adsabs/AstroCLIMB huggingface dataset:
Paper: Validating Stellar Abundance Measurements from Multiresolution Spectroscopy
Authors: Nathan R. Sandford, Daniel R. Weisz, Yuan-Sen Ting, 源森 丁
Figure caption: Same as Figure 9 except for Na, Al, K, and Sc (from top to bottom). We find poor and inconsistent recovery of [Na/H], [Al/H], and [K/H] at nearly all resolutions owing to the sparsity of absorption features. [Sc/H] is recovered consistently as a function of resolution with modest systematic uncertainties.
Paper: Analysis of SEP Events and Their Possible Precursors Based on the GSEP Catalog
Authors: Sumanth Rotti, Petrus C. Martens
Figure caption: Plots of parent eruptions followed by an SEP event on 2011 August 9 indexed as gsep_292 in the GSEP data set. (a) A solar flare of magnitude X6.9 seen in in 193 Å erupted from active region 11263 with spatial extents: lon = 69, lat = 17. Image courtesy of SDO/AIA. (b) A halo CME traveling at a mean speed of ≈1610 km s−1 was launched less than 4 minutes after the parent flare. Image courtesy of SOHO/LASCO-C2. (c) Proton intensity profile plot of the SEP event with a peak flux of 26 pfu in the E ≥10 MeV integral channel measured by the GOES-SEM suite.
Paper: Analysis of SEP Events and Their Possible Precursors Based on the GSEP Catalog
Authors: Sumanth Rotti, Petrus C. Martens
Figure caption: Plots of parent eruptions followed by an SEP event on 2014-04-18 indexed as gsep_330 in the GSEP data set. (a) A solar flare of magnitude M7.3 erupted from active region 12033 with spatial extents: lon = 34, lat = −20. Image courtesy of SDO/AIA. (b) A halo CME traveling at a mean speed of ≈1203 km s−1 was launched less than 3 minutes after the parent flare. Image courtesy of SOHO/LASCO. (c) Proton intensity profile plot of the SEP event with a peak flux of 58 pfu measured by the GOES-SEM instrument in the E ≥10 MeV integral channel.
Paper: Analysis of SEP Events and Their Possible Precursors Based on the GSEP Catalog
Authors: Sumanth Rotti, Petrus C. Martens
Figure caption: This plot shows the strength of solar activity in terms of SEP events between 1986 and 2017. A total of 163, 160, and 110 events have been identified in cycles 22, 23, and 24, respectively. In the legend, “large” events are defined as those crossing the SWPC threshold of 10 pfu in the E ≥10 MeV channel, and “weak” events are ≥0.5 pfu but <10 pfu.
Paper: S-type Stars from LAMOST DR10: Classification of Intrinsic and Extrinsic Stars
Authors: Jing Chen, Yin-Bi Li, A-Li Luo, Xiao-Xiao Ma, Shuo Li
Figure caption: The infrared color criteria from the decision tree with the highest accuracy of classification between intrinsic and extrinsic stars. The red and blue dots denote intrinsic and extrinsic S-type stars collected from literature, respectively. The red and blue areas represent the regions of intrinsic and extrinsic S-type stars, respectively, and the yellow areas indicate stars in them need further classification with the following diagrams. The dashed vertical and horizontal lines represent the color criteria to classify intrinsic and extrinsic S-type stars in different color–color diagrams.
Paper: S-type Stars from LAMOST DR10: Classification of Intrinsic and Extrinsic Stars
Authors: Jing Chen, Yin-Bi Li, A-Li Luo, Xiao-Xiao Ma, Shuo Li
Figure caption: The C/O distribution for 2920 S-type stars estimated by the MARCS S-type stars model.
Paper: S-type Stars from LAMOST DR10: Classification of Intrinsic and Extrinsic Stars
Authors: Jing Chen, Yin-Bi Li, A-Li Luo, Xiao-Xiao Ma, Shuo Li
Figure caption: The top 30 most important features chosen by the XGBoost method, and the horizontal axis shows their wavelengths.
