adsabs/AstroCLIMB huggingface dataset:
Paper: Jupiter and Saturn as Spectral Analogs for Extrasolar Gas Giants and Brown Dwarfs
Authors: Daniel J. Coulter, Jason W. Barnes, Jonathan J. Fortney
Figure caption: Spectral comparison of two ring geometries: edge-on rings from cube V1518276136_1 (green) and rings at an inclination of approximately 20° from cube V1469259344_1 (magenta). Spectra with the rings and their shadows removed are shown for comparison.
Paper: Jupiter and Saturn as Spectral Analogs for Extrasolar Gas Giants and Brown Dwarfs
Authors: Daniel J. Coulter, Jason W. Barnes, Jonathan J. Fortney
Figure caption: Signal-to-noise ratio as a function of wavelength for both Jupiter and Saturn. As expected, the signal-to-noise ratio is very low in the major absorption bands.(The data used to create this figure are available.)
Paper: Multiple Stellar Populations of Globular Clusters from Homogeneous Ca–CN–CH–NH Photometry. VII. Metal-poor Populations in 47 Tucanae (NGC 104) 
Authors: Jae-Woo Lee
Figure caption: (a) Comparison of [Fe/H] of Carretta et al. (2009) against that of Codero et al. (2014) for 28 RGB stars in 47 Tuc in common between the two studies. The filled red circles indicate the RGB stars using the same instrument between the two studies. (b) Histogram of the [Fe/H] distribution by Codero et al. (2014). (c) Histogram of the [Fe/H] distribution by Carretta et al. (2009). (d) Histograms of the [Fe/H] measurements from literature. The red, blue, and green solid lines are for the RGB stars by Carretta et al. (2009), Codero et al. (2014), and Wang et al. (2017). The thick red dashed line is for the RHB stars by Gratton et al. (2013), while the thick blue dashed line is for the SGB stars by Marino et al. (2016). Except for the RGB [Fe/H] distribution by Carretta et al. (2009), the other four measurements show nonunimodal [Fe/H] distributions with large metallicity dispersions.
Paper: Multiple Stellar Populations of Globular Clusters from Homogeneous Ca–CN–CH–NH Photometry. VII. Metal-poor Populations in 47 Tucanae (NGC 104) 
Authors: Jae-Woo Lee
Figure caption: Parallelized CMDs with histograms for various color indices used in our study. Note that our y and ﹩\parallel \,{{cn}}_{\mathrm{JWL}}^{{\prime} }﹩ indices show discrete double RGB sequences in 47 Tuc. We also note that both the ∥(b− y) and ∥hk JWL, both of which are good metallicity indicators, show asymmetric distributions toward smaller color indices.
Paper: Multiple Stellar Populations of Globular Clusters from Homogeneous Ca–CN–CH–NH Photometry. VII. Metal-poor Populations in 47 Tucanae (NGC 104) 
Authors: Jae-Woo Lee
Figure caption: (a) Positions of bright stars with V ≤ 17 mag that match with the Gaia EDR3 and classified as 47 Tuc’s members. (b) Positions of bright stars with V ≤ 17 mag that match with the Gaia EDR3 but classified as 47 Tuc’s nonmembers. The thick red circle indicates the radial distance of 300″ from the cluster’s center. (c) Positions of bright stars with V ≤ 17 mag that have no counterpart in the Gaia EDR3. (d) (b − y) vs. V CMD for (a). (e) (b − y) vs. V CMD for (b). Note the presence of the SMC stars in the faint regime. The red dots show the CMD from stars located within 300″ from the center that are considered as proper-motion nonmembers of the cluster. (f) (b − y) vs. V CMD for stars with no Gaia EDR3 counterpart.
Paper: Multiple Stellar Populations of Globular Clusters from Homogeneous Ca–CN–CH–NH Photometry. VII. Metal-poor Populations in 47 Tucanae (NGC 104) 
Authors: Jae-Woo Lee
Figure caption: (a) A ﹩\parallel \,{{cn}}_{\mathrm{JWL}}^{{\prime} }﹩ vs. V CMD for the proper-motion member RGB stars (case (1)). The blue and red dots denote the CN-w and CN-s RGB stars in 47 Tuc returned from our EM estimator. (b) The black line denotes the ﹩{{cn}}_{\mathrm{JWL}}^{{\prime} }﹩ histogram of 47 Tuc RGB stars. The blue and red solid lines are the histograms returned from our EM estimator, and the gray solid line is for that of the total RGB population. (c) Same as (a) but for all RGB stars (case (2)). (d) Same as (b) but for all RGB stars.
