adsabs/AstroCLIMB huggingface dataset:
Paper: Volatile Abundances, Extended Coma Sources, and Nucleus Ice Associations in Comet C/2014 Q2 (Lovejoy)
Authors: Neil Dello Russo, Ronald J. Vervack, Hideyo Kawakita, Boncho P. Bonev, Michael A. DiSanti, Erika L. Gibb, Adam J. McKay, Anita Cochran, Harold A. Weaver, Nicolas Biver, Jacques Crovisier, Dominique Bockelée-Morvan, Hitomi Kobayashi, Walter M. Harris, Nathan X. Roth, Mohammad Saki, and Younas Khan
Figure caption: Flux-calibrated, high-resolution (λ/Δλ ∼ 25,000) 3 spectral × 9 spatial pixel spectral extracts, residuals, and best-fit fluorescence models for C/2014 Q2 (Lovejoy) on February 2. (a) Spectral extracts zoomed in three regions within setting KL1 order 24 showing the eight C2H4 emissions used for the analysis (‡). Solid blue traces are the comet spectral extracts with best-fit synthetic atmospheric models superimposed (dashed red traces). Unidentified emissions (?) and regions of low atmospheric transmittance (areas of low flux density) are shown. (b) Spectral residuals (solid black traces on top of the panel) with the estimated ±1σ channel-by-channel photon noise envelope superimposed (dashed red traces) covering the same spectral regions as panel (a) and showing the C2H4 emissions used in the analysis (‡), as well as unidentified emissions. Best-fit fluorescence models (total model with all contributing species in blue and the C2H4 model below that in turquoise) are also shown. (c) Spectral extracts zoomed in two regions within setting KL3 order 23 showing the seven C2H4 emissions used for the analysis (‡). All other information is the same as for panel (a). (d) Same as panel (b), but covering the same spectral regions as shown in panel (c). The 15 lines used in the February 2 analysis were chosen because they are in regions of relatively high atmospheric transmittance and are not blended with other known species. Line fluxes for the C2H4 emissions are given in Tables A1 and A2.
Paper: Volatile Abundances, Extended Coma Sources, and Nucleus Ice Associations in Comet C/2014 Q2 (Lovejoy)
Authors: Neil Dello Russo, Ronald J. Vervack, Hideyo Kawakita, Boncho P. Bonev, Michael A. DiSanti, Erika L. Gibb, Adam J. McKay, Anita Cochran, Harold A. Weaver, Nicolas Biver, Jacques Crovisier, Dominique Bockelée-Morvan, Hitomi Kobayashi, Walter M. Harris, Nathan X. Roth, Mohammad Saki, and Younas Khan
Figure caption: Spectral profiles of (a) C2H4 and (b) CH4 showing the spectral line shapes for the strongest unblended lines within a setting. C2H4 is compared with CH4 to show that the spectral line shape of C2H4 is consistent with the expected line shape of a clearly detected volatile species obtained within the same order and setting. The estimated 1σ uncertainty level (dashed line) is shown for the C2H4 profile.
Paper: Volatile Abundances, Extended Coma Sources, and Nucleus Ice Associations in Comet C/2014 Q2 (Lovejoy)
Authors: Neil Dello Russo, Ronald J. Vervack, Hideyo Kawakita, Boncho P. Bonev, Michael A. DiSanti, Erika L. Gibb, Adam J. McKay, Anita Cochran, Harold A. Weaver, Nicolas Biver, Jacques Crovisier, Dominique Bockelée-Morvan, Hitomi Kobayashi, Walter M. Harris, Nathan X. Roth, Mohammad Saki, and Younas Khan
Figure caption: Flux-calibrated high-resolution (λ/Δλ ∼ 25,000) spectral residuals and best-fit fluorescence models for C/2014 Q2 (Lovejoy) on (a) February 2, setting KL1 order 26, and (b) February 2, setting KL1 order 24. On the top of each frame are spectral residuals co-added over 3 spectral × 9 spatial pixel extracts (0.″432 × 1.″71) centered on the peak of the gas emission. The dashed red curves superimposed on the comet residuals are the estimated ±1σ channel-by-channel photon noise. The solid blue curves directly below the spectral residuals are the total best-fit fluorescence models convolved to the resolution of the comet spectra that include all molecules. Subsequent color traces below this are the best-fit fluorescence models at the derived or assumed rotational temperatures for each individual molecule.