Paper: S-type Stars from LAMOST DR10: Classification of Intrinsic and Extrinsic Stars
Authors: Jing Chen, Yin-Bi Li, A-Li Luo, Xiao-Xiao Ma, Shuo Li
Figure caption: ROC curves for the 15 input features mentioned in Section 3.1.2.
Paper: S-type Stars from LAMOST DR10: Classification of Intrinsic and Extrinsic Stars
Authors: Jing Chen, Yin-Bi Li, A-Li Luo, Xiao-Xiao Ma, Shuo Li
Figure caption: The most accurate decision tree of the XGBoost model in this work.
Paper: S-type Stars from LAMOST DR10: Classification of Intrinsic and Extrinsic Stars
Authors: Jing Chen, Yin-Bi Li, A-Li Luo, Xiao-Xiao Ma, Shuo Li
Figure caption: The spatial distribution of the 381 intrinsic and 495 extrinsic S-type stars, which were classified by the trained XGBoost model. The top panel shows the distribution on the Galactic plane, and the bottom panel shows the distribution above or below the Galactic disk. The green and pink dots represent extrinsic and intrinsic S-type stars, respectively, and the red star and filled plus denote the Sun and Galactic center, respectively.
Paper: S-type Stars from LAMOST DR10: Classification of Intrinsic and Extrinsic Stars
Authors: Jing Chen, Yin-Bi Li, A-Li Luo, Xiao-Xiao Ma, Shuo Li
Figure caption: The C/O distribution for 132 S-type stars with [C/Fe] and [O/Fe] of APOGEE DR17, and the red dashed line denotes C/O = 0.5.
Paper: S-type Stars from LAMOST DR10: Classification of Intrinsic and Extrinsic Stars
Authors: Jing Chen, Yin-Bi Li, A-Li Luo, Xiao-Xiao Ma, Shuo Li
Figure caption: Three example spectra of the 18 S-type stars with C/O < 0.5, which were estimated by [C/Fe] and [O/Fe] of APOGEE DR17.
Paper: S-type Stars from LAMOST DR10: Classification of Intrinsic and Extrinsic Stars
Authors: Jing Chen, Yin-Bi Li, A-Li Luo, Xiao-Xiao Ma, Shuo Li
Figure caption: Input features ranked based on their importance.
Paper: Chemical Differentiation around Five Massive Protostars Revealed by ALMA: Carbon-chain Species and Oxygen/Nitrogen-bearing Complex Organic Molecules
Authors: Kotomi Taniguchi, Liton Majumdar, Paola Caselli, Shigehisa Takakuwa, Tien-Hao Hsieh, Masao Saito, Zhi-Yun Li, Kazuhito Dobashi, Tomomi Shimoikura, Fumitaka Nakamura, Jonathan C. Tan, Eric Herbst
Figure caption: Plots of infrared fluxes and the modified blackbody models which can reproduce the observed fluxes best. Blue and orange curves indicate cold and warm components, respectively. Red curves show sums of the cold and warm components. Black points are data points taken from the archival data. T  c  and T  w  indicate temperatures of cold and warm components, respectively. Ω w /Ω c  indicates applied solid-angle ratios between warm and cold components.
Paper: Chemical Differentiation around Five Massive Protostars Revealed by ALMA: Carbon-chain Species and Oxygen/Nitrogen-bearing Complex Organic Molecules
Authors: Kotomi Taniguchi, Liton Majumdar, Paola Caselli, Shigehisa Takakuwa, Tien-Hao Hsieh, Masao Saito, Zhi-Yun Li, Kazuhito Dobashi, Tomomi Shimoikura, Fumitaka Nakamura, Jonathan C. Tan, Eric Herbst
Figure caption: Comparisons of results obtained by chemical simulations with three different cosmic-ray ionization rates (red: 1.3 × 10−17 s−1, green: 3.0 × 10−16 s−1, blue: 4.0 × 10−14 s−1). The black dashed curves indicate the temperature.
