adsabs/AstroCLIMB huggingface dataset:
Paper: History and Habitability of the LP 890-9 Planetary System
Authors: Rory Barnes, Laura N. R. do Amaral, Jessica Birky, Ludmila Carone, Peter Driscoll, Joseph R. Livesey, David Graham, Juliette Becker, Kaiming Cui, Martin Schlecker, Rodolfo Garcia, Megan Gialluca, Arthur Adams, MD Redyan Ahmed, Paul Bonney, Wynter Broussard, Chetan Chawla, Mario Damasso, William C. Danchi, Russell Deitrick, Elsa Ducrot, Emeline F. Fromont, Brandt A. L. Gaches, Sakshi Gupta, Michelle L. Hill, James A. G. Jackman, Estelle M. Janin, Mikołaj Karawacki, Matheus Daniel Koren, Roberto La Greca, Michaela Leung, Arturo Miranda-Rosete, Michael Kent A. Olohoy, Cecelia Ngo, Daria Paul, Chandan Kumar Sahu, Debajyoti Basu Sarkar, Mohammad Afzal Shadab, Edward W. Schwieterman, Melissa Sedler, Katie Texeira, Allona Vazan, Karen N. Delgado Vega, Rohit Vijayakumar, Jonathan T. Wojack
Figure caption: The results of a parameter sweep over the mass, orbital eccentricity, and viscosity activation energy for each planet. Individual trials are plotted as thin solid curves. The evolution of the fiducial case is overlaid in the left panel with thick curves. The distribution of the fraction of the total internal heat generated by radiogenic heating at the present day (a stellar age of 7.2 Gyr) is plotted as a histogram for each planet in the right panel. The orbit of the inner planet, LP 890-9 b, always circularizes by the end of the integration, leaving the primary source of internal heating to be radiogenic heating in all integrations. The outer planet, LP 890-9 c, has a much more varied range of heating ratios at the end of the integration so that the primary internal heat source at present day cannot be securely determined.
Paper: History and Habitability of the LP 890-9 Planetary System
Authors: Rory Barnes, Laura N. R. do Amaral, Jessica Birky, Ludmila Carone, Peter Driscoll, Joseph R. Livesey, David Graham, Juliette Becker, Kaiming Cui, Martin Schlecker, Rodolfo Garcia, Megan Gialluca, Arthur Adams, MD Redyan Ahmed, Paul Bonney, Wynter Broussard, Chetan Chawla, Mario Damasso, William C. Danchi, Russell Deitrick, Elsa Ducrot, Emeline F. Fromont, Brandt A. L. Gaches, Sakshi Gupta, Michelle L. Hill, James A. G. Jackman, Estelle M. Janin, Mikołaj Karawacki, Matheus Daniel Koren, Roberto La Greca, Michaela Leung, Arturo Miranda-Rosete, Michael Kent A. Olohoy, Cecelia Ngo, Daria Paul, Chandan Kumar Sahu, Debajyoti Basu Sarkar, Mohammad Afzal Shadab, Edward W. Schwieterman, Melissa Sedler, Katie Texeira, Allona Vazan, Karen N. Delgado Vega, Rohit Vijayakumar, Jonathan T. Wojack
Figure caption: Evolution of the atmospheric parameters for LP 890-9 b (red) and c (blue), with an initial surface water content of 1 TO (left panels), 3 TO (middle panels), and 10 TO (right panels). First row: surface water content. The solid, dashed, and dotted curves represent an initial envelope mass of 0, 0.01, and 0.1 M⊕, respectively. Curves with high and low opacity represent the cases when the oxygen does or does not react with the surface, respectively. Second row: O2 in the mantle. Third row: O2 accumulated in the atmosphere Fourth row: crossover mass. The horizontal light blue line represents the limit where the oxygen can be dragged along the hydrogen background out of the atmosphere.
