adsabs/AstroCLIMB huggingface dataset:
Paper: TRIDENT Ice Mining Drill for Lunar Volatile Prospecting for PRIME-1 and VIPER Missions
Authors: Kris Zacny, Philip Chu, Vincent Vendiola, Gale Paulsen, Paul Creekmore, Samuel Goldman, Jameil Bailey, Philip Ng, Carter Fortuin, Jaqueline Stamboltsian, Alex Wang, Anchal Jain, Paul Chow, Emily Seto, Nicholas Bottomley, Robert Huddleston, Ezra Bailey-Kelly, Raymond Zheng, Aaron Norlinger, Isabel King, Zach Mank, Jack Wilson, Jake Fishman, Helen Xu, Dean Bergman, Erik Mumm, Kiel Davis, Jason Beck, Stella Dearing, Mark Hill, Jackie Quinn, Amy Eichenbaum, Janine Captain, Julie Kleinhenz, Anthony Colaprete, Rick Elphic, Kimberly Ennico-Smith, Darlene S. S. Lim, Zara Mirmalek, David Lees, Valentin T. Bickel, Ariel N. Deutsch, Nicholas C. Schmerr, Kevin Lewis, Benjamin Fernando, Kathryn Gansler
Figure caption: TRIDENT FUs for VIPER (left) and PRIME-1 (right) staged in the Honeybee Robotics clean room prior to delivery.
Paper: TRIDENT Ice Mining Drill for Lunar Volatile Prospecting for PRIME-1 and VIPER Missions
Authors: Kris Zacny, Philip Chu, Vincent Vendiola, Gale Paulsen, Paul Creekmore, Samuel Goldman, Jameil Bailey, Philip Ng, Carter Fortuin, Jaqueline Stamboltsian, Alex Wang, Anchal Jain, Paul Chow, Emily Seto, Nicholas Bottomley, Robert Huddleston, Ezra Bailey-Kelly, Raymond Zheng, Aaron Norlinger, Isabel King, Zach Mank, Jack Wilson, Jake Fishman, Helen Xu, Dean Bergman, Erik Mumm, Kiel Davis, Jason Beck, Stella Dearing, Mark Hill, Jackie Quinn, Amy Eichenbaum, Janine Captain, Julie Kleinhenz, Anthony Colaprete, Rick Elphic, Kimberly Ennico-Smith, Darlene S. S. Lim, Zara Mirmalek, David Lees, Valentin T. Bickel, Ariel N. Deutsch, Nicholas C. Schmerr, Kevin Lewis, Benjamin Fernando, Kathryn Gansler
Figure caption: TRIDENT integration team following the installation of the TRIDENT FU and avionics onto an IM-2 lander panel at Intuitive Machines in Houston. Courtesy NASA Bill Stafford.
Paper: TRIDENT Ice Mining Drill for Lunar Volatile Prospecting for PRIME-1 and VIPER Missions
Authors: Kris Zacny, Philip Chu, Vincent Vendiola, Gale Paulsen, Paul Creekmore, Samuel Goldman, Jameil Bailey, Philip Ng, Carter Fortuin, Jaqueline Stamboltsian, Alex Wang, Anchal Jain, Paul Chow, Emily Seto, Nicholas Bottomley, Robert Huddleston, Ezra Bailey-Kelly, Raymond Zheng, Aaron Norlinger, Isabel King, Zach Mank, Jack Wilson, Jake Fishman, Helen Xu, Dean Bergman, Erik Mumm, Kiel Davis, Jason Beck, Stella Dearing, Mark Hill, Jackie Quinn, Amy Eichenbaum, Janine Captain, Julie Kleinhenz, Anthony Colaprete, Rick Elphic, Kimberly Ennico-Smith, Darlene S. S. Lim, Zara Mirmalek, David Lees, Valentin T. Bickel, Ariel N. Deutsch, Nicholas C. Schmerr, Kevin Lewis, Benjamin Fernando, Kathryn Gansler
Figure caption: Moments before integrating the VIPER TRIDENT FU into the chassis of VIPER at Johnson Space Center in Houston. Courtesy NASA Bill Stafford.