Paper: Fantastic Fits with fantasy of Active Galactic Nuclei Spectra: Exploring the Fe II Emission near the Hα Line
Authors: Dragana Ilić, Nemanja Rakić, Luka Č. Popović
Figure caption: Partial Grotrian diagram for Fe II, showing the transitions considered in the presented model of Fe II emission in the wavelength range 3700–11000 Å. The upper levels u4(D, F, P) are populated by Lyα photons, from which the cascades to lower levels are shown: red lines show the NIR transitions (bumps at 9200 Å and 1 μm) and dark cyan lines represent the transitions in the optical band (centered at 4570 and 5270 Å, which are the two strongest bumps around Hβ). The gray lines represent the transitions responsible for populating the upper levels, mainly through UV emission, to illustrate the path.
Paper: Validating Stellar Abundance Measurements from Multiresolution Spectroscopy
Authors: Nathan R. Sandford, Daniel R. Weisz, Yuan-Sen Ting, 源森 丁
Figure caption: The T eff (top), ﹩\mathrm{log}g﹩ (middle), and [Fe/H] (bottom) measured for each of the eight stars in our sample using the full-spectrum fitting techniques presented in this paper (black stars). For comparison, we also plot the values for T eff, ﹩\mathrm{log}g﹩, and [Fe/H] reported in a representative sample of literature studies of the same stars (colored circles). In instances where studies report separate values for neutral and ionized atomic species, the ionized value is represented by an open circle. Error bars represent 1σ uncertainties when provided and are too small to be visible for our own measurement uncertainties. Scatter is added in the x-dimension for clarity; points are ordered from left to right in order of increasing mean observed wavelength. A key to the abbreviated references is provided in Table 9.
Paper: Fantastic Fits with fantasy of Active Galactic Nuclei Spectra: Exploring the Fe II Emission near the Hα Line
Authors: Dragana Ilić, Nemanja Rakić, Luka Č. Popović
Figure caption: Fe II model in the wavelength range 3700–11000 Å, with atomic groups indicated in the bottom panel. The position of the hydrogen Balmer and Paschen series are also indicated with the dashed vertical lines, whereas the shaded areas indicate the positions of iron bands used later in the analysis: Fe II blue (4340–4680 Å), Fe II green (5100–5600 Å), and Fe II red (6100–6650 Å).
Paper: Validating Stellar Abundance Measurements from Multiresolution Spectroscopy
Authors: Nathan R. Sandford, Daniel R. Weisz, Yuan-Sen Ting, 源森 丁
Figure caption: The detailed chemical composition of the eight M15 stars as measured in this study (black stars) and as reported in the literature (colored circles; the same as in Figure 25). Ninety-five percent upper and lower limits are plotted where appropriate (see Section 3.3.4) and when reported by the literature. As in Figure 25, when separate abundances are provided for neutral and ionized atomic species, the ionized values are represented with open circles. Scatter is added in the x-dimension for clarity; points are ordered from left to right in order of increasing mean observed wavelength.
Paper: Fantastic Fits with fantasy of Active Galactic Nuclei Spectra: Exploring the Fe II Emission near the Hα Line
Authors: Dragana Ilić, Nemanja Rakić, Luka Č. Popović
Figure caption: Comparison of the Fe II model (black solid line) in the wavelength range 7000–11000 Å, with the Fe II model provided for the wavelength range 8200–11400 Å in Garcia-Rissmann et al. (2012; red dashed line, see text for details). The position of the Fe II lines identified in Landt et al. (2008) and Marinello et al. (2020) are marked with vertical lines.
Paper: Fantastic Fits with fantasy of Active Galactic Nuclei Spectra: Exploring the Fe II Emission near the Hα Line
Authors: Dragana Ilić, Nemanja Rakić, Luka Č. Popović
Figure caption: Distribution of the SDSS sample of 655 objects with cosmological redshift (upper panel) and continuum luminosity at 5100 Å (bottom panel) presented with stacked bars showing the pop A (red) and pop B (blue) subsamples.
