adsabs/AstroCLIMB huggingface dataset:
Paper: Water Shielding in the Terrestrial Planet-forming Zone: Implication for Inner Disk Organics
Authors: Sara E. Duval, Arthur D. Bosman, Edwin A. Bergin
Figure caption: 2D distributions of the inner 5 au of the disk showing the structure of the gas temperature and density, dust density, gas-to-dust ratio, and UV and X-ray radiation fields for the model with water UV shielding. The UV radiation field is relative to the interstellar radiation field (Draine 1978). The red line at z/r ∼ 0.15 signifies our estimation of the location of the IR-emitting layer.
Paper: 10 Yr Transformation of the Obscuring Wind in NGC 5548
Authors: Missagh Mehdipour, Gerard A. Kriss, Elisa Costantini, Liyi Gu, Jelle S. Kaastra, Hermine Landt, Junjie Mao
Figure caption: Illustration of the long-term transformation of the obscuring disk wind in NGC 5548. The outflowing streams from the disk have become more porous and permeable in 2022, hence the observed decline in the X-ray and UV covering fractions (C X and C UV). The originally continuous gas supply from the disk in 2013 has gradually become more intermittently powered by the disk.
Paper: Photobombing Earth 2.0: Diffraction-limit-related Contamination and Uncertainty in Habitable Planet Spectra
Authors: Prabal Saxena
Figure caption: Diffraction limit comparisons for future telescopes of 6 and 30 m mirror size at 200 nm and 2.5 μm vs. HZ widths and mid-HZ Earth-twin Hill radii for G2V, G9V, and K5V stars as a function of distance.
Paper: Photobombing Earth 2.0: Diffraction-limit-related Contamination and Uncertainty in Habitable Planet Spectra
Authors: Prabal Saxena
Figure caption: Time-series figures displaying which planets would fall into Earth’s PSF from 2020 to 2030 if observed by a 6 and 12 m telescope in the 0.76 μm/0.94 μm oxygen/water bands from different distances. The total yearly photobombing duration for each planet is given in Table 1.
Paper: Photobombing Earth 2.0: Diffraction-limit-related Contamination and Uncertainty in Habitable Planet Spectra
Authors: Prabal Saxena
Figure caption: Spectral contrast of a photobombed Venus Twin for different scenarios (left) and plausible orbital periods for potential photobombers of an Earth twin in the blue visible from 10 pc away (right).
Paper: Photobombing Earth 2.0: Diffraction-limit-related Contamination and Uncertainty in Habitable Planet Spectra
Authors: Prabal Saxena
Figure caption: Figures of spectral contrast in the visible (left) and near-infrared (right) of a photobombed Earth twin for different scenarios. Noise assumptions are given in config files in the supplementary .tar.gz package.
Paper: Observational Evidence for a Spin-up Line in the P–﹩\dot{P}﹩ Diagram of Millisecond Pulsars
Authors: Xiao-Jin Liu, Zhi-Qiang You, Xing-Jiang Zhu
Figure caption: The P–﹩\dot{P}﹩ diagram of the MSPs used in the analysis. The observed ﹩\dot{P}﹩ is shown by gray stars, while the corrected ﹩\dot{P}﹩ is shown by (filled) circles with error bars. The isolated and binary cluster MSPs are colored in green and red, respectively, while the Galactic-field pulsars are in purple. The orange and light blue bands are the 90% credible intervals of the spin-up line if we include or exclude two “anomalous” pulsars (J1823−3021A and J1824−2452A), respectively. The dashed line represents a constraint set by gravitational radiation, due to a minimum ellipticity ϵ = 10−9 (Woan et al. 2018) plotted assuming I = 1038 kg m2. The gray line with the shaded region indicates the pulsar death valley (Rudak & Ritter 1994). The P–﹩\dot{P}﹩ data to reproduce this plot are available at https://github.com/zhuxj1/MSPspinUp.
