adsabs/AstroCLIMB huggingface dataset:
Paper: Detection of an NH3 Absorption Band at 2.2 μm on Europa
Authors: A. Emran
Figure caption: Two-step noise removal process applied in this study. Left panel: Minnaert-corrected reflectance image at 2.36 μm in the NIMS observation 11ENCYCLOD01A (M. Malaska et al. 2024). Middle panel: spectral denoising using a median filter (three-band window) applied along the spectral axis at each pixel location (random noise reduction). Right panel: spatial smoothing applied to each spectral slice using a 3 × 3 pixel filter (average) on the median-filtered image (radiation noise reduction). Missing pixels in the middle and right panels result from invalid or missing data values at one or more wavelengths at the corresponding pixel locations.
Paper: Detection of an NH3 Absorption Band at 2.2 μm on Europa
Authors: A. Emran
Figure caption: An example spectrum following the two-step noise removal process used in this study. Black dots show the Minnaert-corrected reflectance spectrum at a single pixel (M. Malaska et al. 2018, 2024). The red line represents the result after applying a three-band median filter along the spectral axis (random noise reduced; despiked). The blue line represents the final spectrum after using a 3 × 3 pixel spatial smoothing filter (average) on each spectral slice of the median-filtered image (radiation noise reduced). The x, y coordinates are the location of the pixel in NIMS observation 11ENCYCLOD01A of M. Malaska et al. (2024).
Paper: Calculating Occultation Light Curves Using Wavelets: Exponential Atmospheres and the Constraints of Static Stability
Authors: Leslie A. Young, Michael J. Person
Figure caption: Light-curve morphology limits. Here we summarize the various effects discussed in Section 4. The baseline light-curve flux level (effectively depth into the shadow) is plotted against the log of the fluctuation wavelengths. The labeled regions (A–E) show which diagnostic regime results. For waves with wavelengths longer than 5.14H0, region A, spikes are not possible for statically stable waves in an exponential baseline atmosphere. Waves with vertical wavelengths longer than 0.60H0, regions A–B, cannot make spikes brighter than the unocculted flux. Even waves with fairly small vertical wavelengths (Lz/H0 > 0.13 at half-light), regions A–C, do not lead to ray crossing. And even waves with very small vertical wavelengths (Lz/H0 > 0.003 at half-light), regions A–D, cannot deflect the incoming starlight by more than a wavelength.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Calculating Occultation Light Curves Using Wavelets: Exponential Atmospheres and the Constraints of Static Stability
Authors: Leslie A. Young, Michael J. Person
Figure caption: Statically stable fluctuations assuming Meyer wavelets for ψν, using s = 1, Δ = 0, c = ccrit = 0.054. On the left we show the fluctuations in refractivity, pressure, temperature, and temperature gradient vs. hydrostatic altitude in units of scale height. On the right we show the absolute value of the Fourier transform of these fluctuations. The fluctuations are given by ccritψν, ccritψp, ccritψT, and ﹩{c}_{\mathrm{crit}}{\psi }^{{T}_{r}}﹩, where ccrit is determined by Equation (28). This figure shows the differences in amplitude and phase of the various fluctuations and how the changes in the Fourier transform lead to subtle changes in shape.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Calculating Occultation Light Curves Using Wavelets: Exponential Atmospheres and the Constraints of Static Stability
Authors: Leslie A. Young, Michael J. Person
Figure caption: Statically stable fluctuations assuming Meyer wavelets for ψν, using s = 1, Δ = 0, c = ccrit = 0.054. On the left we show the fluctuations in the line-of-sight integral of refractivity, bending angle, and its derivatives vs. hydrostatic altitude in units of scale height. On the right we show the absolute value of the Fourier transform of these fluctuations. The fluctuations are given by ccritψα, ccritψθ, ﹩{c}_{\mathrm{crit}}{\psi }_{}^{{\theta }_{r}}﹩, and ﹩{c}_{\mathrm{crit}}{\psi }^{{\theta }_{rr}}﹩, where ccrit is determined by Equation (28). As with Figure 3, this figure shows the differences in amplitude and phase of the various fluctuations and how the changes in the Fourier transform lead to subtle changes in shape.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Calculating Occultation Light Curves Using Wavelets: Exponential Atmospheres and the Constraints of Static Stability
Authors: Leslie A. Young, Michael J. Person
Figure caption: The Uranus occultation of 1995 September 9 from SAAO. Here we plot the immersion in normalized stellar flux vs. distance in the shadow plane, relative to half-light and scaled by the atmospheric scale height. Altitude increases to the right, and, for this immersion light curve, time increases to the left. This light curve shows many of the characteristics discussed in this paper, such as multiple examples of resolved spikes, some that reach higher than the unocculted flux level and some that are observed out to 45 scale heights with wider spacing and decreased maximum flux.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Calculating Occultation Light Curves Using Wavelets: Exponential Atmospheres and the Constraints of Static Stability
Authors: Leslie A. Young, Michael J. Person
Figure caption: The mother wavelet, ψ (left), and its Fourier transform, ﹩\hat{\psi }﹩ (right). On the left we plot the wavelet in the time domain, and on the right we plot the absolute value of the complex wavelet in the frequency domain. For the Meyer wavelet used by K. Sato & M. Yamada (1994) and in this work, the wavelet in the time domain is extremely smooth, and the wavelet in the frequency domain is compact, being zero except for at a small range of frequencies.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Calculating Occultation Light Curves Using Wavelets: Exponential Atmospheres and the Constraints of Static Stability
Authors: Leslie A. Young, Michael J. Person
Figure caption: Refraction during a stellar occultation by a distant spherically symmetric atmosphere with a small bending angle. This schematic drawing shows the coordinates used here, where the body plane is perpendicular to the incident rays of starlight and passes through the center of the body. After J. L. Elliot & L. A. Young (1992).
