adsabs/AstroCLIMB huggingface dataset:
Paper: The Stellar Disk Structure Revealed by the Mono-age Populations of the LAMOST Red Clump Star Sample
Authors: Zheng Yu, Bingqiu Chen, Jianhui Lian, Chun Wang, Xiaowei Liu
Figure caption: [Fe/H]–[α/Fe] distributions for our RC sample stars across two age populations: 0–3 Gyr (left column) and >9 Gyr (right column). The red demarcations in panels (a) and (b) distinguish the chemical thin and thick disk stars. Panels (c) and (e) respectively depict double exponential fits for high- and low-α sequences of the 0–3 Gyr population within the 9  < R <  10 kpc range. Similarly, panels (d) and (f), respectively, present double exponential fits for high- and low-α sequences of the >9 Gyr population.
Paper: The Stellar Disk Structure Revealed by the Mono-age Populations of the LAMOST Red Clump Star Sample
Authors: Zheng Yu, Bingqiu Chen, Jianhui Lian, Chun Wang, Xiaowei Liu
Figure caption: Fitting of vertical stellar number density for the mono-age population (5–7 Gyr) using a double exponential function. Each panel shows results for a specific Ri bin, marked at the top. Median values and standard errors in 100 pc wide vertical bins (Zbins) are depicted by blue lines and error bars, respectively. Red lines represent the best-fit curves.
Paper: The Stellar Disk Structure Revealed by the Mono-age Populations of the LAMOST Red Clump Star Sample
Authors: Zheng Yu, Bingqiu Chen, Jianhui Lian, Chun Wang, Xiaowei Liu
Figure caption: Distribution of stellar number density in the disk R–Z plane for different mono-age populations, indicated in the upper right corner of each panel. The density map uses a bin size of 0.125 × 0.125 kpc. Each panel represents a distinct age group, with density variations shown through a color gradient from blue (low density) to red (high density).
Paper: The Stellar Disk Structure Revealed by the Mono-age Populations of the LAMOST Red Clump Star Sample
Authors: Zheng Yu, Bingqiu Chen, Jianhui Lian, Chun Wang, Xiaowei Liu
Figure caption: Figures analogous to Figure 4 showing the fitting results of 0–3 Gyr mono-age populations.
Paper: The Stellar Disk Structure Revealed by the Mono-age Populations of the LAMOST Red Clump Star Sample
Authors: Zheng Yu, Bingqiu Chen, Jianhui Lian, Chun Wang, Xiaowei Liu
Figure caption: Figures analogous to Figure 4 showing the fitting results of 3–5 Gyr mono-age populations.
Paper: Atmospheric Mass Loss from TOI-1259 A b, a Gas Giant Planet with a White Dwarf Companion
Authors: Morgan Saidel, Shreyas Vissapragada, Jessica Spake, Heather A. Knutson, Dion Linssen, Michael Zhang, Michael Greklek-McKeon, Jorge Pérez-González, Antonija Oklopčić
Figure caption: Top: excess absorption of TOI-1259 A b, in percent, in the planetary rest frame as a function of time and wavelength, as observed with Keck/NIRSPEC. The white horizontal lines mark the beginning (bottom) and end (top) of transit. The red vertical dashed lines mark the locations of the three helium lines. We mask out strong telluric and stellar lines as part of our analysis, which are seen as gaps at 1.0830057 μm (stellar silicon line) and 1.08351 μm (water line). Bottom: excess absorption spectra in the planetary rest frame as a function of wavelength. The black line represents the excess absorption spectrum calculated using all in-transit data (T1–T4). The gray line represents the average excess absorption spectrum calculated for the time period where the planet is fully in front of the star (T2–T3). Representative error bars for each spectrum are shown in the upper left corner.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Atmospheric Mass Loss from TOI-1259 A b, a Gas Giant Planet with a White Dwarf Companion