Paper: Volatile Abundances, Extended Coma Sources, and Nucleus Ice Associations in Comet C/2014 Q2 (Lovejoy)
Authors: Neil Dello Russo, Ronald J. Vervack, Hideyo Kawakita, Boncho P. Bonev, Michael A. DiSanti, Erika L. Gibb, Adam J. McKay, Anita Cochran, Harold A. Weaver, Nicolas Biver, Jacques Crovisier, Dominique Bockelée-Morvan, Hitomi Kobayashi, Walter M. Harris, Nathan X. Roth, Mohammad Saki, and Younas Khan
Figure caption: Similar to Figure A1, but for (a) February 3, setting KL4 order 25, and (b) February 3, setting M2 order 16.
Paper: Volatile Abundances, Extended Coma Sources, and Nucleus Ice Associations in Comet C/2014 Q2 (Lovejoy)
Authors: Neil Dello Russo, Ronald J. Vervack, Hideyo Kawakita, Boncho P. Bonev, Michael A. DiSanti, Erika L. Gibb, Adam J. McKay, Anita Cochran, Harold A. Weaver, Nicolas Biver, Jacques Crovisier, Dominique Bockelée-Morvan, Hitomi Kobayashi, Walter M. Harris, Nathan X. Roth, Mohammad Saki, and Younas Khan
Figure caption: Flux-calibrated high-resolution (λ/Δλ ∼ 25,000) spectral residuals and best-fit fluorescence models for C/2014 Q2 (Lovejoy) on (a) February 2, setting KL3 order 25, and (b) February 2, setting KL1 order 26, illustrating the emissions used for the HC3N and NH3 analyses. On the top of each frame are spectral residuals co-added over 3 spectral × 9 spatial pixel extracts (0.″432 × 1.″71) centered on the peak of the gas emission. The dashed red curves superimposed on the comet residuals are the estimated ±1σ channel-by-channel photon noise. The solid blue curves directly below the spectral residuals are the total best-fit fluorescence models convolved to the resolution of the comet spectra that include all molecules. Below the total models are the best-fit C2H4 and NH3 models. The unblended emissions that are used in the analysis are labeled (‡).
Paper: Volatile Abundances, Extended Coma Sources, and Nucleus Ice Associations in Comet C/2014 Q2 (Lovejoy)
Authors: Neil Dello Russo, Ronald J. Vervack, Hideyo Kawakita, Boncho P. Bonev, Michael A. DiSanti, Erika L. Gibb, Adam J. McKay, Anita Cochran, Harold A. Weaver, Nicolas Biver, Jacques Crovisier, Dominique Bockelée-Morvan, Hitomi Kobayashi, Walter M. Harris, Nathan X. Roth, Mohammad Saki, and Younas Khan
Figure caption: Flux-calibrated high-resolution (λ/Δλ ∼ 25,000) spectral residuals and best-fit fluorescence models for C/2014 Q2 (Lovejoy) zoomed in on regions of interest in Figure 2, primarily highlighting C2H2 and NH3 emissions, as well as emissions from other species and a strong unidentified line (line #8 in Table A9). (a) February 2, setting KL2 order 25. (b) February 2, setting KL3 order 25. On the top of each frame are spectral residuals co-added over 3 spectral × 9 spatial pixel extracts (0.″432 × 1.″71) centered on the peak of the gas emission. Dashed red curves superimposed on the comet residuals are the estimated ±1σ channel-by-channel photon noise. Solid blue curves directly below the spectral residuals are the total best-fit fluorescence models convolved to the resolution of the comet spectra including all molecules. Below the total models are the best-fit models for individual species.
Paper: Volatile Abundances, Extended Coma Sources, and Nucleus Ice Associations in Comet C/2014 Q2 (Lovejoy)
Authors: Neil Dello Russo, Ronald J. Vervack, Hideyo Kawakita, Boncho P. Bonev, Michael A. DiSanti, Erika L. Gibb, Adam J. McKay, Anita Cochran, Harold A. Weaver, Nicolas Biver, Jacques Crovisier, Dominique Bockelée-Morvan, Hitomi Kobayashi, Walter M. Harris, Nathan X. Roth, Mohammad Saki, and Younas Khan
Figure caption: An iterative fitting based on Levenberg–Marquardt χ2 minimization of the comet residuals in setting KL3 order 25. The top traces are the flux-calibrated spectrum (black trace) with best-fit continuum model (violet trace). The middle red trace is the best-fit fluorescence emission model. The bottom black trace is the measured spectrum minus the continuum and emission models (multiplied by 2), outlined in red by the ±1σ channel-by-channel photon noise. Unidentified features are marked with an asterisk.