Paper: TRIDENT Ice Mining Drill for Lunar Volatile Prospecting for PRIME-1 and VIPER Missions
Authors: Kris Zacny, Philip Chu, Vincent Vendiola, Gale Paulsen, Paul Creekmore, Samuel Goldman, Jameil Bailey, Philip Ng, Carter Fortuin, Jaqueline Stamboltsian, Alex Wang, Anchal Jain, Paul Chow, Emily Seto, Nicholas Bottomley, Robert Huddleston, Ezra Bailey-Kelly, Raymond Zheng, Aaron Norlinger, Isabel King, Zach Mank, Jack Wilson, Jake Fishman, Helen Xu, Dean Bergman, Erik Mumm, Kiel Davis, Jason Beck, Stella Dearing, Mark Hill, Jackie Quinn, Amy Eichenbaum, Janine Captain, Julie Kleinhenz, Anthony Colaprete, Rick Elphic, Kimberly Ennico-Smith, Darlene S. S. Lim, Zara Mirmalek, David Lees, Valentin T. Bickel, Ariel N. Deutsch, Nicholas C. Schmerr, Kevin Lewis, Benjamin Fernando, Kathryn Gansler
Figure caption: Camera view during TRIDENT EU testing simulates the NIRVSS AIM camera view on VIPER.
Paper: TRIDENT Ice Mining Drill for Lunar Volatile Prospecting for PRIME-1 and VIPER Missions
Authors: Kris Zacny, Philip Chu, Vincent Vendiola, Gale Paulsen, Paul Creekmore, Samuel Goldman, Jameil Bailey, Philip Ng, Carter Fortuin, Jaqueline Stamboltsian, Alex Wang, Anchal Jain, Paul Chow, Emily Seto, Nicholas Bottomley, Robert Huddleston, Ezra Bailey-Kelly, Raymond Zheng, Aaron Norlinger, Isabel King, Zach Mank, Jack Wilson, Jake Fishman, Helen Xu, Dean Bergman, Erik Mumm, Kiel Davis, Jason Beck, Stella Dearing, Mark Hill, Jackie Quinn, Amy Eichenbaum, Janine Captain, Julie Kleinhenz, Anthony Colaprete, Rick Elphic, Kimberly Ennico-Smith, Darlene S. S. Lim, Zara Mirmalek, David Lees, Valentin T. Bickel, Ariel N. Deutsch, Nicholas C. Schmerr, Kevin Lewis, Benjamin Fernando, Kathryn Gansler
Figure caption: Typical locations and channels of communication for TRIDENT operations on VIPER.
Paper: TRIDENT Ice Mining Drill for Lunar Volatile Prospecting for PRIME-1 and VIPER Missions
Authors: Kris Zacny, Philip Chu, Vincent Vendiola, Gale Paulsen, Paul Creekmore, Samuel Goldman, Jameil Bailey, Philip Ng, Carter Fortuin, Jaqueline Stamboltsian, Alex Wang, Anchal Jain, Paul Chow, Emily Seto, Nicholas Bottomley, Robert Huddleston, Ezra Bailey-Kelly, Raymond Zheng, Aaron Norlinger, Isabel King, Zach Mank, Jack Wilson, Jake Fishman, Helen Xu, Dean Bergman, Erik Mumm, Kiel Davis, Jason Beck, Stella Dearing, Mark Hill, Jackie Quinn, Amy Eichenbaum, Janine Captain, Julie Kleinhenz, Anthony Colaprete, Rick Elphic, Kimberly Ennico-Smith, Darlene S. S. Lim, Zara Mirmalek, David Lees, Valentin T. Bickel, Ariel N. Deutsch, Nicholas C. Schmerr, Kevin Lewis, Benjamin Fernando, Kathryn Gansler
Figure caption: Example seismic recordings of TRIDENT drilling operations by a commercial IMU. (A) Two WitMotion SINDT-TTL accelerometers positioned on the drill housing ∼20 cm apart, with the +Y-axis in the direction of gravity. Data shown are from the vertical component of IMU1. (B) Continuous wavelet transform analysis (J. M. Lilly 2017) of a single percussion by the drill with labeling of events. (C) Accelerogram for ±4 s around the percussion window. (D) Continuous wavelet transform for IMU data acquired during bite 4 while drilling from 30 to 40 cm in the TRIDENT EU testing with labeling of events. (E) IMU1 accelerogram for drilling operations during bite 4.