Paper: Observational Evidence for a Spin-up Line in the P–﹩\dot{P}﹩ Diagram of Millisecond Pulsars
Authors: Xiao-Jin Liu, Zhi-Qiang You, Xing-Jiang Zhu
Figure caption: Joint posterior distribution of the spin-up relation parameter ﹩{ \mathcal A }﹩ and the order of the magnetic multipole l. The solid line marks l = 1 corresponding to a pure magnetic dipole. The orange and blue contours are for the case where we include and exclude PSRs J1823−3021A and J1824−2452A, respectively.
Paper: Observational Evidence for a Spin-up Line in the P–﹩\dot{P}﹩ Diagram of Millisecond Pulsars
Authors: Xiao-Jin Liu, Zhi-Qiang You, Xing-Jiang Zhu
Figure caption: A comparison of the joint posterior distribution of ﹩{ \mathcal A }﹩ and l for different MSP spin period cuts. The blue contour is taken from Figure 2 (P < 30 ms), while the orange one is for a smaller sample with 109 pulsars of P < 10 ms. In both cases, PSRs J1823−3021A and J1824−2452A are excluded.
Paper: Observational Evidence for a Spin-up Line in the P–﹩\dot{P}﹩ Diagram of Millisecond Pulsars
Authors: Xiao-Jin Liu, Zhi-Qiang You, Xing-Jiang Zhu
Figure caption: Posterior distributions of the accretion parameters defined in Equation (3). Posteriors obtained using all of the P–﹩\dot{P}﹩ data are in orange, while those obtained by excluding PSRs J1823−3021A and J1824−2452A are in blue. The intervals on the 1D posterior distributions are at 1σ.
Paper: Direct-imaging Discovery and Dynamical Mass of a Substellar Companion Orbiting an Accelerating Hyades Sun-like Star with SCExAO/CHARIS 
Authors: Masayuki Kuzuhara, Thayne Currie, Takuya Takarada, Timothy D. Brandt, Bun'ei Sato, Taichi Uyama, Markus Janson, Jeffrey Chilcote, Taylor Tobin, Kellen Lawson, Yasunori Hori, Olivier Guyon, Tyler D. Groff, Julien Lozi, Sebastien Vievard, Ananya Sahoo, Vincent Deo, Nemanja Jovanovic, Kyohoon Ahn, Frantz Martinache, Nour Skaf, Eiji Akiyama, Barnaby R. Norris, Mickaël Bonnefoy, Krzysztof G. Hełminiak, Tomoyuki Kudo, Michael W. McElwain, Matthias Samland, Kevin Wagner, John Wisniewski, Gillian R. Knapp, Jungmi Kwon, Jun Nishikawa, Eugene Serabyn, Masahiko Hayashi, Motohide Tamura
Figure caption: Color–magnitude diagram comparing HIP 21152 B (red open circle) to other substellar objects. (Left) J − K vs. absolute J magnitude (M J) and (right) ﹩H-{L}^{{\prime} }﹩ vs. absolute ﹩{L}^{{\prime} }﹩ magnitude (﹩{M}_{{{\rm{L}}}^{{\prime} }}﹩). Triangle plots correspond to young or low surface-gravity MLT-type dwarfs. Some of the known representative substellar companions are shown by plots with 1σ error bars (data are from Dupuy & Liu 2012; Janson et al. 2013; Kuzuhara et al. 2013; De Rosa et al. 2016; Rajan et al. 2017; Best et al. 2020; Currie et al. 2020a); the planets around HR 8799 are indicated by the filled circles, which are made with the data from Marois et al. (2008), Metchev et al. (2009), Skemer et al. (2014), Currie et al. (2014), Zurlo et al. (2016), and the star’s 2MASS magnitudes (Skrutskie et al. 2006) from IRSA (Skrutskie et al. 2003). The distance-modulus values of the substellar companions are based on Bailer-Jones et al. (2021). All data of the MLT dwarfs are in the Maunakea Observatories passbands and taken from the compilations in Dupuy & Liu (2012), Leggett et al. (2010), and the database of Best et al. (2020). Star symbols represent the Hyades members (Banyan-Σ probabilities >80%): photometry, parallax, and membership data are from Lodieu et al. (2019) and Best et al. (2020).
