adsabs/AstroCLIMB huggingface dataset:
Paper: Doomed Worlds. I. No New Evidence for Orbital Decay in a Long-term Survey of 43 Ultrahot Jupiters
Authors: Elisabeth R. Adams, Brian Jackson, Amanda A. Sickafoose, Jeffrey P. Morgenthaler, Hannah Worters, Hailey Stubbers, Dallon Carlson, Sakhee Bhure, Stijn Dekeyser, Chelsea X. Huang, Nevin N. Weinberg
Figure caption: ΔBIC values for 43 planets for which we report at least one new light curve. All panels: positive ΔBIC values indicate that a quadratic model is preferred over a linear model. Negative values of ﹩\dot{P}﹩ (decreasing orbital periods) are shown in blue and positive ﹩\dot{P}﹩ (increasing orbital periods) in red. Two horizontal lines show arbitrary cutoffs at ΔBIC = 30 (dashed) and 10 (dotted). Top panel: nominal ΔBIC values (Table 7) with WASP-12 b clearly standing apart from the other planets. Middle panel: same data as top, but zoomed in to show all four systems with ΔBIC ≥ 30 (WASP-121 b, TrES-1 b, WASP-46 b, and WASP-12 b). These four systems also all have at least marginally significant (≥2.5σ) values for ﹩\dot{P}﹩, with σ values plotted below the bar. Bottom panel: recalculated values of ΔBIC using error bars on all points that have been uniformly rescaled so that the χ 2 value of the fit is equal to 1 (see description of the rescaling test in Section 5.4). Few planets retain positive ΔBIC values, indicating that in many cases high nominal ΔBIC values may be due to underestimated errors.
Paper: Doomed Worlds. I. No New Evidence for Orbital Decay in a Long-term Survey of 43 Ultrahot Jupiters
Authors: Elisabeth R. Adams, Brian Jackson, Amanda A. Sickafoose, Jeffrey P. Morgenthaler, Hannah Worters, Hailey Stubbers, Dallon Carlson, Sakhee Bhure, Stijn Dekeyser, Chelsea X. Huang, Nevin N. Weinberg
Figure caption: Timing results for WASP-12 b. Panels are listed from top. Panel (1): observed minus calculated times assuming a linear ephemeris. Midtimes derived from light curves that we fitted are in green (TESS) and blue (new ground-based observations). Literature midtimes compiled by Ivshina & Winn (2022) are in black, while those from the ETD are in gray. If there were critical points from the third panel, they would also appear as red diamonds. Panel (2): ΔBIC from observations (solid orange line) and from analytical calculation assuming our value of ﹩\dot{P}﹩ (dashed orange line; see Jackson et al. 2023). The expected evolution of ΔBIC if ﹩\dot{P}=-29.7\,\mathrm{ms}\ {\mathrm{yr}}^{-1}﹩, as for WASP-12 b in Yee et al. (2020), is shown by the gray dashed line, with its final value noted in the legend. Panel (3): final ΔBIC using all data (dashed orange line), compared to the final ΔBIC if just one point were omitted. If there are any points that lead to large shifts (final ΔBIC changes by ≥25% and at least 5), they are highlighted with red diamonds in panels one and three. Panel (4): observed minus calculated times for the best-fit quadratic ephemeris.
Paper: Doomed Worlds. I. No New Evidence for Orbital Decay in a Long-term Survey of 43 Ultrahot Jupiters
Authors: Elisabeth R. Adams, Brian Jackson, Amanda A. Sickafoose, Jeffrey P. Morgenthaler, Hannah Worters, Hailey Stubbers, Dallon Carlson, Sakhee Bhure, Stijn Dekeyser, Chelsea X. Huang, Nevin N. Weinberg
Figure caption: Timing results for WASP-19 b using unmodified literature times, as discussed in Section 6.2. The description of the data is the same as in Figure 3, except that times from three works are highlighted: six transits from Espinoza et al. (2019), which appear as purple triangles, center; three transits from Tregloan-Reed et al. (2013), which appear as a single orange square, left; and three transits from Sedaghati et al. (2017), which appear as orange squares, center. These works all either have errors or are responsible for critical points that strongly affect ΔBIC; see discussion in the text.
