adsabs/AstroCLIMB huggingface dataset:
Paper: Kronoseismology. VI. Reading the Recent History of Saturn’s Gravity Field in Its Rings
Authors: M.M. Hedman, P.D. Nicholson, M. El Moutamid, and S. Smotherman
Figure caption: An example of using wavelet transforms to document recent ring history. The top left panel of this image shows three profiles of the density wave generated in the Cassini Division by the 7:5 resonances with Janus and Epimetheus. Note that the structure of this wave changes over time due to the moons’ orbital swaps every four years. The bottom three panels on the left show wavelet transforms of these three profiles, giving the strength of the periodic signals as functions of radius and wavenumber. Overlaid on these plots are horizontal lines corresponding to the times when the moons undergo an orbital swap. Note the changes in the slopes and locations of the wave signals at these times. The lower right three panels show wavelet transforms that have been adjusted to remove the outward propagation of the wave patterns, assuming a surface mass density of 11 g cm−2. These plots also include overlaid vertical lines marking the positions of the resonances with the two moons as functions of time. The top right panel shows the normalized average signal strength in the indicated time range for each of the below transforms, showing the consistent relative strength of the signals from the two moons.
Paper: Kronoseismology. VI. Reading the Recent History of Saturn’s Gravity Field in Its Rings
Authors: M.M. Hedman, P.D. Nicholson, M. El Moutamid, and S. Smotherman
Figure caption: Plots of the normalized wavelet amplitudes Aw for waves generated in the year 2000 as a function of the observed position at the three observation epochs. Note that since all three profiles correspond to a fixed absolute initiation time, each profile is for a different wavenumber value in the wavelet. The signal peaks move to larger radii over time, consistent with the trends observed in Figure 1.
Paper: Kronoseismology. VI. Reading the Recent History of Saturn’s Gravity Field in Its Rings
Authors: M.M. Hedman, P.D. Nicholson, M. El Moutamid, and S. Smotherman
Figure caption: Estimates of the ring’s surface mass density derived from the observed group velocities of the waves. The colored diamonds are the results of this analysis, while the plus signs are based on standard density wave analyses (Baillié et al. 2011; Hedman & Nicholson 2013).
Paper: Kronoseismology. VI. Reading the Recent History of Saturn’s Gravity Field in Its Rings
Authors: M.M. Hedman, P.D. Nicholson, M. El Moutamid, and S. Smotherman
Figure caption: Plots of the peak wavelet amplitude Aw and inferred gravitational potential perturbation amplitude ﹩{{\rm{\Phi }}}_{3}^{{\prime} }﹩ as a function of δt for three m = 3 satellite waves for the three observation epochs. For the Mimas 6:2 wave, the top panel shows the measured peak wavelet amplitudes Aw from the three observation epochs, along with the average of the three profiles. The second panel shows the estimated gravitational potential perturbation amplitudes ﹩{{\rm{\Phi }}}_{3}^{{\prime} }﹩ based on this template. The other panels show the observed peak wavelet amplitudes and derived potential perturbation amplitudes for the weaker Pandora and Prometheus 4:2 waves.
Paper: Kronoseismology. VI. Reading the Recent History of Saturn’s Gravity Field in Its Rings
Authors: M.M. Hedman, P.D. Nicholson, M. El Moutamid, and S. Smotherman
Figure caption: The results of the wavelet analysis of the Mimas 6:2 and Pandora 4:2 waves. The top row shows the power ratios ﹩{{ \mathcal R }}^{\max }﹩ as functions of initial pattern speed and formation time, while the bottom row shows the estimated potential perturbations ﹩{{\rm{\Phi }}}_{m}^{{\prime} }﹩. Each of the right three panels shows the arrays derived from one of the Cassini epochs, while the left panels show the peak values of ﹩{{ \mathcal R }}^{\max }﹩ and ﹩{{\rm{\Phi }}}_{m}^{{\prime} }﹩ as functions of formation time. Note that the gray dotted lines in the left panels correspond to the grayscale levels in the corresponding images. Also, data are only displayed for times where the normalization curve is at least 0.25 its peak value. In this case, the two vertical bands in the images correspond to the perturbations from the Pandora 4:2 resonance at 762.°8 day−1 and the Mimas 6:2 resonance around 762.°9 day−1. Note that the amplitudes of these signals are roughly constant around 30 cm2 s−2, and the pattern speeds do not change much with time, consistent with standard satellite resonances.