Paper: Fantastic Fits with fantasy of Active Galactic Nuclei Spectra: Exploring the Fe II Emission near the Hα Line
Authors: Dragana Ilić, Nemanja Rakić, Luka Č. Popović
Figure caption: Different Fe II templates compared to the I Zw 1 spectrum from which the continuum emission was subtracted. The Fe II model presented here is the result of fitting the observations and also includes [Fe II] lines that are strong in this object (see Section 3.2.1 for details).
Paper: Fantastic Fits with fantasy of Active Galactic Nuclei Spectra: Exploring the Fe II Emission near the Hα Line
Authors: Dragana Ilić, Nemanja Rakić, Luka Č. Popović
Figure caption: Comparison of the semiempirical Fe II model presented in Kovačević et al. (2010) and Shapovalova et al. (2012) with the model of Fe II emission presented in this work, which relies solely on atomic data.
Paper: Panchromatic Photometry of Low-redshift, Massive Galaxies Selected from SDSS Stripe 82
Authors: Yang A. Li, Luis C. Ho, Jinyi Shangguan, Ming-Yang Zhuang, Ruancun Li
Figure caption: Comparison between our measurements and the AllWISE measurements obtained from profile fitting (left) and elliptical aperture photometry (right) for (a) W1, (b) W2, (c) W3, and (d) W4. For W1 and W2, unresolved and resolved sources are plotted in black and gray points, respectively. The upper limits (S/N < 2) from our measurements are shown in red triangles. The upper panels show the differences between the two sets of measurements (this work − WISE). The dotted lines give the quadrature sum of the typical uncertainties of the two sets of measurements. The median and standard deviation derived through survival analysis are shown in the upper left of the bottom panels. For W1 and W2, the numbers in parentheses pertain to the resolved sources.
Paper: Panchromatic Photometry of Low-redshift, Massive Galaxies Selected from SDSS Stripe 82
Authors: Yang A. Li, Luis C. Ho, Jinyi Shangguan, Ming-Yang Zhuang, Ruancun Li
Figure caption: Comparison between the measurements and RF-predicted magnitudes of the test sample of stars. The median and standard deviation between the measurements and the prediction, as well as the R 2 score, are displayed in the upper-left corner of each panel. The red dashed line indicates the 1:1 relation. The color code indicates the number density of objects.
Paper: Panchromatic Photometry of Low-redshift, Massive Galaxies Selected from SDSS Stripe 82
Authors: Yang A. Li, Luis C. Ho, Jinyi Shangguan, Ming-Yang Zhuang, Ruancun Li
Figure caption: Flux recovery fractions from the PSF-fitting test described in Appendix B on (a) W3 and (b) W4 data. Galaxies with low (n < 3.5; blue) and high (n ≥ 3.5; red) Sérsic indices are shown as a function of effective radius R  e . We fit the relations with a linear function (dashed lines).
Paper: Panchromatic Photometry of Low-redshift, Massive Galaxies Selected from SDSS Stripe 82
Authors: Yang A. Li, Luis C. Ho, Jinyi Shangguan, Ming-Yang Zhuang, Ruancun Li
Figure caption: Comparison between our measurements and the measurements from the unWISE catalog for (a) W1, (b) W2, (c) W3, and (d) W4. The upper limits (S/N < 2) from our measurements are shown in red triangles. The upper panels show the differences between the two sets of measurements (this work − unWISE). The dotted lines give the quadrature sum of the typical uncertainties of the two sets of measurements. The median and standard deviation derived through survival analysis are shown in the upper left of the bottom panels.
Paper: Panchromatic Photometry of Low-redshift, Massive Galaxies Selected from SDSS Stripe 82
Authors: Yang A. Li, Luis C. Ho, Jinyi Shangguan, Ming-Yang Zhuang, Ruancun Li
Figure caption: Relation between Sérsic R  e  and Petrosian R 50 for our galaxies. The black dashed line is the 1-to-1 relation. The blue line indicates the best-fit linear relation.
