adsabs/AstroCLIMB huggingface dataset:
Paper: Ammonia Abundance Derived from Juno MWR and VLA Observations of Jupiter
Authors: Chris Moeckel, Imke de Pater, David DeBoer
Figure caption: Comparison of the atmospheric structure at the locations indicated in Figure 9. The two models developed for this work agree well on the overall structure of the atmosphere despite different modeling frameworks. The biggest difference in the ammonia distribution between our results and VLA results (dashed lines; de Pater et al. 2016, 2019b) is that we add more information about the fine-scale vertical structure. Compared to the PJ1 results (Li et al. 2017), we find no strong evidence for the inversion at midlatitudes.
Paper: Ammonia Abundance Derived from Juno MWR and VLA Observations of Jupiter
Authors: Chris Moeckel, Imke de Pater, David DeBoer
Figure caption: Forward-modeling results based on the best-fit distribution of ammonia trace gases compared to the Juno observations, plotted against latitude. The Juno nadir brightness temperatures are the solid black lines, with their uncertainties represented by the shading. The red and blue lines correspond to temperatures based on the ammonia distributions as shown in Figure 9. The shading of the red and blue lines indicates the sensitivity of the results to the uncertainties (n = 1, 10). The green line is the forward model based on the VLA data (de Pater et al. 2019b). Overall, our forward models fit the brightness temperature well within the uncertainties.
Paper: Ammonia Abundance Derived from Juno MWR and VLA Observations of Jupiter
Authors: Chris Moeckel, Imke de Pater, David DeBoer
Figure caption: Compilation of the relevant temperature profiles that we assume for our retrieval. The temperature profiles are anchored at the 1-bar level to the radio occultation measurements of Voyager (Lindal et al. 1981) and to the Galileo probe measurements (Seiff et al. 1996). Above the 0.7-bar level we use profiles obtained via infrared measurements (Fletcher et al. 2009). Below the 1.0-bar level we use the expected wet and dry adiabatic lapse rate until the two profiles merge at the height of the water cloud. The little cutout shows the anchor points at the 1-bar level, with the corresponding uncertainties. (The data used to create this figure are available.)
Paper: Ammonia Abundance Derived from Juno MWR and VLA Observations of Jupiter
Authors: Chris Moeckel, Imke de Pater, David DeBoer
Figure caption: Globally averaged [−45°, 45°] ammonia profile as a function of depth. The red line corresponds to our thermochemical equilibrium model, and the blue line corresponds to our stochastic model, with the shading corresponding to n = 1, 10. The blue dashed line is based on the results of Li et al. (2017), and the green line is based on the VLA data from de Pater et al. (2019b). The radio attenuation (Folkner et al. 1998) and Galileo Probe Mass Spectrometer (GPMS; Wong et al. 2004) are superimposed. (The data used to create this figure are available.)
Paper: Ammonia Abundance Derived from Juno MWR and VLA Observations of Jupiter
Authors: Chris Moeckel, Imke de Pater, David DeBoer
Figure caption: Same as Figure 11, but for the limb-darkening coefficient. While we can fit the overall structure of the atmosphere within the uncertainties, the solutions for Channel 2 all result in less limb darkening compared to the observations. The solution closest to the observations (upper end of the shaded area) corresponds to the retrieval that creates a larger mismatch for the brightness temperature. The results that best fit the brightness temperature (10σ) have the largest misfit for the Channel 2 limb darkening, and the 1σ results fit the limb darkening best.
Paper: Ammonia Abundance Derived from Juno MWR and VLA Observations of Jupiter
Authors: Chris Moeckel, Imke de Pater, David DeBoer
Figure caption: Nadir brightness temperature for the six channels between −60° and 60°, where the thick lines indicate the orbit-averaged values and the dashed thin lines correspond to the individual PJs. The dotted line represents the orbit-averaged value based on a deconvolution algorithm (Oyafuso et al. 2020) and shows a good agreement between the two methods, validating both our approaches. (The data used to create this figure are available.)
