adsabs/AstroCLIMB huggingface dataset:
Paper: The ESA Hera Mission: Detailed Characterization of the DART Impact Outcome and of the Binary Asteroid (65803) Didymos
Authors: Patrick Michel, Michael Küppers, Adriano Campo Bagatin, Benoit Carry, Sébastien Charnoz, Julia de Leon, Alan Fitzsimmons, Paulo Gordo, Simon F. Green, Alain Hérique, Martin Juzi, Özgür Karatekin, Tomas Kohout, Monica Lazzarin, Naomi Murdoch, Tatsuaki Okada, Ernesto Palomba, Petr Pravec, Colin Snodgrass, Paolo Tortora, Kleomenis Tsiganis, Stephan Ulamec, Jean-Baptiste Vincent, Kai Wünnemann, Yun Zhang, Sabina D. Raducan, Elisabetta Dotto, Nancy Chabot, Andy F. Cheng, Andy Rivkin, Olivier Barnouin, Carolyn Ernst, Angela Stickle, Derek C. Richardson, Cristina Thomas, Masahiko Arakawa, Hirdy Miyamoto, Akiko Nakamura, Seiji Sugita, Makoto Yoshikawa, Paul Abell, Erik Asphaug, Ronald-Louis Ballouz, William F. Bottke, Dante S. Lauretta, Kevin J. Walsh, Paolo Martino, Ian Carnelli
Figure caption: Organization of the Hera Science Team; see also https://www.heramission.space/team.
Paper: The ESA Hera Mission: Detailed Characterization of the DART Impact Outcome and of the Binary Asteroid (65803) Didymos
Authors: Patrick Michel, Michael Küppers, Adriano Campo Bagatin, Benoit Carry, Sébastien Charnoz, Julia de Leon, Alan Fitzsimmons, Paulo Gordo, Simon F. Green, Alain Hérique, Martin Juzi, Özgür Karatekin, Tomas Kohout, Monica Lazzarin, Naomi Murdoch, Tatsuaki Okada, Ernesto Palomba, Petr Pravec, Colin Snodgrass, Paolo Tortora, Kleomenis Tsiganis, Stephan Ulamec, Jean-Baptiste Vincent, Kai Wünnemann, Yun Zhang, Sabina D. Raducan, Elisabetta Dotto, Nancy Chabot, Andy F. Cheng, Andy Rivkin, Olivier Barnouin, Carolyn Ernst, Angela Stickle, Derek C. Richardson, Cristina Thomas, Masahiko Arakawa, Hirdy Miyamoto, Akiko Nakamura, Seiji Sugita, Makoto Yoshikawa, Paul Abell, Erik Asphaug, Ronald-Louis Ballouz, William F. Bottke, Dante S. Lauretta, Kevin J. Walsh, Paolo Martino, Ian Carnelli
Figure caption: Rendering of the Milani CubeSat.
Paper: New Constraints on the Volatile Deposit in Mercury’s North Polar Crater, Prokofiev
Authors: Michael K. Barker, Nancy L. Chabot, Erwan Mazarico, Matthew A. Siegler, Jose M. Martinez-Camacho, Colin D. Hamill, Stefano Bertone
Figure caption: Left: elevation residuals of MLA altimetry in radar-bright (green) and non-radar-bright areas (orange) relative to the best-fit radial profile in Figure 8. Right: elevation residuals (in kilometers) with radar-bright regions overlaid (white lines). The solid gray and magenta circles denote the initial and best-fit crater centroid, respectively.
Paper: Autonomous Navigation Performance Using Natural Feature Tracking during the OSIRIS-REx Touch-and-Go Sample Collection Event
Authors: C. D. Norman, C. J. Miller, R. D. Olds, C. E. Mario, E. E. Palmer, O. S. Barnouin, M. G. Daly, J. R. Weirich, J. A. Seabrook, C. A. Bennett, B. Rizk, B. J. Bos, D. S. Lauretta
Figure caption: A view of the safe-home orbit (green) and TAG trajectory (blue). The very dark asteroid Bennu is in the center. The Orbit Departure Maneuver (ODM) is indicated with the yellow triangle, Checkpoint (CP) with the orange triangle, and Matchpoint (MP) with the red triangle.