Paper: History and Habitability of the LP 890-9 Planetary System
Authors: Rory Barnes, Laura N. R. do Amaral, Jessica Birky, Ludmila Carone, Peter Driscoll, Joseph R. Livesey, David Graham, Juliette Becker, Kaiming Cui, Martin Schlecker, Rodolfo Garcia, Megan Gialluca, Arthur Adams, MD Redyan Ahmed, Paul Bonney, Wynter Broussard, Chetan Chawla, Mario Damasso, William C. Danchi, Russell Deitrick, Elsa Ducrot, Emeline F. Fromont, Brandt A. L. Gaches, Sakshi Gupta, Michelle L. Hill, James A. G. Jackman, Estelle M. Janin, Mikołaj Karawacki, Matheus Daniel Koren, Roberto La Greca, Michaela Leung, Arturo Miranda-Rosete, Michael Kent A. Olohoy, Cecelia Ngo, Daria Paul, Chandan Kumar Sahu, Debajyoti Basu Sarkar, Mohammad Afzal Shadab, Edward W. Schwieterman, Melissa Sedler, Katie Texeira, Allona Vazan, Karen N. Delgado Vega, Rohit Vijayakumar, Jonathan T. Wojack
Figure caption: Left: magma ocean solidification time of LP 890-9 c vs. initial water content in TO for different planetary masses and for disk dissipation times t(0) of 20 Myr (solid lines) and 6 Myr (dashed lines), respectively. (We note that the solid orange line lies underneath the solid green line.) Right: abiotic oxygen build-up (partial pressures of O2 in bar) in LP 890-9c during the magma ocean stage as a function of initial water mass.
Paper: History and Habitability of the LP 890-9 Planetary System
Authors: Rory Barnes, Laura N. R. do Amaral, Jessica Birky, Ludmila Carone, Peter Driscoll, Joseph R. Livesey, David Graham, Juliette Becker, Kaiming Cui, Martin Schlecker, Rodolfo Garcia, Megan Gialluca, Arthur Adams, MD Redyan Ahmed, Paul Bonney, Wynter Broussard, Chetan Chawla, Mario Damasso, William C. Danchi, Russell Deitrick, Elsa Ducrot, Emeline F. Fromont, Brandt A. L. Gaches, Sakshi Gupta, Michelle L. Hill, James A. G. Jackman, Estelle M. Janin, Mikołaj Karawacki, Matheus Daniel Koren, Roberto La Greca, Michaela Leung, Arturo Miranda-Rosete, Michael Kent A. Olohoy, Cecelia Ngo, Daria Paul, Chandan Kumar Sahu, Debajyoti Basu Sarkar, Mohammad Afzal Shadab, Edward W. Schwieterman, Melissa Sedler, Katie Texeira, Allona Vazan, Karen N. Delgado Vega, Rohit Vijayakumar, Jonathan T. Wojack
Figure caption: Evolution of some of LP 890-9’s stellar properties. Note that the “Time” in each panel is offset by 5 Myr from the I. Baraffe et al. (2015) model grids that form the foundation for the stellar evolution model, see Section 2.1. Each panel includes 10% of 1000 trials sampled within the ranges described in the main text. The red lines and shading represent the best fit and 1σ uncertainties of each parameter, if available. Top left: bolometric luminosity. Top right: XUV luminosity. The blue curve is the best-fit history of the star. Bottom left: effective temperature. Bottom right: radius.
Paper: History and Habitability of the LP 890-9 Planetary System
Authors: Rory Barnes, Laura N. R. do Amaral, Jessica Birky, Ludmila Carone, Peter Driscoll, Joseph R. Livesey, David Graham, Juliette Becker, Kaiming Cui, Martin Schlecker, Rodolfo Garcia, Megan Gialluca, Arthur Adams, MD Redyan Ahmed, Paul Bonney, Wynter Broussard, Chetan Chawla, Mario Damasso, William C. Danchi, Russell Deitrick, Elsa Ducrot, Emeline F. Fromont, Brandt A. L. Gaches, Sakshi Gupta, Michelle L. Hill, James A. G. Jackman, Estelle M. Janin, Mikołaj Karawacki, Matheus Daniel Koren, Roberto La Greca, Michaela Leung, Arturo Miranda-Rosete, Michael Kent A. Olohoy, Cecelia Ngo, Daria Paul, Chandan Kumar Sahu, Debajyoti Basu Sarkar, Mohammad Afzal Shadab, Edward W. Schwieterman, Melissa Sedler, Katie Texeira, Allona Vazan, Karen N. Delgado Vega, Rohit Vijayakumar, Jonathan T. Wojack
Figure caption: Time evolution of planetary radius (upper panel), hydrogen envelope mass (middle panel), and XUV flux at the planetary atmosphere (bottom panel). The horizontal orange line in the bottom panel indicates the XUV flux on the present Earth. Horizontal lines in the top panel indicate the observed planetary radii of LP 890-9 b and c (L. Delrez et al. 2022). The shadow in the inset of the top panel shows the planetary radius uncertainty.
