adsabs/AstroCLIMB huggingface dataset:
Paper: New Mass and Radius Constraints on the LHS 1140 Planets: LHS 1140 b Is either a Temperate Mini-Neptune or a Water World
Authors: Charles Cadieux, Mykhaylo Plotnykov, René Doyon, Diana Valencia, Farbod Jahandar, Lisa Dang, Martin Turbet, Thomas J. Fauchez, Ryan Cloutier, Collin Cherubim, Étienne Artigau, Neil J. Cook, Billy Edwards, Tim Hallatt, Benjamin Charnay, François Bouchy, Romain Allart, Lucile Mignon, Frédérique Baron, Susana C. C. Barros, Björn Benneke, B. L. Canto Martins, Nicolas B. Cowan, J. R. De Medeiros, Xavier Delfosse, Elisa Delgado-Mena, Xavier Dumusque, David Ehrenreich, Yolanda G. C. Frensch, J. I. González Hernández, Nathan C. Hara, David Lafrenière, Gaspare Lo Curto, Lison Malo, Claudio Melo, Dany Mounzer, Vera Maria Passeger, Francesco Pepe, Anne-Sophie Poulin-Girard, Nuno C. Santos, Danuta Sosnowska, Alejandro Suárez Mascareño, Simon Thibault, Valentina Vaulato, Gregg A. Wade, François Wildi
Figure caption: Validating Keplerian signals in the ESPRESSO spectral domain of LHS 1140. Left panels: semiamplitudes K  λ  obtained with model ﹩{{ \mathcal M }}_{3\mathrm{cp}}﹩ from LBL RVs extracted for different bands (Δλ ≈ 20 nm). The per-band velocities have uncertainties (σ RV) varying from 4.73 to 0.65 m s−1 (orange dashed lines). A genuine Keplerian signal is achromatic (dK  λ /d λ = 0). We measure no chromatic slopes for LHS 1140 b and c, but the signal of candidate LHS 1140 d is marginally larger in the blue wavelengths of ESPRESSO (dK  λ /d λ = −0.42 ± 0.26  m s−1 per 100 nm). A coherent signal such as a Doppler shift affecting all wavelengths should produce consistent K between the full spectrum constraints (1σ confidence regions in blue) and the weighted average of K  λ  (1σ confidence interval between the red dotted lines). Assuming a coherent signal, the K d inferred from the full ESPRESSO domain should have an uncertainty ﹩{\sigma }_{{K}_{{\rm{d}}}}\sim 0.18﹩ m s−1, which is inconsistent with observations. Right panels: semiamplitude uncertainties σ  K  with increasing RV precision (smaller σ RV). A coherent signal in wavelengths should follow the Cloutier et al. (2018) formalism (﹩{\sigma }_{K}={\sigma }_{\mathrm{RV}}\sqrt{2/{N}_{\mathrm{RV}}}﹩), which is not seen for LHS 1140 d. The LBL data set shows no evidence of an 80 day signal associated with the candidate planet LHS 1140 d.
Paper: New Mass and Radius Constraints on the LHS 1140 Planets: LHS 1140 b Is either a Temperate Mini-Neptune or a Water World
Authors: Charles Cadieux, Mykhaylo Plotnykov, René Doyon, Diana Valencia, Farbod Jahandar, Lisa Dang, Martin Turbet, Thomas J. Fauchez, Ryan Cloutier, Collin Cherubim, Étienne Artigau, Neil J. Cook, Billy Edwards, Tim Hallatt, Benjamin Charnay, François Bouchy, Romain Allart, Lucile Mignon, Frédérique Baron, Susana C. C. Barros, Björn Benneke, B. L. Canto Martins, Nicolas B. Cowan, J. R. De Medeiros, Xavier Delfosse, Elisa Delgado-Mena, Xavier Dumusque, David Ehrenreich, Yolanda G. C. Frensch, J. I. González Hernández, Nathan C. Hara, David Lafrenière, Gaspare Lo Curto, Lison Malo, Claudio Melo, Dany Mounzer, Vera Maria Passeger, Francesco Pepe, Anne-Sophie Poulin-Girard, Nuno C. Santos, Danuta Sosnowska, Alejandro Suárez Mascareño, Simon Thibault, Valentina Vaulato, Gregg A. Wade, François Wildi
Figure caption: Predicted transmission spectrum of LHS 1140 b from 0.6 to 5.5 μm for the Earth-like (black) and 5 bar CO2 (blue) global climate models (GCM, Figure 5). The bottom panel is a zoom of the top panel. Simulated JWST/NIRSpec data with the G235H (green) and G395H (orange) dispersers are shown. We estimate that 20 transits equally divided between G235H and G395H are required to detect a secondary atmosphere around LHS 1140 b at 4σ. The red dashed curve is a GCM-based representation of a mini-Neptune (H/He-rich) that can be easily detected with a single visit.