Paper: Direct-imaging Discovery and Dynamical Mass of a Substellar Companion Orbiting an Accelerating Hyades Sun-like Star with SCExAO/CHARIS 
Authors: Masayuki Kuzuhara, Thayne Currie, Takuya Takarada, Timothy D. Brandt, Bun'ei Sato, Taichi Uyama, Markus Janson, Jeffrey Chilcote, Taylor Tobin, Kellen Lawson, Yasunori Hori, Olivier Guyon, Tyler D. Groff, Julien Lozi, Sebastien Vievard, Ananya Sahoo, Vincent Deo, Nemanja Jovanovic, Kyohoon Ahn, Frantz Martinache, Nour Skaf, Eiji Akiyama, Barnaby R. Norris, Mickaël Bonnefoy, Krzysztof G. Hełminiak, Tomoyuki Kudo, Michael W. McElwain, Matthias Samland, Kevin Wagner, John Wisniewski, Gillian R. Knapp, Jungmi Kwon, Jun Nishikawa, Eugene Serabyn, Masahiko Hayashi, Motohide Tamura
Figure caption: Images of HIP 21152 B (circled) detected from our SCExAO/CHARIS and Keck/NIRC2 data. The areas close to the central star are masked.
Paper: Discovery of a Bimodal Environmental Distribution of Compact Ellipticals in the Local Universe
Authors: Guangwen Chen, Hong-Xin Zhang, Xu Kong, Zesen Lin, Zhixiong Liang, Zuyi Chen, Yimeng Tang, Xinkai Chen
Figure caption: Upper panel: g-band absolute magnitude distributions for galaxies from the NASA Sloan Atlas catalog (NSA; Blanton et al. 2011) within the same redshift range as our sample for ordinary dwarf galaxies from Eigenthaler et al. (2018), and for CSSs in this work, are plotted as gray, green, and red histograms, respectively. Lower panel: R e–M  g  distribution. Red squares represent our CSSs and symbols with arrows attached indicate unresolved CSSs. The black contours enclose the central 68% and 95% of NSA galaxies. Only 3000 randomly chosen galaxies in the NSA catalog are plotted (gray dots). The green shaded region encloses 95% of ordinary dwarf galaxies. Nuclear star clusters (Brodie et al. 2011; Misgeld & Hilker 2011) are plotted as filled triangles. UCDs (Zhang et al. 2015; Liu et al. 2020; Saifollahi et al. 2021) and cEs (Huxor et al. 2013; Paudel et al. 2014; Guérou et al. 2015) are plotted as blue and purple dots, respectively. CSSs from Norris et al. (2014) are plotted as small brown squares. M32, M60-UCD1 (Strader et al. 2013), and M59-UCD3 (Liu et al. 2015b) are plotted as filled stars. The diagonal lines represent constant g-band surface brightness.
Paper: Discovery of a Bimodal Environmental Distribution of Compact Ellipticals in the Local Universe
Authors: Guangwen Chen, Hong-Xin Zhang, Xu Kong, Zesen Lin, Zhixiong Liang, Zuyi Chen, Yimeng Tang, Xinkai Chen
Figure caption: Normalized distribution of the environmental parameters of CSSs (red filled histogram) and control sample (gray hatched histogram). The left panel is for the projected distances to the nearest luminous neighboring galaxy selected with the default method described in the text, and the middle panel is for the projected distances to the nearest luminous neighboring galaxy selected with the method in Kim et al. (2020). The projected distances have been normalized by the virial radii of the selected nearest neighbors. The right panel shows the distributions of the projected number density of nearby galaxies. The best-fit Gaussian curves from the GMM fit to each sample are overplotted on the histograms. The inset figure in each panel shows the ΔBIC ≡ BIC(Component = n) − BIC(Component = 1) for a GMM fit with a different number n of components. See Section 3.1 for details of the environmental parameters plotted here.
