adsabs/AstroCLIMB huggingface dataset:
Paper: Visible-infrared Spectra of keV Electron Irradiated Cryogenic Salts with Implications for Europa Surface Composition
Authors: C. A. Hibbitts, K. Stockstill-Cahill, E. Lloyd, E. Gloesener, M. Choukroun, C. Paranicas, R. N. Clark
Figure caption: Spectra before and after irradiation of samples at ∼130–150 K show keV electron irradiation; (a) and (b) consistently affect visible wavelengths, but (c) and (d) induce little to no alteration in the infrared. Most spectra are scaled to 1 at 1.1 μm and then offset. A cyan dashed line is placed at 3.1 μm to emphasize the Fresnel reflection related to water.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: A Multiarc Approach to Detecting Uranus’s Normal Modes via Doppler Tracking of a Planetary Orbiter
Authors: Marzia Parisi, Seho Kim, Chris Mankovich, James Fuller, A. James Friedson, Steven Markham
Figure caption: Spectrum of f-mode oscillations for the selected Uranus interior model. The surface potential perturbation (in units of GM/R) is shown as a function of the corotating frequency for the high-energy case (purple dots); (b) moderate-energy case (teal dots); and (c) low-energy case (green dots). The larger symbols represent the zonal modes (m = 0) for each value of ℓ between 2 and 10, while the smaller symbols indicate modes with other values of ∣m∣ ≤ l.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: A Multiarc Approach to Detecting Uranus’s Normal Modes via Doppler Tracking of a Planetary Orbiter
Authors: Marzia Parisi, Seho Kim, Chris Mankovich, James Fuller, A. James Friedson, Steven Markham
Figure caption: Potential perturbations ﹩{\tilde{{\rm{\Phi }}}}^{{\prime} }﹩ of Uranus f-modes are shown for different energy levels. The high-, moderate-, and low-energy profiles represent how the mode amplitudes decrease with increasing angular degree ℓ: weakly for high energy (purple line), at an intermediate rate for moderate energy (teal line), and steeply for low energy (green line). The shaded gray area represents the range of measured amplitudes for Saturn’s f-modes (V. M. Afigbo et al. 2025).
Paper: A Multiarc Approach to Detecting Uranus’s Normal Modes via Doppler Tracking of a Planetary Orbiter
Authors: Marzia Parisi, Seho Kim, Chris Mankovich, James Fuller, A. James Friedson, Steven Markham
Figure caption: Range-rate changes during the first periapsis are shown for T1 (left panel) and T3 (right panel) as a function of time relative to periapsis. The solid lines indicate different energy levels of the selected normal mode (ℓ = −m = 2). The transparent lines show the perturbations resulting from shifting the normal mode phase within its period.
Paper: A Multiarc Approach to Detecting Uranus’s Normal Modes via Doppler Tracking of a Planetary Orbiter
Authors: Marzia Parisi, Seho Kim, Chris Mankovich, James Fuller, A. James Friedson, Steven Markham
Figure caption: The SNR from single passes as a function of angular degree ℓ is shown for T1 (left panel) and T3 (right panel). The SNR is shown in response to a sectoral f-mode with ℓ = −m. Solid lines represent the average of SNR across all periapses at different energy levels, while transparent lines of the same color show the SNR for periapses one through eight.
Paper: A Multiarc Approach to Detecting Uranus’s Normal Modes via Doppler Tracking of a Planetary Orbiter
Authors: Marzia Parisi, Seho Kim, Chris Mankovich, James Fuller, A. James Friedson, Steven Markham
Figure caption: Ground tracks in Uranus’s rotating reference frame (B. A. Archinal et al. 2018) for T1 and T3, showing the spacecraft altitude during a 20 minute interval centered around each close approach (with position ticks every 60 s). Altitudes are computed relative to Uranus’s atmosphere using the 1 bar pressure surface defined by R. Helled et al. (2010).
Paper: A Multiarc Approach to Detecting Uranus’s Normal Modes via Doppler Tracking of a Planetary Orbiter
Authors: Marzia Parisi, Seho Kim, Chris Mankovich, James Fuller, A. James Friedson, Steven Markham
Figure caption: Sectoral (top row) and zonal (bottom row) harmonic functions on the sphere, for ℓ = 2, 5, and 10. Representative ground tracks for T1 and T3 are shown as solid black lines.