Paper: Multiple Stellar Populations of Globular Clusters from Homogeneous Ca–CN–CH–NH Photometry. VII. Metal-poor Populations in 47 Tucanae (NGC 104) 
Authors: Jae-Woo Lee
Figure caption: CMDs for proper-motion membership stars in 47 Tuc. We also show the mean measurement uncertainties at a given V magnitude bin with blue error bars. Note the broad RGB sequences in m1, cy and the discrete double RGB sequences in ﹩{{cn}}_{\mathrm{JWL}}﹩ and ﹩{{cn}}_{\mathrm{JWL}}^{{\prime} }﹩ CMDs.
Paper: Multiple Stellar Populations of Globular Clusters from Homogeneous Ca–CN–CH–NH Photometry. VII. Metal-poor Populations in 47 Tucanae (NGC 104) 
Authors: Jae-Woo Lee
Figure caption: Gaia EDR3 proper motions of our FOV. The red ellipse indicates the boundary (3σ) of the 47 Tuc member stars shown with blue dots. The red dots are stars located within 300″ from 47 Tuc, and they are classified as nonmember stars based on the proper-motion study.
Paper: Multiple Stellar Populations of Globular Clusters from Homogeneous Ca–CN–CH–NH Photometry. VII. Metal-poor Populations in 47 Tucanae (NGC 104) 
Authors: Jae-Woo Lee
Figure caption: (a) A (b − y) vs. V CMD of the CN-s MP RHB stars in 47 Tuc. The vertical and horizontal thin lines are for the mean (b − y) and V of each population: orange (CN-s MP), dark-green (CN-s MR), and navy (CN-w). The thick magenta solid line represents the BaSTI HB isochrone for ([Fe/H], Y, age) = (−0.9, 0.257, 12.0 Gyr), while the green and yellow solid lines are for (−0.8, 0.275, 12.0 Gyr) and (−0.7, 0.300, 12.0 Gyr). We used the distance modulus of (m − M)0 = 13.21 mag and the interstellar reddening of E(B − V) = 0.03 mag (Brogaard et al. 2017). (b) Same as (a) but for the CN-s MR RHB stars. The thick cyan solid line represents the BaSTI HB isochrone for (−0.7, 0.275, 12.0 Gyr). (c) Same as (c) but for the CN-w RHB stars. The thick gray solid line represents the BaSTI HB isochrone for (−0.7, 0.257, 12.0 Gyr). (d)–(f) The (b − y) distributions of each population: orange (CN-s MP), dark-green (CN-s MR), and navy (CN-w). The dashed vertical lines denote the peak (b − y) values. (g) The V distributions of each population. The dashed horizontal lines denote the peak V magnitudes. (h) Synthetic HB models for the CN-s MP RHB stars using the BaSTI model isochrone for ([Fe/H], Y, age) = (−0.9, 0.257, 12.0 Gyr). (i) Same as (h) but for CN-s MR RHB stars using the BaSTI model isochrone for (−0.7, 0.275, 12.0 Gyr). (j) Same as (h) but for CN-w RHB stars using the BaSTI model isochrone for (−0.7, 0.257, 12.0 Gyr). (k)–(m) Same as (d)–(f) but for the mean distributions of 1000 synthetic model simulation runs. (n) Same as (g) but for the mean distributions of 1000 synthetic model simulation runs.
Paper: Multiple Stellar Populations of Globular Clusters from Homogeneous Ca–CN–CH–NH Photometry. VII. Metal-poor Populations in 47 Tucanae (NGC 104) 
Authors: Jae-Woo Lee
Figure caption: (a) A plot of hk JWL vs. ﹩{{cn}}_{\mathrm{JWL}}^{{\prime} }﹩ of the RHB stars in 47 Tuc, showing clustered distributions of the RHB stars. The gray solid line denotes the boundary between the CN-w(RHB) and CN-s(RHB) populations. The navy, dark-green, and orange plus signs are for the CN-w(RHB), CN-s MR(RHB), and CN-s MP(RHB), respectively. (b) The RHB distribution on the rotated plane, where the boundary between the two main bodies of the RHB stars in panel (a) is parallel to the vertical axis. (c) The histogram of the RHB stars along the x-axis, showing a distinctive bimodal distribution. We also show the results returned from our EM estimator. (d) The histogram of the CN-s(RHB) along the y-axis, showing an asymmetric distribution. We show the results from our EM estimator.