Paper: New Constraints on the Volatile Deposit in Mercury’s North Polar Crater, Prokofiev
Authors: Michael K. Barker, Nancy L. Chabot, Erwan Mazarico, Matthew A. Siegler, Jose M. Martinez-Camacho, Colin D. Hamill, Stefano Bertone
Figure caption: Distribution of T max for Prokofiev compared to that of the smaller, lower-latitude dark deposit craters studied in H20. Prokofiev’s non-radar-bright floor exhibits a peak at T max ∼ 310 K.
Paper: New Constraints on the Volatile Deposit in Mercury’s North Polar Crater, Prokofiev
Authors: Michael K. Barker, Nancy L. Chabot, Erwan Mazarico, Matthew A. Siegler, Jose M. Martinez-Camacho, Colin D. Hamill, Stefano Bertone
Figure caption: Histograms of slope (left) and roughness (right) over baselines ≤1 km inside (red) and outside (blue) radar-bright regions within a crater-centric radius of 20–38 km. Error bars represent the standard deviation of a bootstrap sample size of 1000 (see text for details). Roughness is computed only for slopes <10°.
Paper: New Constraints on the Volatile Deposit in Mercury’s North Polar Crater, Prokofiev
Authors: Michael K. Barker, Nancy L. Chabot, Erwan Mazarico, Matthew A. Siegler, Jose M. Martinez-Camacho, Colin D. Hamill, Stefano Bertone
Figure caption: Left: slope (in degrees) of plane fits to MLA footprints over a maximum baseline of 1 km. Right: roughness (in meters) computed as the corresponding slope-detrended standard deviation. Gray pixels contain too few (<5) MLA footprints for the analysis.
Paper: Autonomous Navigation Performance Using Natural Feature Tracking during the OSIRIS-REx Touch-and-Go Sample Collection Event
Authors: C. D. Norman, C. J. Miller, R. D. Olds, C. E. Mario, E. E. Palmer, O. S. Barnouin, M. G. Daly, J. R. Weirich, J. A. Seabrook, C. A. Bennett, B. Rizk, B. J. Bos, D. S. Lauretta
Figure caption: Potential NFT image footprint for image 21 of the Nightingale TAG trajectory. The dark-blue area represents the nominal NFT image footprint for image 21, the green area represents the 1σ potential NFT image footprint, and the orange area represents the 3σ potential NFT image footprint.
Paper: Autonomous Navigation Performance Using Natural Feature Tracking during the OSIRIS-REx Touch-and-Go Sample Collection Event
Authors: C. D. Norman, C. J. Miller, R. D. Olds, C. E. Mario, E. E. Palmer, O. S. Barnouin, M. G. Daly, J. R. Weirich, J. A. Seabrook, C. A. Bennett, B. Rizk, B. J. Bos, D. S. Lauretta
Figure caption: Example of the type of terrain that constitutes a strong feature. Feature M4248 is outlined in green. The green box is approximately 4 m × 4 m. Cropped from an OCAMS PolyCam image, with north downward in the image.
Paper: Autonomous Navigation Performance Using Natural Feature Tracking during the OSIRIS-REx Touch-and-Go Sample Collection Event
Authors: C. D. Norman, C. J. Miller, R. D. Olds, C. E. Mario, E. E. Palmer, O. S. Barnouin, M. G. Daly, J. R. Weirich, J. A. Seabrook, C. A. Bennett, B. Rizk, B. J. Bos, D. S. Lauretta
Figure caption: As-flown TAG feature correlation performance. Blue circles represent primary correlation peaks seen during TAG, and red crosses represent secondary or false correlation peaks from TAG. The dashed line at a correlation value 0.45 represents the minimum threshold at which NFT accepts measurements.
