocchia, Olga Kuhn, Neil Pearson, Barry Rothberg, Christian Veillet, Richard Wainscoat
Figure caption: Near-infrared spectra of 2020 SO and a Centaur-D R/B showing similar features. Both spectra are normalized at 1.5 μm. Two absorption bands from PVF consistent with those seen on 2020 SO are indicated with vertical arrows.
Paper: Challenges in Identifying Artificial Objects in the Near-Earth Object Population: Spectral Characterization of 2020 SO
Authors: Adam Battle, Vishnu Reddy, Juan A. Sanchez, Benjamin Sharkey, Tanner Campbell, Paul Chodas, Al Conrad, Daniel P. Engelhart, James Frith, Roberto Furfaro, Davide Farnocchia, Olga Kuhn, Neil Pearson, Barry Rothberg, Christian Veillet, Richard Wainscoat
Figure caption: Photograph of a Centaur upper stage being installed and readied at the General Dynamics factory in 1962. The photo shows the stainless-steel body and engines with the white polyvinyl fluoride on the aft bulkhead radiation shield. Image credit: NASA GRC.
Paper: Subsurface Thermophysical Properties of Europa’s Leading and Trailing Hemispheres as Revealed by ALMA
Authors: Alexander E. Thelen, Katherine de Kleer, Maria Camarca, Alex Akins, Mark Gurwell, Bryan Butler, Imke de Pater
Figure caption: Top: Residuals (data-model) for single, hemispheric best-fit porosity values for Europa’s leading hemisphere (∼90°W longitude) from Band 3 (97.5 GHz/3.05 mm; (A)), Band 6 (233 GHz/1.25 mm; (B)), and Band 7 (343.5 GHz/0.88 mm; (C)). All images are aligned with Europa’s north pole along the vertical axis. Bottom: Residual contours are plotted on projected image maps of Europa’s surface from the USGS Voyager and Galileo SSI composite map. Positive temperature contours are shown as redscale, solid lines; negative contours are in bluescale, dashed lines. Contour levels increase in increments of 3σ (rms noise varies between observation, on the order of 0.1–1 K). The approximate locations of leading hemisphere regiones are denoted for reference in panel (D).
Paper: Subsurface Thermophysical Properties of Europa’s Leading and Trailing Hemispheres as Revealed by ALMA
Authors: Alexander E. Thelen, Katherine de Kleer, Maria Camarca, Alex Akins, Mark Gurwell, Bryan Butler, Imke de Pater
Figure caption: (A) ALMA Band 3 (3.05 mm) residuals from 50% porosity models projected into cylindrical latitude and longitude coordinates, and only including data for emission angles less than 75°. The synthesized ALMA beam for each observation (without projecting to cylindrical coordinates) is shown below both leading and trailing hemisphere projections as a hashed ellipse. (B) Combined residuals from Band 6 (1.25 mm) and Band 7 (0.88 mm) models of the global average values of Europa’s leading and trailing hemisphere (64% in Band 6, 52% in Band 7) projected in cylindrical latitude and longitude coordinates. The representative average ALMA beam over all Band 6 and 7 observations is shown as the hashed ellipse for comparison. (C) Averaged positive (light-red solid contours) and negative (light-blue dashed contours) residuals from (B) with magnitudes >3 × the average rms (∼0.8 K) overlaid onto a deprojected mosaic of Europa’s surface from Galileo SSI and Voyager images. Europa’s surface quadrants are demarcated by dotted lines (Doggett et al. 2009). Relevant geographic features are labeled and approximate outlines defined by Leonard et al. (2017) are shown in all panels: black contours show Europa’s chaos regions, and purple contours show the locations of the ringed terrain and ejecta blankets surrounding Pwyll, Tyre, and Taliesin craters. Artifacts exist in both the colormap in (B) and contours in (C) due to the combination of data from multiple executions in both ALMA bands.