Paper: Multiple Stellar Populations of Globular Clusters from Homogeneous Ca–CN–CH–NH Photometry. VII. Metal-poor Populations in 47 Tucanae (NGC 104) 
Authors: Jae-Woo Lee
Figure caption: (a) CRDs of individual RHB populations (solid lines) along with the whole RGB populations (dashed lines). The blue, red, and pink solid lines are for the CN-w(RHB), CN-s MR(RHB), and CN-s MP(RHB) while the blue and red dashed lines are for the CN-w(RGB) and CN-s(RGB). The gray error bars show the fractions of the CN-w RHB population with a binning radial distance of the half-light radius, while the pink error bars show those of the CN-w RGB population. The vertical gray dashed lines denote the core and half-light radii of 47 Tuc. The green-shaded box indicates the fraction of the first generation by Milone et al. (2017) measured in the central part of the cluster. (b) Same as (a) but for the bright RGB stars with V ≤ 15.0 mag.
Paper: Multigroup Radiation Magnetohydrodynamics Based on Discrete Ordinates including Compton Scattering
Authors: Yan-Fei Jiang, 燕飞 姜
Figure caption: Spectrum of steady-state Bondi-type solution as described in Section 4.6 at radii r/r  B  = 0.2 (dashed black line), r/r  B  = 0.01 (dashed red line), and r/r  B  = 0.0012 (dashed green line). The monochromatic radiation energy density ﹩{E}_{r}(\tilde{\nu })﹩ is scaled with ﹩{E}_{r}/{\tilde{\nu }}_{0}﹩ at each radius. The solid blue line is a blackbody spectrum fitted to ﹩{E}_{r}(\tilde{\nu })﹩ at r/r  B  = 0.0012. The spectra at frequencies ﹩\tilde{\nu }\gt 1﹩ can be fitted with a power law ﹩{\tilde{\nu }}^{-2.4}﹩.
Paper: Multigroup Radiation Magnetohydrodynamics Based on Discrete Ordinates including Compton Scattering
Authors: Yan-Fei Jiang, 燕飞 姜
Figure caption: Spectra of the monochromatic radiation energy density from the surface of a column when total scattering optical depth varies from 300 to 10 as described in Section 4.4.4. The Compton y parameter varies from 15 to 0.05 correspondingly.
Paper: Multigroup Radiation Magnetohydrodynamics Based on Discrete Ordinates including Compton Scattering
Authors: Yan-Fei Jiang, 燕飞 姜
Figure caption: Radiation energy densities of the two frequency groups used in the shadow test described in Section 4.5. The top panel shows spatial distribution of radiation energy density E  r,0 in the first frequency group, which comes from thermal emission of the gas. The bottom panel shows the radiation energy density in the second frequency group E  r,1, which is dominated by radiation coming from the left boundary and casts shadows behind the cloud.
Paper: Multigroup Radiation Magnetohydrodynamics Based on Discrete Ordinates including Compton Scattering
Authors: Yan-Fei Jiang, 燕飞 姜
Figure caption: Spectrum of the spatially averaged monochromatic radiation energy density ﹩{E}_{r}(\tilde{\nu })﹩ resulting from the bulk Compton of a shear flow as described in Section 4.4.3. The black and red lines are for the initial blackbody spectrum and spectrum at time t = 2 corresponding to the Compton y parameter 2.76. The dashed green line is a spectrum with Bose–Einstein distribution at the effective temperature 1.99T based on Kaufman & Blaes (2016), where the gas temperature T = 1 in our unit system. We fix the chemical potential in the distribution based on the total radiation energy density of the numerical solution at this time.
Paper: Multigroup Radiation Magnetohydrodynamics Based on Discrete Ordinates including Compton Scattering
Authors: Yan-Fei Jiang, 燕飞 姜
Figure caption: Radial profiles of density (ρ, top panel), gas (P  g ) and radiation (P  r ) pressure (middle panel), inflow velocity (v  r ), and isothermal sound speed (c  s ) as defined by the total pressure (bottom panel) for the Bondi-type solution as described in Section 4.6. The solid lines are for the steady-state solution while the dashed lines are from the initial condition, which is calculated based on the classical Bondi solution. The dotted vertical line indicates the location of effective absorption photosphere for the frequency group centered at ﹩\tilde{\nu }=0.02﹩.