Paper: History and Habitability of the LP 890-9 Planetary System
Authors: Rory Barnes, Laura N. R. do Amaral, Jessica Birky, Ludmila Carone, Peter Driscoll, Joseph R. Livesey, David Graham, Juliette Becker, Kaiming Cui, Martin Schlecker, Rodolfo Garcia, Megan Gialluca, Arthur Adams, MD Redyan Ahmed, Paul Bonney, Wynter Broussard, Chetan Chawla, Mario Damasso, William C. Danchi, Russell Deitrick, Elsa Ducrot, Emeline F. Fromont, Brandt A. L. Gaches, Sakshi Gupta, Michelle L. Hill, James A. G. Jackman, Estelle M. Janin, Mikołaj Karawacki, Matheus Daniel Koren, Roberto La Greca, Michaela Leung, Arturo Miranda-Rosete, Michael Kent A. Olohoy, Cecelia Ngo, Daria Paul, Chandan Kumar Sahu, Debajyoti Basu Sarkar, Mohammad Afzal Shadab, Edward W. Schwieterman, Melissa Sedler, Katie Texeira, Allona Vazan, Karen N. Delgado Vega, Rohit Vijayakumar, Jonathan T. Wojack
Figure caption: Example simulation of LP 890-9 c assuming a mass of 2.2 M⊕ and 5 TO of initial water content, assuming disk dissipation at 6 Myr. Left: water evolution during the magma ocean stage shows all water is lost from the atmosphere after 18 Myr. Right: oxygen evolution during the magma ocean stage, where the majority of the O2 escapes into space.
Paper: History and Habitability of the LP 890-9 Planetary System
Authors: Rory Barnes, Laura N. R. do Amaral, Jessica Birky, Ludmila Carone, Peter Driscoll, Joseph R. Livesey, David Graham, Juliette Becker, Kaiming Cui, Martin Schlecker, Rodolfo Garcia, Megan Gialluca, Arthur Adams, MD Redyan Ahmed, Paul Bonney, Wynter Broussard, Chetan Chawla, Mario Damasso, William C. Danchi, Russell Deitrick, Elsa Ducrot, Emeline F. Fromont, Brandt A. L. Gaches, Sakshi Gupta, Michelle L. Hill, James A. G. Jackman, Estelle M. Janin, Mikołaj Karawacki, Matheus Daniel Koren, Roberto La Greca, Michaela Leung, Arturo Miranda-Rosete, Michael Kent A. Olohoy, Cecelia Ngo, Daria Paul, Chandan Kumar Sahu, Debajyoti Basu Sarkar, Mohammad Afzal Shadab, Edward W. Schwieterman, Melissa Sedler, Katie Texeira, Allona Vazan, Karen N. Delgado Vega, Rohit Vijayakumar, Jonathan T. Wojack
Figure caption: Evolution of LP 890-9’s HZ for 10% of the 1000 trials. The pale blue curves correspond to the “early Mars” limit, dark blue to “maximum greenhouse,” orange to “runaway greenhouse,” and red to “recent Venus” (R. K. Kopparapu et al. 2013). Thin curves represent individual trials, while the thick line is the average. The current orbits of planets b and c, assuming the best-fit stellar mass, are shown with dashed black lines.
Paper: History and Habitability of the LP 890-9 Planetary System
Authors: Rory Barnes, Laura N. R. do Amaral, Jessica Birky, Ludmila Carone, Peter Driscoll, Joseph R. Livesey, David Graham, Juliette Becker, Kaiming Cui, Martin Schlecker, Rodolfo Garcia, Megan Gialluca, Arthur Adams, MD Redyan Ahmed, Paul Bonney, Wynter Broussard, Chetan Chawla, Mario Damasso, William C. Danchi, Russell Deitrick, Elsa Ducrot, Emeline F. Fromont, Brandt A. L. Gaches, Sakshi Gupta, Michelle L. Hill, James A. G. Jackman, Estelle M. Janin, Mikołaj Karawacki, Matheus Daniel Koren, Roberto La Greca, Michaela Leung, Arturo Miranda-Rosete, Michael Kent A. Olohoy, Cecelia Ngo, Daria Paul, Chandan Kumar Sahu, Debajyoti Basu Sarkar, Mohammad Afzal Shadab, Edward W. Schwieterman, Melissa Sedler, Katie Texeira, Allona Vazan, Karen N. Delgado Vega, Rohit Vijayakumar, Jonathan T. Wojack
Figure caption: Example of the coupled tidal + orbital evolution of the LP 890-9 planetary system over 100 Myr. Dashed lines represent the best-fit values and the shaded gray regions demarcate the 1σ credible intervals from L. Delrez et al. (2022).