Paper: Panchromatic Photometry of Low-redshift, Massive Galaxies Selected from SDSS Stripe 82
Authors: Yang A. Li, Luis C. Ho, Jinyi Shangguan, Ming-Yang Zhuang, Ruancun Li
Figure caption: Example of a target galaxy (marked by the red cross) blended with a bright star. The aperture of the galaxy (blue ellipse) encloses a significant fraction of the star.
Paper: Slow Solar Wind Connection Science during Solar Orbiter’s First Close Perihelion Passage
Authors: Stephanie L. Yardley, Christopher J. Owen, David M. Long, Deborah Baker, David H. Brooks, Vanessa Polito, Lucie M. Green, Sarah Matthews, Mathew Owens, Mike Lockwood, David Stansby, Alexander W. James, Gherardo Valori, Alessandra Giunta, Miho Janvier, Nawin Ngampoopun, Teodora Mihailescu, Andy S. H. To, Lidia van Driel-Gesztelyi, Pascal Démoulin, Raffaella D'Amicis, Ryan J. French, Gabriel H. H. Suen, Alexis P. Rouillard, Rui F. Pinto, Victor Réville, Christopher J. Watson, Andrew P. Walsh, Anik De Groof, David R. Williams, Ioannis Zouganelis, Daniel Müller, David Berghmans, Frédéric Auchère, Louise Harra, Udo Schuehle, Krysztof Barczynski, Éric Buchlin, Regina Aznar Cuadrado, Emil Kraaikamp, Sudip Mandal, Susanna Parenti, Hardi Peter, Luciano Rodriguez, Conrad Schwanitz, Phil Smith, Luca Teriaca, Cis Verbeeck, Andrei N. Zhukov, Bart De Pontieu, Tim Horbury, Sami K. Solanki, Jose Carlos del Toro Iniesta, Joachim Woch, Achim Gandorfer, Johann Hirzberger, David Orozco Súarez, Thierry Appourchaux, Daniele Calchetti, Jonas Sinjan, Fatima Kahil, Kinga Albert, Reiner Volkmer, Mats Carlsson, Andrzej Fludra, Don Hassler, Martin Caldwell, Terje Fredvik, Tim Grundy, Steve Guest, Margit Haberreiter, Sarah Leeks, Gabriel Pelouze, Joseph Plowman, Werner Schmutz, Sunil Sidher, William T. Thompson, Philippe Louarn, Andrei Federov
Figure caption: Panel (a) shows the projection of Solar Orbiter’s orbit in the ecliptic plane in geocentric solar ecliptic (GSE) coordinates, during long-term planning period number 6 (LTP6; from 2021 December 27 until 2022 April 11). This time period includes the three remote-sensing windows (yellow, red, and blue) during the first perihelion of Solar Orbiter. RSW1 and RSW2 refer to time period of the two remote-sensing windows of the slow wind SOOP in 2022 March. Panel (b) shows the remote-sensing observations and in situ measurements designed as part of the Slow Wind SOOP.
Paper: Ultradiffuse Galaxies (UDGs) with Hyper Suprime-Cam. I. Revised Catalog of Coma Cluster UDGs 
Authors: Jose Miguel G. Bautista, Jin Koda, Masafumi Yagi, Yutaka Komiyama, Hitomi Yamanoi
Figure caption: Step-by-step demonstration of our cleaning procedure for a UDG. Top: from left to right: none (original raw image), high brightness objects, smaller objects in isolation, and smaller objects on top of the UDG. Bottom: the removed objects.