Paper: Ammonia Abundance Derived from Juno MWR and VLA Observations of Jupiter
Authors: Chris Moeckel, Imke de Pater, David DeBoer
Figure caption: Same as Figure 4, but for the limb-darkening parameter. (The data used to create this figure are available.)
Paper: Ammonia Abundance Derived from Juno MWR and VLA Observations of Jupiter
Authors: Chris Moeckel, Imke de Pater, David DeBoer
Figure caption: Testing the robustness of the vertical structure against various assumptions in the retrieval compared to various other retrievals (different line styles). Model 1 and Model 2 are slices through Figure 16, the ammonia abundance map based on the joint retrieval of the combined VLA and Juno MWR data set. In panel (a) we retrieve the atmospheric structure for a wet-adiabatic temperature profile (see Figure 6) and show a large increase of the ammonia abundance (note the different scale for this panel). We compare this to the vertical profile of the nominal dry adiabat in panel (b). Panel (c) relaxes the assumption that the atmosphere approaches a globally well-mixed ammonia abundance, and instead we retrieve the deep ammonia abundance simultaneously. Panel (d) shows the effect of including absorption by cloud particles.
Paper: Ammonia Abundance Derived from Juno MWR and VLA Observations of Jupiter
Authors: Chris Moeckel, Imke de Pater, David DeBoer
Figure caption: Testing for the inversion signal at midlatitudes as seen by Li et al. (2017), by retrieving an atmosphere based on both VLA and Juno data. We test the effect of vertical regularization on the midlatitude structure to show the confidence in the retrieved midlatitude structure. The panels correspond to no (panel (a)), mild (panel (b)), and moderate vertical regularization (panel (d)). The various line styles correspond to the various retrievals, with the dotted–dashed line and the shading indicating the 0.16 and 0.84 quantiles of the MCMC results. Panel (c) uses mild vertical regularization but reduces the uncertainty fidelity to n = 1. Regardless of chosen regularization, we cannot reproduce the magnitude of the inversion as seen by the dotted line.
Paper: Ammonia Abundance Derived from Juno MWR and VLA Observations of Jupiter
Authors: Chris Moeckel, Imke de Pater, David DeBoer
Figure caption: Corner plots for the nominal model (panel (b) in Figure 23), where we show the average between the eight mixing gradients in the atmosphere between 100 and 1 bars. The combined VLA and Juno retrieval indicates a lower humidity in the EZ compared to the pure Juno retrieval (see Figure 18), but the mixing gradient clearly shows a well-defined increase of ammonia abundance with altitude.
Paper: Ammonia Abundance Derived from Juno MWR and VLA Observations of Jupiter
Authors: Chris Moeckel, Imke de Pater, David DeBoer
Figure caption: Relationship between the beam-convolved emission angle and boresight emission angle. The different colors indicate the integration region in units of the HPBW. Farther away from the beam center, the beam sensitivity is dropping rapidly, and the contribution to the averaging becomes small. Therefore, the results converge for sufficiently large integration regions. Our final results are based on 2.5 HPBW, which contains 99% of the emission. This example is for PJ1—Channel 2 observations just before closest approach to the planet.
Paper: Ammonia Abundance Derived from Juno MWR and VLA Observations of Jupiter
Authors: Chris Moeckel, Imke de Pater, David DeBoer
Figure caption: Corner plots for the equatorial inversion corresponding to the profiles shown in Figure 23. In this retrieval we relaxed the assumption that the ammonia is well mixed and allow the deep ammonia to vary in the fit.
Paper: Ammonia Abundance Derived from Juno MWR and VLA Observations of Jupiter
Authors: Chris Moeckel, Imke de Pater, David DeBoer
Figure caption: Same as Figure 2, but for a latitude where the synchrotron contribution is noticeable. Note that there are two branches in Channels 1 and 2 that have a large difference in the temperature for the same emission angle. The increase in temperature is due to the synchrotron leaking in through the sidelobes. Our spatial restriction can handle the synchrotron contribution well, ignoring the upper, contaminated branch of the observations.
Paper: Ammonia Abundance Derived from Juno MWR and VLA Observations of Jupiter
Authors: Chris Moeckel, Imke de Pater, David DeBoer
Figure caption: Corner plots for the equatorial inversion, including the effect of radio absorption by cloud particles. The mixing gradients 1-H indicates mixing above 6 bars, and 2-H corresponds to mixing below the 6 bar level.