Paper: TRIDENT Ice Mining Drill for Lunar Volatile Prospecting for PRIME-1 and VIPER Missions
Authors: Kris Zacny, Philip Chu, Vincent Vendiola, Gale Paulsen, Paul Creekmore, Samuel Goldman, Jameil Bailey, Philip Ng, Carter Fortuin, Jaqueline Stamboltsian, Alex Wang, Anchal Jain, Paul Chow, Emily Seto, Nicholas Bottomley, Robert Huddleston, Ezra Bailey-Kelly, Raymond Zheng, Aaron Norlinger, Isabel King, Zach Mank, Jack Wilson, Jake Fishman, Helen Xu, Dean Bergman, Erik Mumm, Kiel Davis, Jason Beck, Stella Dearing, Mark Hill, Jackie Quinn, Amy Eichenbaum, Janine Captain, Julie Kleinhenz, Anthony Colaprete, Rick Elphic, Kimberly Ennico-Smith, Darlene S. S. Lim, Zara Mirmalek, David Lees, Valentin T. Bickel, Ariel N. Deutsch, Nicholas C. Schmerr, Kevin Lewis, Benjamin Fernando, Kathryn Gansler
Figure caption: Example heater telemetry collected during TRIDENT EU testing in an icy lunar regolith simulant (8.5 wt% H2O LSP-2) provides total energy and power supplied, along with temperature response from a nearby PRT. The step pattern is due to the temperature being shown to within 1°.
Paper: TRIDENT Ice Mining Drill for Lunar Volatile Prospecting for PRIME-1 and VIPER Missions
Authors: Kris Zacny, Philip Chu, Vincent Vendiola, Gale Paulsen, Paul Creekmore, Samuel Goldman, Jameil Bailey, Philip Ng, Carter Fortuin, Jaqueline Stamboltsian, Alex Wang, Anchal Jain, Paul Chow, Emily Seto, Nicholas Bottomley, Robert Huddleston, Ezra Bailey-Kelly, Raymond Zheng, Aaron Norlinger, Isabel King, Zach Mank, Jack Wilson, Jake Fishman, Helen Xu, Dean Bergman, Erik Mumm, Kiel Davis, Jason Beck, Stella Dearing, Mark Hill, Jackie Quinn, Amy Eichenbaum, Janine Captain, Julie Kleinhenz, Anthony Colaprete, Rick Elphic, Kimberly Ennico-Smith, Darlene S. S. Lim, Zara Mirmalek, David Lees, Valentin T. Bickel, Ariel N. Deutsch, Nicholas C. Schmerr, Kevin Lewis, Benjamin Fernando, Kathryn Gansler
Figure caption: Difference in bit temperature and soil temperature over time. There is a notable difference in behavior between dry and icy soil, as the lunar soil is insulating and the drill stem retains much more heat in dry soil. The step pattern is due to the temperature being shown to within 1°.