Authors: Morgan Saidel, Shreyas Vissapragada, Jessica Spake, Heather A. Knutson, Dion Linssen, Michael Zhang, Michael Greklek-McKeon, Jorge Pérez-González, Antonija Oklopčić
Figure caption: Mass vs. period distribution for the sample of confirmed exoplanets as drawn from the NASA Exoplanet Archive on 2024 January 23 (R. L. Akeson et al. 2013; NASA Exoplanet Archive 2024). The boundaries of the Neptune desert from T. Mazeh et al. (2016) are overplotted as black dotted lines. Green points indicate planets with published detections of atmospheric escape using the helium line, red points indicate published nondetections, and yellow points denote tentative detections. The location of TOI-1259 A b is indicated by a green star. Each point's size is scaled based on the host star's J magnitude (except for TOI-1259, which has a J magnitude of 10.2). For a full list of planets see G. Guilluy et al. (2023) and the review by L. A. Dos Santos (2023); we also include detections for TOI-1268 b (J. Pérez González et al. 2023), HAT-P-67 b (M. Gully-Santiago et al. 2023), and TOI-2134 b (M. Zhang et al. 2023) and the nondetection for LTT 9779 b (B. Edwards et al. 2023; S. Vissapragada et al. 2024).
Paper: Atmospheric Mass Loss from TOI-1259 A b, a Gas Giant Planet with a White Dwarf Companion
Authors: Morgan Saidel, Shreyas Vissapragada, Jessica Spake, Heather A. Knutson, Dion Linssen, Michael Zhang, Michael Greklek-McKeon, Jorge Pérez-González, Antonija Oklopčić
Figure caption: Transit light curve (top left) and residuals (bottom left) for both WIRC transit observations of TOI-1259 A b. Unbinned data from the first and second nights of observation are shown as gray circles and triangles, respectively. Data from both nights are binned together in 10-minute intervals, which are shown as black circles. The red curve is the best-fit WIRC transit model from the joint fit, with red shading indicating the 1σ uncertainty in the transit depth. The blue curve is the same transit model with ﹩{({R}_{p}/{R}_{\mathrm{star}})}^{2}﹩ fixed to the value obtained by fitting the broadband TESS data. The corresponding TESS transit light curve (top right) and residuals (bottom right) are shown for comparison. Unbinned data are plotted in gray, with data points binned to 10 minutes shown in black. The best-fit TESS transit model is overplotted in blue.
Paper: Atmospheric Mass Loss from TOI-1259 A b, a Gas Giant Planet with a White Dwarf Companion
Authors: Morgan Saidel, Shreyas Vissapragada, Jessica Spake, Heather A. Knutson, Dion Linssen, Michael Zhang, Michael Greklek-McKeon, Jorge Pérez-González, Antonija Oklopčić
Figure caption: The average excess absorption during the first half of transit (T1 to mid-transit; gray) and second half of transit (mid-transit to T4; black). The best-fit Gaussian model for the first half of transit is shown in blue, and the best-fit Gaussian model for the second half of transit is shown in red. Red vertical dashed lines denote the rest wavelengths of the three helium lines.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Atmospheric Mass Loss from TOI-1259 A b, a Gas Giant Planet with a White Dwarf Companion
Authors: Morgan Saidel, Shreyas Vissapragada, Jessica Spake, Heather A. Knutson, Dion Linssen, Michael Zhang, Michael Greklek-McKeon, Jorge Pérez-González, Antonija Oklopčić
Figure caption: The mass-loss and temperature model results from Cloudy models for the measured Palomar/WIRC excess absorption (left) and Keck/NIRSPEC excess absorption (T1–T4: middle; T2–T3: right) using HD 40307. The orange line and orange shading represent the 2σ (light orange) and 1σ (dark orange) confidence intervals from the constrained temperature structure. The blue line and blue shading indicate the 2σ (light blue) and 1σ (dark blue) best-fit models of the mass loss.