Paper: A Multiarc Approach to Detecting Uranus’s Normal Modes via Doppler Tracking of a Planetary Orbiter
Authors: Marzia Parisi, Seho Kim, Chris Mankovich, James Fuller, A. James Friedson, Steven Markham
Figure caption: Same as Figure 5 but for a single zonal f-mode ℓ = 2 and m = 0.
Paper: Exploring the Interior Structure and Mode of Tidal Heating in Enceladus
Authors: Amirhossein Bagheri, Mark Simons, Ryan S. Park, Alexander Berne, Douglas Hemingway, Mohit Melwani Daswani, Steven D. Vance
Figure caption: Exploration of the key geophysical interior model parameters corresponding to Figure 4. Multiple peaks observed in the pdfs of the viscosities of the ice shell and the core correspond to separate tidal dissipation regimes that can match the inferred global heat loss. Shear moduli are presented in GPa, Dshell and ﹩{R}_{\mathrm{core}}﹩ are in kilometers, and other parameters are presented in their SI units. Ice shell thickness and shear moduli are plotted in logarithmic axes. Black and yellow colors indicate the lowest and highest likelihoods.
Paper: Exploring the Interior Structure and Mode of Tidal Heating in Enceladus
Authors: Amirhossein Bagheri, Mark Simons, Ryan S. Park, Alexander Berne, Douglas Hemingway, Mohit Melwani Daswani, Steven D. Vance
Figure caption: Vertical and horizontal displacement Love numbers (∣h2∣, ∣l2∣) and phase lags (﹩{\epsilon }_{{h}_{2}}﹩, ﹩{\epsilon }_{{l}_{2}}﹩) are presented for the core-dominated and shell-dominated tidal dissipation. The heat flux is assumed to be ﹩15\,{\rm{GW}}\lt \dot{E}\lt 40\,{\rm{GW}}﹩, covering estimates in D. Hemingway et al. (2018) and R. S. Park et al. (2024) and the direct measurements (C. Howett et al. 2011). Libration is conservatively assumed to be in the range 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩082 < γ < 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩169, covering the estimates in I. Nadezhdina et al. (2016), P. Thomas et al. (2016), and R. S. Park et al. (2024). The top axis in the plots for h2 and l2 indicates the associated maximum radial and maximum easterly displacements in the bottom axis, respectively.
Paper: Exploring the Interior Structure and Mode of Tidal Heating in Enceladus
Authors: Amirhossein Bagheri, Mark Simons, Ryan S. Park, Alexander Berne, Douglas Hemingway, Mohit Melwani Daswani, Steven D. Vance
Figure caption: (a) Exploration of the correlation between the model parameters associated with Figure 5 for the case where tidal dissipation is dominated in the shell. Black and yellow colors indicate lowest and highest likelihoods. Units and plotting conventions are similar to Figure 18. (b) Exploration of the correlation between the model parameters associated with Figure 5 for the case where tidal dissipation is dominated in the shell. Units and plotting conventions are similar to Figure 18. Blue and red colors indicate the lowest and highest likelihoods.
Paper: Exploring the Interior Structure and Mode of Tidal Heating in Enceladus
Authors: Amirhossein Bagheri, Mark Simons, Ryan S. Park, Alexander Berne, Douglas Hemingway, Mohit Melwani Daswani, Steven D. Vance
Figure caption: Variation of the amplitude of the libration as a function of ice shell thickness and the effective viscosities of the shell (a) and the core (b). In panel (a), the core viscosity is assumed equal to 1020 Pa. s. The region between the red lines shows the libration amplitude spanning the same range in Figure 1. Other interior structure parameters are the same as in Figure 3. The shell thickness and amplitude of libration are plotted in logarithmic scales.
Paper: Exploring the Interior Structure and Mode of Tidal Heating in Enceladus
Authors: Amirhossein Bagheri, Mark Simons, Ryan S. Park, Alexander Berne, Douglas Hemingway, Mohit Melwani Daswani, Steven D. Vance
Figure caption: (a) Natural libration period and (b) amplitude of forced physical libration of Enceladus as functions of the product of shell thickness and density as a representative of its shell MoI. The plots are produced for fine grids of shell thickness and densities in the ranges [1–60] km and [400–900] kg m−3. The color bar indicates the associated shell thickness.