Paper: Doomed Worlds. I. No New Evidence for Orbital Decay in a Long-term Survey of 43 Ultrahot Jupiters
Authors: Elisabeth R. Adams, Brian Jackson, Amanda A. Sickafoose, Jeffrey P. Morgenthaler, Hannah Worters, Hailey Stubbers, Dallon Carlson, Sakhee Bhure, Stijn Dekeyser, Chelsea X. Huang, Nevin N. Weinberg
Figure caption: Timing results for WASP-19 b using the modified literature times, as discussed in Section 6.2. Description of the data is the same as Figure 3, except that times from two works are highlighted: three transits from Tregloan-Reed et al. (2013), which appear as a single orange square at left, and three transits from Sedaghati et al. (2017), which appear as orange squares at center. Note that the timing for three transits from Tregloan-Reed et al. (2013) have been corrected and six transits from Espinoza et al. (2019) have been removed, compared to Figure 4. Meanwhile, the times from Sedaghati et al. (2017) are no longer critical points that strongly impact the fitted value for ΔBIC. See discussion in the text.
Paper: Doomed Worlds. I. No New Evidence for Orbital Decay in a Long-term Survey of 43 Ultrahot Jupiters
Authors: Elisabeth R. Adams, Brian Jackson, Amanda A. Sickafoose, Jeffrey P. Morgenthaler, Hannah Worters, Hailey Stubbers, Dallon Carlson, Sakhee Bhure, Stijn Dekeyser, Chelsea X. Huang, Nevin N. Weinberg
Figure caption: Twenty-three new light curves of six planets: CoRoT-2 b, TrES-1 b, WASP-12 b, WASP-19 b, WASP-46 b, and WASP-121 b. The date and site of each observation are given in the panel header (see Section 2). Normalized relative flux is plotted vs. truncated time, where the time of the first observation in each sequence has been subtracted for clarity of display. Data are shown as gray points, with binned data shown as blue points. A transit light-curve model fit is overplotted in red. These light curves are available as supplementary data.
Paper: Doomed Worlds. I. No New Evidence for Orbital Decay in a Long-term Survey of 43 Ultrahot Jupiters
Authors: Elisabeth R. Adams, Brian Jackson, Amanda A. Sickafoose, Jeffrey P. Morgenthaler, Hannah Worters, Hailey Stubbers, Dallon Carlson, Sakhee Bhure, Stijn Dekeyser, Chelsea X. Huang, Nevin N. Weinberg
Figure caption: Constraints on ﹩{Q}_{\star }^{{\prime} }﹩ placed by observations. Lower limits are shown as upward-facing triangles and represent the 3σ lower limit for ﹩{Q}_{\star }^{{\prime} };﹩ these were calculated even for systems that had marginally positive values for ﹩\dot{P}﹩ (increasing periods), so long as the 3σ value is below 0 (only WASP-121 b does not have this constraint). If ﹩\dot{P}﹩ is nominally negative but insignificant (<3σ detection), the corresponding value for ﹩{Q}_{\star }^{{\prime} }﹩ is shown as an open blue circle; the two systems with significant values for ﹩\dot{P}﹩, WASP-12 b and TrES-1 b, are shown as filled blue circles. Finally, we plotted the theoretical estimates for ﹩{Q}_{\star }^{{\prime} }﹩ from Table 7 based on the work of Weinberg et al. (2024) as purple plus signs. See Table 7 for all parameter values.
Paper: Doomed Worlds. I. No New Evidence for Orbital Decay in a Long-term Survey of 43 Ultrahot Jupiters
Authors: Elisabeth R. Adams, Brian Jackson, Amanda A. Sickafoose, Jeffrey P. Morgenthaler, Hannah Worters, Hailey Stubbers, Dallon Carlson, Sakhee Bhure, Stijn Dekeyser, Chelsea X. Huang, Nevin N. Weinberg
Figure caption: Timing results for TrES-1 b. The description of the data is the same as in Figure 3.