Paper: Autonomous Navigation Performance Using Natural Feature Tracking during the OSIRIS-REx Touch-and-Go Sample Collection Event
Authors: C. D. Norman, C. J. Miller, R. D. Olds, C. E. Mario, E. E. Palmer, O. S. Barnouin, M. G. Daly, J. R. Weirich, J. A. Seabrook, C. A. Bennett, B. Rizk, B. J. Bos, D. S. Lauretta
Figure caption: Post-update residuals as a multiple of the GSD of the feature in the image. Features 35, 38, 39, 58, 69, and 90 are shown by colored crosses. The six features show twice (or more) the residual of the next-largest residual in at least one image.
Paper: Autonomous Navigation Performance Using Natural Feature Tracking during the OSIRIS-REx Touch-and-Go Sample Collection Event
Authors: C. D. Norman, C. J. Miller, R. D. Olds, C. E. Mario, E. E. Palmer, O. S. Barnouin, M. G. Daly, J. R. Weirich, J. A. Seabrook, C. A. Bennett, B. Rizk, B. J. Bos, D. S. Lauretta
Figure caption: A correlation example showing probable feature position error. The left panel shows a cropped portion of image 20 centered on the predicted location of feature 38. The middle panel shows the rendering of the feature produced by NFT, and the right panel shows the resulting correlation surface. Note that the correlation surface peak in the right panel is shifted up and left relative to the expected center location, as is the matched location in the left panel.
Paper: Autonomous Navigation Performance Using Natural Feature Tracking during the OSIRIS-REx Touch-and-Go Sample Collection Event
Authors: C. D. Norman, C. J. Miller, R. D. Olds, C. E. Mario, E. E. Palmer, O. S. Barnouin, M. G. Daly, J. R. Weirich, J. A. Seabrook, C. A. Bennett, B. Rizk, B. J. Bos, D. S. Lauretta
Figure caption: Measured feature residuals for Checkpoint rehearsal (CPR), Matchpoint rehearsal (MPR), and TAG. Pre-CP images are those taken between the ODM and Checkpoint. CP-MP images are those taken between Checkpoint and Matchpoint. Post-MP images are those taken after Matchpoint. All residuals were less than 50 cm except in the case of four images (not shown).
Paper: Autonomous Navigation Performance Using Natural Feature Tracking during the OSIRIS-REx Touch-and-Go Sample Collection Event
Authors: C. D. Norman, C. J. Miller, R. D. Olds, C. E. Mario, E. E. Palmer, O. S. Barnouin, M. G. Daly, J. R. Weirich, J. A. Seabrook, C. A. Bennett, B. Rizk, B. J. Bos, D. S. Lauretta
Figure caption: The residuals for TAG are shown for both the pre-update (measurement residuals) and post-update (ground post-processing). The post-update residuals are smaller for the majority of features, as would be expected.
Paper: Autonomous Navigation Performance Using Natural Feature Tracking during the OSIRIS-REx Touch-and-Go Sample Collection Event
Authors: C. D. Norman, C. J. Miller, R. D. Olds, C. E. Mario, E. E. Palmer, O. S. Barnouin, M. G. Daly, J. R. Weirich, J. A. Seabrook, C. A. Bennett, B. Rizk, B. J. Bos, D. S. Lauretta
Figure caption: Comparison of imagery and rendering of feature 90 in NFT image 30 during TAG. The image on the left is the portion of NFT image 30 during TAG that is consistent with the feature location. The image on the right is NFT's rendering of feature 90. The feature is approximately 1 m across at a resolution of 1.14 cm pixel−1.
Paper: Autonomous Navigation Performance Using Natural Feature Tracking during the OSIRIS-REx Touch-and-Go Sample Collection Event
Authors: C. D. Norman, C. J. Miller, R. D. Olds, C. E. Mario, E. E. Palmer, O. S. Barnouin, M. G. Daly, J. R. Weirich, J. A. Seabrook, C. A. Bennett, B. Rizk, B. J. Bos, D. S. Lauretta
Figure caption: As-flown emission (top) and incidence (bottom) angles for feature measurements during TAG.
