adsabs/AstroCLIMB huggingface dataset:
Paper: 3D Morphology and Motions of the Canis Major Region from Gaia DR3
Authors: Yiwei Dong, Ye Xu, Chaojie Hao, Yingjie Li, Dejian Liu, Yan Sun, Zehao Lin
Figure caption: Division of subregions of CMa. Black solid lines delineate the boundaries of seven subregions. Red stars denote the center of the CMa shell (B. Fernandes et al. 2019). (a) Velocity distribution map of 13CO. Black dashed circles mark H II regions (parameters from the Wide-field Infrared Survey Explorer (WISE) catalog; L. D. Anderson et al. 2014). (b) Locations of YSOs. The YSOs are displayed as circles color-coded by their parallaxes. The background gray contours delineate the regions traced by 13CO. (c) Motions of YSOs. Blue arrows represent residual tangential motions after subtracting the average motions of YSOs. (d) The average positions of 12CO, 13CO, C18O, and YSOs of subregions are shown as blue, green, red, and black crosses, respectively. Black arrows represent the average residual tangential velocities (converted to km s−1) of YSOs within subregions.
Paper: 3D Morphology and Motions of the Canis Major Region from Gaia DR3
Authors: Yiwei Dong, Ye Xu, Chaojie Hao, Yingjie Li, Dejian Liu, Yan Sun, Zehao Lin
Figure caption: 3D distributions and motions of the subregions. The red star at the origin of the coordinate system is the center of the CMa shell, and the positive directions of the x c, y c, and z c axes are consistent with the Galactic Cartesian coordinate system of M. J. Reid et al. (2019). The positions and motions of the subregions are marked with colored circles and black arrows, respectively. The circle colors are aligned with Figure 3, and the circle sizes are proportional to the logarithm of the molecular masses of the subregions (listed in Table 4). Upper panel: 3D view, with gray grid lines depicting a spherical shell with a radius of ∼47 pc. Lower panels: projected views on the x c–y c (left), x c–z c (middle), and y c–z c (right) planes. Red arrows indicate the line-of-sight direction. The averaged radial components of velocities of the subregions are indicated in the bottom right corners, with positive values pointing outwards and negative values pointing inwards.
Paper: 3D Morphology and Motions of the Canis Major Region from Gaia DR3
Authors: Yiwei Dong, Ye Xu, Chaojie Hao, Yingjie Li, Dejian Liu, Yan Sun, Zehao Lin
Figure caption: Parallaxes and proper motions of YSOs. Subregions A, B, C1, C2, D, E, and F are plotted in orange, red, dark green, light green, cyan, purple, and brown, respectively. Left: average values (crosses) and standard deviations (vertical bars) of parallaxes. Right: distribution of YSOs in the proper motion space.
Paper: 3D Morphology and Motions of the Canis Major Region from Gaia DR3
Authors: Yiwei Dong, Ye Xu, Chaojie Hao, Yingjie Li, Dejian Liu, Yan Sun, Zehao Lin
Figure caption: Gas column density features of the CMa region. Left panel: distribution of ﹩{N}_{{{\rm{H}}}_{2}}﹩ traced by 12CO, with the center of the CMa shell marked by a red star. Red arrows represent the six directions for P–﹩{N}_{{{\rm{H}}}_{2}}﹩ slicing. Right panels: column density profiles along the six directions, arranged in order of the arrows in the left panel, with the blue, green, and red lines depicting ﹩{N}_{{{\rm{H}}}_{2}}﹩ traced by 12CO, 13CO, and C18O, respectively.
Paper: 3D Morphology and Motions of the Canis Major Region from Gaia DR3
Authors: Yiwei Dong, Ye Xu, Chaojie Hao, Yingjie Li, Dejian Liu, Yan Sun, Zehao Lin
Figure caption: The sum of the distances between the seven subregions Σd(i, j) as a function of evolutionary time, normalized by its maximum value. The red shaded area represents the standard deviations of the Monte Carlo sampling. The time range is ±20 Myr with a step size of 0.1 Myr. The vertical dashed line marks the moment when Σd(i, j) reaches a minimum.