Paper: Kronoseismology. VI. Reading the Recent History of Saturn’s Gravity Field in Its Rings
Authors: M.M. Hedman, P.D. Nicholson, M. El Moutamid, and S. Smotherman
Figure caption: The results of the wavelet analysis of the Prometheus 4:2 wave in the same format as Figure 15. In this case, the vertical bands in the wavelet maps correspond to the signal from the Prometheus 4:2 resonance at 782.°1 day−1. Note that the amplitude of this signal is roughly constant around 20 cm2 s−2, and the pattern speeds do not change much with time, consistent with a standard satellite resonance.
Paper: Kronoseismology. VI. Reading the Recent History of Saturn’s Gravity Field in Its Rings
Authors: M.M. Hedman, P.D. Nicholson, M. El Moutamid, and S. Smotherman
Figure caption: An overview of the m = 3 and m = −1 waves in the middle C ring. The top panel shows an optical depth profile of the rings, while the lower panels show the peak values of the potential perturbation ﹩{{\rm{\Phi }}}_{m}^{{\prime} }﹩ and power ratio ﹩{{ \mathcal R }}^{\max }﹩ for elapsed times between 7 and 40 yr as functions of the corresponding initial pattern speed of the waves (the plotted curves are the averages of the data from the three epochs, since the differences between the epochs were generally small). The gray shaded band in these plots corresponds to the W84.64 wave, which contaminates the ﹩{{\rm{\Phi }}}_{m}^{{\prime} }﹩ profiles.
Paper: Kronoseismology. VI. Reading the Recent History of Saturn’s Gravity Field in Its Rings
Authors: M.M. Hedman, P.D. Nicholson, M. El Moutamid, and S. Smotherman
Figure caption: The results of the wavelet analysis of the region around wave W84.86 in the same format as Figure 15. For all three epochs, there is a clear peak in the perturbation amplitude at a pattern speed of 833.°0 day−1 that started sometime in the 1980s, reached a peak value of around 70 cm2 s−2 in 1999, and then dissipated around 2003.
Paper: Kronoseismology. VI. Reading the Recent History of Saturn’s Gravity Field in Its Rings
Authors: M.M. Hedman, P.D. Nicholson, M. El Moutamid, and S. Smotherman
Figure caption: The results of the wavelet analysis of the region around wave W84.82 in the same format as Figure 15. The strongest signals here are around 833.°5 day−1. For all three epochs, we see a signal in the perturbation amplitude that first appeared in the late 1990s, before reaching a peak of around 120 cm2 s−2 in 1999. This signal faded significantly in the early 2000s, but the data from Epochs 2 and 3 show that it reappeared a few years later, probably peaking again in 2008. In addition to these particularly strong signals, there is also a series of weaker signals between 833.°7 and 834.°1 day−1 that appear to have been most active in the 1990s, and other signals around 833.°7 day−1 that were most active in the 1980s and early 2000s.
Paper: Kronoseismology. VI. Reading the Recent History of Saturn’s Gravity Field in Its Rings
Authors: M.M. Hedman, P.D. Nicholson, M. El Moutamid, and S. Smotherman
Figure caption: The results of the wavelet analysis of the region around the m = 3 wave W86.40 in the same format as Figure 15. In this case, there appears to be a single perturbation that has existed since 1970 and whose pattern speed has steadily increased over four decades from 810° to 810.°5 day−1. Note that the amplitude of the perturbation has changed substantially over time, decreasing to a minimum of around 30 cm2 s−2 around 1990, rising to a value of around 50 cm2 s−2 around 1994, then falling briefly again before reaching a maximum of around 100 cm2 s−2 in the mid-2000s.