Paper: Autonomous Navigation Performance Using Natural Feature Tracking during the OSIRIS-REx Touch-and-Go Sample Collection Event
Authors: C. D. Norman, C. J. Miller, R. D. Olds, C. E. Mario, E. E. Palmer, O. S. Barnouin, M. G. Daly, J. R. Weirich, J. A. Seabrook, C. A. Bennett, B. Rizk, B. J. Bos, D. S. Lauretta
Figure caption: As-flown phase angles for feature measurements during TAG. The red circle highlights the poorer-performing feature 30.
Paper: Autonomous Navigation Performance Using Natural Feature Tracking during the OSIRIS-REx Touch-and-Go Sample Collection Event
Authors: C. D. Norman, C. J. Miller, R. D. Olds, C. E. Mario, E. E. Palmer, O. S. Barnouin, M. G. Daly, J. R. Weirich, J. A. Seabrook, C. A. Bennett, B. Rizk, B. J. Bos, D. S. Lauretta
Figure caption: As-flown GSDs for feature measurements during TAG.
Paper: Dynamical Evolution of Ejecta from the DART Impact on Dimorphos
Authors: Alessandro Rossi, Francesco Marzari, John Robert Brucato, Vincenzo Della Corte, Elisabetta Dotto, Simone Ieva, Stavro Lambrov Ivanovski, Alice Lucchetti, Elena Mazzotta Epifani, Maurizio Pajola, Giovanni Poggiali, Angelo Zinzi
Figure caption: Left panel: distribution of the impact velocities for the ejecta particles reimpacting either against Dimorphos (blue line) or against Didymos (red line). Right panel: distribution of the epochs of impact for the ejecta particles reimpacting either against Dimorphos (blue line) or against Didymos (red line).
Paper: Neptune’s Pole-on Magnetosphere: Dayside Reconnection Observations by Voyager 2
Authors: Jamie M. Jasinski, Neil Murphy, Xianzhe Jia, James A. Slavin
Figure caption: The V2 in situ measurements for the Neptune flyby on 1989 August 24. The different regions are labeled (with the solar wind labeled as “SW” and magnetosphere as “M'sphere”), and the boundaries of the bow shock, magnetopause, and the open closed field line boundary (OCB) marked by vertical dashed–dotted lines. Arrows identify features described in the text. “PDL” identifies the plasma depletion layer. The top two panels show LECP data for the electron 22–35 keV energy channel, with colored shading and bars displaying measurement uncertainties. Panel (a) shows the average count rate from all sectors, and panel (b) shows the count rates for three separate sectors with different pitch angle coverage. Panel (c) shows an electron spectrogram from PLS taken from Zhang et al. (1991), and panel (d) shows electron density. Panels (e)–(g) show the three components of the magnetic field measured by the magnetometer in NSO coordinates, and panel (h) shows the magnetic field magnitude.
Paper: Neptune’s Pole-on Magnetosphere: Dayside Reconnection Observations by Voyager 2
Authors: Jamie M. Jasinski, Neil Murphy, Xianzhe Jia, James A. Slavin
Figure caption: Schematic of the pole-on configuration of Neptune’s magnetosphere during the V2 flyby in 1989. The red line demonstrates the trajectory of V2 through the dayside magnetospheric boundaries and approximately corresponds to the data (time series) shown in Figure 2.
Paper: Neptune’s Pole-on Magnetosphere: Dayside Reconnection Observations by Voyager 2
Authors: Jamie M. Jasinski, Neil Murphy, Xianzhe Jia, James A. Slavin
Figure caption: Magnetic field measurements during the TCR observed at Neptune's cusp. Panels (a)–(d) show the three components of the magnetic field in NSO coordinates, as well as the magnitude.