Paper: Ammonia Abundance Derived from Juno MWR and VLA Observations of Jupiter
Authors: Chris Moeckel, Imke de Pater, David DeBoer
Figure caption: Same as Figure 27, but for Channel 5.
Paper: The Dynamical Consequences of a Super-Earth in the Solar System
Authors: Stephen R. Kane
Figure caption: Semimajor axis evolution, expressed as a fractional change from the initial value, of the solar system outer planets (top four panels) for a 107 yr simulation, where the additional planet (bottom panel) has a mass and semimajor axis of 7.0 M ⊕ and 3.79 au, respectively.
Paper: The Dynamical Consequences of a Super-Earth in the Solar System
Authors: Stephen R. Kane
Figure caption: Intensity plot showing the ratio of eccentricity variation amplitude to those from the baseline solar system model, as a function of added planet mass and semimajor axis. Results are shown for Mercury (top panel) and Venus (bottom panel).
Paper: The Dynamical Consequences of a Super-Earth in the Solar System
Authors: Stephen R. Kane
Figure caption: Intensity plot showing the ratio of eccentricity variation amplitude to those from the baseline solar system model, as a function of added planet mass and semimajor axis. Results are shown for Earth (top panel) and Mars (bottom panel).
Paper: The Dynamical Consequences of a Super-Earth in the Solar System
Authors: Stephen R. Kane
Figure caption: Semimajor axis evolution, expressed as a fractional change from the initial value, of the solar system outer planets (top four panels) for a 107 yr simulation, where the additional planet (bottom panel) has a mass and semimajor axis of 7.0 M ⊕ and 3.80 au, respectively.
Paper: The Dynamical Consequences of a Super-Earth in the Solar System
Authors: Stephen R. Kane
Figure caption: Intensity plot showing the ratio of eccentricity variation amplitude to those from the baseline solar system model, as a function of added planet mass and semimajor axis. Results are shown for Jupiter (top panel) and Saturn (bottom panel).
Paper: The Dynamical Consequences of a Super-Earth in the Solar System
Authors: Stephen R. Kane
Figure caption: Intensity plot showing the ratio of eccentricity variation amplitude to those from the baseline solar system model, as a function of added planet mass and semimajor axis. Results are shown for Uranus (top panel) and Neptune (bottom panel).
Paper: The Dynamical Consequences of a Super-Earth in the Solar System
Authors: Stephen R. Kane
Figure caption: Eccentricity evolution of the solar system outer planets (top four panels) for a 107 yr simulation, where the additional planet (bottom panel) has a mass and semimajor axis of 7.0 M ⊕ and 3.80 au, respectively.
Paper: TNO or Comet? The Search for Activity and Characterization of Distant Object 418993 (2009 MS9)
Authors: Erica Bufanda, Karen J. Meech, Jan T. Kleyna, Olivier R. Hainaut, James M. Bauer, Haynes Stephens, Peter Veres, Marco Micheli, Jacqueline V. Keane, Robert Weryk, Richard Wainscoat, Devendra K. Sahu, Bhuwan C. Bhatt
Figure caption: (a) 2009 MS9 colors pre- and post-perihelion in comparison to various SMASS-2 spectral types of other primitive bodies. The spectral reflectivity indicates a surface that is analogous to D-type asteroids. Pre-perihelion 2009 MS9's colors (blue) are bluer in comparison to its colors post-perihelion (black). (Note that the 12/2018 observation refers to the observation taken on 2018 November 30. It is abbreviated to distinguish it from the observation earlier in the month taken 2018 November 10.) (b) 2009 MS9's spectral slope has subtle changes over time that indicate redder colors post-perihelion, when we believe the target to be active. (c) Comparing 2009 MS9's spectral slopes and their error to one another as a function of time suggests that the target is redder when active; however, this result is not statistically significant. The numbers refer to the epoch of 2009 MS9's orbit in which the colors were measured, which is shown in Figure 6.