Paper: Kronoseismology. VI. Reading the Recent History of Saturn’s Gravity Field in Its Rings
Authors: M.M. Hedman, P.D. Nicholson, M. El Moutamid, and S. Smotherman
Figure caption: The results of the wavelet analysis of the region around the m = −1 wave W85.67 in the same format as Figure 15. These data show evidence of a continuous disturbance whose pattern speed has steadily changed between 2430° and 2431.°5 day−1 between 1970 and 2010. Note that the amplitudes of the perturbations derived from the different epochs are more discordant than those shown in Figure 20, indicating that the normalization model may not be ideal here. Even so, one can see local minima in the perturbation amplitudes around 1990 and 1997 that are very similar to those seen in Figure 20, indicating that these waves may share a common origin.
Paper: Kronoseismology. VI. Reading the Recent History of Saturn’s Gravity Field in Its Rings
Authors: M.M. Hedman, P.D. Nicholson, M. El Moutamid, and S. Smotherman
Figure caption: The results of the wavelet analysis of an extended region around the m = −1 wave W85.67 in the same format as Figure 15, except that it includes data from the Voyager RSS occultation, and the amplitudes are normalized using a template scaled by 80% in elapsed time. With this normalization, the amplitude of the perturbation appears to have declined over the past four decades. Also, the Voyager data allows us to extend the time evolution of this perturbation back to 1960. Also note that weaker signals can be seen between 2427° and 2430° day−1 in the 1980s and 1990s.
Paper: Kronoseismology. VI. Reading the Recent History of Saturn’s Gravity Field in Its Rings
Authors: M.M. Hedman, P.D. Nicholson, M. El Moutamid, and S. Smotherman
Figure caption: The results of the wavelet analysis applied to the region around W86.58 and W86.59 in the same format as Figure 15. In this case, the more prominent and persistent signal is around 807.°6 day−1, which may have subcomponents and variations over time. In addition, weaker and more transient signals can be seen in the 1990s through early 2000s between 807.°9 and 808.°4 day−1.
Paper: Kronoseismology. VI. Reading the Recent History of Saturn’s Gravity Field in Its Rings
Authors: M.M. Hedman, P.D. Nicholson, M. El Moutamid, and S. Smotherman
Figure caption: The results of the wavelet analysis on the perturbations between 816.°5 and 817.°3 day−1 in the same format as Figure 15. In this case, there is not much visible in the perturbation amplitude, but patchy signals can be seen in the power ratio.
Paper: Kronoseismology. VI. Reading the Recent History of Saturn’s Gravity Field in Its Rings
Authors: M.M. Hedman, P.D. Nicholson, M. El Moutamid, and S. Smotherman
Figure caption: The results of the wavelet analysis of the waves W86.81 and W86.79 in the same format as Figure 15. In this region, all three epochs contain a signal at around 804.°6 day−1 with a relatively constant pattern speed, which we identify with the wave W86.81. Another, weaker signal is seen at 804.°8 day−1, which corresponds to the wave W86.79.
Paper: Kronoseismology. VI. Reading the Recent History of Saturn’s Gravity Field in Its Rings
Authors: M.M. Hedman, P.D. Nicholson, M. El Moutamid, and S. Smotherman
Figure caption: The results of the wavelet analysis of the wave W86.25 in the same format as Figure 15. This region contains a wave signal with a pattern speed of around 812.°6 day−1 during all three epochs.
Paper: Kronoseismology. VI. Reading the Recent History of Saturn’s Gravity Field in Its Rings
Authors: M.M. Hedman, P.D. Nicholson, M. El Moutamid, and S. Smotherman
Figure caption: The results of the wavelet analysis of the wave W86.18 in the same format as Figure 15. This region contains a weak wave signal with a pattern speed of around 813.°5 day−1, which is most obvious in the Epoch 2 data.