Paper: Jupiter’s Tropical Atmosphere: Shallow Weather, Deep Plumes, and Vortices
Authors: Chris Moeckel, Imke de Pater, Robert, J. Sault, Bryan Butler
Figure caption: Residual structure due to misalignment during the deprojection process that was removed for the Ku-band observations with a Gaussian filter of 65 pixels.
Paper: Jupiter’s Tropical Atmosphere: Shallow Weather, Deep Plumes, and Vortices
Authors: Chris Moeckel, Imke de Pater, Robert, J. Sault, Bryan Butler
Figure caption: Same as Figure 15, but for K-band observations around 20 GHz.
Paper: Jupiter’s Tropical Atmosphere: Shallow Weather, Deep Plumes, and Vortices
Authors: Chris Moeckel, Imke de Pater, Robert, J. Sault, Bryan Butler
Figure caption: Same as Figure 15, but for K-band observations around 24 GHz.
Paper: VIPER’s Mass Spectrometer Observing Lunar Operations (MSolo)
Authors: Roberto Aguilar Ayala, Janine E. Captain, James T. Smith, Matthew L. Hancock, Alexander W. Jarnot, Kevin E. Smith, Prital J. Johnson, Christopher S. Johnson, Rodolphe Carro, Rolando J. Nieves, Christopher N. Bond, John Trautwein, Kenneth C. Wright, Jaime L. Winfield, Peter Santariello, Amy McAdam, P. Douglas Archer, Gregory Kreinheder, Jorge A. Diaz, Parvathy Prem, Kathleen E. Mandt, Aleksandra Gawronska, Barbara A. Cohen, Jaqueline W. Quinn
Figure caption: (A) Assembled CGS manifold showing the Mindrum valve (left) and the upper and lower C-seals used to fix the CGS microvalve onto the CGS weldment (upper right). (B) 3D model sectioned view showing the frit location and its proximity to MSolo’s sensor.
Paper: VIPER’s Mass Spectrometer Observing Lunar Operations (MSolo)
Authors: Roberto Aguilar Ayala, Janine E. Captain, James T. Smith, Matthew L. Hancock, Alexander W. Jarnot, Kevin E. Smith, Prital J. Johnson, Christopher S. Johnson, Rodolphe Carro, Rolando J. Nieves, Christopher N. Bond, John Trautwein, Kenneth C. Wright, Jaime L. Winfield, Peter Santariello, Amy McAdam, P. Douglas Archer, Gregory Kreinheder, Jorge A. Diaz, Parvathy Prem, Kathleen E. Mandt, Aleksandra Gawronska, Barbara A. Cohen, Jaqueline W. Quinn
Figure caption: (Top) MSolo block diagram. (Bottom) Exploded 3D model of MSolo.
Paper: VIPER’s Mass Spectrometer Observing Lunar Operations (MSolo)
Authors: Roberto Aguilar Ayala, Janine E. Captain, James T. Smith, Matthew L. Hancock, Alexander W. Jarnot, Kevin E. Smith, Prital J. Johnson, Christopher S. Johnson, Rodolphe Carro, Rolando J. Nieves, Christopher N. Bond, John Trautwein, Kenneth C. Wright, Jaime L. Winfield, Peter Santariello, Amy McAdam, P. Douglas Archer, Gregory Kreinheder, Jorge A. Diaz, Parvathy Prem, Kathleen E. Mandt, Aleksandra Gawronska, Barbara A. Cohen, Jaqueline W. Quinn
Figure caption: Spectral representation of an analog scan using a 1 ppamu method (red) vs. a 10 ppamu method (purple).