Paper: New Mass and Radius Constraints on the LHS 1140 Planets: LHS 1140 b Is either a Temperate Mini-Neptune or a Water World
Authors: Charles Cadieux, Mykhaylo Plotnykov, René Doyon, Diana Valencia, Farbod Jahandar, Lisa Dang, Martin Turbet, Thomas J. Fauchez, Ryan Cloutier, Collin Cherubim, Étienne Artigau, Neil J. Cook, Billy Edwards, Tim Hallatt, Benjamin Charnay, François Bouchy, Romain Allart, Lucile Mignon, Frédérique Baron, Susana C. C. Barros, Björn Benneke, B. L. Canto Martins, Nicolas B. Cowan, J. R. De Medeiros, Xavier Delfosse, Elisa Delgado-Mena, Xavier Dumusque, David Ehrenreich, Yolanda G. C. Frensch, J. I. González Hernández, Nathan C. Hara, David Lafrenière, Gaspare Lo Curto, Lison Malo, Claudio Melo, Dany Mounzer, Vera Maria Passeger, Francesco Pepe, Anne-Sophie Poulin-Girard, Nuno C. Santos, Danuta Sosnowska, Alejandro Suárez Mascareño, Simon Thibault, Valentina Vaulato, Gregg A. Wade, François Wildi
Figure caption: Left panel: stellar density (ρ ⋆) distribution of LHS 1140 using mass and radius from Mann et al. (2015, 2019; black) and posterior distributions of ρ ⋆ inferred from TESS (red), TESS+Spitzer (purple), and TESS+Spitzer+HST (blue) transits. Right panel: Bayesian inference of the stellar mass and radius of LHS 1140 using the TESS+Spitzer+HST constraints on ρ ⋆ as a measurement and Mann et al. (2015, 2019) as a prior. The positive covariance in M ⋆–R ⋆ space indicates that both parameters are likely to vary in the same direction to produce a constant ρ ⋆ constrained by the transits.
Paper: New Mass and Radius Constraints on the LHS 1140 Planets: LHS 1140 b Is either a Temperate Mini-Neptune or a Water World
Authors: Charles Cadieux, Mykhaylo Plotnykov, René Doyon, Diana Valencia, Farbod Jahandar, Lisa Dang, Martin Turbet, Thomas J. Fauchez, Ryan Cloutier, Collin Cherubim, Étienne Artigau, Neil J. Cook, Billy Edwards, Tim Hallatt, Benjamin Charnay, François Bouchy, Romain Allart, Lucile Mignon, Frédérique Baron, Susana C. C. Barros, Björn Benneke, B. L. Canto Martins, Nicolas B. Cowan, J. R. De Medeiros, Xavier Delfosse, Elisa Delgado-Mena, Xavier Dumusque, David Ehrenreich, Yolanda G. C. Frensch, J. I. González Hernández, Nathan C. Hara, David Lafrenière, Gaspare Lo Curto, Lison Malo, Claudio Melo, Dany Mounzer, Vera Maria Passeger, Francesco Pepe, Anne-Sophie Poulin-Girard, Nuno C. Santos, Danuta Sosnowska, Alejandro Suárez Mascareño, Simon Thibault, Valentina Vaulato, Gregg A. Wade, François Wildi
Figure caption: Top panels: normalized PDCSAP light curve of LHS 1140 from TESS sectors 3 and 30. The blue and red vertical ticks and data points highlight the transits of planet b and c. Bottom panels: phase-folded transit of LHS 1140 b (left) and c (right). The open circles represent the binned photometry, respectively, 12 and 8 minute bins for b and c. The best-fit transit models are depicted with blue curves. The residuals of the fits are shown below their respective transit.