Paper: Kronoseismology. VI. Reading the Recent History of Saturn’s Gravity Field in Its Rings
Authors: M.M. Hedman, P.D. Nicholson, M. El Moutamid, and S. Smotherman
Figure caption: The results of the wavelet analysis of the wave W84.26 in the same format as Figure 15. This region contains a wave signal at 842° day−1. Note that unlike the other signals outside the plateaux, the signal is consistently found only after 2000.
Paper: Kronoseismology. VI. Reading the Recent History of Saturn’s Gravity Field in Its Rings
Authors: M.M. Hedman, P.D. Nicholson, M. El Moutamid, and S. Smotherman
Figure caption: A summary of the history of the anomalies in Saturn’s gravitational field, compared with notable aspects of Saturn’s atmosphere and seasons. The top panel shows the rotation rates of Saturn’s winds, using data from García-Melendo et al. (2011). The bottom panel shows a grayscale map of the average perturbations in Saturn’s gravitational field as a function of pattern speed and formation time. For the sake of clarity, signals are only shown where the average power ratio is above a time-dependent threshold (0.35 before 2004, 0.5 between 2004 and 2008, and 0.7 between 2008 and 2011). The vertical dashed line is the estimate of Saturn’s interior rotation rate by Mankovich et al. (2019), while the diamonds mark the rotation rates of notable Saturn storms known as “Great White Spots” (Sánchez-Lavega et al. 2018). The horizontal lines mark Saturn’s solstices and equinoxes.
Paper: Detectability of Chlorofluorocarbons in the Atmospheres of Habitable M-dwarf Planets
Authors: Jacob Haqq-Misra, Ravi Kopparapu, Thomas J. Fauchez, Adam Frank, Jason T. Wright, and Manasvi Lingam
Figure caption: The absorption cross sections for CFC-11 (left) and CFC-12 (right) show the strongest features within a 8–14 μm window (dashed red lines) with one major peak between 8 and 10 μm and a second between 10 and 14 μm. Cross sections are from the HITRAN database with 0.003 μm resolution at 300 K (Sharpe et al. 2004; Harrison 2015; Gordon et al. 2021).
Paper: Detectability of Chlorofluorocarbons in the Atmospheres of Habitable M-dwarf Planets
Authors: Jacob Haqq-Misra, Ravi Kopparapu, Thomas J. Fauchez, Adam Frank, Jason T. Wright, and Manasvi Lingam
Figure caption: Examples of other atmospheric gases on Earth that have overlapping absorption features with CFC-11 and CFC-12 within the 8–14 μm window. Cross sections are from the HITRAN database with 0.003 μm resolution at 300 K (Sharpe et al. 2004; Harrison 2015; Gordon et al. 2021, 2022).
Paper: Detectability of Chlorofluorocarbons in the Atmospheres of Habitable M-dwarf Planets
Authors: Jacob Haqq-Misra, Ravi Kopparapu, Thomas J. Fauchez, Adam Frank, Jason T. Wright, and Manasvi Lingam
Figure caption: Historical measurements of CFC-11 (left) and CFC-12 (right) show a sharp decline that correlates with the adoption of the Montreal Protocol (solid curves). A linear projection shows that CFC abundances of twice as high or greater than today could have been possible if this treaty had not been effective (dashed lines). CFC data are from the National Oceanic and Atmospheric Administration (NOAA) Global Monitoring Laboratory.
Paper: Detectability of Chlorofluorocarbons in the Atmospheres of Habitable M-dwarf Planets
Authors: Jacob Haqq-Misra, Ravi Kopparapu, Thomas J. Fauchez, Adam Frank, Jason T. Wright, and Manasvi Lingam
Figure caption: Transit spectra for TRAPPIST-1e (left) and an Earth-like planet around a 3300 K host star (right), showing the spectral features of CFC-11 and CFC-12 for the 0×, 1×, 2×, and 5× scenarios. The features are more pronounced around Trappist-1 because of the smaller size of the star. The planets are in the respective habitable zones of their host stars, and the 3300K system is kept at a distance of 5 pc from the solar system (TRAPPIST-1 is at a distance of 12.4 pc).