Paper: TNO or Comet? The Search for Activity and Characterization of Distant Object 418993 (2009 MS9)
Authors: Erica Bufanda, Karen J. Meech, Jan T. Kleyna, Olivier R. Hainaut, James M. Bauer, Haynes Stephens, Peter Veres, Marco Micheli, Jacqueline V. Keane, Robert Weryk, Richard Wainscoat, Devendra K. Sahu, Bhuwan C. Bhatt
Figure caption: Photometric r-band light curve of 2009 MS9 as a function of its orbit assuming CO sublimation for two different activity scenarios. The 0.4 mag variation of 2009 MS9 encloses a range of magnitudes (the gray shaded region represents the nucleus). (a) Modeling CO sublimation pre- and post-perihelion. A baseline FAA of 2.5×10−5 (black line) is needed, an FAA of 4×10−5 (dotted line) post-perihelion to match the photometry. An arbitrary nucleus size of 8 km (gray) is shown. (b) CO sublimation (black line) post-perihelion with an FAA of 5 × 10−6 assuming prior inactivity. The nucleus is 11.5 km (gray) from WISE.
Paper: TNO or Comet? The Search for Activity and Characterization of Distant Object 418993 (2009 MS9)
Authors: Erica Bufanda, Karen J. Meech, Jan T. Kleyna, Olivier R. Hainaut, James M. Bauer, Haynes Stephens, Peter Veres, Marco Micheli, Jacqueline V. Keane, Robert Weryk, Richard Wainscoat, Devendra K. Sahu, Bhuwan C. Bhatt
Figure caption: Process of creating a composite r-band image of 2009 MS9 using 45 images from CFHT obtained on 2011 July 31. (a) One frame with an exposure time of 120 s, where 2009 MS9 is highlighted by red circle. (b) Sum composite image, where 2009 MS9 is seen as trailed. (c) Star template from a median composite image for the night of 2011 July 31, which is used for stellar radial profiles and subtraction. (d) Average composite image shifted by the KBO apparent rate of motion or 2009 MS9's astrometric position per night.
Paper: TNO or Comet? The Search for Activity and Characterization of Distant Object 418993 (2009 MS9)
Authors: Erica Bufanda, Karen J. Meech, Jan T. Kleyna, Olivier R. Hainaut, James M. Bauer, Haynes Stephens, Peter Veres, Marco Micheli, Jacqueline V. Keane, Robert Weryk, Richard Wainscoat, Devendra K. Sahu, Bhuwan C. Bhatt
Figure caption: Three sublimation models showing how the light curve changes between volatile species CO and CO2 in comparison to photometry. Top: CO2 model matched to the brightnesses of the last data points of the target. Here the sublimation light curve does not match near-perihelion observations. Middle: CO2 model matched to the initial photometry of the target. Observations after TA = 50 do not match the sublimation model. Bottom: CO sublimation matched to the photometry. This provides the best fit up to TA = 65; however, past this is too bright for observations.
Paper: TNO or Comet? The Search for Activity and Characterization of Distant Object 418993 (2009 MS9)
Authors: Erica Bufanda, Karen J. Meech, Jan T. Kleyna, Olivier R. Hainaut, James M. Bauer, Haynes Stephens, Peter Veres, Marco Micheli, Jacqueline V. Keane, Robert Weryk, Richard Wainscoat, Devendra K. Sahu, Bhuwan C. Bhatt
Figure caption: The FP modeling of the dust for 2009 MS9 for different epochs. Each panel is labeled with the viewing geometry quality (bad, fair, or good). Bad quality represents when the viewing geometry is far from the plane of the orbit. Good quality represents when the viewing geometry is close to the orbital plane. For the latter, dust is more likely to be detected because the synchrones and syndynes are concentrated and overlap in a smaller area.