Paper: Particle Accretion in Microgravity. I. Particle Sizes and Bulk Densities
Authors: Akbar D. Whizin, Daniel D. Durda, Constantine C. C. Tsang, Stanley G. Love
Figure caption: Measured aggregate size ratios of the four materials we tested for the 10 g sample mass (0.069 g cm−3) for the >500 μm PSD. Insufficient quantities of ALH 83100 were available for this PSD.
Paper: Particle Accretion in Microgravity. I. Particle Sizes and Bulk Densities
Authors: Akbar D. Whizin, Daniel D. Durda, Constantine C. C. Tsang, Stanley G. Love
Figure caption: The median aggregate size (measured cross sections in the imagery) of aggregates for the three bulk densities flown for all compositions. Colors and symbols delineate composition.
Paper: Particle Accretion in Microgravity. I. Particle Sizes and Bulk Densities
Authors: Akbar D. Whizin, Daniel D. Durda, Constantine C. C. Tsang, Stanley G. Love
Figure caption: Measured aggregate size ratios of the five materials we tested for the 19.5 g sample mass (0.014 g cm−3) for the 125–250 μm PSD.
Paper: Particle Accretion in Microgravity. I. Particle Sizes and Bulk Densities
Authors: Akbar D. Whizin, Daniel D. Durda, Constantine C. C. Tsang, Stanley G. Love
Figure caption: Measured aggregate size ratios of the five materials we tested for the 10 g sample mass (0.0069 g cm−3) for the 500–1000 μm PSD.
Paper: Particle Accretion in Microgravity. I. Particle Sizes and Bulk Densities
Authors: Akbar D. Whizin, Daniel D. Durda, Constantine C. C. Tsang, Stanley G. Love
Figure caption: Measured aggregate size ratios of the five materials we tested for the 10 g sample mass (0.0069 g cm−3) for the 125–250 μm PSD.
Paper: Particle Accretion in Microgravity. I. Particle Sizes and Bulk Densities
Authors: Akbar D. Whizin, Daniel D. Durda, Constantine C. C. Tsang, Stanley G. Love
Figure caption: Aggregate size ratios for the 10 g samples for the different PSDs used; trend lines are linear regressions to the mean across samples.
Paper: Particle Accretion in Microgravity. I. Particle Sizes and Bulk Densities
Authors: Akbar D. Whizin, Daniel D. Durda, Constantine C. C. Tsang, Stanley G. Love
Figure caption: Aggregate size ratios for the 3 g samples for the different PSDs used; trend lines are linear regressions to the mean across samples.
Paper: Particle Accretion in Microgravity. I. Particle Sizes and Bulk Densities
Authors: Akbar D. Whizin, Daniel D. Durda, Constantine C. C. Tsang, Stanley G. Love
Figure caption: The fitted trends over varying bulk density for the 125–250 μm PSD samples from Figure 15, normalized to the mean of the ratios.
Paper: Particle Accretion in Microgravity. I. Particle Sizes and Bulk Densities
Authors: Akbar D. Whizin, Daniel D. Durda, Constantine C. C. Tsang, Stanley G. Love
Figure caption: Mean aggregate size ratios (to the geometric mean of the PSD) at the three bulk densities flown for all compositions.
Paper: Particle Accretion in Microgravity. I. Particle Sizes and Bulk Densities
Authors: Akbar D. Whizin, Daniel D. Durda, Constantine C. C. Tsang, Stanley G. Love
Figure caption: Aggregate size variances for the sample densities flown.
Paper: Particle Accretion in Microgravity. I. Particle Sizes and Bulk Densities
Authors: Akbar D. Whizin, Daniel D. Durda, Constantine C. C. Tsang, Stanley G. Love
Figure caption: Aggregate size variances for the PSDs flown.
Paper: Particle Accretion in Microgravity. I. Particle Sizes and Bulk Densities
Authors: Akbar D. Whizin, Daniel D. Durda, Constantine C. C. Tsang, Stanley G. Love
Figure caption: All sets of PSDs and bulk density experiments performed in this study (125–250 μm samples averaged together). The symbol shapes and colors represent the PSD with power-law trend lines fit to them.