Paper: Discovery of a Bimodal Environmental Distribution of Compact Ellipticals in the Local Universe
Authors: Guangwen Chen, Hong-Xin Zhang, Xu Kong, Zesen Lin, Zhixiong Liang, Zuyi Chen, Yimeng Tang, Xinkai Chen
Figure caption: Size–mass distribution of our CSSs. Iso-number density contours that enclose 68% of the field and satellite CSSs are overplotted with the same color scheme as the data points. The arrows indicate unresolved CSSs. Literature cEs (Guérou et al. 2015; Ferré-Mateu et al. 2018) and CSSs (Janz et al. 2016) are plotted as purple dots and brown squares, respectively. Lines of iso- ﹩{{\rm{\Sigma }}}_{{\rm{e}}}\equiv {M}_{\star }/(2\pi {R}_{{\rm{e}}}^{2})﹩ are indicated by brown slanted lines. The brown dashed line represents the maximum effective stellar mass density (﹩{{\rm{\Sigma }}}_{max}\simeq {10}^{5.5}{M}_{\odot }\,{{\rm{pc}}}^{-2}﹩) expected for CSSs in the local universe (Hopkins et al. 2010).
Paper: Discovery of a Bimodal Environmental Distribution of Compact Ellipticals in the Local Universe
Authors: Guangwen Chen, Hong-Xin Zhang, Xu Kong, Zesen Lin, Zhixiong Liang, Zuyi Chen, Yimeng Tang, Xinkai Chen
Figure caption: Comparison of the input and best-fit R  e  (by GALFIT) of mock galaxies. The squares correspond to mock galaxies with the same structural parameters with the cE NGC 5846cE, and the other symbols correspond to single-Sérsic mock galaxies with different Sérsic indices n. The same mock galaxies are put at a series of redshift, i.e., 0.1, 0.05, 0.02, 0.01, and 0.006. The filled (open) symbols correspond to GALFIT fitting with single (double) Sérsic functions. The vertical dashed lines indicate the R  e  measurement limit adopted in our work, which is about 1/3 × PSF FWHM. Note that a Gaussian distribution has R  e  ≃ 1/2 × FWHM.
Paper: Discovery of a Bimodal Environmental Distribution of Compact Ellipticals in the Local Universe
Authors: Guangwen Chen, Hong-Xin Zhang, Xu Kong, Zesen Lin, Zhixiong Liang, Zuyi Chen, Yimeng Tang, Xinkai Chen
Figure caption: Age−[Z/H] diagram. The median values of the field and satellite subsamples of our CSSs are shown as big filled squares. The contour curves enclose 68% of the CSSs in each of our subsamples. Literature CSSs (Janz et al. 2016) or cEs (Chilingarian & Zolotukhin 2015; Guérou et al. 2015; Ferré-Mateu et al. 2018; Kim et al. 2020) are plotted with symbols indicated in the legend. The error bars of the median values of our CSSs are determined by random resampling of the original subsamples with replacement for 1000 times.
Paper: Faculae Cancel out on the Surfaces of Active Suns
Authors: N.-E. Nèmec, A. I. Shapiro, E. Işık, K. Sowmya, S. K. Solanki, N. A. Krivova, R. H. Cameron, L. Gizon
Figure caption: Magnetic alteration of stellar brightness in Strömgren (b+y)/2 as a function of S-index. Plotted are 365 day binned values (blue dots; see the text) and standard deviations of brightness within each of the bins (vertical blue bars, which are mostly smaller than the dot size). The solid blue line gives the fit of the second-degree polynomial in the form of aS 2 + bS + c, with the coefficients of the fit shown in the legend. The horizontal black dashed line indicates the zero level, and the vertical gray dashed line points to the S-index value, at which the transition from faculae-to-spot magnetic alteration occurs. Vertical dotted gray lines indicated the minimum and maximum value of the calculations representing the Sun.