Paper: Doomed Worlds. I. No New Evidence for Orbital Decay in a Long-term Survey of 43 Ultrahot Jupiters
Authors: Elisabeth R. Adams, Brian Jackson, Amanda A. Sickafoose, Jeffrey P. Morgenthaler, Hannah Worters, Hailey Stubbers, Dallon Carlson, Sakhee Bhure, Stijn Dekeyser, Chelsea X. Huang, Nevin N. Weinberg
Figure caption: Timing results for WASP-46 b. The description of the data is the same as in Figure 3.
Paper: Doomed Worlds. I. No New Evidence for Orbital Decay in a Long-term Survey of 43 Ultrahot Jupiters
Authors: Elisabeth R. Adams, Brian Jackson, Amanda A. Sickafoose, Jeffrey P. Morgenthaler, Hannah Worters, Hailey Stubbers, Dallon Carlson, Sakhee Bhure, Stijn Dekeyser, Chelsea X. Huang, Nevin N. Weinberg
Figure caption: Timing results for Kepler-1658 b, using data from Vissapragada et al. (2022). The description of the data is the same as in Figure 3.
Paper: Doomed Worlds. I. No New Evidence for Orbital Decay in a Long-term Survey of 43 Ultrahot Jupiters
Authors: Elisabeth R. Adams, Brian Jackson, Amanda A. Sickafoose, Jeffrey P. Morgenthaler, Hannah Worters, Hailey Stubbers, Dallon Carlson, Sakhee Bhure, Stijn Dekeyser, Chelsea X. Huang, Nevin N. Weinberg
Figure caption: Timing results for CoRoT-2 b with new fit values for CoRoT mission data replacing the values used by Öztürk & Erdem (2019) and Ivshina & Winn (2022). Instead of a strong negative curvature, CoRoT-2 b shows no signs of nonlinearity. The description of the data is the same as in Figure 3.
Paper: Doomed Worlds. I. No New Evidence for Orbital Decay in a Long-term Survey of 43 Ultrahot Jupiters
Authors: Elisabeth R. Adams, Brian Jackson, Amanda A. Sickafoose, Jeffrey P. Morgenthaler, Hannah Worters, Hailey Stubbers, Dallon Carlson, Sakhee Bhure, Stijn Dekeyser, Chelsea X. Huang, Nevin N. Weinberg
Figure caption: Timing results for WASP-121 b. The description of the data is the same as in Figure 3.
Paper: The Vulcan Mission to Io: Lessons Learned during the 2022 JPL Planetary Science Summer School
Authors: K. G. Hanley, Q. McKown, E. M. Cangi, C. Sands, N. North, P. M. Miklavčič, M. S. Bramble, J. M. Bretzfelder, B. D. Byron, J. Caggiano, J. T. Haber, S. J. Laham, D. Morrison-Fogel, K. A. Napier, R. F. Phillips, S. Ray, M. Sandford, P. Sinha, T. Hudson, J. E. C. Scully, L. Lowes
Figure caption: Potential differentiation states of Io's mantle based on our current knowledge. The left side of this figure shows the potential states of Io's upper mantle (red shaded boxes) based on the composition of lava (by silica wt%) at its surface. The gray shaded boxes at the bottom indicate our current understanding of Io's lava composition based on temperature data from previous missions (McEwen et al. 1998; de Kleer et al. 2019), which suggest several possible differentiation states of Io's upper mantle, from a global subsurface magma ocean to a highly differentiated mantle with a low melt fraction (as shown in the cross section of Io on the right). Vulcan would confirm the silica composition of lava at Io's surface (orange shaded boxes), which would indicate which scenario best describes Io's mantle structure (as indicated by the red arrows from findings to interpretations).