Paper: Exploring the Interior Structure and Mode of Tidal Heating in Enceladus
Authors: Amirhossein Bagheri, Mark Simons, Ryan S. Park, Alexander Berne, Douglas Hemingway, Mohit Melwani Daswani, Steven D. Vance
Figure caption: (a) Natural libration period (hours) and (b) the amplitude of the forced physical libration of Enceladus as functions of the shell thickness and rigidity. Libration amplitude is shown in meters.
Paper: Surface Changes on Io Observed by Large Binocular Telescope/SHARK in Early 2025
Authors: Ashley Gerard Davies, Gianluca Li Causi, Jason E. Perry, Stuart M. Jefferies, Fernando Pedichini, Dino Mesa, David A. Williams, Imke de Pater, David M. Nelson, Fabien R. Baron, Albert R. Conrad, Katherine de Kleer, Simone Antoniucci, Douglas Hope, Maria Bergomi, Francesco D'Alessio, Simone Filomeno, Tania S. Gomes Machado, Fulvio Laudisio, Luca Marafatto, Ester Marini, Roberto Piazzesi, Davide Ricci, Vincenzo Testa, Piero Vaccari, Daniele Vassallo
Figure caption: Eruption at Seth. Panel (a) shows the JIRAM observation of 2023 October 15 (PJ55; see Figure 18 in J. E. Perry et al. 2025). Panel (b) shows the Galileo SSI C21 (1999 June) mosaic. Panel (c) shows the geological map of the Seth area (D. A. Williams et al. 2011). The JIRAM thermal feature Seth Flow A in panel (a) lies on a pink geological map unit designated as bright flows, which fanned out north and northeast from Seth Patera (panel (b)). Panel (d) shows the SHARK-VIS data from 2025 February 23; the dark pyroclastic fan to the north, which is surrounded by a lighter unit (likely a SO2-rich deposit); and the streak of red material to the south of the hot spot cluster in panel (a). North is up.
Paper: Surface Changes on Io Observed by Large Binocular Telescope/SHARK in Early 2025
Authors: Ashley Gerard Davies, Gianluca Li Causi, Jason E. Perry, Stuart M. Jefferies, Fernando Pedichini, Dino Mesa, David A. Williams, Imke de Pater, David M. Nelson, Fabien R. Baron, Albert R. Conrad, Katherine de Kleer, Simone Antoniucci, Douglas Hope, Maria Bergomi, Francesco D'Alessio, Simone Filomeno, Tania S. Gomes Machado, Fulvio Laudisio, Luca Marafatto, Ester Marini, Roberto Piazzesi, Davide Ricci, Vincenzo Testa, Piero Vaccari, Daniele Vassallo
Figure caption: SHARK-VIS observation and thermal emission as mapped by Juno JIRAM. This image shows the central portion of the SHARK-VIS data obtained on 2025 February 23. Both SHARK-VIS (panel (a)) and Juno JIRAM thermal emission data, seen here superimposed on the SHARK-VIS data (panel (b)), have been reprojected to cylindrical projection perspective. The JIRAM M-band (4.78 μm) data are from Juno perijove PJ55, obtained on 2023 October 23 (J. E. Perry et al. 2025). Image centered on 150°W, −5°N. North is up. Major hot spots in the JIRAM data and locations cited in the text where SHARK-VIS detected change are labeled.
Paper: Surface Changes on Io Observed by Large Binocular Telescope/SHARK in Early 2025
Authors: Ashley Gerard Davies, Gianluca Li Causi, Jason E. Perry, Stuart M. Jefferies, Fernando Pedichini, Dino Mesa, David A. Williams, Imke de Pater, David M. Nelson, Fabien R. Baron, Albert R. Conrad, Katherine de Kleer, Simone Antoniucci, Douglas Hope, Maria Bergomi, Francesco D'Alessio, Simone Filomeno, Tania S. Gomes Machado, Fulvio Laudisio, Luca Marafatto, Ester Marini, Roberto Piazzesi, Davide Ricci, Vincenzo Testa, Piero Vaccari, Daniele Vassallo
Figure caption: Changes at Amirani highlighted by SHARK-VIS. The left panel shows bright areas of volcanic thermal emission from the Amirani region volcanoes as detected in the M band (4.78 μm) by Juno JIRAM during PJ55 (2023 October 23; J. E. Perry et al. 2025). The middle panel shows the SHARK-VIS image from 2025 February 23. The right panel shows the same area as seen by Galileo SSI. In the middle and right panels the outlines of the areas of JIRAM thermal emission are overlaid on the image data. At Amirani, detected volcanic thermal emission is confined to the southern half of the lava flow field imaged by Galileo (see J. E. Perry et al. (2025), consistent with the low-albedo area imaged by SHARK-VIS. Dusura Patera (another large, thermally active, low-albedo feature) is also resolved by SHARK-VIS. Other low-albedo features in the Galileo image are detectable in the infrared by JIRAM, while not being clearly resolved in the lower spatial resolution SHARK-VIS data.