Paper: Subsurface Thermophysical Properties of Europa’s Leading and Trailing Hemispheres as Revealed by ALMA
Authors: Alexander E. Thelen, Katherine de Kleer, Maria Camarca, Alex Akins, Mark Gurwell, Bryan Butler, Imke de Pater
Figure caption: Top: Residuals (data-model) for single, hemispheric best-fit porosity values for Europa’s trailing hemisphere (∼270°W longitude) from Band 3 (A), Band 6 (B)–(C), and Band 7 (D). Note the different colorbars between the three ALMA bands. All images are aligned with Europa’s north pole along the vertical axis. Bottom: Residual contours are plotted on projected image maps of Europa’s surface from the USGS as in Figure 2. Contour levels increase in increments of 3σ, e.g., 3× the image rms noise. The approximate locations of regiones and Pwyll crater are denoted for reference in panels (E) and (H).
Paper: Subsurface Thermophysical Properties of Europa’s Leading and Trailing Hemispheres as Revealed by ALMA
Authors: Alexander E. Thelen, Katherine de Kleer, Maria Camarca, Alex Akins, Mark Gurwell, Bryan Butler, Imke de Pater
Figure caption: (A) Comparison of Europa’s disk-averaged brightness temperatures as a function of frequency from ALMA (weighted averages from this work; purple), other radio/(sub)millimeter facilities including the VLA (de Pater et al. 1984; Muhleman et al. 1986; Butler 2012), the IRAM 30 m dish (Altenhoff et al. 1988), the SMA (Gurwell et al. 2024, private communication), OVRO (Muhleman & Berge 1991), and infrared measurements using SOFIA (de Pater et al. 2021a) and the NASA IRTF (de Pater et al. 1989). Predictions of the maximum surface temperatures at visible wavelengths from Morrison et al. (1977) are shown in black. (B) Brightness temperatures as a function of frequency in the (sub)millimeter wavelength regime from both the leading (crosses) and trailing (diamonds) hemispheres as measured by ALMA (this work; purple) and the SMA (Gurwell et al. 2024, private communication; red). Data from the IRAM 30 m telescope are also shown (Altenhoff et al. 1988; blue).
Paper: Subsurface Thermophysical Properties of Europa’s Leading and Trailing Hemispheres as Revealed by ALMA
Authors: Alexander E. Thelen, Katherine de Kleer, Maria Camarca, Alex Akins, Mark Gurwell, Bryan Butler, Imke de Pater
Figure caption: Image targeting Europa’s leading hemisphere in Band 7 (top right-hand side) with Ganymede in the extended ALMA field (lower left-hand side), approximately 15″ away. Primary beam correction has been applied to normalize the gain across the extended FOV. The ALMA beam size appears as the white ellipse in the lower left corner.
Paper: Subsurface Thermophysical Properties of Europa’s Leading and Trailing Hemispheres as Revealed by ALMA
Authors: Alexander E. Thelen, Katherine de Kleer, Maria Camarca, Alex Akins, Mark Gurwell, Bryan Butler, Imke de Pater
Figure caption: Brightness temperature maps of Europa’s leading hemisphere (∼90°W longitude; top row) and trailing hemisphere (∼270°W longitude; bottom row) from Band 3 (3.05 mm; (A), (E)), Band 6 (1.25 mm; B, (F)–(H)), and Band 7 (0.88 mm; (C), (G)). The ALMA beam (the full-width at half-maximum of the ALMA point-spread function) is shown as a hashed ellipse in the bottom left-hand corner. All images are aligned with Europa’s north pole along the vertical axis.
Paper: Subsurface Thermophysical Properties of Europa’s Leading and Trailing Hemispheres as Revealed by ALMA
Authors: Alexander E. Thelen, Katherine de Kleer, Maria Camarca, Alex Akins, Mark Gurwell, Bryan Butler, Imke de Pater
Figure caption: Comparisons of ALMA Band 7 residuals of Europa’s leading hemisphere: the initial deconvolution, without taking into account the interloping satellite (A), and the final deconvolution with the inclusion of Ganymede (B); the latter is comparable to Figure 6 (C). Note the change in colorbar scale between the two images. Europa’s surface is shown (dashed circle), as are separate contours for each image (solid lines): 1σ intervals (A) and 3σ intervals (B).