adsabs/AstroCLIMB huggingface dataset:
Paper: Planetary Waves Drive Horizontal Variations in Trace Species in the Venus Deep Atmosphere
Authors: Maureen Cohen, James Holmes, Stephen Lewis, Manish Patel
Figure caption: Vertical wind velocities measured by Vega balloons 1 (a) and 2 (b) over a period of 45 hr while they traversed one-third of the planet at equatorial latitudes, compared to the long-term (∼30 Earth yr) mean vertical wind velocities for a comparable altitude and latitude from the Surface simulation (c). In all plots, the black line is the vertical wind. The red line is the fundamental frequency when all periodic frequencies have been filtered out, i.e., the background wind neglecting wave activity. The red text gives the value of this background wind. Note both the x-axis and y-axis differ between (a)/(b) and (c).
Paper: Planetary Waves Drive Horizontal Variations in Trace Species in the Venus Deep Atmosphere
Authors: Maureen Cohen, James Holmes, Stephen Lewis, Manish Patel
Figure caption: Power spectral density of the periodicities in the three vertical wind time series shown in Figure 8. The colors indicating the different altitudes are identical to those in Figure 8. Frequencies are given in units of cycles per Venus day (cycles per 117 Earth days; the spectral peak at 3.25 Venus days corresponds to 36 Earth days).
Paper: Planetary Waves Drive Horizontal Variations in Trace Species in the Venus Deep Atmosphere
Authors: Maureen Cohen, James Holmes, Stephen Lewis, Manish Patel
Figure caption: Venus Express/VIRTIS observations of the southern hemisphere taken on 2007 March 22 (top left), 2007 May 17 (bottom left), 2007 February 15 (top right), and 2007 May 6 (bottom right). The left column of each subfigure shows the radiance at 2.3 μm. The right column shows the CO abundance in ppmv expressed as the radiance ratio at 2.30/2.32. The image from May 17 (bottom left) depicts a temporary, longitudinally and latitudinally localized enhancement of CO. Images reproduced from C. C. C. Tsang et al. (2009).
Paper: Grain Size Effects on Visible and Near-infrared (0.35–2.5 μm) Laboratory Spectra of Rare Meteorite Classes
Authors: K. I. Ridenhour, V. Reddy, A. Battle, D. Cantillo, N. C. Pearson, J. A. Sanchez
Figure caption: VNIR spectra of different grain sizes for Abee, an EH4 enstatite chondrite. The top panel shows absolute reflectance, while the bottom panel shows normalized reflectance. For Figures A1–A11, the bottom panel is normalized to 1.5 μm. Slab was not included and separated onto its own figure, so the trend between changing reflectance and grain size can be seen clearly.
Paper: Grain Size Effects on Visible and Near-infrared (0.35–2.5 μm) Laboratory Spectra of Rare Meteorite Classes
Authors: K. I. Ridenhour, V. Reddy, A. Battle, D. Cantillo, N. C. Pearson, J. A. Sanchez
Figure caption: VNIR spectra of grain sizes for Norton County, which is classified as an aubrite.
Paper: Grain Size Effects on Visible and Near-infrared (0.35–2.5 μm) Laboratory Spectra of Rare Meteorite Classes
Authors: K. I. Ridenhour, V. Reddy, A. Battle, D. Cantillo, N. C. Pearson, J. A. Sanchez
Figure caption: VNIR spectra of grain sizes for NWA 4024, which is classified as a winonaite. The drastic absolute reflectance difference between 90–150 μm and the other grain sizes shortward of 1.25 μm is from the higher metal content.
Paper: Grain Size Effects on Visible and Near-infrared (0.35–2.5 μm) Laboratory Spectra of Rare Meteorite Classes
Authors: K. I. Ridenhour, V. Reddy, A. Battle, D. Cantillo, N. C. Pearson, J. A. Sanchez
Figure caption: VNIR spectra of grain sizes for Oued Namous 001 (O.N. 001), which is classified as an angrite.
Paper: Grain Size Effects on Visible and Near-infrared (0.35–2.5 μm) Laboratory Spectra of Rare Meteorite Classes
Authors: K. I. Ridenhour, V. Reddy, A. Battle, D. Cantillo, N. C. Pearson, J. A. Sanchez
Figure caption: VNIR spectra of grain sizes for Fukang, which is classified as a main-group pallasite.
