adsabs/AstroCLIMB huggingface dataset:
Paper: SCExAO/CHARIS Near-infrared Scattered-light Imaging and Integral Field Spectropolarimetry of the AB Aurigae Protoplanetary System
Authors: Erica Dykes, Thayne Currie, Kellen Lawson, Miles Lucas, Tomoyuki Kudo, Minghan Chen, Olivier Guyon, Tyler D. Groff, Julien Lozi, Jeffrey Chilcote, Timothy D. Brandt, Sebastien Vievard, Nour Skaf, Vincent Deo, Mona El Morsy, Danielle Bovie, Taichi Uyama, Carol Grady, Michael Sitko, Jun Hashimoto, Frantz Martinache, Nemanja Jovanovic, Motohide Tamura, N. Jeremy Kasdin
Figure caption: SCExAO/CHARIS AB Aur broadband Q  ϕ  images (wavelength collapsed) from 2020 October 4 obtained from PDI processing. The reduction described in Section 2 was used for both the linearly scaled (left) and radius-squared-scaled (right) images shown. The image color map intensity scaling goes from the 10th to 99.7th percentiles of count values (i.e., np.nanpercentile(image, (10, 99.7)) in the Python NumPy package).
Paper: SCExAO/CHARIS Near-infrared Scattered-light Imaging and Integral Field Spectropolarimetry of the AB Aurigae Protoplanetary System
Authors: Erica Dykes, Thayne Currie, Kellen Lawson, Miles Lucas, Tomoyuki Kudo, Minghan Chen, Olivier Guyon, Tyler D. Groff, Julien Lozi, Jeffrey Chilcote, Timothy D. Brandt, Sebastien Vievard, Nour Skaf, Vincent Deo, Mona El Morsy, Danielle Bovie, Taichi Uyama, Carol Grady, Michael Sitko, Jun Hashimoto, Frantz Martinache, Nemanja Jovanovic, Motohide Tamura, N. Jeremy Kasdin
Figure caption: (Top) color excess as a function of radial separation for the major and minor axis. J − H is shown in yellow, H − Ks in blue, and J − Ks in gray. AB Aur b’s J − Ks, J − H, and H − K colors are also shown for reference (pink, blue, and purple dot, respectively) at its corresponding separation, though it is important to note that it does not physically lie along the minor axis. AB Aur b’s J − H and H − K colors are offset from the actual separation value for clarity. (Bottom) color excess with stellar color subtracted as a function of radial separation along the major and minor axis of AB Aur’s disk. J − H is shown in yellow, H − Ks in blue, and J − Ks in gray.
Paper: Theoretical Diagnostics for Narrow-line Regions of Active Galactic Nuclei
Authors: Peixin Zhu, Lisa J. Kewley, Ralph S. Sutherland
Figure caption: The effect of nitrogen scaling relation on UV and optical E peak diagnostics for the AGN narrow-line regions as predicted by AGN models with ﹩\mathrm{log}(P/k)=7.0﹩ and ﹩\mathrm{log}(U)=﹩−3.0. As in Figure 7, but with line styles representing the nitrogen scaling relation used in the AGN models. (NHlow in solid lines and NHhigh in dashed lines).
Paper: SCExAO/CHARIS Near-infrared Scattered-light Imaging and Integral Field Spectropolarimetry of the AB Aurigae Protoplanetary System
Authors: Erica Dykes, Thayne Currie, Kellen Lawson, Miles Lucas, Tomoyuki Kudo, Minghan Chen, Olivier Guyon, Tyler D. Groff, Julien Lozi, Jeffrey Chilcote, Timothy D. Brandt, Sebastien Vievard, Nour Skaf, Vincent Deo, Mona El Morsy, Danielle Bovie, Taichi Uyama, Carol Grady, Michael Sitko, Jun Hashimoto, Frantz Martinache, Nemanja Jovanovic, Motohide Tamura, N. Jeremy Kasdin
Figure caption: SNR maps for PI (top row) and total intensity (bottom row) observations in J, H, and K passbands.