Paper: TNO or Comet? The Search for Activity and Characterization of Distant Object 418993 (2009 MS9)
Authors: Erica Bufanda, Karen J. Meech, Jan T. Kleyna, Olivier R. Hainaut, James M. Bauer, Haynes Stephens, Peter Veres, Marco Micheli, Jacqueline V. Keane, Robert Weryk, Richard Wainscoat, Devendra K. Sahu, Bhuwan C. Bhatt
Figure caption: Temperature profile as a function of depth for different positions (color coded in the main panel and matched to the stars of the same color scheme in the inset panel) along the orbit of comet 2009 MS9. As 2009 MS9 gets closer to the Sun, the temperature at its surface increases, and this propagates to the interior following 1D heat conduction. We map the temperature profile of the near surface of the comet by integrating from 1880, where the object is too far (130 au) to start CO sublimation, up until perihelion in 2013 with integration steps of 1 day. At the object’s perihelion is where we predict the onset of activity, and at this time, the depth with the temperature corresponding to peak CO sublimation (25 K) is ≈3.9 m from the surface.
Paper: TNO or Comet? The Search for Activity and Characterization of Distant Object 418993 (2009 MS9)
Authors: Erica Bufanda, Karen J. Meech, Jan T. Kleyna, Olivier R. Hainaut, James M. Bauer, Haynes Stephens, Peter Veres, Marco Micheli, Jacqueline V. Keane, Robert Weryk, Richard Wainscoat, Devendra K. Sahu, Bhuwan C. Bhatt
Figure caption: For each composite image, we bin the photon flux as a function of radius and calculate the average stellar radial profile of 2009 MS9 (black) vs. the average star profile (blue). From these profiles, we can calculate the limits on dust production (red).
Paper: TNO or Comet? The Search for Activity and Characterization of Distant Object 418993 (2009 MS9)
Authors: Erica Bufanda, Karen J. Meech, Jan T. Kleyna, Olivier R. Hainaut, James M. Bauer, Haynes Stephens, Peter Veres, Marco Micheli, Jacqueline V. Keane, Robert Weryk, Richard Wainscoat, Devendra K. Sahu, Bhuwan C. Bhatt
Figure caption: Heliocentric light curve of 2009 MS9 shown with data from the MPC, which consists primarily of photometry from various sources, including amateur telescopes. The asymmetry of brightening post-perihelion is suggestive of activity.
Paper: The Dynamical Consequences of a Super-Earth in the Solar System
Authors: Stephen R. Kane
Figure caption: Eccentricity evolution of the solar system outer planets (top four panels) for a 107 yr simulation, where the additional planet (bottom panel) has a mass and semimajor axis of 7.0 M ⊕ and 3.79 au, respectively.
Paper: The Dynamical Consequences of a Super-Earth in the Solar System
Authors: Stephen R. Kane
Figure caption: Top-down view of the solar system planetary orbits (shown as solid lines) out to the orbit of Jupiter. The red shaded region indicates the locations in which a planet in the mass range 1–10 M ⊕ was added to the solar system architecture. The dotted lines show a grid with 1 au resolution; the full figure scale is 12 au along one side.
Paper: The Dynamical Consequences of a Super-Earth in the Solar System
Authors: Stephen R. Kane
Figure caption: Eccentricity evolution of the solar system terrestrial planets (top four panels) for a 107 yr simulation, where the additional planet (bottom panel) has a mass and semimajor axis of 8.0 M ⊕ and 3.70 au, respectively.
Paper: The Dynamical Consequences of a Super-Earth in the Solar System
Authors: Stephen R. Kane
Figure caption: Semimajor axis evolution, expressed as a fractional change from the initial value, of the solar system terrestrial planets (top four panels) for a 107 yr simulation, where the additional planet (bottom panel) has a mass and semimajor axis of 7.0 M ⊕ and 2.00 au, respectively.
Paper: The Dynamical Consequences of a Super-Earth in the Solar System
Authors: Stephen R. Kane
Figure caption: Eccentricity evolution of the solar system terrestrial planets (top four panels) for a 107 yr simulation, where the additional planet (bottom panel) has a mass and semimajor axis of 7.0 M ⊕ and 2.00 au, respectively.
Paper: The Dynamical Consequences of a Super-Earth in the Solar System
Authors: Stephen R. Kane
Figure caption: Semimajor axis evolution, expressed as a fractional change from the initial value, of the solar system terrestrial planets (top four panels) for a 107 yr simulation, where the additional planet (bottom panel) has a mass and semimajor axis of 8.0 M ⊕ and 3.70 au, respectively.