Paper: Grain Size Effects on Visible and Near-infrared (0.35–2.5 μm) Laboratory Spectra of Rare Meteorite Classes
Authors: K. I. Ridenhour, V. Reddy, A. Battle, D. Cantillo, N. C. Pearson, J. A. Sanchez
Figure caption: VNIR spectra of different grain sizes for the ureilite component of Almahata Sitta.
Paper: Grain Size Effects on Visible and Near-infrared (0.35–2.5 μm) Laboratory Spectra of Rare Meteorite Classes
Authors: K. I. Ridenhour, V. Reddy, A. Battle, D. Cantillo, N. C. Pearson, J. A. Sanchez
Figure caption: VNIR spectra of grain sizes for Dhofar 125, which is classified as an acapulcoite.
Paper: Grain Size Effects on Visible and Near-infrared (0.35–2.5 μm) Laboratory Spectra of Rare Meteorite Classes
Authors: K. I. Ridenhour, V. Reddy, A. Battle, D. Cantillo, N. C. Pearson, J. A. Sanchez
Figure caption: VNIR spectra of grain sizes for NWA 753, which is classified as an R chondrite.
Paper: Grain Size Effects on Visible and Near-infrared (0.35–2.5 μm) Laboratory Spectra of Rare Meteorite Classes
Authors: K. I. Ridenhour, V. Reddy, A. Battle, D. Cantillo, N. C. Pearson, J. A. Sanchez
Figure caption: VNIR spectra of different grain sizes for Eagle, an EL6 enstatite chondrite.
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: Photographs of DRACO during ground testing: (a) throughput testing; (b) before vibration testing; (c) during setup of thermal testing.
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: An exploded-view drawing of DRACO with major components labeled. The field-flattening lens is located near the base of the lens baffle tube.
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: (a) The initial, 2560 × 2160 pixel (unbinned) flat-field image before being cropped to the central 2048 × 2048 pixel region (large red square). Vignetting can be seen in the corners, and other structures are apparent. The two halves display different responsivity levels. (b) The 1024 × 1024 binned flat-field correction image derived from the central 2048 × 2048 unbinned region of the full detector. The two circles indicate the locations of the main (central) and secondary ghosts. The squares indicate some of the observed dust particles. Column noise and PRNU (horizontal and vertical features) can also be seen. Panels (a) and (b) are both displayed here with the image origin at the lower left (detector A is on the bottom and contains the ghosts) and with a linear stretch from 0.96 to 1.04. The images are not shown to scale. (c) A histogram (with a logarithmic-scale y-axis) of the central 2048 × 2048 pixel flat field. The bimodal structure reflects the two halves of the detector, with detector A primarily containing values greater than 1 (right group) and detector B containing values less than 1 (left group). The small bump on the side of the detector A distribution is the main ghost.
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: Gain curve measurements as measured for each shutter mode / gain state combination from ground characterization images using the photon transfer technique. The detector was sufficiently nonlinear that radiometric lookup tables were derived to convert from DN into electrons (see Figure 35). Detectors A and B exhibit similar, but not identical, trends. Gain and DN values here are for unbinned pixels, because the lookup tables derived from these gain curves and used in the calibration pipeline were based on unbinned pixel values. The rapid rise at the high-illumination end reflects the saturation of the detector (this rise existed for all cases but was cut off in some of the plots). The lamp intensity and exposure times were such that the signal in the global shutter, 30× gain setup did not exceed ∼900 DN, so a full gain curve was not produced in that configuration.
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: Comparisons of gain curves for the global 1× data processed in the original manner (“reset-only”) and in the updated method (“data-reset”). The original processing method led to a spurious, large increase in gain at low DN levels that was due to popcorn noise. The updated processing method produced a gain curve for global 1× that is far more linear at lower DN levels and is similar to the gain curve for rolling 1×. The y-axis has been truncated to gain values between 0 and 40 e− DN−1. The full range of gain values for the reset-only gain curve was −7879 to 9442 e− DN−1.
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: Radiometric lookup tables for each shutter mode / gain state combination derived from the gain curves (see Figure 34). As noted for the gain curves, detectors A and B exhibit similar, but not identical, trends. The S-shaped features in the gain curve measurements appear as small dips. Electron and DN values here are for unbinned pixels, because the lookup tables derived from these gain curves and used in the calibration pipeline were based on unbinned pixel values. The maximum values shown approximate the full-well capacity of the detector.