Paper: The Vulcan Mission to Io: Lessons Learned during the 2022 JPL Planetary Science Summer School
Authors: K. G. Hanley, Q. McKown, E. M. Cangi, C. Sands, N. North, P. M. Miklavčič, M. S. Bramble, J. M. Bretzfelder, B. D. Byron, J. Caggiano, J. T. Haber, S. J. Laham, D. Morrison-Fogel, K. A. Napier, R. F. Phillips, S. Ray, M. Sandford, P. Sinha, T. Hudson, J. E. C. Scully, L. Lowes
Figure caption: Comparison of Ionian ridge fields at Prometheus Patera and dune fields at Pluto and Mars. (A) Ridges on Io seen by the Galileo Solid State Imaging instrument, after McDonald et al. (2022). Image PIA02557 (available online from the NASA JPL Photojournal). (B) Ice dunes on Pluto imaged by the New Horizons Multispectral Visible Imaging Camera, after Telfer et al. (2018). Image PIA20213 (available online from the NASA JPL Photojournal). (C) Dunes and ripples on Mars imaged by the High Resolution Imaging Science Experiment (HiRISE; McEwen et al. 2007), with an image resolution of ∼25 cm pixel−1. HiRISE image ESP_025042_1375 (available online via the University of Arizona).
Paper: The Vulcan Mission to Io: Lessons Learned during the 2022 JPL Planetary Science Summer School
Authors: K. G. Hanley, Q. McKown, E. M. Cangi, C. Sands, N. North, P. M. Miklavčič, M. S. Bramble, J. M. Bretzfelder, B. D. Byron, J. Caggiano, J. T. Haber, S. J. Laham, D. Morrison-Fogel, K. A. Napier, R. F. Phillips, S. Ray, M. Sandford, P. Sinha, T. Hudson, J. E. C. Scully, L. Lowes
Figure caption: (A) Single flyby WAC ground cover area with different imaging resolutions denoted by color: >2.5 km pixel−1 (red), >1.5 km pixel−1 (green), >0.75 km pixel−1 (cyan), and <0.75 km pixel−1 (blue). (B) Six flyby NAC ground cover areas with different imaging resolutions denoted by color: >15 m pixel−1 (red), >10 m pixel−1 (yellow), >5 m pixel−1 (green), >1 m pixel−1 (cyan), and >0.5 m pixel−1 (blue).
Paper: The Vulcan Mission to Io: Lessons Learned during the 2022 JPL Planetary Science Summer School
Authors: K. G. Hanley, Q. McKown, E. M. Cangi, C. Sands, N. North, P. M. Miklavčič, M. S. Bramble, J. M. Bretzfelder, B. D. Byron, J. Caggiano, J. T. Haber, S. J. Laham, D. Morrison-Fogel, K. A. Napier, R. F. Phillips, S. Ray, M. Sandford, P. Sinha, T. Hudson, J. E. C. Scully, L. Lowes
Figure caption: A shortened version of Vulcan’s science traceability matrix. The Vulcan mission consists of two overarching goals that are composed of four science objectives. Instrument acronyms are spelled out in Section 3 as well as in Table 2.
Paper: The Vulcan Mission to Io: Lessons Learned during the 2022 JPL Planetary Science Summer School
Authors: K. G. Hanley, Q. McKown, E. M. Cangi, C. Sands, N. North, P. M. Miklavčič, M. S. Bramble, J. M. Bretzfelder, B. D. Byron, J. Caggiano, J. T. Haber, S. J. Laham, D. Morrison-Fogel, K. A. Napier, R. F. Phillips, S. Ray, M. Sandford, P. Sinha, T. Hudson, J. E. C. Scully, L. Lowes
Figure caption: (A) The Vulcan mission logo was designed by team member Skylar Laham. It features a cartoon of the spacecraft flying past Io, with a smaller image of Jupiter in the background. (B) The Vulcan mission patch was designed by team member Macey Sandford.