Paper: SCExAO/CHARIS Near-infrared Scattered-light Imaging and Integral Field Spectropolarimetry of the AB Aurigae Protoplanetary System
Authors: Erica Dykes, Thayne Currie, Kellen Lawson, Miles Lucas, Tomoyuki Kudo, Minghan Chen, Olivier Guyon, Tyler D. Groff, Julien Lozi, Jeffrey Chilcote, Timothy D. Brandt, Sebastien Vievard, Nour Skaf, Vincent Deo, Mona El Morsy, Danielle Bovie, Taichi Uyama, Carol Grady, Michael Sitko, Jun Hashimoto, Frantz Martinache, Nemanja Jovanovic, Motohide Tamura, N. Jeremy Kasdin
Figure caption: Surface brightness as a function of radial separation along the major (right) and minor axis (left) of AB Aur’s disk. The values for J, H, and K are shown in blue, turquoise, and orange, respectively.
Paper: Cosmic-Ray North–South Anisotropy: Rigidity Spectrum and Solar Cycle Variations Observed by Ground-based Muon Detectors
Authors: M. Kozai, Y. Hayashi, K. Fujii, K. Munakata, C. Kato, N. Miyashita, A. Kadokura, R. Kataoka, S. Miyake, M. L. Duldig, J. E. Humble, K. Iwai
Figure caption: Results of Bayesian estimation for the rigidity spectrum of the NS anisotropy [%] in sample years (a) 2009 and (b) 2015. A solid black line in each upper panel is the mean spectrum Θ, while dashed lines above and below the spectrum represent its error range. A horizontal blue line is the mean vector Θ  G  of the prior probability distribution. Filled circles in each lower panel show a scatter plot between the observable ﹩{\eta }_{l}^{{TA}}﹩'s of all channel pairs (vertical axis) and their expected values ﹩{\tilde{\eta }}_{l}^{{TA}}﹩'s from the mean spectrum (horizontal axis). An open circle in each lower panel represents the observed and expected values of Nagoya-GG.
Paper: Cosmic-Ray North–South Anisotropy: Rigidity Spectrum and Solar Cycle Variations Observed by Ground-based Muon Detectors
Authors: M. Kozai, Y. Hayashi, K. Fujii, K. Munakata, C. Kato, N. Miyashita, A. Kadokura, R. Kataoka, S. Miyake, M. L. Duldig, J. E. Humble, K. Iwai
Figure caption: Differential response of each channel pair to the NS anisotropy.
Paper: Cosmic-Ray North–South Anisotropy: Rigidity Spectrum and Solar Cycle Variations Observed by Ground-based Muon Detectors
Authors: M. Kozai, Y. Hayashi, K. Fujii, K. Munakata, C. Kato, N. Miyashita, A. Kadokura, R. Kataoka, S. Miyake, M. L. Duldig, J. E. Humble, K. Iwai
Figure caption: Visualization of general graph matching for optimizing channel pairs. Each node corresponds to a directional channel, and each edge connecting the nodes represents each channel pair. The line width of each edge is proportional to the sensitivity a  ij  of each pair ij, and red edges represent the pairs derived as the optimal solution.
Paper: Semisupervised Learning for Detecting Inverse Compton Emission in Galaxy Clusters
Authors: Sheng-Chieh Lin, Yuanyuan Su, Fabio Gastaldello, Nathan Jacobs
Figure caption: Performance measures (precision, recall, and BAcc) as a function of thermal parameters for CAE (blue) and spectral-fitting results (red). The ground-truth labels from left to right are redshift (z), temperature (kT), metallicity (Z), and normalization (norm.) of apec. The thermal parameters of the Coma cluster, obtained from the spectral fitting, are indicated by the dashed lines, for which redshift is fixed at 0.023 (F. Gastaldello et al. 2015). Note that the redshift fixed in fitting is estimated from the velocity dispersion of member galaxies (M. F. Struble & H. J. Rood 1999).
Paper: Semisupervised Learning for Detecting Inverse Compton Emission in Galaxy Clusters
Authors: Sheng-Chieh Lin, Yuanyuan Su, Fabio Gastaldello, Nathan Jacobs
Figure caption: Relation between recall and precision. CAE is shown as orange, and the ordinary autoencoder (AE) is shown as gray. The red and blue points mark the values when using the chosen selection threshold of R  a  = 0.00042. The horizontal dashed line marks a precision of 0.5, representing the performance of a random classifier.
Paper: Semisupervised Learning for Detecting Inverse Compton Emission in Galaxy Clusters
Authors: Sheng-Chieh Lin, Yuanyuan Su, Fabio Gastaldello, Nathan Jacobs
Figure caption: Latent representations as functions of thermal parameters θ = {kT, Z, z, n} of apec. The x-axis is the ground truth θ; the y-axis is the constrained latent representation. True 1T+IC data are marked as red open circles, and true 2T data are marked as blue circles. The ground-truth temperature and normalization of the 2T spectra are obtained by fitting the data with a 1T apec model. The black dashed line marks the 1:1 relation.