Paper: Approaches for Retrieving Sulfur Species Abundances from Dual X–Ka-band Radio Occultations of Venus with EnVision and VERITAS
Authors: Alex B. Akins, Tatiana M. Bocanegra-Bahamón, Kuo-Nung Wang, Panagiotis Vergados, Chi O. Ao, Sami W. Asmar, Robert A. Preston
Figure caption: Covariance matrices computed for X- and Ka-band atmospheric absorptivity from RO simulations for the set (1) model atmosphere. The corresponding 1σ uncertainties are shown in context bracketing the absorptivity profiles.
Paper: Approaches for Retrieving Sulfur Species Abundances from Dual X–Ka-band Radio Occultations of Venus with EnVision and VERITAS
Authors: Alex B. Akins, Tatiana M. Bocanegra-Bahamón, Kuo-Nung Wang, Panagiotis Vergados, Chi O. Ao, Sami W. Asmar, Robert A. Preston
Figure caption:  X- (left) and Ka- (right) band atmospheric opacity of neutral atmosphere microwave absorbers for an equatorial model atmosphere. The bulk CO2/N2 atmosphere and sulfur species dictate the microwave opacity of the atmosphere, and the contribution of other trace gases is minimal. Shaded regions show 1σ uncertainties associated with opacity models.
Paper: Approaches for Retrieving Sulfur Species Abundances from Dual X–Ka-band Radio Occultations of Venus with EnVision and VERITAS
Authors: Alex B. Akins, Tatiana M. Bocanegra-Bahamón, Kuo-Nung Wang, Panagiotis Vergados, Chi O. Ao, Sami W. Asmar, Robert A. Preston
Figure caption: Minimum uncertainty estimates (see text) for X–Ka-band RO retrievals of H2SO4 and SO2 abundances at 0.5 km resolution compared to S–X-band retrievals assuming other absorber abundances are known exactly. Inflection points occur at altitudes where the statistical uncertainty exceeds the abundance necessary to match the set (2) model atmosphere absorptivities.
Paper: Approaches for Retrieving Sulfur Species Abundances from Dual X–Ka-band Radio Occultations of Venus with EnVision and VERITAS
Authors: Alex B. Akins, Tatiana M. Bocanegra-Bahamón, Kuo-Nung Wang, Panagiotis Vergados, Chi O. Ao, Sami W. Asmar, Robert A. Preston
Figure caption: Retrievals of sets (1)–(8) model atmosphere abundances of SO2 and H2SO4 aerosol with uncertainties.
Paper: Approaches for Retrieving Sulfur Species Abundances from Dual X–Ka-band Radio Occultations of Venus with EnVision and VERITAS
Authors: Alex B. Akins, Tatiana M. Bocanegra-Bahamón, Kuo-Nung Wang, Panagiotis Vergados, Chi O. Ao, Sami W. Asmar, Robert A. Preston
Figure caption: Left: SO2 mole fraction profiles from the chemical models of Krasnopolsky (2012), Zhang et al. (2012), Bierson & Zhang (2020), Rimmer et al. (2021), and Vega ISAV spectrometer measurements (Bertaux et al. 1996). Right: cloud bulk density profiles from 2D transport models of Imamura & Hashimoto (1998), Oschlisniok et al. (2021) and Pioneer Venus LCPS measurements (Knollenberg & Hunten 1980).
Paper: Approaches for Retrieving Sulfur Species Abundances from Dual X–Ka-band Radio Occultations of Venus with EnVision and VERITAS
Authors: Alex B. Akins, Tatiana M. Bocanegra-Bahamón, Kuo-Nung Wang, Panagiotis Vergados, Chi O. Ao, Sami W. Asmar, Robert A. Preston
Figure caption: Abundances of H2SO4 and SO2 (top) retrieved from simulated dual X–Ka-band RO absorptivities (bottom) for the set (1) model atmosphere, with uncertainties determined using Equation (30). Seed profiles were provided to the final optimization stage from the outputs of the atmospheric transport and MCMC steps (see text).