Paper: Ultradiffuse Galaxies (UDGs) with Hyper Suprime-Cam. I. Revised Catalog of Coma Cluster UDGs 
Authors: Jose Miguel G. Bautista, Jin Koda, Masafumi Yagi, Yutaka Komiyama, Hitomi Yamanoi
Figure caption: Effect of cleaning on the ability of SEXTRACTOR to detect a UDG intact. (a) Raw image of a UDG before cleaning. (b) Corresponding segmentation map overlaid on the raw image. Different objects found by SEXTRACTOR are separated by color. The UDG is oversplit by the presence of objects on and around it. (c) Raw image after cleaning. (d) Corresponding segmentation map overlaid on the cleaned image. The UDG is now detected as a single object.
Paper: Ultradiffuse Galaxies (UDGs) with Hyper Suprime-Cam. I. Revised Catalog of Coma Cluster UDGs 
Authors: Jose Miguel G. Bautista, Jin Koda, Masafumi Yagi, Yutaka Komiyama, Hitomi Yamanoi
Figure caption: (a) Raw cutout of a UDG, (b) raw cutout with the mask of each contaminant overlaid (color coded), (c) modeled 2D Sérsic profile from GALFIT, and (d) residual image after subtracting the GALFIT model from the raw image.
Paper: Ultradiffuse Galaxies (UDGs) with Hyper Suprime-Cam. I. Revised Catalog of Coma Cluster UDGs 
Authors: Jose Miguel G. Bautista, Jin Koda, Masafumi Yagi, Yutaka Komiyama, Hitomi Yamanoi
Figure caption: Coverage of the Coma Cluster by HSC. The rough footprints of the camera for the seven pointings are shown in green. The red circle marks 3 Mpc, the virial radius of the cluster, in projected cluster radius.
Paper: Ultradiffuse Galaxies (UDGs) with Hyper Suprime-Cam. I. Revised Catalog of Coma Cluster UDGs 
Authors: Jose Miguel G. Bautista, Jin Koda, Masafumi Yagi, Yutaka Komiyama, Hitomi Yamanoi
Figure caption: Examples of objects removed during visual inspection. (a) A stellar halo, where the source star is beyond the left edge of the cutout. (b) A tidal feature associated to the large galaxy to the right top of the cutout. (c) Optical ghosts.
Paper: Ultradiffuse Galaxies (UDGs) with Hyper Suprime-Cam. I. Revised Catalog of Coma Cluster UDGs 
Authors: Jose Miguel G. Bautista, Jin Koda, Masafumi Yagi, Yutaka Komiyama, Hitomi Yamanoi
Figure caption: Comparison between the SEXTRACTOR-measured FWHM and the half light radius (FLUX_RADIUS with FLUX_FRAC = 0.5) for all detected objects (blue). Overplotted are catalog objects in the limited surface brightness range 25.5 ≤ 〈μ r〉eff ≤ 26 (yellow), to demonstrate the distribution of UDGs. Criteria 4 and 5 are the magenta lines.
Paper: Ultradiffuse Galaxies (UDGs) with Hyper Suprime-Cam. I. Revised Catalog of Coma Cluster UDGs 
Authors: Jose Miguel G. Bautista, Jin Koda, Masafumi Yagi, Yutaka Komiyama, Hitomi Yamanoi
Figure caption: Example contaminants left by cleaning. (a) A bright object whose outer emission is detected as a UDG. (b) An aggregation of compact objects that was detected as a UDG due to blending.
Paper: Ultradiffuse Galaxies (UDGs) with Hyper Suprime-Cam. I. Revised Catalog of Coma Cluster UDGs 
Authors: Jose Miguel G. Bautista, Jin Koda, Masafumi Yagi, Yutaka Komiyama, Hitomi Yamanoi
Figure caption: Example UDGs organized by r eff, r. Columns from left to right: UDGs larger than 1, 2, 3, and 4 kpc. DF44 is shown in the bottom of the third column (ID = 351). Each UDG’s ID number in this catalog is shown in the bottom right of each cutout.