Paper: The Vulcan Mission to Io: Lessons Learned during the 2022 JPL Planetary Science Summer School
Authors: K. G. Hanley, Q. McKown, E. M. Cangi, C. Sands, N. North, P. M. Miklavčič, M. S. Bramble, J. M. Bretzfelder, B. D. Byron, J. Caggiano, J. T. Haber, S. J. Laham, D. Morrison-Fogel, K. A. Napier, R. F. Phillips, S. Ray, M. Sandford, P. Sinha, T. Hudson, J. E. C. Scully, L. Lowes
Figure caption: A schematic of the Vulcan spacecraft with the stowed assets in their fully deployed configuration. They include the two 6 m diameter UltraFlex solar arrays and the 8 m boom for the MAGs.
Paper: The Vulcan Mission to Io: Lessons Learned during the 2022 JPL Planetary Science Summer School
Authors: K. G. Hanley, Q. McKown, E. M. Cangi, C. Sands, N. North, P. M. Miklavčič, M. S. Bramble, J. M. Bretzfelder, B. D. Byron, J. Caggiano, J. T. Haber, S. J. Laham, D. Morrison-Fogel, K. A. Napier, R. F. Phillips, S. Ray, M. Sandford, P. Sinha, T. Hudson, J. E. C. Scully, L. Lowes
Figure caption: A flowchart illustrating the relationships between the instruments used to collect the data relevant to each objective, the observation targets, the physical quantities deduced from the collected observations, the possible results from measuring each quantity, and the two hypotheses proposed in each objective. Instrument acronyms are spelled out in Section 3 as well as in Table 2.
Paper: The Vulcan Mission to Io: Lessons Learned during the 2022 JPL Planetary Science Summer School
Authors: K. G. Hanley, Q. McKown, E. M. Cangi, C. Sands, N. North, P. M. Miklavčič, M. S. Bramble, J. M. Bretzfelder, B. D. Byron, J. Caggiano, J. T. Haber, S. J. Laham, D. Morrison-Fogel, K. A. Napier, R. F. Phillips, S. Ray, M. Sandford, P. Sinha, T. Hudson, J. E. C. Scully, L. Lowes
Figure caption: A schematic of Vulcan’s thermal subsystem. Four louvers with radiators surround the vaulted instruments and electronics, and other components of the thermal subsystem include miniheaters and electronics, multilayer insulation, and 4 m of heat pipes.
Paper: The Vulcan Mission to Io: Lessons Learned during the 2022 JPL Planetary Science Summer School
Authors: K. G. Hanley, Q. McKown, E. M. Cangi, C. Sands, N. North, P. M. Miklavčič, M. S. Bramble, J. M. Bretzfelder, B. D. Byron, J. Caggiano, J. T. Haber, S. J. Laham, D. Morrison-Fogel, K. A. Napier, R. F. Phillips, S. Ray, M. Sandford, P. Sinha, T. Hudson, J. E. C. Scully, L. Lowes
Figure caption: A projection of the 66 primary science flyby ground tracks (32 dayside, 34 nightside) onto a map of Io’s surface from Williams et al. (2011b). The color of the ground track represents the type of surface feature targeted by that orbit, while dots indicate Vulcan’s 30 (10 per objective) observation targets: paterae are shown in yellow, lava flows in red, and ridge fields in blue. Dayside (nightside) ground tracks are shown by solid (dashed) lines. The 12 flybys whose ground tracks are not shown would focus on gravity science rather than surface imaging.
Paper: The Vulcan Mission to Io: Lessons Learned during the 2022 JPL Planetary Science Summer School
Authors: K. G. Hanley, Q. McKown, E. M. Cangi, C. Sands, N. North, P. M. Miklavčič, M. S. Bramble, J. M. Bretzfelder, B. D. Byron, J. Caggiano, J. T. Haber, S. J. Laham, D. Morrison-Fogel, K. A. Napier, R. F. Phillips, S. Ray, M. Sandford, P. Sinha, T. Hudson, J. E. C. Scully, L. Lowes
Figure caption: Mission traceability matrix for the Vulcan mission. The mission requirements are given for each of the science objectives. These mission requirements fed forward into mission design and spacecraft requirements. Text color is used to indicate traceability between noncontiguous columns.