Paper: Erratum: “The Impact of the Free-floating Planet (FFP) Mass Function on the Event Rate for the Accurate Microlensing Parallax Determination: Application to Euclid and Roman Parallax Observation” (2023, AJ, 166, 250)
Authors: M. Ban
Figure caption: Event rate [event/year/deg2] for accurately measured microlensing parallax for different FFP mass functions. The FFP mass on the x-axis is binned by ﹩{{d}{\rm{l}}{\rm{o}}{\rm{g}}}_{10}{M}_{{\rm{FFP}}}\sim 0.1﹩. The least acceptable discrepancy is assumed as <100%, which corresponds to a factor of 2 uncertainty. The limitations of the finite source effect are ρ/u 0 < 0.5 in solid and <1.0 in dashed curves. Two solutions of the microlensing parallax are not considered in this plot and the δ u 0 is taken from a typical subtraction formula.
Paper: Erratum: “The Impact of the Free-floating Planet (FFP) Mass Function on the Event Rate for the Accurate Microlensing Parallax Determination: Application to Euclid and Roman Parallax Observation” (2023, AJ, 166, 250)
Authors: M. Ban
Figure caption: Three different FFP mass functions in the solid curves and the slope of the population factor as a power law (β) in Equation (18) in the dashed curves. The left y-axis corresponds to the mass function values, and the right y-axis corresponds to the β value.
Paper: UOCS XIV: Study of the Open Cluster NGC 2627 Using UVIT/AstroSat
Authors: Pinapati Saketh, Anju Panthi, Kaushar Vaidya
Figure caption: The optical and UV–optical CMDs of NGC 2627. The left panel shows the optical CMD with the cluster members determined using ML-MOC shown as blue dots. The membership probabilities of each of these sources are shown in the color bar. The sources observed in the UVIT/F148W filter are marked by magenta circles. The BSSs, YSSs, RC star, the BL candidate, and the binary candidates observed in UVIT are marked with different symbols as shown in the legend. The BSSs are labeled according to the coordinates given in Table 2. A PARSEC isochrone of age = 1.7 Gyr, and distance = 1.84 kpc, is shown as a black curve. An equal-mass binary isochrone obtained by adding 0.75 mag to the single isochrone is shown as a brown dashed curve. The right panel shows the UV–optical CMD of the cluster members detected in the UVIT/F148W filter. The membership probability of these sources is shown in the color bar. The BSSs, the YSS, the BL, the RC star, and the binary candidates are marked with the same symbols as in the optical CMD. A BaSTI isochrone of the same cluster parameters as used in the optical CMD is shown as a black curve after applying the extinction correction of A F148W = 0.356 and a reddening correction of E(F148W − G) = .0.262.
Paper: UOCS XIV: Study of the Open Cluster NGC 2627 Using UVIT/AstroSat
Authors: Pinapati Saketh, Anju Panthi, Kaushar Vaidya
Figure caption: The binary-component SEDs. In each upper panel, the blue data points indicate extinction-corrected flux values, with the black error bars representing flux errors. The green dashed line corresponds to the fit of the cool component, while the brown dashed line represents the fit for the hot components. Orange curves illustrate the iteration residuals. The composite fit is shown as a purple curve, and gray data points signify those not considered in the fits. VOSA does not consider these data points for fitting, due either to their bad photometry or to being the upper limits of the fluxes. Each bottom panel displays fractional residuals for single and composite fits. On the x-axis, black error bars denote fractional errors. The SED-derived parameters for the cool and hot components, along with their estimated errors, are shown at the top of the plots.
Paper: UOCS XIV: Study of the Open Cluster NGC 2627 Using UVIT/AstroSat
Authors: Pinapati Saketh, Anju Panthi, Kaushar Vaidya
Figure caption: The H-R diagram of NGC 2627. The left panel contains a PARSEC isochrone with an age of 1.77 Gyr and a distance of 1.84 kpc, along with a zero-age main sequence (ZAMS), which is constructed by stitching the ZAMS of log(age/yr) = 8.0, 8.5, and 9.0. We have shown the cool and hot companions of BSS3, the YSS, the RC star, and the binary candidates, along with the hot BSS companions of other open clusters. Moreover, the objects with a single-component fit in NGC 2627 are shown with the mentioned labels. The WD cooling curves of different masses are also shown as various gray curves. The right panel shows the hot companions of the above-mentioned objects lying on the cooling curves of WDs of different ages, indicating their approximate cooling ages.