Paper: Faculae Cancel out on the Surfaces of Active Suns
Authors: N.-E. Nèmec, A. I. Shapiro, E. Işık, K. Sowmya, S. K. Solanki, N. A. Krivova, R. H. Cameron, L. Gizon
Figure caption: The dependence of the facular area coverage on that of spots as returned by our forward model (blue) and retrieved from solar observations (black). Dots represent 58 day binned values (see the text); the vertical lines represent the standard deviations in the corresponding bins. The solid curves represent least-squares fits with the function ﹩{A}_{f}=a\cdot \sqrt{{A}_{s}+c}+d﹩, and shaded areas are the 1σ uncertainties of the fits.
Paper: Faculae Cancel out on the Surfaces of Active Suns
Authors: N.-E. Nèmec, A. I. Shapiro, E. Işık, K. Sowmya, S. K. Solanki, N. A. Krivova, R. H. Cameron, L. Gizon
Figure caption: Δ[(b + y)/2]/ΔS plotted against the mean chromospheric activity expressed through ﹩\mathrm{log}R{{\prime} }_{{HK}}﹩. The blue and orange solid lines represent the modeled dependencies for i = 90° and i = 0°, respectively, while asterisks show the Lowell and Fairborn measurements (Radick et al. 2018). Black asterisks indicate stars with effective temperatures ±200 K around the solar value (5777 K) and with uncertainty in Δ[(b + y)/2]/ΔS (as indicated by the black bars) below 0.1. Gray asterisks depict the rest of the Lowell and Fairborn sample. The dashed horizontal line indicates the zero level, where the transition between faculae-to-spot dominated occurs, and the two vertical gray dashed lines indicate the minimum and maximum values of solar activity during cycle 22. The gray-shaded band shows the result of the Bayesian linear regression to the black asterisks using Gaussian priors for the parameters of a quadratic polynomial. The solid curve shows the maximum of the posteriori estimate and the shaded region represents the probability density of the posterior distribution. The dashed curves denote the 2σ posterior boundaries.
Paper: Faculae Cancel out on the Surfaces of Active Suns
Authors: N.-E. Nèmec, A. I. Shapiro, E. Işık, K. Sowmya, S. K. Solanki, N. A. Krivova, R. H. Cameron, L. Gizon
Figure caption: Similar to Figure 1, but the forward-modeled dependence is plotted for stars with different levels of magnetic activity. Panel (b) gives the fraction of faculae in total area of active regions as a function of the spot area.
Paper: Faculae Cancel out on the Surfaces of Active Suns
Authors: N.-E. Nèmec, A. I. Shapiro, E. Işık, K. Sowmya, S. K. Solanki, N. A. Krivova, R. H. Cameron, L. Gizon
Figure caption: Demonstration of the effect of flux cancellation on the magnetic field and facular area coverages. Shown are calculations with 1 (﹩\tilde{s}=﹩ 1, blue), 16 (﹩\tilde{s}=﹩ 16, orange), and 64 (﹩\tilde{s}=﹩ 64, orange) active regions. Panel (a) shows the evolution of the surface magnetic flux normalized to corresponding value at the moment of emergence (t = 0). Panel (b) shows the surface area coverage by faculae in percent. Panel (c) shows the ratios of facular coverages for ﹩\tilde{s}=﹩ 16 and ﹩\tilde{s}=﹩ 64 cases to that for ﹩\tilde{s}=﹩ 1 case (orange and green curves, respectively). Calculations are based on the magnetograms shown in Figure 5.
Paper: Theoretically Modeling Photoionized Regions with Fractal Geometry in Three Dimensions
Authors: Yifei Jin, 刈非 金, Lisa J. Kewley, Ralph S. Sutherland
Figure caption: Maps of fundamental parameters across the Z = 0 pc slice of the nebula. Gray contours indicate the distribution of the input of ISM density. We present maps of the dimensionless ionization parameter U, the electron temperature T  e , the electron density n  e  and the distribution of fluxes of the Hα, Hβ, [O III], [O I], [N II], and [S II] emission lines. The nebula is assumed to be at the distance of the Large Magellanic Cloud of 48.5 kpc.