Paper: New Mass and Radius Constraints on the LHS 1140 Planets: LHS 1140 b Is either a Temperate Mini-Neptune or a Water World
Authors: Charles Cadieux, Mykhaylo Plotnykov, René Doyon, Diana Valencia, Farbod Jahandar, Lisa Dang, Martin Turbet, Thomas J. Fauchez, Ryan Cloutier, Collin Cherubim, Étienne Artigau, Neil J. Cook, Billy Edwards, Tim Hallatt, Benjamin Charnay, François Bouchy, Romain Allart, Lucile Mignon, Frédérique Baron, Susana C. C. Barros, Björn Benneke, B. L. Canto Martins, Nicolas B. Cowan, J. R. De Medeiros, Xavier Delfosse, Elisa Delgado-Mena, Xavier Dumusque, David Ehrenreich, Yolanda G. C. Frensch, J. I. González Hernández, Nathan C. Hara, David Lafrenière, Gaspare Lo Curto, Lison Malo, Claudio Melo, Dany Mounzer, Vera Maria Passeger, Francesco Pepe, Anne-Sophie Poulin-Girard, Nuno C. Santos, Danuta Sosnowska, Alejandro Suárez Mascareño, Simon Thibault, Valentina Vaulato, Gregg A. Wade, François Wildi
Figure caption: RV time series of LHS 1140 with ESPRESSO produced with the LBL method. The data before (pre) and after (post) the fiber upgrade of ESPRESSO (2019 June) are distinguished with open and filled circles, respectively. The full RV model (planet b, planet c, and activity GP) is represented by an orange curve, with the activity GP component highlighted with a green dashed curve (details in Appendix D.1).
Paper: New Mass and Radius Constraints on the LHS 1140 Planets: LHS 1140 b Is either a Temperate Mini-Neptune or a Water World
Authors: Charles Cadieux, Mykhaylo Plotnykov, René Doyon, Diana Valencia, Farbod Jahandar, Lisa Dang, Martin Turbet, Thomas J. Fauchez, Ryan Cloutier, Collin Cherubim, Étienne Artigau, Neil J. Cook, Billy Edwards, Tim Hallatt, Benjamin Charnay, François Bouchy, Romain Allart, Lucile Mignon, Frédérique Baron, Susana C. C. Barros, Björn Benneke, B. L. Canto Martins, Nicolas B. Cowan, J. R. De Medeiros, Xavier Delfosse, Elisa Delgado-Mena, Xavier Dumusque, David Ehrenreich, Yolanda G. C. Frensch, J. I. González Hernández, Nathan C. Hara, David Lafrenière, Gaspare Lo Curto, Lison Malo, Claudio Melo, Dany Mounzer, Vera Maria Passeger, Francesco Pepe, Anne-Sophie Poulin-Girard, Nuno C. Santos, Danuta Sosnowska, Alejandro Suárez Mascareño, Simon Thibault, Valentina Vaulato, Gregg A. Wade, François Wildi
Figure caption: Posterior distributions (1σ and 2σ contours) for the transit impact parameter (b) and scaled radius (p = R p/R ⋆) of LHS 1140 b and c. Different colors refer to the fit on TESS (red), Spitzer (purple), and HST (blue) data only. The black contours are the final joint posteriors on all available instruments. A ∼4σ tension in p exists between Spitzer and TESS for LHS 1140 c.