Paper: Ultradiffuse Galaxies (UDGs) with Hyper Suprime-Cam. I. Revised Catalog of Coma Cluster UDGs 
Authors: Jose Miguel G. Bautista, Jin Koda, Masafumi Yagi, Yutaka Komiyama, Hitomi Yamanoi
Figure caption: Magnitudes of the r-band PSF components vs. Sérsic components from the Sérsic+PSF fitting. UDGs judged as nonnucleated by BIC are shown as black crosses, and nucleated UDGs are shown as blue dots. The m psf values of the latter are almost completely confined to m psf ≲ 26.0. When additional noise is included in the image before fitting, UDGs that are still classified as nucleated are marked with red open circles. With additional noise in the image, the upper limit on m psf has dropped to m psf ≲ 25.0.
Paper: Ultradiffuse Galaxies (UDGs) with Hyper Suprime-Cam. I. Revised Catalog of Coma Cluster UDGs 
Authors: Jose Miguel G. Bautista, Jin Koda, Masafumi Yagi, Yutaka Komiyama, Hitomi Yamanoi
Figure caption: Aperture color–magnitude diagram for UDGs (blue) in this work and SDSS galaxies (black) within a 4°×4° box around the Coma Cluster center and in the redshift range 0.018 ≤ z ≤ 0.028. The SDSS red sequence (red dashed line) is taken as the linear fit of the peak in the color distribution vs. m r per 0.5 mag bin. The red points and error bars show the typical error of this work.
Paper: Ultradiffuse Galaxies (UDGs) with Hyper Suprime-Cam. I. Revised Catalog of Coma Cluster UDGs 
Authors: Jose Miguel G. Bautista, Jin Koda, Masafumi Yagi, Yutaka Komiyama, Hitomi Yamanoi
Figure caption:  GALFIT r eff, r vs. m r for UDGs using a distance modulus of 35.05 (red crosses for r eff, r ≥ 1.5, blue crosses for 1.0 ≤ r eff, r <1.5). For comparison, we plot the r eff, r (expRad_R) vs. m r of SDSS DR17 galaxies (black dots) near the cluster redshift (0.01 ≤ z ≤ 0.04) in a 3° radius region around the cluster center. The cyan and orange shaded regions show the typical distributions for elliptical and dwarf galaxies, respectively.
Paper: Ultradiffuse Galaxies (UDGs) with Hyper Suprime-Cam. I. Revised Catalog of Coma Cluster UDGs 
Authors: Jose Miguel G. Bautista, Jin Koda, Masafumi Yagi, Yutaka Komiyama, Hitomi Yamanoi
Figure caption: Scatter plot of GALFIT (a) m, (b) r eff, and (c) q between the g- and r-band values. The Sérsic index in the g band is held fixed to the r-band value when performing the fit. Lines of equality (black dashes) are plotted for r eff and q, while the red dashed line is shifted by the median color of 0.55.
Paper: Ultradiffuse Galaxies (UDGs) with Hyper Suprime-Cam. I. Revised Catalog of Coma Cluster UDGs 
Authors: Jose Miguel G. Bautista, Jin Koda, Masafumi Yagi, Yutaka Komiyama, Hitomi Yamanoi
Figure caption: Comparison of best-fit GALFIT r-band (a) m, (b) r eff, and (c) n, when compact objects on top of the UDG are masked or unmasked. The blacked dashed lines have unit slope. Some of the parameters derived without the compact-object mask deviate from the line, and they tend to be skewed toward brighter and larger fits.
Paper: Ultradiffuse Galaxies (UDGs) with Hyper Suprime-Cam. I. Revised Catalog of Coma Cluster UDGs 
Authors: Jose Miguel G. Bautista, Jin Koda, Masafumi Yagi, Yutaka Komiyama, Hitomi Yamanoi
Figure caption: Same as Figure 23, but with the Sérsic index independent between the two bands. Red dots are 1σ outliers of the Sérsic index correlation plot. σ is calculated relative to the line of unity, except in panel (a) where it is relative to the line shifted by the median color of 0.55.