Paper: Theoretically Modeling Photoionized Regions with Fractal Geometry in Three Dimensions
Authors: Yifei Jin, 刈非 金, Lisa J. Kewley, Ralph S. Sutherland
Figure caption: The comparison of diagnostic emission-line ratios from the fractal model against the spherical photoionization model. We employ the [N II]/Hα vs. [O III]/Hβ (left column), [S II]/Hα vs. [O III]/Hβ (middle column), and [O I]/Hα vs. [O III]/Hβ (right column) diagrams. The background grayscale indicates the number density of spaxels from the collapsed 2D map of the fractal model. The red stars are the spaxels from the imitated long-slit data of the spherical model. The solid line in each panel is the demarcation line given by Kewley et al. (2001) to separate star-forming galaxies/H II regions from AGNs. The dashed line in the [N II]/Hα vs. [O III]/Hβ panel is the demarcation line given by Kauffmann et al. (2003) to separate star-forming galaxies/H II regions from AGNs.
Paper: Theoretically Modeling Photoionized Regions with Fractal Geometry in Three Dimensions
Authors: Yifei Jin, 刈非 金, Lisa J. Kewley, Ralph S. Sutherland
Figure caption: Upper panel: the projected Hβ luminosity map of the 3D nebula with fractal geometry. Lower panel: the projected distribution of log-normally distributed ISM. The white curve outlines the shape of our modeled nebula. The ionizing source is at the center of the domain (indicated by the white star).
Paper: Theoretically Modeling Photoionized Regions with Fractal Geometry in Three Dimensions
Authors: Yifei Jin, 刈非 金, Lisa J. Kewley, Ralph S. Sutherland
Figure caption: The comparison of integrated emission-line fluxes and ratios between the fractal model and the spherical model. The emission lines are classified into three categories, which are the Balmer lines (gray shadow), the Volume species (blue shadow), and the Boundary species (red shadow). The black horizontal dashed line indicates no changes in the line fluxes and ratios between the fractal model and the spherical model.
Paper: Theoretically Modeling Photoionized Regions with Fractal Geometry in Three Dimensions
Authors: Yifei Jin, 刈非 金, Lisa J. Kewley, Ralph S. Sutherland
Figure caption: Spherical MAPPINGS V model. The spherical model has the same inputs as the fractal model except for the geometry. Here, we present the radial distribution of the [O III], [O I], [N II], and [S II] lines.
Paper: Direct-imaging Discovery and Dynamical Mass of a Substellar Companion Orbiting an Accelerating Hyades Sun-like Star with SCExAO/CHARIS 
Authors: Masayuki Kuzuhara, Thayne Currie, Takuya Takarada, Timothy D. Brandt, Bun'ei Sato, Taichi Uyama, Markus Janson, Jeffrey Chilcote, Taylor Tobin, Kellen Lawson, Yasunori Hori, Olivier Guyon, Tyler D. Groff, Julien Lozi, Sebastien Vievard, Ananya Sahoo, Vincent Deo, Nemanja Jovanovic, Kyohoon Ahn, Frantz Martinache, Nour Skaf, Eiji Akiyama, Barnaby R. Norris, Mickaël Bonnefoy, Krzysztof G. Hełminiak, Tomoyuki Kudo, Michael W. McElwain, Matthias Samland, Kevin Wagner, John Wisniewski, Gillian R. Knapp, Jungmi Kwon, Jun Nishikawa, Eugene Serabyn, Masahiko Hayashi, Motohide Tamura
Figure caption: The 2020 October JHK spectra of HIP 21152 B. (Left) The three lines correspond to the fiducial ADI, ASDI, and alternate ADI (labeled as “alt”) reductions. 1σ error bars are appended to the ADI spectra. (Right) Comparisons between the fiducial spectrum of HIP 21152 B (blue dashed lines) and three template spectra from the Montreal Spectral Library (gray solid lines). The wavelengths where telluric absorption is significant are masked and were not used in our spectral typing. The reduced chi-square values (﹩{\chi }_{\nu }^{2}﹩) computed by least-squares fitting (15 DOF = 16 data points minus 1 optimized parameter for spectrum scaling) are shown above each comparison with the names of the compared BDs and their spectral types.