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: Read noise measured on a nonflight detector in rolling shutter mode for unbinned pixels in 16 100 × 100 pixel boxes (numbers 1–16) and two 900 × 900 pixel boxes (numbers 17 and 18) across each detector half (A and B) for each gain state (using 25 image pairs). Error bars are the standard deviation of read noise within each box. No significant spatial variation was observed, so it was decided that one value could represent the read noise of each detector half.
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: Comparison of read noise for all four gain states in rolling shutter mode for binned pixels. In all cases, the values were statistically indistinguishable from the ground measurements. White symbols depict the ground calibration values, light-blue symbols are flight images taken during commissioning with the door closed (doy 336), and dark-blue symbols are flight images taken during commissioning with the door open (doy 341). An additional set of door-open flight images is shown for 30×, taken during Star Cal A. Read noise for global shutter could not be assessed in flight owing to the onboard reset frame subtraction.
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: The mean bias level for detectors A and B in rolling shutter mode at 30× gain during flight. DN values are for binned pixels. The three outliers correspond to collections with known differences from nominal flight conditions. No systematic changes were observed in the bias level over the course of the 10-month flight period. Index numbers on the x-axis are mapped to acquisition dates in Table A2.
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: (Top) The locations of profiles taken across the main and secondary ghosts to evaluate their effect on the brightness. The image has a linear stretch from 1 to 1.04 and shows only detector A, with the origin at the lower left. (Bottom) The profiles across the main and secondary ghosts.
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: Image histograms generated from Fe55 test images, for gain states 1×, 2×, and 10×, from left to right. The histograms show number of pixels vs. DN over the range of DN encompassing Mn Kα and Kβ.
Paper: Visible Spectral Atlas of Geostationary Satellites from Tucson, AZ for Differentiating Between Natural and Artificial Objects
Authors: Adam Battle, Vishnu Reddy, Roberto Furfaro, Tanner Campbell
Figure caption: (Left) NIR spectrum (extrapolated into the visible) of metal-rich NEA (6178) 1986 DA from J. A. Sanchez et al. (2021) and (right) spectrum of Earth quasi-satellite Kamo’oalewa from B. N. L. Sharkey et al. (2021) compared with the median satellite bus spectra.
Paper: Visible Spectral Atlas of Geostationary Satellites from Tucson, AZ for Differentiating Between Natural and Artificial Objects
Authors: Adam Battle, Vishnu Reddy, Roberto Furfaro, Tanner Campbell
Figure caption: Comparison between the median spectra of each GEO bus type and select planetary materials. All spectra are normalized to unity at 700 nm. (Left) The average spectra for the T- and L-type asteroids from the Bus-DeMeo taxonomy are shown. (Right) The average spectra for the S- and D-type asteroids are shown. Asteroids are shown with 1σ variation bands.
Paper: Visible Spectral Atlas of Geostationary Satellites from Tucson, AZ for Differentiating Between Natural and Artificial Objects
Authors: Adam Battle, Vishnu Reddy, Roberto Furfaro, Tanner Campbell
Figure caption: Reflectance spectra for two common spacecraft materials compared to the median bus spectrum of the topmost observed buses. (Left) Stainless steel from K. M. Jorgensen (2000) and K. Jorgensen et al. (2001b) has a red, featureless spectrum. (Right) Aluminum sheet metal has a flatter slope and a distinct ∼820 nm absorption band (R. Kokaly et al. 2017).
Paper: Visible Spectral Atlas of Geostationary Satellites from Tucson, AZ for Differentiating Between Natural and Artificial Objects
Authors: Adam Battle, Vishnu Reddy, Roberto Furfaro, Tanner Campbell
Figure caption: Full-night median spectra for Wildblue 1 (29643) in four consecutive months. The same target can show large amounts of seasonal variations over the course of the year. Each spectrum is labeled as Month-Year.
Paper: Visible Spectral Atlas of Geostationary Satellites from Tucson, AZ for Differentiating Between Natural and Artificial Objects
Authors: Adam Battle, Vishnu Reddy, Roberto Furfaro, Tanner Campbell
Figure caption: Median spectrum for each of the five most observed bus types. Variance bands for each median spectrum are calculated as the median across LPA of the 25th and 75th percentiles from stacking spectral phase maps of each bus.