Paper: Detectability of Chlorofluorocarbons in the Atmospheres of Habitable M-dwarf Planets
Authors: Jacob Haqq-Misra, Ravi Kopparapu, Thomas J. Fauchez, Adam Frank, Jason T. Wright, and Manasvi Lingam
Figure caption: In-transit time (i.e., no overheads) S/N estimates as a function of CFC concentration for TRAPPIST-1e (left) and a planet around a 3300K star (right). The left panel shows JWST MIRI-LRS simulated observations of TRAPPIST-1e at observing times ranging from 1 to 1200 hr with a lower limit of the noise floor of 10 ppm and a higher limit of 50 ppm. With an optimistic 10 ppm noise floor, current Earth-level CFCs (1×) could be detectable with an S/N ∼ 3 in about ∼100 hr of JWST MIRI-LRS in-transit observations. Past Earth-level (2×) CFCs could be detectable on TRAPPIST-1e with an S/N ∼ 5 for the same amount of time. However, a very conservative 50 ppm noise floor would render even a 5× present Earth-level CFC abundance challenging to detect. The right panel shows simulated observations with Origins for a planet around a 3300 K star, with a noise floor of 5 ppm. Despite the lower noise floor, detection of CFCs around this star would be difficult due to the larger size of the star.
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 extracts and residuals in C/2014 Q2 (Lovejoy) in setting KL2 order 22. The spectrum is co-added over a 3 spectral × 9 spatial pixel extract (0.″432 × 1.″71) centered on the peak of the gas emission. The solid blue trace at the top of the panel is the comet spectrum with the best-fit synthetic atmospheric model superimposed (dashed red trace). Molecular lines from the comet are seen as emissions in the comet spectrum above the atmospheric model. The Solid blue trace on the bottom of the panel is the continuum-subtracted spectral residuals. The dotted black curves superimposed on the comet residuals represent the estimated ±1σ channel-by-channel photon noise envelope.
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 KL2 order 25, and (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. The dashed red curves superimposed on the comet residuals represent the estimated ±1σ channel-by-channel photon noise envelope. The 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. Color traces below this are the best-fit fluorescence models at the derived or assumed rotational temperatures for each individual molecule. Zoomed-in regions of these spectra are given in Figure A4.
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 2, but for (a) February 2, setting KL1 order 23, and (b) February 2, setting KL3 order 23.
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 2, but for (a) February 2, setting KL3 order 21, and (b) February 2, setting M1 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: Spatial profiles for volatiles (a–c) H2O, (d–f) CH3OH, (g–i) C2H6, (j–l) CH4, (m–o) NH3, and co-measured dust along the slit at different times (settings, as indicated atop each column) on February 2 in 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). For all panels in Figures 5–7, the sunward-facing hemisphere is to the left.
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 5, but for volatiles (a–c) H2O, (d–e) HCN, (f) CO, (g–h) C2H2, (i–j) H2CO, and co-measured dust along the slit at different times (settings) on February 2.
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 5, but for volatiles (a–c) H2O, (d–e) CH3OH, (f) CO, (g–h) C2H6, (i–j) CH4, (k) HCN, (l) H2CO, and co-measured dust along the slit at different times (settings) on February 3 in C/2014 Q2 (Lovejoy). In the left two columns, the slit was in rotator mode, so the position angle with respect to the Sun varied in the clockwise direction with time. In the right column, the slit was in stationary mode and the Sun position remained fixed relative to the slit.
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 volatile spatial profiles compared with the co-measured dust for (a) February 2 and (b) February 3. Differences are measured in spatial pixels with 1 pixel ∼ 110 km projected distance at the comet.