Paper: Direct-imaging Discovery and Dynamical Mass of a Substellar Companion Orbiting an Accelerating Hyades Sun-like Star with SCExAO/CHARIS 
Authors: Masayuki Kuzuhara, Thayne Currie, Takuya Takarada, Timothy D. Brandt, Bun'ei Sato, Taichi Uyama, Markus Janson, Jeffrey Chilcote, Taylor Tobin, Kellen Lawson, Yasunori Hori, Olivier Guyon, Tyler D. Groff, Julien Lozi, Sebastien Vievard, Ananya Sahoo, Vincent Deo, Nemanja Jovanovic, Kyohoon Ahn, Frantz Martinache, Nour Skaf, Eiji Akiyama, Barnaby R. Norris, Mickaël Bonnefoy, Krzysztof G. Hełminiak, Tomoyuki Kudo, Michael W. McElwain, Matthias Samland, Kevin Wagner, John Wisniewski, Gillian R. Knapp, Jungmi Kwon, Jun Nishikawa, Eugene Serabyn, Masahiko Hayashi, Motohide Tamura
Figure caption: Corner plot showing MCMC posterior distributions of the host-star mass (M pri in units of M ⊙), companion mass (M                      ﹩{}_{\sec }﹩ in units of M Jup), semimajor axis (a), eccentricity (e), and inclination (i). HIDES RV measurements of HIP 21152 A (lower inset) and relative astrometry of HIP 21152 B from CHARIS and NIRC2 (upper inset) are shown, with the best-fit orbit (black solid line) along with 100 orbits randomly taken from our MCMC chains that are color-coded by HIP 21152 B’s mass corresponding to the color bars near the inset panels. See also Appendix D.2 for the fitting results to the other measurements.
Paper: Direct-imaging Discovery and Dynamical Mass of a Substellar Companion Orbiting an Accelerating Hyades Sun-like Star with SCExAO/CHARIS 
Authors: Masayuki Kuzuhara, Thayne Currie, Takuya Takarada, Timothy D. Brandt, Bun'ei Sato, Taichi Uyama, Markus Janson, Jeffrey Chilcote, Taylor Tobin, Kellen Lawson, Yasunori Hori, Olivier Guyon, Tyler D. Groff, Julien Lozi, Sebastien Vievard, Ananya Sahoo, Vincent Deo, Nemanja Jovanovic, Kyohoon Ahn, Frantz Martinache, Nour Skaf, Eiji Akiyama, Barnaby R. Norris, Mickaël Bonnefoy, Krzysztof G. Hełminiak, Tomoyuki Kudo, Michael W. McElwain, Matthias Samland, Kevin Wagner, John Wisniewski, Gillian R. Knapp, Jungmi Kwon, Jun Nishikawa, Eugene Serabyn, Masahiko Hayashi, Motohide Tamura
Figure caption: Common proper-motion analysis for HIP 21152 B. The projected separation (ρ) and position angle (PA) measurements for HIP 21152 B are shown at the top and bottom panels, respectively. The horizontal axes indicate the time elapsed from the 2020 October epoch. An expected motion assuming HIP 21152 B is a background star is shown by the solid lines encompassed by their 1σ errors (dashed lines). It is clearly demonstrated that HIP 21152 B cannot be a background star given the large difference between the expected background motion and the measured ρ and PA at the latest epoch (October 2021): 16σ in ρ and 11σ in PA.