Paper: Modeling Ice and Dust in Comet C/2017 K2 (Pan-STARRS)’s Coma
Authors: Megan Firgard, Theodore Kareta
Figure caption: The upper panel shows the reflectance spectra of K2 taken on 2021 April 30 plotted with three different level 1 models in different colors (all assuming B. Hapke 1993 style scattering). They are as follows: intimate mixing with crystalline water ice at 100 K and O. Edoh (1983) amorphous carbon (blue), intimate mixing with amorphous water ice at low temperatures and O. Edoh (1983) amorphous carbon (orange), and linear mixing with crystalline water ice at 150 K and O. Edoh (1983) amorphous carbon (red). The lower panel shows the residuals (the modeled data subtracted from the actual data) for each point. The colors of the points in the bottom panel match those of the top panel. The shaded gray regions in both panels are the areas of high telluric absorption, as in Figure 1. The linear mixing model noticeably does not fit the depth of the water ice feature at 2.0 μm as well as the two intimate mixing models do despite having a similar reduced-χ2 value. None of the three models capture the 2.2 μm and longward reflective behavior well.
Paper: Modeling Ice and Dust in Comet C/2017 K2 (Pan-STARRS)’s Coma
Authors: Megan Firgard, Theodore Kareta
Figure caption: The trends of the median estimates for the ice percentage and α of two models plotted as a function of heliocentric distance. The left panel plots ice percentage against heliocentric distance, and the right panel plots α against heliocentric distance. The two models are the same two presented for all three data sets in Section 4; specifically, the red line is the linear mixing with Mie scattering, crystalline water ice at 100 K and Hapke scattering, F. Rouleau & P. G. Martin (1991) amorphous carbon model, and the blue line is the linear mixing with Mie scattering, amorphous water ice at low temperatures and Hapke scattering, F. Rouleau & P. G. Martin (1991) amorphous carbon model. Each dot is one of our three data sets. These graphs show how the two components of K2’s coma, the ice and the dust, change as the comet approaches the Sun and crosses the water ice line at ∼3 au.
Paper: Modeling Ice and Dust in Comet C/2017 K2 (Pan-STARRS)’s Coma
Authors: Megan Firgard, Theodore Kareta
Figure caption: Two corner plots showing the MCMC distributions of values for two different models of K2’s spectrum from 2021 April 30: linear mixing with Mie scattered crystalline water ice at 100 K and Hapke scattering, F. Rouleau & P. G. Martin (1991) amorphous carbon (left; first presented in Figure 4), and linear mixing with Mie scattered amorphous water ice at low temperatures and Hapke scattering, F. Rouleau & P. G. Martin (1991) amorphous carbon (right). The bimodal, or two-peaked distributions, seen in parts of both corner plots are indicative of a real degeneracy in our ability to fit these spectra, and is a clear indication that a least squares fitting approach is insufficient in many cases. This is described at length in the text.
Paper: Modeling Ice and Dust in Comet C/2017 K2 (Pan-STARRS)’s Coma
Authors: Megan Firgard, Theodore Kareta
Figure caption: The corner plot (left) and reflectance spectrum taken on 2021 April 30 with residuals (right) of K2. The data are shown in black, and a level 3 model, composed of a linear mix of single-sized 100 K crystalline ice grains in the Mie regime and a power-law distribution of dust sizes using the F. Rouleau & P. G. Martin (1991) amorphous carbon optical constants, is shown in red. The reflectance spectra and residuals have the same layout as in Figure 2. The corner plot likewise has the same format as in Figure 3, but this time with five parameters: α (which governs the power-law size distribution of dust grains), fvac (a proxy for porosity in the dust grains), Dice, fice, and ﹩{\mathrm{log}}\,f﹩ As is described in the text, the bimodal distribution (e.g., of fice vs. α) is indicative of there being two classes of solutions which can model the same data equally well.
Paper: Modeling Ice and Dust in Comet C/2017 K2 (Pan-STARRS)’s Coma
Authors: Megan Firgard, Theodore Kareta
Figure caption: The corner plot (left) and reflectance spectra taken on 2021 April 30 with residuals (right, formatted the same as previous graphs) of K2 for the level 2 model of Hapke intimate mixing with crystalline water ice at 100 K and O. Edoh (1983) amorphous carbon (red). The corner plot shows the distribution of points picked by the MCMC walkers for the three parameters Deff, fice, and ﹩{\mathrm{log}}\,f﹩. The two-dimensional frames show how the parameters vary with one another, the darkest contours representing the most picked values, and the one-dimensional histograms along the diagonal show how each parameter varies with itself. We note that the histograms in this graph are well approximated by normal distributions; this is not necessarily the case in our later plots.