Paper: Neptune’s Pole-on Magnetosphere: Dayside Reconnection Observations by Voyager 2
Authors: Jamie M. Jasinski, Neil Murphy, Xianzhe Jia, James A. Slavin
Figure caption: Location of antiparallel magnetic shear at the dayside magnetopause surface in the Y–Z plane (view from the Sun) for different IMF clock angles defined as ﹩| \arctan ({B}_{Y},{B}_{Z})| ﹩, where 0° and 180° are northward and southward, respectively, and 90° is dawnward/duskward; this is adapted from Masters (2015), who modeled the magnetopause conditions for magnetic reconnection at Neptune.
Paper: Spatially Resolved Observations of Europa’s Surface with Subaru/IRCS at 1.0–1.8 μm: Upper Limits to the Abundances of Hydrated Cl-bearing Salts
Authors: Shuya Tan, Yasuhito Sekine, Masayuki Kuzuhara
Figure caption: Reflectance spectra of Cl-bearing salts, H2O ice, H2SO4 · 8H2O, MgSO4 · 7H2O, and Europa’s surface. Data of Cl-bearing salts were obtained at 80 K (derived from Hanley et al. 2014), except for NaCl · 2H2O at 100 K (derived from Fox-Powell et al. 2019). The spectrum of NaCl · 2H2O is derived from the natural sample possibly containing impurities. VLT and Galileo/NIMS spectra were obtained at coordinates 195°W, 0°N and 130°–260°W, 35°S–35°N and taken from Ligier et al. (2016) and McCord et al. (1999), respectively. Reflectance spectra of H2O ice, H2SO4 · 8H2O, and MgSO4 · 7H2O were calculated using the Hapke model (Hapke 1981, 1993, 2002) with the optical constants for amorphous H2O ice at 70–130 K (Mastrapa et al. 2008), H2SO4 · 8H2O at ∼77 K (Carlson et al. 2005), and MgSO4 · 7H2O at 120 K (Dalton & Pitman 2012). Reflectance spectra are shown with positive offsets for clarification. Gray bars represent the wavelengths corresponding to possible absorptions of hydrated Cl-bearing salts (1.15–1.25 μm).
Paper: Spatially Resolved Observations of Europa’s Surface with Subaru/IRCS at 1.0–1.8 μm: Upper Limits to the Abundances of Hydrated Cl-bearing Salts
Authors: Shuya Tan, Yasuhito Sekine, Masayuki Kuzuhara
Figure caption: Illustration of the alignment of the slit for our observations of Europa. The slit was aligned in the east–west direction as applied to Europa. On Europa’s surface, the images were separated by ∼0.″087 in the slit-length direction. Apparent north pole position angles are the angles of Europa’s north pole with respect to the direction of the celestial north pole. The angular diameters and apparent north pole position angles were provided by NASA JPL Horizons (http://ssd.jpl.nasa.gov/).
Paper: Spatially Resolved Observations of Europa’s Surface with Subaru/IRCS at 1.0–1.8 μm: Upper Limits to the Abundances of Hydrated Cl-bearing Salts
Authors: Shuya Tan, Yasuhito Sekine, Masayuki Kuzuhara
Figure caption: Signal strength of Europa in the two-dimensional spectral images. (a) Europa’s signal strength extends in the wavelength direction. The flux distribution was extracted to produce two-dimensional spectra with a width of 40 pixels (see the narrow yellow rectangle). (b) Close-up of the two-dimensional spectra of Europa, corresponding to the range of the small blue rectangle in panel (a). Two-dimensional, 1.6-pixel-wide spectra were extracted in the direction of the slit length. Yellow dashed lines enclose sections with a width of 1.6 pixels each, corresponding to the spatial resolution of the Subaru AO system (∼0.″087).