Paper: UOCS XIV: Study of the Open Cluster NGC 2627 Using UVIT/AstroSat
Authors: Pinapati Saketh, Anju Panthi, Kaushar Vaidya
Figure caption: The spatial distribution, proper motion, and parallax distributions of the members and sample sources, determined using the ML-MOC algorithm.
Paper: UOCS XIV: Study of the Open Cluster NGC 2627 Using UVIT/AstroSat
Authors: Pinapati Saketh, Anju Panthi, Kaushar Vaidya
Figure caption: The cumulative radial distributions of equal-mass binary, massive single, and low-mass single populations. The BSSs are within a radius of 10r  c , shown by the brown dashed line. The x-axis represents the radial distance in units of the core radius, r  c , and the y-axis represents the normalized numbers of the three populations.
Paper: UOCS XIV: Study of the Open Cluster NGC 2627 Using UVIT/AstroSat
Authors: Pinapati Saketh, Anju Panthi, Kaushar Vaidya
Figure caption: The single-component SEDs. The upper panels show the extinction-corrected flux values, marked as blue squares, with the errors in fluxes shown as black bars. The purple curve represents the model fit. The data points that are not considered for fitting by VOSA are marked as gray dots. This is because these filters either have bad photometric data points or have upper limits of fluxes. The bottom panels show the residual between extinction-corrected observed fluxes and the model fluxes across the filters from UV to IR wavelengths.
Paper: UOCS XIV: Study of the Open Cluster NGC 2627 Using UVIT/AstroSat
Authors: Pinapati Saketh, Anju Panthi, Kaushar Vaidya
Figure caption: The radial density profile of the cluster members with membership probabilities greater than 0.8, with the error bars representing 1σ Poisson errors. In the bottom left corner, the parameters (normalization factor, core radius, and tidal radius) obtained from the fit with King’s function are shown.
Paper: Electron Density Distribution in H II Regions in IC 10
Authors: Fiorella L. Polles, Dario Fadda, William D. Vacca, Nicholas P. Abel, Mélanie Chevance, Christian Fischer, James M. Jackson, Vianney Lebouteiller, Suzanne Madden, Lise Ramambason
Figure caption: Intensity maps (watts per square meter per pixel) of IC 10. Top: Hα map with the regions observed in [O III] λ52 μm delineated in white (left), [O III] λ52 μm map (middle), [O III] λ88 μm map (right). Bottom: 24 μm map (left), 70 μm map (middle) and 100 μm map (right). The black circle in the lower left corner of each map corresponds to the beam of each observation. The spatial resolution is about 2.″2 for Hα, 6.″6 for [O III] λ52 μm, 9.″5 for [O III] λ88 μm, 6.″0 for 24 μm, 5.″6 for 70 μm, and 6.″8 for 100 μm.
Paper: Electron Density Distribution in H II Regions in IC 10
Authors: Fiorella L. Polles, Dario Fadda, William D. Vacca, Nicholas P. Abel, Mélanie Chevance, Christian Fischer, James M. Jackson, Vianney Lebouteiller, Suzanne Madden, Lise Ramambason
Figure caption: The white circles indicating the regions and subregions described in Section 3 overlap with the intensity maps (watt per square meter per pixel) of IC 10. Top: Hα map (left), [O III] λ52 μm map (middle), [O III] λ88 μm map (right). All three maps are shown at the spatial resolution of 9.″5. Bottom: [S III] λ18 μm map (left) and [S III] λ33 μm map (right), both shown at the spatial resolution of 12″.
Paper: Electron Density Distribution in H II Regions in IC 10
Authors: Fiorella L. Polles, Dario Fadda, William D. Vacca, Nicholas P. Abel, Mélanie Chevance, Christian Fischer, James M. Jackson, Vianney Lebouteiller, Suzanne Madden, Lise Ramambason
Figure caption: Left: increasing distribution of the 100 μm fluxes, with a zoom on the distribution showing the point where the emission starts to increase rapidly. The black line shows the upper limit of the fluxes used to calculate the foreground emission, while the red line corresponds to the derived foreground emission. Right: map of the continuum 100 μm emission showing only the pixels with a flux higher than the upper limit used to identify the “tail” (black line on the plot on the left).