Paper: The Vulcan Mission to Io: Lessons Learned during the 2022 JPL Planetary Science Summer School
Authors: K. G. Hanley, Q. McKown, E. M. Cangi, C. Sands, N. North, P. M. Miklavčič, M. S. Bramble, J. M. Bretzfelder, B. D. Byron, J. Caggiano, J. T. Haber, S. J. Laham, D. Morrison-Fogel, K. A. Napier, R. F. Phillips, S. Ray, M. Sandford, P. Sinha, T. Hudson, J. E. C. Scully, L. Lowes
Figure caption: A block diagram of the telecommunications subsystem providing the Vulcan mission with a fully redundant X/X and Ka/Ka subsystem using a high-gain antenna to achieve 2 Kb s–1 science downlink and a medium-gain antenna and low-gain antenna to achieve 7.8 b s–1 uplink and 10 b s–1 downlink for safe mode commanding and telemetry.
Paper: The Vulcan Mission to Io: Lessons Learned during the 2022 JPL Planetary Science Summer School
Authors: K. G. Hanley, Q. McKown, E. M. Cangi, C. Sands, N. North, P. M. Miklavčič, M. S. Bramble, J. M. Bretzfelder, B. D. Byron, J. Caggiano, J. T. Haber, S. J. Laham, D. Morrison-Fogel, K. A. Napier, R. F. Phillips, S. Ray, M. Sandford, P. Sinha, T. Hudson, J. E. C. Scully, L. Lowes
Figure caption: A breakout of the dry mass subsystem values for the Vulcan spacecraft, with a mass value as well as a percentage of the whole presented for each subsystem.
Paper: The Vulcan Mission to Io: Lessons Learned during the 2022 JPL Planetary Science Summer School
Authors: K. G. Hanley, Q. McKown, E. M. Cangi, C. Sands, N. North, P. M. Miklavčič, M. S. Bramble, J. M. Bretzfelder, B. D. Byron, J. Caggiano, J. T. Haber, S. J. Laham, D. Morrison-Fogel, K. A. Napier, R. F. Phillips, S. Ray, M. Sandford, P. Sinha, T. Hudson, J. E. C. Scully, L. Lowes
Figure caption: A schematic of the Vulcan spacecraft in launch configuration. Vulcan’s dimensions fit within the 4.6 m diameter fairing envelope.
Paper: The Vulcan Mission to Io: Lessons Learned during the 2022 JPL Planetary Science Summer School
Authors: K. G. Hanley, Q. McKown, E. M. Cangi, C. Sands, N. North, P. M. Miklavčič, M. S. Bramble, J. M. Bretzfelder, B. D. Byron, J. Caggiano, J. T. Haber, S. J. Laham, D. Morrison-Fogel, K. A. Napier, R. F. Phillips, S. Ray, M. Sandford, P. Sinha, T. Hudson, J. E. C. Scully, L. Lowes
Figure caption: A schematic of the Vulcan spacecraft in stowed configuration with major spacecraft components labeled.
Paper: Improved Orthorectification and Empirical Reduction of Topographic Effects in Monostatic Mini-RF S-band Observations of the Moon
Authors: Caleb I. Fassett, Ali M. Bramson, Joshua T. S. Cahill, Cameron P. Harris, Gareth A. Morgan, Catherine D. Neish, Cole A. Nypaver, G. Wesley Patterson, Edgard Rivera-Valentin, Patrick A. Taylor, Bradley J. Thomson
Figure caption: Mosaic (90 m pixel−1) showing ﹩\delta {S}_{{1}_{\mathrm{norm}}}﹩ for all S-band monostatic collects; the base map is LOLA hillshade. Where collects overlap, the mosaic is the mean of all pixel values at a given location. Tycho ray crossing near the south pole is labeled with a yellow arrow.