Paper: Semisupervised Learning for Detecting Inverse Compton Emission in Galaxy Clusters
Authors: Sheng-Chieh Lin, Yuanyuan Su, Fabio Gastaldello, Nathan Jacobs
Figure caption: Confusion matrices of CAE, AE, and spectral-fitting methods. The y-axis labels the true spectra type, and the x-axis marks the predictions using these approaches.
Paper: Low-latitude Auroras: Insights from 2023 April 23 Solar Storm
Authors: Geeta Vichare, Ankush Bhaskar, Rahul Rawat, Virendra Yadav, Wageesh Mishra, Dorje Angchuk, Anand Kumar Singh
Figure caption: Horizontal magnetic field variation at different latitudes between the 70°E and 115°E longitude sectors. The Sym-H index is shown on top in the left panel. Station code, GGLat, and LT are shown on the right side of each plot. The left and right panels are separated based on the nature of the variation between the two vertical dotted lines.
Paper: Low-latitude Auroras: Insights from 2023 April 23 Solar Storm
Authors: Geeta Vichare, Ankush Bhaskar, Rahul Rawat, Virendra Yadav, Wageesh Mishra, Dorje Angchuk, Anand Kumar Singh
Figure caption: Equatorward auroral boundary based on (a) DMSP-F18 observations and the fitted GUVI model global boundary (GGLat red dashed curve) and (b) Swarm (GGLat, red open circles, and GMLat, black filled circles) for the Northern Hemisphere during 2023 April 23–24.
Paper: Low-latitude Auroras: Insights from 2023 April 23 Solar Storm
Authors: Geeta Vichare, Ankush Bhaskar, Rahul Rawat, Virendra Yadav, Wageesh Mishra, Dorje Angchuk, Anand Kumar Singh
Figure caption: Sketch showing the geometry of auroral visibility at observer latitude (θ  o ). C is the center of the Earth; a is the radius of the Earth, 6370 km; P is the point of auroral precipitation at height “h” km at GGLat θ  A , and A is the point on the surface of the Earth. B is the tangent point at the surface of the Earth line originating from point P, and θ  A  is the latitude of that point. β is the maximum elevation angle of the aurora seen by the observer. The sketch is not to scale.
Paper: Low-latitude Auroras: Insights from 2023 April 23 Solar Storm
Authors: Geeta Vichare, Ankush Bhaskar, Rahul Rawat, Virendra Yadav, Wageesh Mishra, Dorje Angchuk, Anand Kumar Singh
Figure caption: Aurora seen from Indian Antarctic station Maitri on 2023 April 23: (a) photograph at 22:01 UT, (b) all-sky camera at 19:22 UT.
Paper: Low-latitude Auroras: Insights from 2023 April 23 Solar Storm
Authors: Geeta Vichare, Ankush Bhaskar, Rahul Rawat, Virendra Yadav, Wageesh Mishra, Dorje Angchuk, Anand Kumar Singh
Figure caption: Pi2 pulsations observed at low-latitude night stations; bandpass between 5 and 25 mHz.
Paper: Low-latitude Auroras: Insights from 2023 April 23 Solar Storm
Authors: Geeta Vichare, Ankush Bhaskar, Rahul Rawat, Virendra Yadav, Wageesh Mishra, Dorje Angchuk, Anand Kumar Singh
Figure caption: Electron flux (left) and proton flux (right) of various energies in the GMLat–GGLon frame. The color scale is the same in all the plots. The start and end of each satellite trajectory are indicated by Ⓢ and ﹩\varnothing ﹩ symbols, respectively.
Paper: Low-latitude Auroras: Insights from 2023 April 23 Solar Storm
Authors: Geeta Vichare, Ankush Bhaskar, Rahul Rawat, Virendra Yadav, Wageesh Mishra, Dorje Angchuk, Anand Kumar Singh
Figure caption: Trajectories (GMLat–time frame) of various NOAA (N15, N18, N19) and Metop1 satellites during 19–20 UT on 2023 April 23.