Paper: Surface Changes on Io Observed by Large Binocular Telescope/SHARK in Early 2025
Authors: Ashley Gerard Davies, Gianluca Li Causi, Jason E. Perry, Stuart M. Jefferies, Fernando Pedichini, Dino Mesa, David A. Williams, Imke de Pater, David M. Nelson, Fabien R. Baron, Albert R. Conrad, Katherine de Kleer, Simone Antoniucci, Douglas Hope, Maria Bergomi, Francesco D'Alessio, Simone Filomeno, Tania S. Gomes Machado, Fulvio Laudisio, Luca Marafatto, Ester Marini, Roberto Piazzesi, Davide Ricci, Vincenzo Testa, Piero Vaccari, Daniele Vassallo
Figure caption: Changes at Tvashtar Paterae and Thor. (a) SHARK-VIS image from 2025 February 23 orthographically reprojected so the disk center is at 120.3°W, 60.9°N, centered on hot spot Tvashtar Patera C (J. E. Perry et al. 2025). (b) Galileo orbit C21 (1999 June) SSI mosaic reprojected to the same point. The large box encompasses the Tvashtar plume deposit. The small box surrounds the Thor eruptive center. (c) The Galileo orbit I31 (2001 August) SSI mosaic, showing a bright, annular deposit around a dark center at Thor. (d) The New Horizons (2007 February) mosaic, one of the last high-resolution observations of Io before Juno. A large plume deposit from a plume hundreds of kilometers high has erased the deposits around Thor. Much of the Tvashtar deposit as seen by New Horizons has faded by the Juno epoch.
Paper: Surface Changes on Io Observed by Large Binocular Telescope/SHARK in Early 2025
Authors: Ashley Gerard Davies, Gianluca Li Causi, Jason E. Perry, Stuart M. Jefferies, Fernando Pedichini, Dino Mesa, David A. Williams, Imke de Pater, David M. Nelson, Fabien R. Baron, Albert R. Conrad, Katherine de Kleer, Simone Antoniucci, Douglas Hope, Maria Bergomi, Francesco D'Alessio, Simone Filomeno, Tania S. Gomes Machado, Fulvio Laudisio, Luca Marafatto, Ester Marini, Roberto Piazzesi, Davide Ricci, Vincenzo Testa, Piero Vaccari, Daniele Vassallo
Figure caption: Changes in the Prometheus Plume deposit over time. (a) Voyager (1979), images c1636842, c1636838, and c1636834. (b) Galileo (2001), mosaic 21ISCOLOR01. (c) SHARK-VIS (2025 February 23). The source of the plume moved 80 km westward between 1979 and 1996 (A. S. McEwen et al. 1998). In 2025, in the SHARK-VIS data, the western part of the annular plume has broadened eastward, suggesting a similar shift in the main plume source location to the east. The plume of red material now extends in a more northeasterly direction when compared with the Galileo data.
Paper: Surface Changes on Io Observed by Large Binocular Telescope/SHARK in Early 2025
Authors: Ashley Gerard Davies, Gianluca Li Causi, Jason E. Perry, Stuart M. Jefferies, Fernando Pedichini, Dino Mesa, David A. Williams, Imke de Pater, David M. Nelson, Fabien R. Baron, Albert R. Conrad, Katherine de Kleer, Simone Antoniucci, Douglas Hope, Maria Bergomi, Francesco D'Alessio, Simone Filomeno, Tania S. Gomes Machado, Fulvio Laudisio, Luca Marafatto, Ester Marini, Roberto Piazzesi, Davide Ricci, Vincenzo Testa, Piero Vaccari, Daniele Vassallo
Figure caption: SHARK-NIR observations of Io through the Fe II filter (panel (a)), at UT 2025-02-23T03:14:30, and the PaB filter (panel (b)), at UT 2025-02-23T03:18:30. The images are centered on 153.4°W, 2.6°N. Panels (c) and (d) show the deconvolved images after processing. The effective PSF is shown in the lower left corner of each image (see text for details). See Table 3 for image resolutions. North is up.