Paper: Multiple Stellar Populations of Globular Clusters from Homogeneous Ca–CN–CH–NH Photometry. VII. Metal-poor Populations in 47 Tucanae (NGC 104) 
Authors: Jae-Woo Lee
Figure caption: The (B − V), (B − I), and (U − V) CMDs using the multicolor photometry of Stetson et al. (2019) with three different radial zones, 60″ ≤ r < 200″ (zone (1)), 200″ ≤r < 400″ (zone (2)), and 400″ ≤r < 600″ (zone (3)), in 47 Tuc. Note that we used stars with low photometric measurement uncertainties, σ(B − V) ≤ 0.01 mag. The pink, navy, orange, and dark-green colors denote model isochrones with ([Fe/H], Y, CNO) = (−0.90 dex, 0.25, CN-w), (−0.70 dex, 0.25, CN-w), (−0.90 dex, 0.25, CN-s), and (−0.70 dex, 0.28, CN-s), respectively, for 12 Gyr.
Paper: Multiple Stellar Populations of Globular Clusters from Homogeneous Ca–CN–CH–NH Photometry. VII. Metal-poor Populations in 47 Tucanae (NGC 104) 
Authors: Jae-Woo Lee
Figure caption: (a) Plots of (B − V) vs. V CMD for the CN-w population using the photometric data by Stetson et al. (2019). The blue and red dots denote the CN-w MP and CN-w MR stars based on the ∥(B − V) distribution. The horizontal long-dashed lines and yellow boxes denote the V bump and measurement uncertainties for the CN-w MP (pink) and CN-w MR (navy) populations based on our own photometry. (b) Differential LFs of the CN-w MP (blue) and CN-w MR (red). The error bars denote the measurement uncertainties using the data by Stetson et al. (2019). (c) Same as (a) but for the CN-s population. (d) Same as (b) but for the CN-s population.
Paper: Multiple Stellar Populations of Globular Clusters from Homogeneous Ca–CN–CH–NH Photometry. VII. Metal-poor Populations in 47 Tucanae (NGC 104) 
Authors: Jae-Woo Lee
Figure caption: (a) A plot of V bump vs. [Fe/H] using the Y 2 isochrones for Y = 0.250, 0.275, and 0.300 along with those of four populations in 47 Tuc. The ΔV indicates the V magnitude offset in model isochrones to match our V bump magnitude the CN-w MR population. The colors are the same as Figure 7. (b) Same as (a) but using the PGPUC isochrones. (c) A plot of V bump vs. [Fe/H] using the BaSTI isochrones for Y = 0.255, 0.275, and 0.300. (d) A plot of (V bump − V TO) vs. [Fe/H] using the Y 2 isochrones. (e) Same as (d) but using the PGPUC isochrones. (f) Same as (d) but using the BaSTI isochrones.
Paper: Multiple Stellar Populations of Globular Clusters from Homogeneous Ca–CN–CH–NH Photometry. VII. Metal-poor Populations in 47 Tucanae (NGC 104) 
Authors: Jae-Woo Lee
Figure caption: Metallicity distributions of individual populations. The pink, navy, orange, and dark-green colors denote the CN-w MP, CN-w MR, CN-s MP, and CN-s MR, respectively. Gray color denotes the whole population. The error bars are for ± 1σ. In upper-left corner of panel (a), we show the measurement uncertainties (±1σ) using the bootstrap method, ± 0.019 dex.
Paper: Multiple Stellar Populations of Globular Clusters from Homogeneous Ca–CN–CH–NH Photometry. VII. Metal-poor Populations in 47 Tucanae (NGC 104) 
Authors: Jae-Woo Lee
Figure caption: (a) The moving average of the adjacent 50 points for the ﹩\parallel \,{{cn}}_{\mathrm{JWL}}^{{\prime} }﹩ index of the proper-motion member RGB stars plotted as functions of radial distance. The vertical thin gray error bars denote the standard error of the mean, and the vertical red dashed lines denote the core and the half-light radii of 47 Tuc. (b) Same as the top panel, but for [Fe/H]. (c) Same as (a) but for using all RGB stars. (d) Same as (b) but for using all RGB stars.