Paper: New Mass and Radius Constraints on the LHS 1140 Planets: LHS 1140 b Is either a Temperate Mini-Neptune or a Water World
Authors: Charles Cadieux, Mykhaylo Plotnykov, René Doyon, Diana Valencia, Farbod Jahandar, Lisa Dang, Martin Turbet, Thomas J. Fauchez, Ryan Cloutier, Collin Cherubim, Étienne Artigau, Neil J. Cook, Billy Edwards, Tim Hallatt, Benjamin Charnay, François Bouchy, Romain Allart, Lucile Mignon, Frédérique Baron, Susana C. C. Barros, Björn Benneke, B. L. Canto Martins, Nicolas B. Cowan, J. R. De Medeiros, Xavier Delfosse, Elisa Delgado-Mena, Xavier Dumusque, David Ehrenreich, Yolanda G. C. Frensch, J. I. González Hernández, Nathan C. Hara, David Lafrenière, Gaspare Lo Curto, Lison Malo, Claudio Melo, Dany Mounzer, Vera Maria Passeger, Francesco Pepe, Anne-Sophie Poulin-Girard, Nuno C. Santos, Danuta Sosnowska, Alejandro Suárez Mascareño, Simon Thibault, Valentina Vaulato, Gregg A. Wade, François Wildi
Figure caption: NIRPS template spectrum of LHS 1140 (black dashed line) around the Al I line (1675.514 nm). The orange envelope depicts the flux dispersion measured on 29 individual observations. Three ACES models with a fixed T eff = 3100 K and metallicities of −0.5 (red line), 0.0 (blue line), and 0.5 (green line) dex are shown. For this single line, we measure [Al/H] = 0.0 ± 0.1 dex. This figure illustrates the precision of the NIRPS data to constrain elemental abundances that are often different from that of iron ([Fe/H] = −0.15 ± 0.09 dex).
Paper: New Mass and Radius Constraints on the LHS 1140 Planets: LHS 1140 b Is either a Temperate Mini-Neptune or a Water World
Authors: Charles Cadieux, Mykhaylo Plotnykov, René Doyon, Diana Valencia, Farbod Jahandar, Lisa Dang, Martin Turbet, Thomas J. Fauchez, Ryan Cloutier, Collin Cherubim, Étienne Artigau, Neil J. Cook, Billy Edwards, Tim Hallatt, Benjamin Charnay, François Bouchy, Romain Allart, Lucile Mignon, Frédérique Baron, Susana C. C. Barros, Björn Benneke, B. L. Canto Martins, Nicolas B. Cowan, J. R. De Medeiros, Xavier Delfosse, Elisa Delgado-Mena, Xavier Dumusque, David Ehrenreich, Yolanda G. C. Frensch, J. I. González Hernández, Nathan C. Hara, David Lafrenière, Gaspare Lo Curto, Lison Malo, Claudio Melo, Dany Mounzer, Vera Maria Passeger, Francesco Pepe, Anne-Sophie Poulin-Girard, Nuno C. Santos, Danuta Sosnowska, Alejandro Suárez Mascareño, Simon Thibault, Valentina Vaulato, Gregg A. Wade, François Wildi
Figure caption: White light curve transit of LHS 1140 b with the WFC3 on HST. The best-fit transit model is shown in blue, with the residuals of the fit shown in the bottom panel.
Paper: A Radio Counterpart to a Jupiter-mass Binary Object in Orion
Authors: Luis F. Rodríguez, Laurent Loinard, Luis A. Zapata
Figure caption: VLA image of the 6.1 GHz emission from JuMBO 24, made concatenating all the data of project SD0630. The contours start at, and increase by steps of, 9 μJy beam−1. The color scale indicates intensity as shown by the color bar to the right. The white rectangle indicates the position of JuMBO 24 as reported by Pearson & McCaughrean (2023): R.A. (J2000) = 05h35m19.ˢ50616, decl. (J2000) = ﹩-05^\circ 23^{\prime} 39\buildrel{\prime\prime}\over{.} 7303﹩. The red ellipse shows the angular size and orientation of the target in the 2.77 μm JWST images (0.″170 × 0.″132; 97°). The synthesized beam of the radio map is shown at the bottom left of the image.