Paper: Volatile Abundances, Extended Coma Sources, and Nucleus Ice Associations in Comet C/2014 Q2 (Lovejoy)
Authors: Neil Dello Russo, Ronald J. Vervack, Hideyo Kawakita, Boncho P. Bonev, Michael A. DiSanti, Erika L. Gibb, Adam J. McKay, Anita Cochran, Harold A. Weaver, Nicolas Biver, Jacques Crovisier, Dominique Bockelée-Morvan, Hitomi Kobayashi, Walter M. Harris, Nathan X. Roth, Mohammad Saki, and Younas Khan
Figure caption: Spatial profiles of product volatiles (NH2 and OH) and co-measured dust along the slit at different times (settings) on February 2 in the coma of C/2014 Q2 (Lovejoy). Volatile gas column densities (solid colored traces) are compared with simultaneously obtained dust column densities (dashed black traces) scaled to the peak of the gas. The position of the slit with respect to the Sun is given in panel (a).
Paper: Volatile Abundances, Extended Coma Sources, and Nucleus Ice Associations in Comet C/2014 Q2 (Lovejoy)
Authors: Neil Dello Russo, Ronald J. Vervack, Hideyo Kawakita, Boncho P. Bonev, Michael A. DiSanti, Erika L. Gibb, Adam J. McKay, Anita Cochran, Harold A. Weaver, Nicolas Biver, Jacques Crovisier, Dominique Bockelée-Morvan, Hitomi Kobayashi, Walter M. Harris, Nathan X. Roth, Mohammad Saki, and Younas Khan
Figure caption: Comparison of the symmetry of spatial profiles as measured by the ratio of the sunward to antisunward flux (for a projected distance in the range of ∼300–2400 km from the peak of the profile on both sides of the slit) and width (half-width at half-maximum) of volatile spatial profiles relative to the co-measured dust continuum in pixels (1 spatial pixel ∼ 110 km projected distance at the comet). X-axis values = 1 indicate symmetric profiles, whereas values >1 indicate increasing sunward asymmetry, and values <1 indicate increasing antisunward asymmetry. (a) February 2; (b) February 3.
Paper: Volatile Abundances, Extended Coma Sources, and Nucleus Ice Associations in Comet C/2014 Q2 (Lovejoy)
Authors: Neil Dello Russo, Ronald J. Vervack, Hideyo Kawakita, Boncho P. Bonev, Michael A. DiSanti, Erika L. Gibb, Adam J. McKay, Anita Cochran, Harold A. Weaver, Nicolas Biver, Jacques Crovisier, Dominique Bockelée-Morvan, Hitomi Kobayashi, Walter M. Harris, Nathan X. Roth, Mohammad Saki, and Younas Khan
Figure caption: Peak position and width (half-width at half-maximum) of the 16 strongest unidentified emissions (gold numbered points) compared with spatial profiles of identified volatiles and the co-measured dust continuum on February 2. Differences are measured in spatial pixels with 1 pixel ∼ 110 km projected distance at the comet.
Paper: New Constraints on Titan’s Stratospheric n-Butane Abundance
Authors: Brendan L. Steffens, Conor A. Nixon, Keeyoon Sung, Patrick G.J. Irwin, Nicholas A. Lombardo, and Eric Pereira
Figure caption: Molecular geometry of the target of our investigation: (a) n-C4H10 (n-butane), contrasted with its spectroscopically distinct isomer, (b) isobutane, HC(CH3)3.
Paper: New Constraints on Titan’s Stratospheric n-Butane Abundance
Authors: Brendan L. Steffens, Conor A. Nixon, Keeyoon Sung, Patrick G.J. Irwin, Nicholas A. Lombardo, and Eric Pereira
Figure caption: Normalized temperature contribution contours for the 136–216 km EQ data, showing particularly large sensitivity in that altitude range.
Paper: New Constraints on Titan’s Stratospheric n-Butane Abundance
Authors: Brendan L. Steffens, Conor A. Nixon, Keeyoon Sung, Patrick G.J. Irwin, Nicholas A. Lombardo, and Eric Pereira
Figure caption: The n-butane contribution function curves at 1465 cm−1 (near the Q-branch of n-butane’s ν14 band) for each of the nine cases we explored (three data sets, three different profiles). All of our results that follow are reported at the altitudes of the peaks shown in this figure. Note that the legends that appear in the middle panels apply to the other two panels in that row, which belong to the same data set.