Paper: Surface Changes on Io Observed by Large Binocular Telescope/SHARK in Early 2025
Authors: Ashley Gerard Davies, Gianluca Li Causi, Jason E. Perry, Stuart M. Jefferies, Fernando Pedichini, Dino Mesa, David A. Williams, Imke de Pater, David M. Nelson, Fabien R. Baron, Albert R. Conrad, Katherine de Kleer, Simone Antoniucci, Douglas Hope, Maria Bergomi, Francesco D'Alessio, Simone Filomeno, Tania S. Gomes Machado, Fulvio Laudisio, Luca Marafatto, Ester Marini, Roberto Piazzesi, Davide Ricci, Vincenzo Testa, Piero Vaccari, Daniele Vassallo
Figure caption: Band ratio images using 2025 February 23 SHARK-VIS data. Panel (a) shows an enhanced-contrast image of Io. Panel (b) shows the R/V ratio image. Panel (c) shows the I/R ratio image.
Paper: The Caltech Mission to Apophis: Accelerating Planetary Science and Planetary Defense
Authors: Adriana Daca, Masatoshi Hirabayashi, Yaeji Kim, Joseph DeMartini, Carol Raymond, Alain Herique, Mark Haynes, Dirk Plettemeier, Bjorn Davidsson, José Andrade
Figure caption: Apophis’s rotational evolution and displacement along the ξ axis. The closest approach happens 12.5 hr after the simulation starts. Panels (a) and (b) show the deviation of the rotation angle from the rigid-body case along the ξ, η, and ζ axes. Panels (c) and (d) illustrate the displacement along the ξ axis. Panels (a) and (c) display the case with a Young’s modulus of 1 MPa, while panels (b) and (d) describe that with a Young’s modulus of 10 kPa.
Paper: The Caltech Mission to Apophis: Accelerating Planetary Science and Planetary Defense
Authors: Adriana Daca, Masatoshi Hirabayashi, Yaeji Kim, Joseph DeMartini, Carol Raymond, Alain Herique, Mark Haynes, Dirk Plettemeier, Bjorn Davidsson, José Andrade
Figure caption: Radar modes implemented by the Caltech mission to Apophis.
Paper: The Caltech Mission to Apophis: Accelerating Planetary Science and Planetary Defense
Authors: Adriana Daca, Masatoshi Hirabayashi, Yaeji Kim, Joseph DeMartini, Carol Raymond, Alain Herique, Mark Haynes, Dirk Plettemeier, Bjorn Davidsson, José Andrade
Figure caption: Diagram illustrating how the Caltech mission to Apophis complements other missions going to Apophis.
Paper: The Caltech Mission to Apophis: Accelerating Planetary Science and Planetary Defense
Authors: Adriana Daca, Masatoshi Hirabayashi, Yaeji Kim, Joseph DeMartini, Carol Raymond, Alain Herique, Mark Haynes, Dirk Plettemeier, Bjorn Davidsson, José Andrade
Figure caption: Diagrams illustrating radar terminology definitions.
Paper: Detection of an NH3 Absorption Band at 2.2 μm on Europa
Authors: A. Emran
Figure caption: Left panel: the reflectance spectra (offset for clarity) of the water ice, sulfate salts, ammonia hydrate, and SAO at near-infrared wavelengths. The modeled reflectance spectra using the Y. Shkuratov et al. (1999) approach for a 10 μm grain for amorphous and crystalline H2O ice at 120 K (R. Mastrapa et al. 2008, 2009), hexahydrite, epsomite, and bloedite at 120 K (J. Dalton & K. Pitman 2012), sulfuric acid octahydrate (SAO) at 77 K (R. Carlson et al. 2005), and NH3.H2O ice at 77 K (R. H. Brown et al. 1988). Mirabilite spectrum at 10 μm grain was produced from the estimated optical constant at 100 K (S. De Angelis et al. 2021, see the main text for details). Right panel: the reflectance spectra from J. Hanley et al. (2014) for magnesium chlorate (Mg(ClO3)2.6H2O), magnesium perchlorate (Mg(ClO4)2 6H2O), magnesium chloride (MgCl2.2H2O; MgCl2.4H2O; and MgCl2.6H2O), sodium chloride (NaCl), and sodium perchlorate (NaClO4 and NaClO4.2H2O) at 80 K. The gray shades of the vertical area represent the wavelengths between 2.18 and 2.22 μm (2.20 ± 0.02 μm), where NIMS data of the detected pixels show an absorption feature.