Paper: Weakened Magnetic Braking in the Exoplanet Host Star 51 Peg
Authors: Travis S. Metcalfe, Klaus G. Strassmeier, Ilya V. Ilyin, Derek Buzasi, Oleg Kochukhov, Thomas R. Ayres, Sarbani Basu, Ashley Chontos, Adam J. Finley, Victor See, Keivan G. Stassun, Jennifer L. van Saders, Aldo G. Sepulveda, George R. Ricker
Figure caption: Estimated wind braking torque relative to HD 76151 as a function of Rossby number normalized to the solar value. The points are grouped by Gaia color, corresponding to solar analogs (yellow circles) and hotter (blue triangles) or cooler (red squares) stars. The gray shaded area represents our empirical constraint on the critical Rossby number for the onset of WMB (Rocrit/Ro⊙ = 0.92 ± 0.01).
Paper: Weakened Magnetic Braking in the Exoplanet Host Star 51 Peg
Authors: Travis S. Metcalfe, Klaus G. Strassmeier, Ilya V. Ilyin, Derek Buzasi, Oleg Kochukhov, Thomas R. Ayres, Sarbani Basu, Ashley Chontos, Adam J. Finley, Victor See, Keivan G. Stassun, Jennifer L. van Saders, Aldo G. Sepulveda, George R. Ricker
Figure caption: ZDI maps of the radial, meridional, and azimuthal field components of 51 Peg. Contours are shown with a step of 0.5 G. The dotted line corresponds to the lowest visible latitude. The vertical bars at the bottom of each panel show the central longitude of each LBT observation.
Paper: Weakened Magnetic Braking in the Exoplanet Host Star 51 Peg
Authors: Travis S. Metcalfe, Klaus G. Strassmeier, Ilya V. Ilyin, Derek Buzasi, Oleg Kochukhov, Thomas R. Ayres, Sarbani Basu, Ashley Chontos, Adam J. Finley, Victor See, Keivan G. Stassun, Jennifer L. van Saders, Aldo G. Sepulveda, George R. Ricker
Figure caption: ZDI fit to the observed Stokes V LSD profiles for 51 Peg. Observations (points) and model profiles (solid lines) are shifted vertically according to the rotational phase, which is indicated on the right of each profile.
Paper: Weakened Magnetic Braking in the Exoplanet Host Star 51 Peg
Authors: Travis S. Metcalfe, Klaus G. Strassmeier, Ilya V. Ilyin, Derek Buzasi, Oleg Kochukhov, Thomas R. Ayres, Sarbani Basu, Ashley Chontos, Adam J. Finley, Victor See, Keivan G. Stassun, Jennifer L. van Saders, Aldo G. Sepulveda, George R. Ricker
Figure caption: Power spectrum of 51 Peg centered on the power excess due to solar-like oscillations. The shaded region is used to calculate an autocorrelation, shown in the inset. The dashed lines in the inset represent expected peaks in the ACF due to the characteristic spacings of p-modes.
Paper: Subsurface Thermophysical Properties of Europa’s Leading and Trailing Hemispheres as Revealed by ALMA
Authors: Alexander E. Thelen, Katherine de Kleer, Maria Camarca, Alex Akins, Mark Gurwell, Bryan Butler, Imke de Pater
Figure caption: Electrical skin depth (δ  E ) curves (solid lines) as a function of temperature for a range of global porosities at 97.5 GHz (∼3 mm), as covered by continuum observations in ALMA Band 3. Temperature bounds are set by the predicted variability Europa’s surface experiences throughout a nominal diurnal cycle for a given porosity value. The dust fraction is set to 0.3. Thermal skin depths (δ  T ) over the range of temperatures are plotted (dashed lines) for 10, 30, 50, and 70% porosity models, illustrating the depths needed for derived δ  E  values to be below δ  T , and thus not exhibit temperature anomalies due to diurnal variability.