Paper: New Constraints on Titan’s Stratospheric n-Butane Abundance
Authors: Brendan L. Steffens, Conor A. Nixon, Keeyoon Sung, Patrick G.J. Irwin, Nicholas A. Lombardo, and Eric Pereira
Figure caption: Samples of the retrieved temperature profiles for each of the three data sets (solid curves), as well as the a priori profiles (dashed curves) used in all three cases (Achterberg et al. 2014; Teanby et al. 2019). For each colored curve, the corresponding similarly colored shading identifies the 1σ uncertainty in the retrieved profile.
Paper: New Constraints on Titan’s Stratospheric n-Butane Abundance
Authors: Brendan L. Steffens, Conor A. Nixon, Keeyoon Sung, Patrick G.J. Irwin, Nicholas A. Lombardo, and Eric Pereira
Figure caption: Example of the model fit of the Cassini CIRS observations using the constant altitude profile for n-butane. Top: model excluding n-butane (red curve) and including 76 ppb of n-butane (purple curve), with EQ observations for altitude range 136–216 km (black curve) and 1σ noise envelope in gray. Bottom: residuals (data minus model) following the same color scheme, with an additional green curve overlaid showing n-butane’s laboratory transmission spectrum at a cold temperature, ∼200 K (Sung et al. 2020), convolved to the CIRS resolution (0.5 cm−1). The Q-branch of n-butane’s ν14 band can be seen at 1466 cm−1, though its sharp peak is substantially broadened at CIRS resolution. Improvement to the fit is particularly evident around this ν14 region, where the residuals are closer to zero for the purple curve than the red curve.
Paper: New Constraints on Titan’s Stratospheric n-Butane Abundance
Authors: Brendan L. Steffens, Conor A. Nixon, Keeyoon Sung, Patrick G.J. Irwin, Nicholas A. Lombardo, and Eric Pereira
Figure caption: Full gas abundance profiles explored in our work. Black horizontal dashed lines show the approximate altitude region for which our models are sensitive. See Figures 2 and 3 for further details on the sensitivity of our models. Note that the placement of the constant profile (red curve) is arbitrary, since our analysis ultimately included scaling this profile to a set of differing abundances.
Paper: New Constraints on Titan’s Stratospheric n-Butane Abundance
Authors: Brendan L. Steffens, Conor A. Nixon, Keeyoon Sung, Patrick G.J. Irwin, Nicholas A. Lombardo, and Eric Pereira
Figure caption: Sample Δχ2 curve for the 136–216 km EQ data using the constant n-butane profile. Improvement to the fit is seen for n-butane abundances of about 80 ppb, though the statistical significance of that improvement is fairly small (1.25σ). The 1σ, 2σ, and 3σ upper limits on the n-butane abundance are marked by dashed vertical lines, as labeled in the legend.
Paper: New Constraints on Titan’s Stratospheric n-Butane Abundance
Authors: Brendan L. Steffens, Conor A. Nixon, Keeyoon Sung, Patrick G.J. Irwin, Nicholas A. Lombardo, and Eric Pereira
Figure caption: The 1σ, 2σ, and 3σ upper limits for n-butane’s abundance, marked by left-pointing arrows, using the EQ data set. The colors of the upper-limit points correspond to the similarly colored profile curves. The vertical blue dashed line marks the upper limit (513 ppb) derived by Hewett et al. (2020), discussed further in Section 5.
Paper: New Constraints on Titan’s Stratospheric n-Butane Abundance
Authors: Brendan L. Steffens, Conor A. Nixon, Keeyoon Sung, Patrick G.J. Irwin, Nicholas A. Lombardo, and Eric Pereira
Figure caption: The 1σ, 2σ, and 3σ upper limits for n-butane’s abundance, marked by left-pointing arrows, using the T3 data set. The colors of the upper-limit points correspond to the similarly colored profile curves.
Paper: New Constraints on Titan’s Stratospheric n-Butane Abundance
Authors: Brendan L. Steffens, Conor A. Nixon, Keeyoon Sung, Patrick G.J. Irwin, Nicholas A. Lombardo, and Eric Pereira
Figure caption: The 1σ, 2σ, and 3σ upper limits for n-butane’s abundance, marked by left -pointing arrows, using the T35 data set. The colors of the upper-limit points correspond to the similarly colored profile curves.
Paper: New Constraints on Titan’s Stratospheric n-Butane Abundance
Authors: Brendan L. Steffens, Conor A. Nixon, Keeyoon Sung, Patrick G.J. Irwin, Nicholas A. Lombardo, and Eric Pereira
Figure caption: The Δχ2 curve for EQ data using the constant n-butane profile.