Paper: Electron Density Distribution in H II Regions in IC 10
Authors: Fiorella L. Polles, Dario Fadda, William D. Vacca, Nicholas P. Abel, Mélanie Chevance, Christian Fischer, James M. Jackson, Vianney Lebouteiller, Suzanne Madden, Lise Ramambason
Figure caption: Gas temperature profiles calculated by the best-model solution of each of the H II regions studied. The depth is normalized to the value reached at the ionization front (DepthIF).
Paper: A Survey of Protoplanetary Disks Using the Keck/NIRC2 Vortex Coronagraph
Authors: Nicole L. Wallack, Jean-Baptiste Ruffio, Garreth Ruane, Bin B. Ren, 彬 任, Jerry W. Xuan, Marion Villenave, Dimitri Mawet, Karl Stapelfeldt, Jason J. Wang, Michael C. Liu, Olivier Absil, Carlos Alvarez, Jaehan Bae, Charlotte Bond, Michael Bottom, Benjamin Calvin, Élodie Choquet, Valentin Christiaens, Therese Cook, Bruno Femenía Castellá, Carlos Gomez Gonzalez, Greta Guidi, Elsa Huby, Joel Kastner, Heather A. Knutson, Tiffany Meshkat, Henry Ngo, Sam Ragland, Maddalena Reggiani, Luca Ricci, Eugene Serabyn, Taichi Uyama, Jonathan P. Williams, Peter Wizinowich, Zoe Zawol, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Expected planet masses from Wang et al. (2021; diamonds with no associated errors as none were reported) and Zhang et al. (2018; circles with their associated errors), using different values for the disk viscosity, α, are shown as black and gray points. We show our planet mass detection limits for comparison using the AMES-Cond models and AMES-Dusty models (when the masses were within the AMES-Dusty grid) for the subset of our systems observed as part of the DSHARP survey (Andrews et al. 2018) or the survey of the Taurus molecular cloud (Long et al. 2018). The bars therefore represent the range of masses that we would have been sensitive to given our observations. The ages of Elias 2–20 and Elias 2–24 are lower than the youngest age in the grids (1 Myr). Therefore, we show the masses assuming 1 Myr as upper limits to the ages, as younger systems would result in smaller masses.
Paper: Assessing Exoplanetary System Architectures with DYNAMITE Including Observational Upper Limits
Authors: Jamie Dietrich
Figure caption:  DYNAMITE predictions in orbital period space for tau Ceti where the planets have eccentric (top) and circular (bottom) orbits, as well as inclinations of 7° (left) and 35° (right). The eccentricity of the orbits plays a stronger role than the inclination (and therefore mass) of the planets for decreasing the stability of the system with an additional planet. As in Basant et al. (2022b), the habitable zone is plotted here as a function of age of the system (shown on the right vertical axis), to highlight the effect of the host star evolution on the habitable zone location.
Paper: A Survey of Protoplanetary Disks Using the Keck/NIRC2 Vortex Coronagraph
Authors: Nicole L. Wallack, Jean-Baptiste Ruffio, Garreth Ruane, Bin B. Ren, 彬 任, Jerry W. Xuan, Marion Villenave, Dimitri Mawet, Karl Stapelfeldt, Jason J. Wang, Michael C. Liu, Olivier Absil, Carlos Alvarez, Jaehan Bae, Charlotte Bond, Michael Bottom, Benjamin Calvin, Élodie Choquet, Valentin Christiaens, Therese Cook, Bruno Femenía Castellá, Carlos Gomez Gonzalez, Greta Guidi, Elsa Huby, Joel Kastner, Heather A. Knutson, Tiffany Meshkat, Henry Ngo, Sam Ragland, Maddalena Reggiani, Luca Ricci, Eugene Serabyn, Taichi Uyama, Jonathan P. Williams, Peter Wizinowich, Zoe Zawol, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Similar to Figure 9, expected planet masses from Wang et al. (2021; diamonds with no associated errors as none were reported) and Zhang et al. (2018; circles with their associated errors) for the subset of our systems observed as part of the DSHARP survey (Andrews et al. 2018) or the survey of the Taurus molecular cloud (Long et al. 2018) calculated using different values for the disk viscosity, α, are shown as black and gray points. We show the planet mass estimates derived from our 5σ contrast limits for comparison using the AMES-Cond models (Baraffe et al. 2003).