Paper: Spatially Resolved Observations of Europa’s Surface with Subaru/IRCS at 1.0–1.8 μm: Upper Limits to the Abundances of Hydrated Cl-bearing Salts
Authors: Shuya Tan, Yasuhito Sekine, Masayuki Kuzuhara
Figure caption: Example of the slit position and location of Europa on the image as captured by the IRCS imaging mode on 2019 May 18. (a) Image with slit setting. The overlying slit was cut out of the disk of Europa. (b) Image without slit setting. The estimated slit position in panel (a) was applied to the green horizontal strip.
Paper: Spatially Resolved Observations of Europa’s Surface with Subaru/IRCS at 1.0–1.8 μm: Upper Limits to the Abundances of Hydrated Cl-bearing Salts
Authors: Shuya Tan, Yasuhito Sekine, Masayuki Kuzuhara
Figure caption: Observed regions on Europa’s surface map (image credit: USGS Map-a-planet). The green and yellow areas were observed on 2019 May 17 and 18, respectively. The green region covers the southeastern region of the trailing hemisphere (210°–180°W, 20°–50°S) and the southwestern region of the leading hemisphere (180–110°W, 20–50°S). The yellow area covers the southern region of the trailing hemisphere (330°–190°W, 30°–60°S). The gray area covers a part of the northern regions of the trailing hemisphere (256° ± 5°W, 15° ± 14°N). The red area covers a part of the equatorial regions of the leading hemisphere (160° ± 9°W, 3° ± 15°N). The spectral data of two areas are used for the estimations for hydrated Cl-bearing salts (see detailed in Section 4). The regions outlined by thick black lines enclose chaotic terrains (Doggett et al. 2009).
Paper: Spatially Resolved Observations of Europa’s Surface with Subaru/IRCS at 1.0–1.8 μm: Upper Limits to the Abundances of Hydrated Cl-bearing Salts
Authors: Shuya Tan, Yasuhito Sekine, Masayuki Kuzuhara
Figure caption: Typical reflectance spectra of Europa’s surface. Each curve shows spectra of one area (shown as colored regions in the upper right insets). (a) Data for the southern regions in the leading hemisphere observed on 2019 May 17. (b) Data for the southern regions in the trailing hemisphere observed on 2019 May 18. The black curves were obtained using Equation (1). Gray areas represent the uncertainty in the absolute value of the reflectance due to the uncertainties in the photometric correction factors, cos(i), and differences in the observing conditions of the G2V stars (see Section 2.3). The reflectance spectra can be shifted within the gray areas; however, the spectral features do not change.
Paper: Spatially Resolved Observations of Europa’s Surface with Subaru/IRCS at 1.0–1.8 μm: Upper Limits to the Abundances of Hydrated Cl-bearing Salts
Authors: Shuya Tan, Yasuhito Sekine, Masayuki Kuzuhara
Figure caption: Connected reflectance spectra of Europa’s surface at wavelengths of 1.0–1.8 μm. The observed area on Europa is shown in the upper left inset. (a) Data for the southern regions in the leading hemisphere observed on 2019 May 17. (b) Data for the southern regions in the trailing hemisphere observed on 2019 May 18. Gray bars represent the wavelengths corresponding to telluric atmospheric absorption (1.35–1.42 μm). Vertical dashed lines indicate a wavelength of 1.2 μm. In the reflectance spectra, we observe no significant absorption features around 1.2 μm, where hydrated Cl-bearing salts exhibit their characteristic absorption features.