Paper: Low-latitude Auroras: Insights from 2023 April 23 Solar Storm
Authors: Geeta Vichare, Ankush Bhaskar, Rahul Rawat, Virendra Yadav, Wageesh Mishra, Dorje Angchuk, Anand Kumar Singh
Figure caption: (a) Total particle flux over the Northern Hemisphere in the entire low-energy band for electrons and ions. (b) Energy–time spectra for electrons. (c) Energy–time spectra for ions during 19:07–19:23 UT on 2023 April 23.
Paper: Low-latitude Auroras: Insights from 2023 April 23 Solar Storm
Authors: Geeta Vichare, Ankush Bhaskar, Rahul Rawat, Virendra Yadav, Wageesh Mishra, Dorje Angchuk, Anand Kumar Singh
Figure caption: (a) Total particle flux over the Southern Hemisphere in the entire low-energy band for electrons and ions. (b) Energy–time spectra for electrons. (c) Energy–time spectra for ions during 19:38–19:58 UT on 2023 April 23.
Paper: The AH Pictoris Syndrome: Continuous Trains of Stunted Outbursts in Novalike Variables
Authors: Albert Bruch
Figure caption: Light curves of AH Pic. On the left TESS data taken in Sectors 1–13, 27–39 (with a gap corresponding to Sector 36), and Sectors 61–67, respectively, are shown. The upper panel on the right contains the full ∼10 yr ASAS-SN light curve, while the other panels show the seasonal light curves on an expanded timescale. Blue and red dots refer to the V and g bands, respectively. Thin broken lines between the data points are meant to guide the eye.
Paper: The AH Pictoris Syndrome: Continuous Trains of Stunted Outbursts in Novalike Variables
Authors: Albert Bruch
Figure caption: TESS light curves of V1116 Cep, CM Del, V2837 Ori, FY Per, and KIC 9202990.
Paper: The AH Pictoris Syndrome: Continuous Trains of Stunted Outbursts in Novalike Variables
Authors: Albert Bruch
Figure caption: ASAS-SN light curve of PS Eri, structured in the same way as the right side of Figure 1. In the lower frames some deep dips in the light curve are truncated.
Paper: The AH Pictoris Syndrome: Continuous Trains of Stunted Outbursts in Novalike Variables
Authors: Albert Bruch
Figure caption: ASAS-SN light curve of CM Del, structured in the same way as the right side of Figure 1.
Paper: The AH Pictoris Syndrome: Continuous Trains of Stunted Outbursts in Novalike Variables
Authors: Albert Bruch
Figure caption: Power spectra of the SWASP light curve of PS Eri of the (from left to right) the 2006, the 2006 + 2007, and the 2007 observing seasons in a narrow range around a short-term period possibly caused by superhumps with a slightly different frequency in the two seasons.
Paper: The AH Pictoris Syndrome: Continuous Trains of Stunted Outbursts in Novalike Variables
Authors: Albert Bruch
Figure caption: AAVSO and ASAS-SN light curves of V1116 Cep, structured in the same way as Figure 1.
Paper: Photochemical Hazes in Exoplanetary Skies with Diamonds: Microphysical Modeling of Haze Composition Evolution via Chemical Vapor Deposition
Authors: Kazumasa Ohno
Figure caption: (Left) Real and imaginary refractive indices, n and k, of hydrogenated diamonds mixed with soot as a function of wavelengths. Different colored lines show the indices for different soot volume fraction f soot = 1 − f dia. (Right) Extinction coefficient Q ext (top) and single scattering albedo (bottom) of a spherical particle made of a diamond–soot mixture for various soot volume fraction. The particle radius is set to r p = 0.03 μm.
Paper: A Dust Attenuation Model Inspired by the NIHAO-SKIRT-Catalog
Authors: Nicholas Faucher, Michael R. Blanton
Figure caption: Fits of dust attenuation models to face-on orientation of the attenuation curve in magnitudes from the simulated galaxy g5.02e11, allowing all parameters to be free in the fits. In this case, Calzetti has two free parameters, Power Law has six free parameters, Kriek and Conroy has six free parameters, Cardelli has seven free parameters, and the TEA model has three free parameters.
Paper: A Dust Attenuation Model Inspired by the NIHAO-SKIRT-Catalog
Authors: Nicholas Faucher, Michael R. Blanton
Figure caption: RMSEs of the dust attenuation model fits for the face-on (left) and edge-on (right) orientations of the simulated galaxies’ attenuation curves in magnitudes, allowing all parameters to be free.