Paper: Assessing Exoplanetary System Architectures with DYNAMITE Including Observational Upper Limits
Authors: Jamie Dietrich
Figure caption:  DYNAMITE predictions in orbital period space for tau Ceti where the RV limit is 1 m s−1 (top) and 0.5 m s−1 (bottom) for planets with eccentric orbits and inclinations of 7° (left) as well as circular orbits with inclinations of 35° (right). The 1 m s−1 limits do not significantly change the predicted values from those made without limits, while the 0.5 m s−1 limits does cause a lower likelihood of a planet existing near a 10 day orbital period, near the location of planet candidate b from Tuomi et al. (2013). Habitable zones are shown like in Figure 1.
Paper: A Survey of Protoplanetary Disks Using the Keck/NIRC2 Vortex Coronagraph
Authors: Nicole L. Wallack, Jean-Baptiste Ruffio, Garreth Ruane, Bin B. Ren, 彬 任, Jerry W. Xuan, Marion Villenave, Dimitri Mawet, Karl Stapelfeldt, Jason J. Wang, Michael C. Liu, Olivier Absil, Carlos Alvarez, Jaehan Bae, Charlotte Bond, Michael Bottom, Benjamin Calvin, Élodie Choquet, Valentin Christiaens, Therese Cook, Bruno Femenía Castellá, Carlos Gomez Gonzalez, Greta Guidi, Elsa Huby, Joel Kastner, Heather A. Knutson, Tiffany Meshkat, Henry Ngo, Sam Ragland, Maddalena Reggiani, Luca Ricci, Eugene Serabyn, Taichi Uyama, Jonathan P. Williams, Peter Wizinowich, Zoe Zawol, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Upper limits on the mass accretion rates as a function of circumplanetary disk radius, R in, for the subset of our systems observed as part of the DSHARP survey (Andrews et al. 2018) or the survey of the Taurus molecular cloud (Long et al. 2018), derived from Zhu (2015) and determined from our contrast limits and masses from Wang et al. (2021; diamonds) and Zhang et al. (2018; circles) assuming a disk viscosity of α = 10−3.
Paper: A Survey of Protoplanetary Disks Using the Keck/NIRC2 Vortex Coronagraph
Authors: Nicole L. Wallack, Jean-Baptiste Ruffio, Garreth Ruane, Bin B. Ren, 彬 任, Jerry W. Xuan, Marion Villenave, Dimitri Mawet, Karl Stapelfeldt, Jason J. Wang, Michael C. Liu, Olivier Absil, Carlos Alvarez, Jaehan Bae, Charlotte Bond, Michael Bottom, Benjamin Calvin, Élodie Choquet, Valentin Christiaens, Therese Cook, Bruno Femenía Castellá, Carlos Gomez Gonzalez, Greta Guidi, Elsa Huby, Joel Kastner, Heather A. Knutson, Tiffany Meshkat, Henry Ngo, Sam Ragland, Maddalena Reggiani, Luca Ricci, Eugene Serabyn, Taichi Uyama, Jonathan P. Williams, Peter Wizinowich, Zoe Zawol, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Left: Locations of all point sources detected in our observations with S/N > 5. The central 0.″15 and separations >1.″6 are hatched and represent the regions where we do not search for point sources. The clustering of points in radial lines is likely due to diffraction from the telescope support structure. Right: A histogram, weighted by area, of the separations of the detected point sources.
Paper: A Survey of Protoplanetary Disks Using the Keck/NIRC2 Vortex Coronagraph
Authors: Nicole L. Wallack, Jean-Baptiste Ruffio, Garreth Ruane, Bin B. Ren, 彬 任, Jerry W. Xuan, Marion Villenave, Dimitri Mawet, Karl Stapelfeldt, Jason J. Wang, Michael C. Liu, Olivier Absil, Carlos Alvarez, Jaehan Bae, Charlotte Bond, Michael Bottom, Benjamin Calvin, Élodie Choquet, Valentin Christiaens, Therese Cook, Bruno Femenía Castellá, Carlos Gomez Gonzalez, Greta Guidi, Elsa Huby, Joel Kastner, Heather A. Knutson, Tiffany Meshkat, Henry Ngo, Sam Ragland, Maddalena Reggiani, Luca Ricci, Eugene Serabyn, Taichi Uyama, Jonathan P. Williams, Peter Wizinowich, Zoe Zawol, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Similar to Figure 5, but showing the mass estimates derived from our 5σ contrast curves for a number of different system ages for systems observed as part of the DSHARP survey (Andrews et al. 2018) or the survey of the Taurus molecular cloud (Long et al. 2018). We show the ALMA-derived planet masses (in M Jup) as the points with our mass estimates using the AMES-Cond model shown as bars colored by system age. We specify the radial locations of the gaps that we are probing as numbers (in au) above each system name.