Paper: New Constraints on Titan’s Stratospheric n-Butane Abundance
Authors: Brendan L. Steffens, Conor A. Nixon, Keeyoon Sung, Patrick G.J. Irwin, Nicholas A. Lombardo, and Eric Pereira
Figure caption: The Δχ2 curve for T3 data using the constant n-butane profile.
Paper: New Constraints on Titan’s Stratospheric n-Butane Abundance
Authors: Brendan L. Steffens, Conor A. Nixon, Keeyoon Sung, Patrick G.J. Irwin, Nicholas A. Lombardo, and Eric Pereira
Figure caption: The Δχ2 curve for T35 data using the constant n-butane profile.
Paper: New Constraints on Titan’s Stratospheric n-Butane Abundance
Authors: Brendan L. Steffens, Conor A. Nixon, Keeyoon Sung, Patrick G.J. Irwin, Nicholas A. Lombardo, and Eric Pereira
Figure caption: The Δχ2 curve for EQ data using the Loison n-butane profile.
Paper: New Constraints on Titan’s Stratospheric n-Butane Abundance
Authors: Brendan L. Steffens, Conor A. Nixon, Keeyoon Sung, Patrick G.J. Irwin, Nicholas A. Lombardo, and Eric Pereira
Figure caption: The Δχ2 curve for T3 data using the Loison n-butane profile.
Paper: New Constraints on Titan’s Stratospheric n-Butane Abundance
Authors: Brendan L. Steffens, Conor A. Nixon, Keeyoon Sung, Patrick G.J. Irwin, Nicholas A. Lombardo, and Eric Pereira
Figure caption: The Δχ2 curve for EQ data using the Krasnopolsky n-butane profile.
Paper: New Constraints on Titan’s Stratospheric n-Butane Abundance
Authors: Brendan L. Steffens, Conor A. Nixon, Keeyoon Sung, Patrick G.J. Irwin, Nicholas A. Lombardo, and Eric Pereira
Figure caption: The Δχ2 curve for T3 data using the Krasnopolsky n-butane profile.
Paper: New Constraints on Titan’s Stratospheric n-Butane Abundance
Authors: Brendan L. Steffens, Conor A. Nixon, Keeyoon Sung, Patrick G.J. Irwin, Nicholas A. Lombardo, and Eric Pereira
Figure caption: The Δχ2 curve for T35 data using the Krasnopolsky n-butane profile.
Paper: Mars Climate Sounder Observations of Gravity-wave Activity throughout Mars’s Lower Atmosphere
Authors: Nicholas G. Heavens, Alexey Pankine, J. Michael Battalio, Corwin Wright, David M. Kass, Armin Kleinböhl, Sylvain Piqueux, and John T. Schofield
Figure caption: Comparison of the vertical weighting functions for the MRO-MCS A1–A3 channels and nadir geometry for the three input atmospheres, as labeled. The estimated surface contributions are marked with plus signs at 0 km altitude in each panel. The weighting functions have been plotted over a more limited vertical range than calculated to emphasize the altitudes at which they peak. Here A3Kl10 refers to the nadir weighting function for A3 calculated by Kleinböhl et al. (2010).
Paper: Mars Climate Sounder Observations of Gravity-wave Activity throughout Mars’s Lower Atmosphere
Authors: Nicholas G. Heavens, Alexey Pankine, J. Michael Battalio, Corwin Wright, David M. Kass, Armin Kleinböhl, Sylvain Piqueux, and John T. Schofield
Figure caption: Comparison of the vertical weighting functions for the MRO-MCS A1–A3 channels and off-nadir geometry for detectors 1 and 21 for the three input atmospheres, as labeled. The estimated surface contributions are marked with plus signs at 0 km altitude in each panel. The weighting functions have been plotted over a more limited vertical range than calculated to emphasize the altitudes at which they peak. Here ON_21_Kl10 refers to the off-nadir weighting function for detector 21 of the A3 channel (assuming an observation of 9° below the limb) calculated by Kleinböhl et al. (2010), which was obtained from A. Kleinböhl.
Paper: Mars Climate Sounder Observations of Gravity-wave Activity throughout Mars’s Lower Atmosphere
Authors: Nicholas G. Heavens, Alexey Pankine, J. Michael Battalio, Corwin Wright, David M. Kass, Armin Kleinböhl, Sylvain Piqueux, and John T. Schofield
Figure caption: Comparison of the horizontal weighting functions for the MRO-MCS A1–A3 channels and off-nadir geometry for detectors 1, 11, and 21 for the three input atmospheres, as labeled. The weighting functions have been plotted so that they are relative to the intersection point of the optical path of detector 11 (the central detector) with the surface.