Paper: Multiple Stellar Populations of Globular Clusters from Homogeneous Ca–CN–CH–NH Photometry. VII. Metal-poor Populations in 47 Tucanae (NGC 104) 
Authors: Jae-Woo Lee
Figure caption: Plots of by 5 vs. V CMDs and differential LFs of individual populations. We show the mean RGBB V magnitudes of individual populations with gray dotted lines and those of individual populations with dotted lines with respective colors and yellow-shaded boxes. Note that the by 5 values are defined to be by 5 = 5 × (b − y) − 2.5 for the clarity of the figure.
Paper: Multiple Stellar Populations of Globular Clusters from Homogeneous Ca–CN–CH–NH Photometry. VII. Metal-poor Populations in 47 Tucanae (NGC 104) 
Authors: Jae-Woo Lee
Figure caption: CRDs of individual RGB populations. Colors for individual populations are the same as Figures 7 and 9, while the thick blue and red solid lines denote the whole CN-w and CN-s populations. The error bars show the fraction of the CN-w population with a binning radial distance of the half-light radius. The vertical gray dashed lines denote the core and the half-light radii of 47 Tuc. The green-shaded box indicates the fraction of the first generation by Milone et al. (2017), 0.175 ± 0.009, measured in the central part of the cluster, ∼3′ × 3′.
Paper: Multiple Stellar Populations of Globular Clusters from Homogeneous Ca–CN–CH–NH Photometry. VII. Metal-poor Populations in 47 Tucanae (NGC 104) 
Authors: Jae-Woo Lee
Figure caption: (a) A plot of [O/Fe] vs. [Na/Fe] of the RHB stars in 47 Tuc (Gratton et al. 2013). The blue and red dots denote RHB stars with [Na/O] ≤ 0.2 (i.e., equivalent to the CN-w), and > 0.2 dex (i.e., the CN-s), respectively. (b) A plot of (b − y) vs. ﹩{{cn}}_{\mathrm{JWL}}^{{\prime} }﹩ of the RHB stars in 47 Tuc along with RHB stars with [O/Fe] and [Na/Fe] measurements.
Paper: Multiple Stellar Populations of Globular Clusters from Homogeneous Ca–CN–CH–NH Photometry. VII. Metal-poor Populations in 47 Tucanae (NGC 104) 
Authors: Jae-Woo Lee
Figure caption: Comparisons of parallelized color indices of the proper-motion membership 47 Tuc RGB stars with −1.5 ≤ V − V HB ≤ 2.5 mag, showing that our four groups of stars are different stellar populations. Colors are the same as Figure 7.
Paper: Multigroup Radiation Magnetohydrodynamics Based on Discrete Ordinates including Compton Scattering
Authors: Yan-Fei Jiang, 燕飞 姜
Figure caption: Histories of total gas emissivity a rT  4 (the dotted black line) and radiation energy density in three frequency bins (E  r,0, E  r,1, E  r,2) for the thermal equilibrium test described in Section 4.1. In steady state, radiation energy densities match the integrated blackbody emission in each frequency bin as determined using the steady-state temperature.
Paper: Multigroup Radiation Magnetohydrodynamics Based on Discrete Ordinates including Compton Scattering
Authors: Yan-Fei Jiang, 燕飞 姜
Figure caption: Schematic illustrations of mapping comoving-frame specific intensities between two different sets of frequency grids. The top and bottom panels show two cases when the Lorentz transformation factor Γ(n, v) is larger and smaller than 1 respectively.
Paper: A Population of Dipper Stars from the Transiting Exoplanet Survey Satellite Mission
Authors: Benjamin K. Capistrant, Melinda Soares-Furtado, Andrew Vanderburg, Marina Kounkel, Saul A. Rappaport, Mark Omohundro, Brian P. Powell, Robert Gagliano, Thomas Jacobs, Veselin B. Kostov, Martti H. Kristiansen, Daryll M. LaCourse, Allan R. Schmitt, Hans Martin Schwengeler, Ivan A. Terentev
Figure caption: Our custom light curves corresponding to six on-target dipper candidates. Included are TICs 361818250, 954893801, 470475885, 904295318, 343564048, and 436650857. Light curves were generated after isolating candidates in their TPFs. We opted to illustrate a range of flux asymmetry M classifications as described in Section 3.2. The top two light curves are examples of the predominately “bursting” flux asymmetry (M < −0.25), rows three and four illustrate sources with “symmetric” flux asymmetry (−0.25 < M < 0.25) and the bottom two rows illustrate sources with predominately dipping flux asymmetry (M > 0.25). Only sources with M > 0.25 are classified as dippers in our resulting catalog.