Paper: A Survey of Protoplanetary Disks Using the Keck/NIRC2 Vortex Coronagraph
Authors: Nicole L. Wallack, Jean-Baptiste Ruffio, Garreth Ruane, Bin B. Ren, 彬 任, Jerry W. Xuan, Marion Villenave, Dimitri Mawet, Karl Stapelfeldt, Jason J. Wang, Michael C. Liu, Olivier Absil, Carlos Alvarez, Jaehan Bae, Charlotte Bond, Michael Bottom, Benjamin Calvin, Élodie Choquet, Valentin Christiaens, Therese Cook, Bruno Femenía Castellá, Carlos Gomez Gonzalez, Greta Guidi, Elsa Huby, Joel Kastner, Heather A. Knutson, Tiffany Meshkat, Henry Ngo, Sam Ragland, Maddalena Reggiani, Luca Ricci, Eugene Serabyn, Taichi Uyama, Jonathan P. Williams, Peter Wizinowich, Zoe Zawol, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Similar to Figure 6, but showing the mass estimates derived from our 5σ contrast curves for a number of different system ages. We show our mass estimates using the AMES-Cond model as bars colored by system age. We specify the radial locations of the gaps that we are probing as numbers (in au) above each system name. When ages produce mass limits outside of the AMES-Cond model grid, we do not show those limits.
Paper: Analysis of Ring Galaxies Detected Using Deep Learning with Real and Simulated Data
Authors: Harish Krishnakumar, J. Bryce Kalmbach
Figure caption: Nine of the GAN’s 20,000 generations. The identical background sources are discussed in Section 6.
Paper: Analysis of Ring Galaxies Detected Using Deep Learning with Real and Simulated Data
Authors: Harish Krishnakumar, J. Bryce Kalmbach
Figure caption: Frequency histogram of magnitudes in both samples of rings.
Paper: Analysis of Ring Galaxies Detected Using Deep Learning with Real and Simulated Data
Authors: Harish Krishnakumar, J. Bryce Kalmbach
Figure caption: An illustration of the architecture of a basic GAN with a discriminator and a generator.
Paper: Analysis of Ring Galaxies Detected Using Deep Learning with Real and Simulated Data
Authors: Harish Krishnakumar, J. Bryce Kalmbach
Figure caption: A galaxy misclassified as a ring.
Paper: Analysis of Ring Galaxies Detected Using Deep Learning with Real and Simulated Data
Authors: Harish Krishnakumar, J. Bryce Kalmbach
Figure caption: Color–mass diagram for FUV − r color for the newly identified sample of rings and the Galaxy Zoo 2 rings.
Paper: Analysis of Ring Galaxies Detected Using Deep Learning with Real and Simulated Data
Authors: Harish Krishnakumar, J. Bryce Kalmbach
Figure caption: Frequency histogram of masses for the newly identified sample of rings and the Galaxy Zoo 2 rings.
Paper: Analysis of Ring Galaxies Detected Using Deep Learning with Real and Simulated Data
Authors: Harish Krishnakumar, J. Bryce Kalmbach
Figure caption: Frequency histogram of redshifts for newly identified rings.
Paper: Analysis of Ring Galaxies Detected Using Deep Learning with Real and Simulated Data
Authors: Harish Krishnakumar, J. Bryce Kalmbach
Figure caption: 25 galaxies from the catalog of 1967 rings.
Paper: Analysis of Ring Galaxies Detected Using Deep Learning with Real and Simulated Data
Authors: Harish Krishnakumar, J. Bryce Kalmbach
Figure caption: The eCDF of the newly identified sample of rings and the Galaxy Zoo 2 rings.