Paper: Mars Climate Sounder Observations of Gravity-wave Activity throughout Mars’s Lower Atmosphere
Authors: Nicholas G. Heavens, Alexey Pankine, J. Michael Battalio, Corwin Wright, David M. Kass, Armin Kleinböhl, Sylvain Piqueux, and John T. Schofield
Figure caption: Two-dimensional weighting functions (km−2) for the MRO-MCS A3 channel and off-nadir geometry for detectors 21, 11, and 1 for the COSPAR northern hemisphere atmosphere, as labeled. The weighting functions have been plotted so that they are relative to the intersection point of the optical path of detector 11 (the central detector of the line of detectors in a channel) with the surface. Intersection points with the surface for each of the plotted detectors are indicated with white markers at 0 km altitude.
Paper: Mars Climate Sounder Observations of Gravity-wave Activity throughout Mars’s Lower Atmosphere
Authors: Nicholas G. Heavens, Alexey Pankine, J. Michael Battalio, Corwin Wright, David M. Kass, Armin Kleinböhl, Sylvain Piqueux, and John T. Schofield
Figure caption: Comparison of the estimated visibility to GW (%) with the given horizontal and vertical wavelengths of the MRO-MCS A1–A3 channels and nadir geometry for the three input atmospheres, as labeled.
Paper: Mars Climate Sounder Observations of Gravity-wave Activity throughout Mars’s Lower Atmosphere
Authors: Nicholas G. Heavens, Alexey Pankine, J. Michael Battalio, Corwin Wright, David M. Kass, Armin Kleinböhl, Sylvain Piqueux, and John T. Schofield
Figure caption: Comparison of the estimated visibility to GW (%) with the given horizontal and vertical wavelengths of the MRO-MCS A1–A3 channels and off-nadir geometry for the three input atmospheres, as labeled.
Paper: Mars Climate Sounder Observations of Gravity-wave Activity throughout Mars’s Lower Atmosphere
Authors: Nicholas G. Heavens, Alexey Pankine, J. Michael Battalio, Corwin Wright, David M. Kass, Armin Kleinböhl, Sylvain Piqueux, and John T. Schofield
Figure caption: Number of analyzed nadir and off-nadir observations, binned by 30° of Ls, and nightside vs. dayside, as labeled. The titles report the total number of observations analyzed for the A1–A3 survey. The red bars indicate the total number of observations for the A1–A3 survey, the blue horizontal lines indicate the number of observations available for the survey with B1 included, and the green horizontal lines indicate the number of observations for the A1–A3 survey where the maximum surface elevation for any detector in A3 is less than 12 km (the numbers in the other channels are similar).
Paper: Mars Climate Sounder Observations of Gravity-wave Activity throughout Mars’s Lower Atmosphere
Authors: Nicholas G. Heavens, Alexey Pankine, J. Michael Battalio, Corwin Wright, David M. Kass, Armin Kleinböhl, Sylvain Piqueux, and John T. Schofield
Figure caption: The log10 of the estimated surface roughness (m2) labeled with important geographic features mentioned the text. The scale is saturated at 4 and 7 log units to emphasize the roughest features on Mars. Abbreviations OLY (Olympus Mons), FF (Fortuna Fossae), and SCH (Schiaparelli Crater) are used to label smaller-scale features. The rectangular box marks a region of interest plotted in Figures 14–16.
Paper: Mars Climate Sounder Observations of Gravity-wave Activity throughout Mars’s Lower Atmosphere
Authors: Nicholas G. Heavens, Alexey Pankine, J. Michael Battalio, Corwin Wright, David M. Kass, Armin Kleinböhl, Sylvain Piqueux, and John T. Schofield
Figure caption: Mean spatial distribution of GW activity viewed from nadir observations during Ls = 120°–150° of MY 28 averaged at 5° resolution expressed as ﹩{\mathrm{log}}_{10}\hat{{{\rm{\Omega }}}_{\mathrm{GW}}}﹩ (K2 K−2) for the channel and time of day labeled. White space indicates that no data are available in the averaging bin. The lower end of the plotting color scale is saturated at 10−6 K2 K−2, the approximate uncertainty in the planet’s coldest areas (the southern polar cap).