Paper: TRIDENT Ice Mining Drill for Lunar Volatile Prospecting for PRIME-1 and VIPER Missions
Authors: Kris Zacny, Philip Chu, Vincent Vendiola, Gale Paulsen, Paul Creekmore, Samuel Goldman, Jameil Bailey, Philip Ng, Carter Fortuin, Jaqueline Stamboltsian, Alex Wang, Anchal Jain, Paul Chow, Emily Seto, Nicholas Bottomley, Robert Huddleston, Ezra Bailey-Kelly, Raymond Zheng, Aaron Norlinger, Isabel King, Zach Mank, Jack Wilson, Jake Fishman, Helen Xu, Dean Bergman, Erik Mumm, Kiel Davis, Jason Beck, Stella Dearing, Mark Hill, Jackie Quinn, Amy Eichenbaum, Janine Captain, Julie Kleinhenz, Anthony Colaprete, Rick Elphic, Kimberly Ennico-Smith, Darlene S. S. Lim, Zara Mirmalek, David Lees, Valentin T. Bickel, Ariel N. Deutsch, Nicholas C. Schmerr, Kevin Lewis, Benjamin Fernando, Kathryn Gansler
Figure caption: Example drill bit temperature measurement at 50 cm depth performed by the TRIDENT EU in a water-doped lunar regolith simulant (8.5 wt% H2O LSP-2) in a vacuum. Nearby soil temperatures are provided for reference.
Paper: TRIDENT Ice Mining Drill for Lunar Volatile Prospecting for PRIME-1 and VIPER Missions
Authors: Kris Zacny, Philip Chu, Vincent Vendiola, Gale Paulsen, Paul Creekmore, Samuel Goldman, Jameil Bailey, Philip Ng, Carter Fortuin, Jaqueline Stamboltsian, Alex Wang, Anchal Jain, Paul Chow, Emily Seto, Nicholas Bottomley, Robert Huddleston, Ezra Bailey-Kelly, Raymond Zheng, Aaron Norlinger, Isabel King, Zach Mank, Jack Wilson, Jake Fishman, Helen Xu, Dean Bergman, Erik Mumm, Kiel Davis, Jason Beck, Stella Dearing, Mark Hill, Jackie Quinn, Amy Eichenbaum, Janine Captain, Julie Kleinhenz, Anthony Colaprete, Rick Elphic, Kimberly Ennico-Smith, Darlene S. S. Lim, Zara Mirmalek, David Lees, Valentin T. Bickel, Ariel N. Deutsch, Nicholas C. Schmerr, Kevin Lewis, Benjamin Fernando, Kathryn Gansler
Figure caption: ROP when drilling rocks of varying UCS with TRIDENT baseline parameters.
Paper: Orbital Decay Candidates Reconsidered: WASP-4 b Is Not Decaying and Kepler-1658 b Is Not a Planet
Authors: Joshua N. Winn, Guđmundur Stefánsson
Figure caption: Kepler-1658. Upper left: RVs, after shifting the data from each spectrograph to have zero mean. Lower left: deviations between transit times and the best-fit constant-period model (P = 3.849363145 days, tc = 2455005.925555 BJDTDB). In this panel and others, the black curve is the best-fit model including the effects of the hot Jupiter and a wide-orbiting companion, and the gray curves are random draws from the posterior. Upper right: RVs as a function of folded time (i.e., relative to the nearest transit time) after subtracting the best-fit contribution of the wide-orbiting companion. Lower right: RVs after subtracting the best-fit contribution of the hot Jupiter.
Paper: Orbital Decay Candidates Reconsidered: WASP-4 b Is Not Decaying and Kepler-1658 b Is Not a Planet
Authors: Joshua N. Winn, Guđmundur Stefánsson
Figure caption: WASP-4. Upper left: RVs, after shifting the data from each spectrograph to have zero mean. Lower left: deviations between transit times and the best-fit constant-period model (P = 1.338231293 days, tc = 2456180.558583 BJDTDB). In this panel and others, the black curve is the best-fit model including the hot Jupiter and a wide-orbiting companion, and the gray curves are random draws from the posterior. Upper right: RVs as a function of folded time (i.e., relative to the nearest transit time), after subtracting the best-fit contribution from the wide-orbiting companion. Lower right: RVs after subtracting the best-fit contribution of the hot Jupiter.