Paper: Improved Orthorectification and Empirical Reduction of Topographic Effects in Monostatic Mini-RF S-band Observations of the Moon
Authors: Caleb I. Fassett, Ali M. Bramson, Joshua T. S. Cahill, Cameron P. Harris, Gareth A. Morgan, Catherine D. Neish, Cole A. Nypaver, G. Wesley Patterson, Edgard Rivera-Valentin, Patrick A. Taylor, Bradley J. Thomson
Figure caption: Details of radar for three locations in the new mosaics. (a)–(c) Byrgius A crater, whose ejecta (e.g., Neish et al. 2013) is highly radar reflective (enhanced in both ﹩\delta {S}_{{1}_{\mathrm{norm}}}﹩ and δCPR), likely due to rough and blocky ejecta. (d)–(f) The dark ring in the southwestern Orientale Basin, which is a probable pyroclastic deposit (e.g., Head et al. 2002), is seen as a clear area of reduced radar reflectivity in ﹩\delta {S}_{{1}_{\mathrm{norm}}}﹩. The prominent S-band signature implies that the optical anomaly is not just surficial. (g)–(i) Mons Mouton, landing area for the VIPER region (black), is seen as an area of relatively low ﹩\delta {S}_{{1}_{\mathrm{norm}}}﹩ and high δCPR.
Paper: Improved Orthorectification and Empirical Reduction of Topographic Effects in Monostatic Mini-RF S-band Observations of the Moon
Authors: Caleb I. Fassett, Ali M. Bramson, Joshua T. S. Cahill, Cameron P. Harris, Gareth A. Morgan, Catherine D. Neish, Cole A. Nypaver, G. Wesley Patterson, Edgard Rivera-Valentin, Patrick A. Taylor, Bradley J. Thomson
Figure caption: Example of the cross-scene gradient in S-band zoom collect lsz_04531_1cd_xku_37s000_v1. (a) Local incidence angles calculated from observation geometry and SLDEM topography. Radar illumination is from the right/east, shown by a white arrow. (b) Raw measured S 1 Mini-RF swath. The right edge of the collect is at a lower incidence angle (and so should have higher S 1), but the collect is falling off the antenna pattern, so instead, these data exhibit reduced power. (c) The ﹩\delta {S}_{{1}_{\mathrm{norm}}}﹩ for the collect highlights this lower-than-expected return; when the ﹩\delta {S}_{{1}_{\mathrm{norm}}}﹩ fell below 50% (−3.01 dB), we masked the data for all other analyses.
Paper: Improved Orthorectification and Empirical Reduction of Topographic Effects in Monostatic Mini-RF S-band Observations of the Moon
Authors: Caleb I. Fassett, Ali M. Bramson, Joshua T. S. Cahill, Cameron P. Harris, Gareth A. Morgan, Catherine D. Neish, Cole A. Nypaver, G. Wesley Patterson, Edgard Rivera-Valentin, Patrick A. Taylor, Bradley J. Thomson
Figure caption: Mosaic (90 m pixel−1) showing δCPR for all S-band monostatic collects; the base map is LOLA hillshade. Where collects overlap, the mosaic is the mean of the results.
Paper: Improved Orthorectification and Empirical Reduction of Topographic Effects in Monostatic Mini-RF S-band Observations of the Moon
Authors: Caleb I. Fassett, Ali M. Bramson, Joshua T. S. Cahill, Cameron P. Harris, Gareth A. Morgan, Catherine D. Neish, Cole A. Nypaver, G. Wesley Patterson, Edgard Rivera-Valentin, Patrick A. Taylor, Bradley J. Thomson
Figure caption: Histograms of the polar regions (≥80°N and S latitude) showing the differences of terrain in permanent shadow (PSR) and outside permanent shadow (non-PSR). In the north and south, the radar reflectivity as parameterized by the median ﹩\delta {S}_{{1}_{\mathrm{norm}}}﹩ is higher in PSRs than non-PSRs by 0.45 and 0.51 dB, respectively (11%–12%). There is no apparent difference in median δCPR, but the values are shifted to higher values inside PSRs (a fatter right tail) in both the north and south.