Paper: A Dust Attenuation Model Inspired by the NIHAO-SKIRT-Catalog
Authors: Nicholas Faucher, Michael R. Blanton
Figure caption: Similar to Figure 2, but now not allowing any fraction of the stellar light to reach the observer unattenuated. In this case, Calzetti has one free parameter, Power Law has four free parameters, Kriek and Conroy has four free parameters, Cardelli has five free parameters, and the TEA model has three free parameters.
Paper: A Dust Attenuation Model Inspired by the NIHAO-SKIRT-Catalog
Authors: Nicholas Faucher, Michael R. Blanton
Figure caption: Visualization of TEA model attenuation curves in magnitudes over a range of parameters.
Paper: A Dust Attenuation Model Inspired by the NIHAO-SKIRT-Catalog
Authors: Nicholas Faucher, Michael R. Blanton
Figure caption: Similar to Figure 3, but now with the RMSEs shifted by the TEA model’s RMSE for each galaxy.
Paper: Photochemical Hazes in Exoplanetary Skies with Diamonds: Microphysical Modeling of Haze Composition Evolution via Chemical Vapor Deposition
Authors: Kazumasa Ohno
Figure caption: Same as Figure 11, but I used the optical constants of meteoric diamonds (H. Mutschke et al. 2004) as an example of diamond hazes with impurities.
Paper: A Dust Attenuation Model Inspired by the NIHAO-SKIRT-Catalog
Authors: Nicholas Faucher, Michael R. Blanton
Figure caption: Fits of the TEA model to commonly used dust model fits of the face-on orientation of attenuation curve in magnitudes from the simulated galaxy g5.02e11, allowing all parameters to be free in the fits. In this case, Calzetti has two free parameters, Power Law has six free parameters, Kriek and Conroy has six free parameters, Cardelli has seven free parameters, and the TEA model has three free parameters.
Paper: A Dust Attenuation Model Inspired by the NIHAO-SKIRT-Catalog
Authors: Nicholas Faucher, Michael R. Blanton
Figure caption: Distribution of best-fitting ﹩{\mathrm{log}}_{10}({b}_{\mathrm{UV}}\,/\,{A}_{{\rm{V}}})﹩ and p parameters of the TEA model to the NIHAO-SKIRT-Catalog. Here we only include galaxies that have at least one orientation with an A V value greater than 0.2. We also include the equation for the best-fitting line in the legend.
Paper: A Dust Attenuation Model Inspired by the NIHAO-SKIRT-Catalog
Authors: Nicholas Faucher, Michael R. Blanton
Figure caption: Similar to Figure 8, but now not allowing any fraction of the stellar light to reach the observer unattenuated. In this case, Calzetti has one free parameter, Power Law has four free parameters, Kriek and Conroy has four free parameters, Cardelli has five free parameters, and TEA model has three free parameters.
Paper: A Dust Attenuation Model Inspired by the NIHAO-SKIRT-Catalog
Authors: Nicholas Faucher, Michael R. Blanton
Figure caption: Distribution of best-fitting p and ﹩{\mathrm{log}}_{10}({A}_{{\rm{V}}})﹩ parameters of the TEA model to the NIHAO-SKIRT-Catalog. Here we only include galaxies that have at least one orientation with an A V value greater than 0.05 mag. We also include the equation for the best-fitting line in the legend.
Paper: A Dust Attenuation Model Inspired by the NIHAO-SKIRT-Catalog
Authors: Nicholas Faucher, Michael R. Blanton
Figure caption: Comparison of the power-law index to UV-bump height correlation between the TEA model and the Kriek and Conroy model. For both models, we calculate the effective power-law index of the attenuation curves by performing a linear fit on log–log scale with the UV-bump regions masked out.
Paper: A Dust Attenuation Model Inspired by the NIHAO-SKIRT-Catalog
Authors: Nicholas Faucher, Michael R. Blanton
Figure caption: Similar to Figure 3, but now not allowing any fraction of the stellar light to reach the observer unattenuated.
Paper: A Dust Attenuation Model Inspired by the NIHAO-SKIRT-Catalog
Authors: Nicholas Faucher, Michael R. Blanton
Figure caption: RMSEs of the TEA model fit to commonly used model fits for the face-on (left) and edge-on (right) orientations of the simulated galaxies’ attenuation curves in magnitudes.
Paper: A Dust Attenuation Model Inspired by the NIHAO-SKIRT-Catalog
Authors: Nicholas Faucher, Michael R. Blanton
Figure caption: Similar to Figure 9, but now not allowing any fraction of the stellar light to reach the observer unattenuated.