Paper: Subsurface Thermophysical Properties of Europa’s Leading and Trailing Hemispheres as Revealed by ALMA
Authors: Alexander E. Thelen, Katherine de Kleer, Maria Camarca, Alex Akins, Mark Gurwell, Bryan Butler, Imke de Pater
Figure caption: Electrical skin depth as a function of frequency in the range of ALMA receiver bands for temperatures relevant to Europa’s surface and near subsurface for a global 50% porosity model.
Paper: Three Years of ACB Phase Function Observations from the Mars Science Laboratory: Interannual and Diurnal Variability and Constraints on Ice Crystal Habit
Authors: Alex C. Innanen, Brittney A. Cooper, Conor W. Hayes, Charissa L. Campbell, Jacob L. Kloos, Scott D. Guzewich, John E. Moores
Figure caption: Comparison of MY 34 phase functions derived by Cooper et al. (2019) using MCS opacities (black dashed line) and derived using MSL-derived opacities (blue solid line) plotted with 95% confidence intervals. The MSL-derived mean phase function has been normalized by the mean value of that of Cooper et al. (2019).
Paper: Three Years of ACB Phase Function Observations from the Mars Science Laboratory: Interannual and Diurnal Variability and Constraints on Ice Crystal Habit
Authors: Alex C. Innanen, Brittney A. Cooper, Conor W. Hayes, Charissa L. Campbell, Jacob L. Kloos, Scott D. Guzewich, John E. Moores
Figure caption: Mean curves of the derived phase-function data for MYs 35 and 36 displayed over their respective calculated raw data points. Red shaded error bars correspond to the 95% confidence interval, which is given by the expression ﹩1.96\tfrac{\sigma }{\sqrt{n}}﹩, while gray shaded error bars correspond to the standard deviation (σ). As with the mean curve, both were calculated by binning the data points with a window size of 15° of scattering angle. No normalization has been applied to magnitudes.
Paper: Three Years of ACB Phase Function Observations from the Mars Science Laboratory: Interannual and Diurnal Variability and Constraints on Ice Crystal Habit
Authors: Alex C. Innanen, Brittney A. Cooper, Conor W. Hayes, Charissa L. Campbell, Jacob L. Kloos, Scott D. Guzewich, John E. Moores
Figure caption: A spectral radiance map of the second frame of the fifth pointing movie on Sol 2633 with a region of high spectral radiance (black dot) and low spectral radiance (red dot) indicated. The high-radiance region is assumed to be a cloud, while the low-radiance region is assumed to be empty sky. The color bar represents change in radiance relative to the mean value of the entire image.
Paper: Three Years of ACB Phase Function Observations from the Mars Science Laboratory: Interannual and Diurnal Variability and Constraints on Ice Crystal Habit
Authors: Alex C. Innanen, Brittney A. Cooper, Conor W. Hayes, Charissa L. Campbell, Jacob L. Kloos, Scott D. Guzewich, John E. Moores
Figure caption: Mean phase functions for MY 34, 35, and 36, respectively, plotted with the raw calculated phase-function points. These phase-function values are calculated using MSL-derived tau values. The red shaded error bar corresponds to the 95% confidence interval, while the gray shaded error bar corresponds to the standard deviation. Outliers that are greater than 3 standard deviations from the mean have been removed. No normalization has been applied to magnitudes.
Paper: Three Years of ACB Phase Function Observations from the Mars Science Laboratory: Interannual and Diurnal Variability and Constraints on Ice Crystal Habit
Authors: Alex C. Innanen, Brittney A. Cooper, Conor W. Hayes, Charissa L. Campbell, Jacob L. Kloos, Scott D. Guzewich, John E. Moores
Figure caption: Temporal distributions of PFSS observations for the past three MYs. Observations are distributed between morning and afternoon with a ±2.5 hr keep-out around local noon.