Paper: Spatially Resolved Observations of Europa’s Surface with Subaru/IRCS at 1.0–1.8 μm: Upper Limits to the Abundances of Hydrated Cl-bearing Salts
Authors: Shuya Tan, Yasuhito Sekine, Masayuki Kuzuhara
Figure caption: Analysis of the shape of the reflectance spectra at 111° ± 25°W, 38° ± 16°S at wavelengths of 1.100–1.300 μm. (a) Close-up view of the reflectance spectra fitted by the calculated H2O-ice spectra. (b) Normalized spectra of hydrated Cl-bearing salts compared with differences between the observed and fitted H2O-ice spectra as a function of wavelength. Reflectance spectra of H2O ice are calculated using the Hapke model (Hapke 1981, 1993, 2002) with the optical constants for amorphous H2O ice at 70–130 K (Mastrapa et al. 2008), crystalline H2O ice at 120 K (Grundy & Schmidt 1998), and H2SO4 · 8H2O at 77 K (Carlson et al. 2005). The optical constants of H2O ice are supplemented with optical constants from Warren & Brandt (2008). The reflectance of H2O ice is fitted to the observed reflectance using the least-squares method at wavelengths of 1.100–1.130 μm and 1.255–1.300 μm. In the best fit with crystalline H2O ice plus H2SO4 · 8H2O, the mixing ratios of H2O ice and H2SO4 · 8H2O are calculated as 54% and 46%, respectively. Offsets have been added to the differences and the normalized spectra for clarification. The gray bar represents the wavelengths corresponding to telluric atmospheric absorption (1.13–1.15 μm). The normalized spectra of hydrated Cl-bearing salts are not scaled to their upper limits to the abundances.
Paper: Spatially Resolved Observations of Europa’s Surface with Subaru/IRCS at 1.0–1.8 μm: Upper Limits to the Abundances of Hydrated Cl-bearing Salts
Authors: Shuya Tan, Yasuhito Sekine, Masayuki Kuzuhara
Figure caption: Results of our analysis of the noise level of the reflectance spectra at wavelengths of 1.150–1.255 μm. The observed areas on Europa are shown in the top insets. Close-up view of the reflectance spectra fitted by polynomial regression lines of a cubic function at (a) 111° ± 25°W, 38° ± 16°S, (b) 160° ± 9°W, 3° ± 15°N, and (c) 256° ± 5°W, 15° ± 14°N. Differences between the reflectance and polynomial regression lines of the reflectance as a function of wavelength at (d) 111° ± 25°W, 38° ± 16°S, (e) 160° ± 9°W, 3° ± 15°N, and (f) 256° ± 5°W, 15° ± 14°N. The 1σ noise levels are calculated at 1.79 × 10−3, 2.39 × 10−3, and 3.04 × 10−3, respectively.
Paper: Spatially Resolved Observations of Europa’s Surface with Subaru/IRCS at 1.0–1.8 μm: Upper Limits to the Abundances of Hydrated Cl-bearing Salts
Authors: Shuya Tan, Yasuhito Sekine, Masayuki Kuzuhara
Figure caption: Estimated upper limits to the abundances of hydrated Cl-bearing salts in our observations. The observed regions on Europa are shown in the middle inset. (a) Estimated absorption depth of hydrated Cl-bearing salts as a function of abundance compared with the noise levels of our observations. (b) Absorption of hydrated Cl-bearing salts for the estimated upper limits to the abundances at 111° ± 25°W, 38° ± 16°S compared with the residuals of the reflectance spectra fitted by the polynomial regression line at 1.150–1.255 μm (Figure 9(b)). Offsets have been added to the spectra of hydrated Cl-bearing salts and residuals for clarification.
Paper: Spatially Resolved Observations of Europa’s Surface with Subaru/IRCS at 1.0–1.8 μm: Upper Limits to the Abundances of Hydrated Cl-bearing Salts
Authors: Shuya Tan, Yasuhito Sekine, Masayuki Kuzuhara
Figure caption: Extracted signal counts per second from the G2V stars (i.e., the “telluric calibrators” in Table 1). Spectra in the zJH band (0.9–1.5 μm) and the H band (1.49–1.85 μm) were extracted from the spectral images of HD 154805 and HD 160257, respectively. (a) Data observed on 2019 May 17. (b) Data observed on 2019 May 18. In the gray wavelength ranges, spectra contain high levels of noise due to telluric atmospheric absorption (1.35–1.42 μm) and low efficiencies of the grism spectrometer (0.95–1.0 μm and 1.80–1.85 μm).