Paper: A Dust Attenuation Model Inspired by the NIHAO-SKIRT-Catalog
Authors: Nicholas Faucher, Michael R. Blanton
Figure caption: Similar to Figure 6, but now with the RMSEs shifted by the TEA model’s RMSE for each galaxy.
Paper: Exploring the Diversity of Faint Satellites in the M81 Group
Authors: Katya Gozman, Eric F. Bell, In Sung Jang, Jose Marco Arias, Jeremy Bailin, Roelof S. de Jong, Richard D'Souza, Oleg Y. Gnedin, Antonela Monachesi, Paul A. Price, Vaishnav V. Rao, Adam Smercina
Figure caption: Distribution of Local Volume dwarf galaxies and globular clusters in the M  V −r  h  plane. Gray ×’s are globular clusters, red circles are previously known M81 satellites not characterized in this paper from K. Chiboucas et al. (2013). ﹩r{\rm{^{\prime} }}﹩ magnitudes were converted to approximate V-band magnitudes using the formula from K. Chiboucas et al. (2009): ﹩{r}^{{\prime} }=V-0.84(V-R)+0.13﹩ (M. Fukugita et al. 1996) assuming (V − R) ∼ 0.6. All other colored points are from the Local Volume Database. The four galaxies highlighted in this work are shown as black circles with error bars. The conversion for r  h  from arcminutes to parsecs for these galaxies is done assuming the distance of M81, D = 3.6 Mpc. Points outlined in a pink oval are galaxies that are substantially elliptical (ϵ ≥ 0.55), which includes D1009+68 from this work, making it one of the most elliptical UFDs ever found.
Paper: Exploring the Diversity of Faint Satellites in the M81 Group
Authors: Katya Gozman, Eric F. Bell, In Sung Jang, Jose Marco Arias, Jeremy Bailin, Roelof S. de Jong, Richard D'Souza, Oleg Y. Gnedin, Antonela Monachesi, Paul A. Price, Vaishnav V. Rao, Adam Smercina
Figure caption: Color–magnitude diagrams for stars within 2a  h  of each satellite galaxy, as derived by the best-fit structural parameters. Points are color-coded by their completeness fraction (see Section 4). The overall 50% completeness limit is drawn as a dashed line. The best-fit 13 Gyr isochrone for each system is shown as a solid black line, with the metallicity derived from our RBF interpolation method. The region used to select RGB stars to use for structural parameter fitting is shown as a light gray box. Photometric errors are displayed as purple points on the left-hand side of each subplot.
Paper: Exploring the Diversity of Faint Satellites in the M81 Group
Authors: Katya Gozman, Eric F. Bell, In Sung Jang, Jose Marco Arias, Jeremy Bailin, Roelof S. de Jong, Richard D'Souza, Oleg Y. Gnedin, Antonela Monachesi, Paul A. Price, Vaishnav V. Rao, Adam Smercina
Figure caption: Top: HST/ACS F814W images of our four dwarfs. The best-fit ellipses representing 2a  h  are shown in red for each galaxy. Bottom: a map of the M81 group and select satellite galaxies. The background image is composed of images generated by Aladin (F. Bonnarel et al. 2000), stacked to create a red, green, and blue frame using astropy’s make_lupton_rgb. White dots represent stellar halo stars identified in Subaru/HSC data. Satellites highlighted in this work are shown as red dots with white text, other satellites are marked with yellow dots and yellow text.
Paper: Exploring the Diversity of Faint Satellites in the M81 Group
Authors: Katya Gozman, Eric F. Bell, In Sung Jang, Jose Marco Arias, Jeremy Bailin, Roelof S. de Jong, Richard D'Souza, Oleg Y. Gnedin, Antonela Monachesi, Paul A. Price, Vaishnav V. Rao, Adam Smercina
Figure caption: Corner plots showing the posterior probability distributions for various fitted structural parameters in each satellite. The circularized half-light radius ﹩{r}_{h}={a}_{h}\sqrt{1-\epsilon }﹩ is displayed instead of just the fitted elliptical half-light radius a  h . The median values of each parameter along with their 16th and 84th percentile uncertainties are shown as red and dashed lines, respectively. Note that while we fit for N *, we instead display M  V , which is directly derived from N * using Equation (7) described in Section 5.3. The corner plot for D1006+69 also includes the fit for its Sérsic index.