Paper: VIPER’s Mass Spectrometer Observing Lunar Operations (MSolo)
Authors: Roberto Aguilar Ayala, Janine E. Captain, James T. Smith, Matthew L. Hancock, Alexander W. Jarnot, Kevin E. Smith, Prital J. Johnson, Christopher S. Johnson, Rodolphe Carro, Rolando J. Nieves, Christopher N. Bond, John Trautwein, Kenneth C. Wright, Jaime L. Winfield, Peter Santariello, Amy McAdam, P. Douglas Archer, Gregory Kreinheder, Jorge A. Diaz, Parvathy Prem, Kathleen E. Mandt, Aleksandra Gawronska, Barbara A. Cohen, Jaqueline W. Quinn
Figure caption: Screenshot of CNS window showing a mass spectrum of a CO2 standard.
Paper: VIPER’s Mass Spectrometer Observing Lunar Operations (MSolo)
Authors: Roberto Aguilar Ayala, Janine E. Captain, James T. Smith, Matthew L. Hancock, Alexander W. Jarnot, Kevin E. Smith, Prital J. Johnson, Christopher S. Johnson, Rodolphe Carro, Rolando J. Nieves, Christopher N. Bond, John Trautwein, Kenneth C. Wright, Jaime L. Winfield, Peter Santariello, Amy McAdam, P. Douglas Archer, Gregory Kreinheder, Jorge A. Diaz, Parvathy Prem, Kathleen E. Mandt, Aleksandra Gawronska, Barbara A. Cohen, Jaqueline W. Quinn
Figure caption: Fully assembled MSolo (left) and a representation of the dual filament design of the sensor (right), with one filament energized in the top right and the second filament in the bottom right.
Paper: VIPER’s Mass Spectrometer Observing Lunar Operations (MSolo)
Authors: Roberto Aguilar Ayala, Janine E. Captain, James T. Smith, Matthew L. Hancock, Alexander W. Jarnot, Kevin E. Smith, Prital J. Johnson, Christopher S. Johnson, Rodolphe Carro, Rolando J. Nieves, Christopher N. Bond, John Trautwein, Kenneth C. Wright, Jaime L. Winfield, Peter Santariello, Amy McAdam, P. Douglas Archer, Gregory Kreinheder, Jorge A. Diaz, Parvathy Prem, Kathleen E. Mandt, Aleksandra Gawronska, Barbara A. Cohen, Jaqueline W. Quinn
Figure caption: Mass spectra collected at various CPTs throughout V&V.
Paper: VIPER’s Mass Spectrometer Observing Lunar Operations (MSolo)
Authors: Roberto Aguilar Ayala, Janine E. Captain, James T. Smith, Matthew L. Hancock, Alexander W. Jarnot, Kevin E. Smith, Prital J. Johnson, Christopher S. Johnson, Rodolphe Carro, Rolando J. Nieves, Christopher N. Bond, John Trautwein, Kenneth C. Wright, Jaime L. Winfield, Peter Santariello, Amy McAdam, P. Douglas Archer, Gregory Kreinheder, Jorge A. Diaz, Parvathy Prem, Kathleen E. Mandt, Aleksandra Gawronska, Barbara A. Cohen, Jaqueline W. Quinn
Figure caption: Test chamber and some of its subcomponents.
Paper: VIPER’s Mass Spectrometer Observing Lunar Operations (MSolo)
Authors: Roberto Aguilar Ayala, Janine E. Captain, James T. Smith, Matthew L. Hancock, Alexander W. Jarnot, Kevin E. Smith, Prital J. Johnson, Christopher S. Johnson, Rodolphe Carro, Rolando J. Nieves, Christopher N. Bond, John Trautwein, Kenneth C. Wright, Jaime L. Winfield, Peter Santariello, Amy McAdam, P. Douglas Archer, Gregory Kreinheder, Jorge A. Diaz, Parvathy Prem, Kathleen E. Mandt, Aleksandra Gawronska, Barbara A. Cohen, Jaqueline W. Quinn
Figure caption: MSolo FC and EM mode mass spectra with CGS open comparison with key peaks labeled.