Paper: Modeling Ice and Dust in Comet C/2017 K2 (Pan-STARRS)’s Coma
Authors: Megan Firgard, Theodore Kareta
Figure caption: Reflectance spectrum and residuals of K2 from 2021 April 30 for the same two models in Figure 5. The red curve is the linear mixing with Mie scattering, crystalline water ice at 100 K and Hapke scattering, F. Rouleau & P. G. Martin (1991) amorphous carbon model, while the blue curve is the linear mixing with Mie scattering, amorphous water ice at low temperatures and Hapke scattering, F. Rouleau & P. G. Martin (1991) amorphous carbon model. The most noticeable difference in the models are in the way they fit the 1.5 and 2.0 μm water ice bands. The crystalline ice model does a slightly better job at fitting the 2.0 μm absorption feature, but this is not very significant.
Paper: Modeling Ice and Dust in Comet C/2017 K2 (Pan-STARRS)’s Coma
Authors: Megan Firgard, Theodore Kareta
Figure caption: Reflectance spectrum, two models, and respective residuals of K2 from the 2022 June 4 LDT data. The red curve is the linear mixing with Mie scattering, crystalline water ice at 100 K and Hapke scattering, F. Rouleau & P. G. Martin (1991) amorphous carbon model, and the blue curve is the linear mixing with Mie scattering, amorphous water ice at low temperatures and Hapke scattering, F. Rouleau & P. G. Martin (1991) amorphous carbon model. Even without the data in the 2.0 μm region, there is some variation between the two models with different ice characteristics, suggesting that there is still some ice present at the time these data were taken.
Paper: Modeling Ice and Dust in Comet C/2017 K2 (Pan-STARRS)’s Coma
Authors: Megan Firgard, Theodore Kareta
Figure caption: Reflectance spectrum, two models, and respective residuals of K2 from the 2022 September 5 Gemini South data. The red curve is the linear mixing with Mie scattering, crystalline water ice at 100 K and Hapke scattering, F. Rouleau & P. G. Martin (1991) amorphous carbon model, and the blue dashed curve is the linear mixing with Mie scattering, amorphous water ice at low temperatures and Hapke scattering, F. Rouleau & P. G. Martin (1991) amorphous carbon model. The amorphous ice model is dashed in this graph to allow both models to be visible. As both models converge to incredibly low ice fractions and very similar dust properties, these models look very similar.
Paper: Modeling Ice and Dust in Comet C/2017 K2 (Pan-STARRS)’s Coma
Authors: Megan Firgard, Theodore Kareta
Figure caption: Two corner plots showing the MCMC distributions for two different models of K2’s spectrum from the 2022 June 4 LDT data. These models are linear mixing with Mie scattered crystalline water ice at 100 K and Hapke scattering, F. Rouleau & P. G. Martin (1991) amorphous carbon (left), and linear mixing with Mie scattered amorphous water ice at low temperatures and Hapke scattering, F. Rouleau & P. G. Martin (1991) amorphous carbon (right).
Paper: Ejecta Mass Estimates from the DART Impact Plume Inferred from LICIACube Images
Authors: Ramin Lolachi, David A. Glenar, Timothy J. Stubbs, Ludmilla Kolokolova, Olga Muñoz, Tony L. Farnham, Masatoshi Hirabayashi, Pedro H. Hasselmann, Vincenzo Della Corte, J. D. Prasanna Deshapriya, Elisabetta Dotto, Elena Mazzotta Epifani, Alessandro Rossi, Angelo Zinzi
Figure caption: Scatter plot showing measured plume radiance in the green channel, with uncertainties. Large target distance (symbol size is proportional to distance) results in a wide plume capture area (up to ≈3.8 km) and confident estimates of cumulative radiance. At intermediate field sizes (marked “partially clipped” in Table 1), radiance is adjusted for clipping using a shape-matching procedure as described in the text and in Figure 5. This procedure becomes unreliable for heavily clipped cases (gray circles), where rb < 1 km. These exhibit excessive scatter and are excluded from further analysis. Square points indicate reference images from Table 1. Inset images show examples of extreme cases.