Paper: The Upper Atmosphere of Uranus from Stellar Occultations. II. Revised Temperatures in the Upper Stratosphere and Lower Thermosphere
Authors: William R. Saunders, Michael J. Person, Paul Withers, Richard G. French, Chanita Tubthong
Figure caption: Composite one-dimensional atmospheric models (gray) fit to (a) the average profile from the results of this work (blue), (b) the cool profile (lower end of the shaded blue 1σ uncertainty region), and (c) the warm profile (upper end of the shaded blue 1σ uncertainty region). The models were also fit to the radio occultation profiles in the lower atmosphere (black) and the exobase temperatures (green and red arrows). Additional Voyager 2 UVS stellar occultation (green) and solar occultation (red) points are shown for comparison. The shaded magenta region indicates the approximate pressure level of the heat source; the shaded cyan region indicates that of the heat sink. Within each panel, 10 profiles are shown, representative of that family of models. The pressure scale is exact, but the altitude scale is only exact for the best-fit profile on each panel. Note that all 10 composite models converge at altitudes below about 1 μbar in pressure. For none of the models are the 500 K Voyager 2 points at around 10−6 bar even closely represented. For details on the model parameters for each family, see Table 3.
Paper: The Upper Atmosphere of Uranus from Stellar Occultations. II. Revised Temperatures in the Upper Stratosphere and Lower Thermosphere
Authors: William R. Saunders, Michael J. Person, Paul Withers, Richard G. French, Chanita Tubthong
Figure caption: Average temperature (blue, left y-axis) vs. year (x-axis), with sunspot count (dotted black, right y-axis), thermospheric temperatures from ﹩{{\rm{H}}}_{3}^{+}﹩ measurements (green squares, left y-axis), and disk-integrated b-band magnitude (red circles, right y-axis) overplotted. The average is taken over the same pressure range as shown in Figure 3 by interpolating to an evenly spaced logarithmic pressure grid and taking the arithmetic mean. While the occultation temperatures appear to follow one solar cycle, they do not follow the next. There is no clear and compelling trend between the occultation temperatures and the other quantities.
Paper: The Upper Atmosphere of Uranus from Stellar Occultations. II. Revised Temperatures in the Upper Stratosphere and Lower Thermosphere
Authors: William R. Saunders, Michael J. Person, Paul Withers, Richard G. French, Chanita Tubthong
Figure caption: A reproduction of Figure 1 in I. C. F. Mueller-Wodarg et al. (2008), which compares the atmospheres in the solar system, with additions from G. S. Orton et al. (2014a) and this work. Temperature–pressure profiles are from I. C. F. Mueller-Wodarg et al. (2008) and references therein, unless otherwise cited. The dotted Uranus profile shown in I. C. F. Mueller-Wodarg et al. (2008) is originally from S93. The dashed–dotted Uranus profile is that of G. S. Orton et al. (2014a), which was derived from a H87 prior and Spitzer thermal IR observations. The dashed Uranus profile is the best-fit model from this work. We can clearly see how different the three Uranus profiles are, with our new profile aligning much more closely with that of every other giant planet (and some others) around the 1 μbar pressure level. Though the G. S. Orton et al. (2014a) profile is closer to those of the other giant planets, it does not have the isothermal stratospheric feature. Our best profile and the other giant planets all now show consistent stratosphere–thermosphere boundary levels.
Paper: The Upper Atmosphere of Uranus from Stellar Occultations. II. Revised Temperatures in the Upper Stratosphere and Lower Thermosphere
Authors: William R. Saunders, Michael J. Person, Paul Withers, Richard G. French, Chanita Tubthong
Figure caption: Correlation matrices for the parameters in the (a) radiative–convective part of the model and (b) conductive part of the model. A value of 1 (in red) indicates highly correlated values, −1 (in blue) indicates highly anticorrelated values, and 0 (in gray) indicates uncorrelated values. We do not show the parameter n in panel (a) because there were not enough variations to determine correlations. The parameters in the radiative–convective model are much more correlated or anticorrelated than those in the conductive model.
Paper: The Upper Atmosphere of Uranus from Stellar Occultations. II. Revised Temperatures in the Upper Stratosphere and Lower Thermosphere
Authors: William R. Saunders, Michael J. Person, Paul Withers, Richard G. French, Chanita Tubthong
Figure caption: Comparison of the temperature–pressure profiles produced by different remote-sensing measurements, as in Figure 1. The Voyager 2 results are the same as in Figure 1, but the Earth-based stellar occultations have been updated with the 26 reprocessed profiles produced in this work.