Paper: Orbital Decay Candidates Reconsidered: WASP-4 b Is Not Decaying and Kepler-1658 b Is Not a Planet
Authors: Joshua N. Winn, Guđmundur Stefánsson
Figure caption: Spectral line variations of Kepler-1658. Left: representative CCFs based on NEID spectra. They are centered on the systemic velocity of −24 km s−1 and have widths of about 30 km s−1 due to stellar rotation. There are also night-to-night shape variations. Middle: isolation of CCF variations. The median NEID CCF was subtracted from individual CCFs, revealing anomalies of amplitude ∼ 10−2 that shift in velocity. Right: velocity shift of the pattern of residuals relative to an arbitrarily chosen night, as a function of time folded with the 3.8 day transit period. The variation is consistent with 20 km s−1 orbital motion of an unresolved binary with the expected period and phase.
Paper: Orbital Decay Candidates Reconsidered: WASP-4 b Is Not Decaying and Kepler-1658 b Is Not a Planet
Authors: Joshua N. Winn, Guđmundur Stefánsson
Figure caption: WASP-12. Upper left: RVs, after shifting the data from each spectrograph to have zero mean. Lower left: deviations between transit times and the best-fit constant-period model (P = 1.091418667 days, tc = 2456305.45552 BJDTDB). In this panel and others, the black curve is the best-fit model including the effects of the hot Jupiter and a wide-orbiting companion, and the gray curves are random draws from the posterior. Upper right: RVs as a function of folded time (i.e., relative to the nearest transit time), after subtracting the best-fit contribution of the wide-orbiting companion. Lower right: RVs after subtracting the best-fit contribution of the hot Jupiter.
Paper: Orbital Decay Candidates Reconsidered: WASP-4 b Is Not Decaying and Kepler-1658 b Is Not a Planet
Authors: Joshua N. Winn, Guđmundur Stefánsson
Figure caption: Constraints on the wide-orbiting companion of WASP-4 b. Shown are the posteriors for minimum mass and orbital separation, assuming the orbit is nearly circular. The contours enclose 68%, 95%, and 99.7% of the probability.
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 observable constraints from J3, moment of inertia, libration amplitude, and rate of heat loss based on R. S. Park et al. (2024). We present pdfs of predictions for ∣k2∣, ∣h2∣, ∣l2∣, ﹩{\epsilon }_{{k}_{2}}﹩, ﹩{\epsilon }_{{h}_{2}}﹩, and ﹩{\epsilon }_{{l}_{2}}﹩. Both scenarios of tidal dissipation are considered here. The plots of the pdfs for the k2 amplitude and phase lag are notably different than those of the ∣h2∣ and ∣l2∣ amplitudes and phases. Plotting and unit conventions are the same as in Figure 4.
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) Sensitivity of key parameters in determining the heat dissipation consistent with the observables in Figure 7 based on the analysis of the observables by R. S. Park et al. (2024). Rate of heat loss and μshell are shown in GW and GPa, respectively. Blue and red colors demonstrate lowest and highest likelihoods, respectively. (b) Sensitivity of key parameters in determining the ice shell properties associated with observables in Figure 7 based on the analysis of the observables by R. S. Park et al. (2024). J3 is shown multiplied by 106, and γ, Dshell, and ρshell are shown in meters, kilometers, and kg m−3, 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) Results of the MCMC inversion for the case where the tidal dissipation is dominantly in the ice shell and adopting the measurement uncertainty given in Table 3. The shear moduli are plotted in log axes. Results are presented assuming the larger set of uncertainties shown in Table 3. (b) Results of the MCMC inversion for the case where the tidal dissipation is dominantly in the core, provided the uncertainty on the measurements as shown in Table 3. The shear moduli are plotted in log axes. Results are presented assuming the larger set of uncertainties shown in Table 3.
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: Amplitude of tidal deformation in radial, northerly, and easterly directions for two cases of an ice shell with variable thickness as shown in Figure 11 and a constant shell thickness with the same average thickness equal to 30 km. Here, it is assumed that the tidal dissipation is happening in the rocky core and the viscosity of the ice shell is 1020 Pa.s, implying elastic deformations in the shell. Contours denote intervals of 0.05 m
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: Panels (a)–(f): tidal Love numbers and phase lags for heat dissipation in the shell and core based on the constraints by R. S. Park et al. (2024). Panels (g)–(j): Love numbers and phase lags for two dissipation regimes assuming that the real and imaginary parts of k2 are measured with an uncertainty of 0.002.