Paper: Detection of an NH3 Absorption Band at 2.2 μm on Europa
Authors: A. Emran
Figure caption: The reflectance spectra of the NH3-bearing species at near-infrared wavelengths. The modeled reflectance spectra generated using the Y. Shkuratov et al. (1999) approach for a 50 μm grain for amorphous NH3 ice at 40 K (optical constants from J. E. Roser et al. 2021), crystalline NH3 ice at 100 K (optical constants from R. L. Hudson et al. 2022), and NH3.H2O ice at 77 K (optical constants from R. H. Brown et al. 1988). Reflectance spectra of NH4 salts (chloride, carbonate, bicarbonate, sulfate, nitrate, and biphosphate) at grain sizes of 32–80 μm measured at 120 K were obtained from M. Fastelli et al. (2022). The spectrum of NH4 montmorillonite (a phyllosilicate; RELAB ID: c1jb189) was obtained from the RELAB spectral library (R. Milliken et al. 2021). The gray shades of the vertical area represent the wavelengths between 2.18 and 2.22 μm (2.20 ± 0.02 μm), where NIMS data of the detected pixels show an absorption feature. Note that the NH3 ice spectra were smoothed using the Savitzky–Golay filter (A. Savitzky & M. J. Golay 1964), following A. Emran & V. Chevrier (2022).
Paper: Detection of an NH3 Absorption Band at 2.2 μm on Europa
Authors: A. Emran
Figure caption: Top panel: the average reflectance spectrum of the detected clusters (black circles) with standard error bars, along with the best-fit model spectrum (red line) derived using an areal (linear) mixing approach incorporating the optical constants of NH3.H2O. The reduced chi-square value—χ2(Red.)—of the model fit is also provided in the plot. The inset shows a zoomed-in view of the model fit between 2.05 and 2.40 μm, with the corresponding RMSE value. The model spectrum closely matches the observed absorption feature at 2.20 μm, rendering a lower RMSE than the fit shown in Figure 6. Bottom panel: a plot of the residual (observation-model) spectrum over the entire wavelength region at ∼1.2–2.5 μm.
Paper: Detection of an NH3 Absorption Band at 2.2 μm on Europa
Authors: A. Emran
Figure caption: Offset reflectance spectra of various phyllosilicate (clay) minerals in the near-infrared (∼1.2–2.5 μm) range, including Fe/Mg/Al phyllosilicates, saponite, kaolinite, Mg serpentine (lizardite), clinochlore, brucite, Mg/Ca carbonates, and ammonium-bearing clays (NH4 annite and NH4 montmorillonite). All spectra were obtained from the RELAB spectral library (R. Milliken et al. 2021). The shaded vertical region highlights the 2.18–2.22 μm wavelength range (2.20 ± 0.02 μm), where the NIMS spectra of the detected pixels show an absorption feature.
Paper: Detection of an NH3 Absorption Band at 2.2 μm on Europa
Authors: A. Emran
Figure caption: Top panel: the average reflectance spectrum of the detected clusters (black circles) with standard error bars, along with the best-fit model spectrum (red line) derived using an areal (linear) mixing approach that excludes the optical constants of NH3.H2O. The reduced chi-square value—χ2(Red.)—of the model fit is also provided in the plot. The inset shows a zoomed-in view of the model fit between 2.05 and 2.40 μm, with the corresponding RMSE value. The model spectrum fails to reproduce the absorption feature at 2.20 μm seen in the NIMS data and results in a higher RMSE than the fit shown in Figure 5. Bottom panel: a plot of the residual (observation-model) spectrum over the entire wavelength region at ∼1.2–2.5 μm.
Paper: Detection of an NH3 Absorption Band at 2.2 μm on Europa
Authors: A. Emran
Figure caption: Average reflectance spectra of each pixel cluster identified in Figure 4. The approximate central latitudes and longitudes of each cluster are labeled in the corresponding subplot. The gray shaded region indicates the 2.18–2.22 μm (2.20 ± 0.02 μm) wavelength range, where NH3-bearing species exhibit characteristic absorption features.