Paper: Three Years of ACB Phase Function Observations from the Mars Science Laboratory: Interannual and Diurnal Variability and Constraints on Ice Crystal Habit
Authors: Alex C. Innanen, Brittney A. Cooper, Conor W. Hayes, Charissa L. Campbell, Jacob L. Kloos, Scott D. Guzewich, John E. Moores
Figure caption:  b and c values for fitted HG functions for MYs 34–36 plotted alongside the hockey-stick relation for two-term HG functions determined by Hapke (2012b). Error bars show the 95% confidence bounds on b and c.
Paper: Three Years of ACB Phase Function Observations from the Mars Science Laboratory: Interannual and Diurnal Variability and Constraints on Ice Crystal Habit
Authors: Alex C. Innanen, Brittney A. Cooper, Conor W. Hayes, Charissa L. Campbell, Jacob L. Kloos, Scott D. Guzewich, John E. Moores
Figure caption: Comparison of MY 35 and 36 average phase functions with the Cooper et al. (2019) MY 34 phase function. MY 35 and 36 phase functions have been normalized around the average value of the MY 34 phase function. All three phase functions use MCS optical depth values. Shaded error bars show the 95% confidence interval.
Paper: Three Years of ACB Phase Function Observations from the Mars Science Laboratory: Interannual and Diurnal Variability and Constraints on Ice Crystal Habit
Authors: Alex C. Innanen, Brittney A. Cooper, Conor W. Hayes, Charissa L. Campbell, Jacob L. Kloos, Scott D. Guzewich, John E. Moores
Figure caption: Comparison of MY 34, 35, and 36 mean phase functions, using phase function values calculated with MSL-derived tau values. The curves have been normalized to overlap in order to more easily compare their shapes. Shaded error bars show the 95% confidence interval.
Paper: Three Years of ACB Phase Function Observations from the Mars Science Laboratory: Interannual and Diurnal Variability and Constraints on Ice Crystal Habit
Authors: Alex C. Innanen, Brittney A. Cooper, Conor W. Hayes, Charissa L. Campbell, Jacob L. Kloos, Scott D. Guzewich, John E. Moores
Figure caption: Comparisons of morning and afternoon mean phase functions plotted alongside their 95% confidence interval for each MY.
Paper: Three Years of ACB Phase Function Observations from the Mars Science Laboratory: Interannual and Diurnal Variability and Constraints on Ice Crystal Habit
Authors: Alex C. Innanen, Brittney A. Cooper, Conor W. Hayes, Charissa L. Campbell, Jacob L. Kloos, Scott D. Guzewich, John E. Moores
Figure caption:  b and c values for our derived phase functions compared with fitted HG curves for six modeled water-ice crystal geometries (Bi & Yang 2014); Martian dust observed by MSL (Chen-Chen et al. 2019) and Phoenix (Moores et al. 2015) and a simulant similar to dust observed by Mars Exploration Rover Spirit (Johnson et al. 2006); and a theoretical smooth, transparent sphere (McGuire 1995). All values are displayed alongside the hockey-stick relation for two-term HG functions determined by Hapke (2012b). Error bars on our derived phase function are the 95% confidence bounds on our b and c values.
Paper: Juno’s JunoCam Images of Europa
Authors: C. J. Hansen, M. A. Ravine, P. M. Schenk, G. C. Collins, E. J. Leonard, C. B. Phillips, M. A. Caplinger, F. Tosi, S. J. Bolton, Björn Jónsson
Figure caption: (a) The high-incidence-angle perspective on images along the terminator shows new blocks, pits, and the arcuate arm of a new trough discovered along the terminator. The 900 m deep pit is ∼24 km across. The change in identification of chaos described in Section 3.2 is also annotated here. (b) This graphic of the features consistent with true polar wander, taken from Schenk et al. (2020), adds in the cluster of JunoCam pits and the new trough on the left side. The JunoCam features are marked with “JC.”