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 Enceladus’s ice shell thickness based on a modified shape model from R. S. Park et al. (2024) assuming isostasy. Contours denote intervals of 2 km.
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: Difference between tidal observables due to the use of the Maxwell and Andrade rheology: (a) tidal heating (﹩{\rm{\Delta }}\dot{E}﹩), (b) maximum radial displacements (ΔR), (c) k2 and (d) h2 Love numbers (Δk2 and Δh2), and ((e) and (f)) associated phase lags (﹩{\rm{\Delta }}{\epsilon }_{{k}_{2}}﹩ and ﹩{\rm{\Delta }}{\epsilon }_{{h}_{2}}﹩). The four narrow regions constrained by the red lines in panels (a) and (b) indicate the estimated tidal heat (see Figure 2).
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: Effect of changing the Andrade parameter α on the tidal response of Enceladus. Left and right panels show the tidal response parameters for models of tidal dissipation dominantly in the shell and in the core, respectively.
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: Color-composite images of Io from SHARK-VIS data. Panels (a) and (e) are color composites, for 2025 February 18 at 04:44:38.162Z and 2025 February 23 at 03:24:30.641Z, respectively, created by combining the deconvolved images shown in the second and fourth rows of Figure 2 (panels (d), (e), (f) and (j), (k), (l) therein). Here I, R, and V bands are rendered as red, green, and blue respectively, and independently stretched to maximize color contrast. Locations of notable features are labeled in panels (b) and (f). Panels (c) and (g) are flux-calibrated renditions of panels (a) and (e), where the intensities of the I, R, and V bands are corrected from the filters response curves to show approximations of true color (note that both renditions do not show colors as seen by eye, as the filters used are not RGB). For context, panels (d) and (h) show the Voyager−Galileo Io mosaic (T. Becker & P. E. Geissler 2005) reprojected to the SHARK-VIS viewing perspectives, centered on 228.9°W, 2.7°N on 2025 February 18 and 149.1°W, 2.6°N on 2025 February 23. North is up in all images.
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 and Juno observations of Illyrikon from 2024 and 2025. All images are orthographically reprojected so the subobserver viewpoint is 181.0°W, −74.4°N; Illyrikon A in J. E. Perry et al. 2025). (a) SHARK-VIS observation of 2025 February 23. (b) The image in panel (a) with the new, light deposit generated by the West Illyrikon eruption denoted by the area between the two yellow lines. (c) Galileo SSI C21 (1999) mosaic, showing the extent of the red deposits in Io’s south polar region. Panels (d)–(f) show re-projected JunoCam observations obtained during orbits 60 (panel (d)), 68 (panel (e)), and 70 (panel (f)) showing changes at West Illyrikon: a new dark flow, a patchy red ring around the new flow, and a bright deposit both closer to the flow and beyond the red patches. There are no apparent surface changes beyond the bright annulus. SHARK-VIS sees part of the bright annulus and maybe portions of the patchy red ring. (g) JIRAM PJ68 image showing hot spots during the powerful 2024 December eruption (a log stretch has been applied; J. E. Perry et al. 2025, in preparation). Some other prominent hot spots (A. G. Davies et al. 2024; J. E. Perry et al. 2025, 2025, in preparation) are labeled. In all panels, 180°W 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 observations of Io on 2025 February 18 and 23 and their deconvolution. Panels (a), (b), and (c) show the images obtained through the I, R, and V filters, respectively, on 2025 February 18 at 04:44:38.162Z. Panels (d), (e), and (f) show their deconvolution (see text for details). Panels (g), (h), and (i) show the images obtained through the I, R, and V filters, respectively, on 2025 February 23 at 03:24:30.641Z. Panels (j), (k), and (l) show their deconvolution. Panels (d)–(f) and (j)–(l) show the significant improvement in image quality as a result of this additional data processing. In the lower left corner of each frame, the effective PSF is shown. Derivation of the PSFs, from which the resolutions reported in Table 2 have been computed, is described in the text.