Paper: A Population of Dipper Stars from the Transiting Exoplanet Survey Satellite Mission
Authors: Benjamin K. Capistrant, Melinda Soares-Furtado, Andrew Vanderburg, Marina Kounkel, Saul A. Rappaport, Mark Omohundro, Brian P. Powell, Robert Gagliano, Thomas Jacobs, Veselin B. Kostov, Martti H. Kristiansen, Daryll M. LaCourse, Allan R. Schmitt, Hans Martin Schwengeler, Ivan A. Terentev
Figure caption: Stellar ages (Myr) determined in this work by the Sagitta neural network (as described by McBride et al. 2021) plotted against the calculated flux asymmetry metric, M (upper left), and against the calculated periodicity metric, Q (upper right). In the bottom panels, we plot T eff against the M and Q metrics. The points are the true color a human eye would see if viewing a blackbody of that temperature (pixel red, green, blue (RGB) values are obtained from http://www.vendian.org/mncharity/dir3/blackbody/). We find no clear correlations between age or temperature of the source and the variability metrics of the catalog sources.
Paper: A Population of Dipper Stars from the Transiting Exoplanet Survey Satellite Mission
Authors: Benjamin K. Capistrant, Melinda Soares-Furtado, Andrew Vanderburg, Marina Kounkel, Saul A. Rappaport, Mark Omohundro, Brian P. Powell, Robert Gagliano, Thomas Jacobs, Veselin B. Kostov, Martti H. Kristiansen, Daryll M. LaCourse, Allan R. Schmitt, Hans Martin Schwengeler, Ivan A. Terentev
Figure caption: Top panel: ages for all of our dipper candidates (414 stars), as determined by the Sagitta neural network (McBride et al. 2021). Middle panel: ages for a subsample of our dipper candidates (68 stars), as derived by Kerr et al. (2021). Bottom panel: ages for the entire sample (25,324 stars) from Kerr et al. (2021) for comparison. In the top two panels, we fit the histograms with log-normal distributions to find the peak values, which we marked with a dashed red line. In the bottom panel, we used a kernel density estimate to determine the peak.
Paper: A Population of Dipper Stars from the Transiting Exoplanet Survey Satellite Mission
Authors: Benjamin K. Capistrant, Melinda Soares-Furtado, Andrew Vanderburg, Marina Kounkel, Saul A. Rappaport, Mark Omohundro, Brian P. Powell, Robert Gagliano, Thomas Jacobs, Veselin B. Kostov, Martti H. Kristiansen, Daryll M. LaCourse, Allan R. Schmitt, Hans Martin Schwengeler, Ivan A. Terentev
Figure caption: We plot the flux asymmetry (M) vs. periodicity (Q) metrics for our stellar variables (blue), comparing these sources to the young stellar variables analysed by Cody & Hillenbrand (2018) (red). Note that M is reflective of magnitude, and the sign of the variable is inverted from the intuitive value based on flux. Therefore, dipper stars have positive rather than negative M values. The majority of our catalog sources (70%) exhibit predominately dipping flux asymmetries. This is expected based on the search criteria of our visual survey of TESS light curves. In accordance with Cody & Hillenbrand (2018), we find no clear correlation between Q and M.
Paper: A Population of Dipper Stars from the Transiting Exoplanet Survey Satellite Mission
Authors: Benjamin K. Capistrant, Melinda Soares-Furtado, Andrew Vanderburg, Marina Kounkel, Saul A. Rappaport, Mark Omohundro, Brian P. Powell, Robert Gagliano, Thomas Jacobs, Veselin B. Kostov, Martti H. Kristiansen, Daryll M. LaCourse, Allan R. Schmitt, Hans Martin Schwengeler, Ivan A. Terentev
Figure caption: Scatter and contour plot illustrating the GBP – GRP color vs. IR excess for our dipper candidates (red points), which range between 2 and 42 Myr. A control sample of 392 sources from K21 are provided for comparison (blue points). A control star could be identified in the K21 sample for 93% of our dipper candidates. These comparison sources are close in age (within the K21 error bounds) to a given dipper candidate and have not been flagged as dipper variables in the past. We see that across all GBP – GRP values that our dipper candidates exhibit greater IR excess than the K21 control sample.