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: Flash-frozen 23% NaCl brine is bland in the visible with small spectral features in the infrared (arrows). (a) Before irradiation (pristine in gray) and after irradiation at 10 (cyan) and 20 keV (green). The discoloration “saturates” after hundreds of minutes of 10 keV irradiation and reddens more after the irradiation energy is increased to 20 keV. Some spectral “relaxation” occurs after irradiation, and the sample is kept cold with spectra taken after 6 hr 45 min and after another 17 hr 45 minutes (black). (b) After warming overnight under vacuum to room temperature, the brine desiccated and presumably NaCl (gray line) forms. After cooling to ∼144 K and irradiating with 10 keV electrons, the typical halite color center near 0.46 μm forms.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
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: A color center forms at 0.458 μm in the NaCl that was present along with the hydrohalite and deepens with increasing electron beam energy and/or fluence. The infrared is not affected. In (a), energy was increased from 1 to 10 keV and flux was constant at ∼46 nA cm−2, temperature ∼120 K. In (b), flux was increased from ∼8 and 128 nA cm−2 at a constant energy of 10 keV, temperature ∼145 K. In (c), energy was increased from 1 to 30 keV and flux varied, temperature ∼133 K; the infrared spectrum of the pristine sample is affected by a small amount of frost on the sample that is lost once irradiation begins.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
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: Visible spectra pellet before irradiation and after irradiation at 1–40 keV of (a) MgCl2·6H2O and (b) MgCl2·nH2O, where n < 6, at ∼130 K. Hydration state strongly affects the spectral signature of keV electron irradiation.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
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 of pristine (gray) and irradiated 3.5% flash-frozen NaCl brine pellet show spectral change in the visible, while the infrared portion is invariant and essentially indistinguishable from water ice (thin black line), which did not change before or after irradiation.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
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: Epsomite is particularly resistant to spectral alteration. Reddening only begins to become noticeable at 40 keV. The arrow marks the feature in the infrared that is not present in water ice.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
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: Reflectance spectra of FeCl2·4H2O pellet before irradiation (gray) and after irradiating with 40 keV electrons (red). Also shown is a spectrum taken after warming overnight under vacuum to room temperature and then recooling to 207 K (black) but with no irradiation.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
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: (a) XRD spectra of hydrohalite produced at JPL, unfiltered from the water ice matrix. Locations of peak positions are shown as symbols—ice: “solid triangle”; halite: “asterisk”; hydrohalite: “vertical line.” While water-ice lines dominate, NaCl and hydrohalite lines are present at 238 K. (b) The structure of hydrohalite is much more open than the face-centered cubic (box-like) structure of NaCl (not shown).
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: Plan view of the UHV chamber in which the irradiation experiments were conducted and the reflectance spectra were obtained. By rotating the sample to the spectral port, visible near-infrared spectra (green path) could be collected immediately after irradiation (yellow line) while maintaining vacuum. Maintaining vacuum ensures that the spectral characteristics of the color centers were not affected by an interaction between the irradiated pellet and the atmosphere.
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: Schematic of the sample holder assembly showing the placement of the pellet during loading into the sample holder. Also shown is the Faraday cup (same size as the pellet) that is placed at the top of the sample holder. The thermocouple (not shown) is attached to one of the screws holding down the right side of the front plate.
Paper: Doomed Worlds. II. Reassessing Suggestions of Orbital Decay for TrES-5 b
Authors: Marvin Rothmeier, Elisabeth R. Adams, Karsten Schindler, André Beck, Brian Jackson, Jeffrey P. Morgenthaler, Amanda A. Sickafoose, Malia Barker, Luigi Mancini, John Southworth, Daniel Evans, Alfred Krabbe
Figure caption: Timing residuals of a linear model for data available up to the end of 2022, with the best quadratic fit to these data shown in red. This is equivalent to the data available for the timing analyses of S. R. Hagey et al. (2022) and E. S. Ivshina & J. N. Winn (2022). Literature midtimes compiled by E. S. Ivshina & J. N. Winn (2022) are shown in black, while those from the ETD are in gray.
Paper: Doomed Worlds. II. Reassessing Suggestions of Orbital Decay for TrES-5 b
Authors: Marvin Rothmeier, Elisabeth R. Adams, Karsten Schindler, André Beck, Brian Jackson, Jeffrey P. Morgenthaler, Amanda A. Sickafoose, Malia Barker, Luigi Mancini, John Southworth, Daniel Evans, Alfred Krabbe
Figure caption: Folded transits for PSST data from 2007 (blue) and 2009 (orange) using data taken by G. Mandushev et al. (2011).
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 uses a bite-sampling approach. The bottom images show actual cuttings cones formed by delivering 8 cm deep bites to the surface from an 80 cm deep hole. The drill string (upper left) shows the “bite” flute design to increase sample retention in each 10 cm bite.
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: Environmental test chamber used to simulate a lunar environment for TRIDENT EU testing. The bin is approximately 30 cm in diameter.
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: Drilling data from TRIDENT (K. Zacny & P. Chu 2024).
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: SDE compared to the measured UCS of rocks during TRIDENT testing. This baseline can generate an empirical model that takes measured operational parameters and determines a range of in situ material hardness.