Paper: Atmospheric Mass Loss from TOI-1259 A b, a Gas Giant Planet with a White Dwarf Companion
Authors: Morgan Saidel, Shreyas Vissapragada, Jessica Spake, Heather A. Knutson, Dion Linssen, Michael Zhang, Michael Greklek-McKeon, Jorge Pérez-González, Antonija Oklopčić
Figure caption: Synthetic Keck time series in the Palomar/WIRC helium filter (black points) as compared to our Palomar/WIRC transit observation (gray points). We overplot the best-fit transit model for the Keck time series as a red solid line and the best-fit transit model for the Palomar/WIRC time series as a red dashed line.
Paper: Atmospheric Mass Loss from TOI-1259 A b, a Gas Giant Planet with a White Dwarf Companion
Authors: Morgan Saidel, Shreyas Vissapragada, Jessica Spake, Heather A. Knutson, Dion Linssen, Michael Zhang, Michael Greklek-McKeon, Jorge Pérez-González, Antonija Oklopčić
Figure caption: The band-integrated light curve of TOI-1259 A b, integrated within 0.75 Å of the main peak in the helium triplet (10833.0 Å). Gray dashed lines mark the beginning and end of transit. The gray shaded region in the band-integrated light curve denotes a focusing issue.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Atmospheric Mass Loss from TOI-1259 A b, a Gas Giant Planet with a White Dwarf Companion
Authors: Morgan Saidel, Shreyas Vissapragada, Jessica Spake, Heather A. Knutson, Dion Linssen, Michael Zhang, Michael Greklek-McKeon, Jorge Pérez-González, Antonija Oklopčić
Figure caption: Optical spectrum of TOI-1259 A obtained during a single epoch of observation with HIRES on UT 2019 November 28. The Ca II K (top) and H (bottom) lines are used to derive a log ﹩R{{\prime} }_{{\rm{HK}}}﹩ of −4.5 for the planet (Howard Isaacson, private communication) following the methodology in H. Isaacson et al. (2024).
Paper: Color–Magnitude Diagram of NGC 205 and Its RR Lyrae Variables
Authors: Ata Sarajedini
Figure caption: A digitized sky survey image of NGC 205 showing the observed Advanced Camera for Surveys Wide Field Channel (WFC) field analyzed here. The WFC1 channel is the lower rectangle while WFC2 is the upper rectangle. The field observed by A. Saha et al. (1992) is the larger square on the right. Note that the center of M31 is well-off the chart to the lower left. The field of view of this image is 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 on each side, and north is up and east is to the left.
Paper: Color–Magnitude Diagram of NGC 205 and Its RR Lyrae Variables
Authors: Ata Sarajedini
Figure caption: Results of the synthetic light curve simulations. The right panel shows the difference between the input and output F606W amplitude of the simulated light curves as a function of the input F606W amplitudes. The left panel shows the histogram of these differences. See text for details.
Paper: Color–Magnitude Diagram of NGC 205 and Its RR Lyrae Variables
Authors: Ata Sarajedini
Figure caption: Results of the synthetic light curve simulations. The right panel shows the difference between the input and output periods of the simulated light curves as a function of the input periods. The left panel shows the histogram of these differences. See text for details.
Paper: Color–Magnitude Diagram of NGC 205 and Its RR Lyrae Variables
Authors: Ata Sarajedini
Figure caption: Drizzled HST/ACS/WFC image downloaded from MAST showing the observed field of view. Approximate north is up and east is to the left.
Paper: Color–Magnitude Diagram of NGC 205 and Its RR Lyrae Variables
Authors: Ata Sarajedini
Figure caption: The top panel shows the variation of dereddened RGB (F606W − F814W) color as a function of [Fe/H] as determined from the globular cluster RGBs of T. M. Brown et al. (2005; black points) and from the DSEP theoretical isochrones (red points). The lower panel shows the same data as the upper panel except that the inverse of the dereddened color is shown in an attempt to make its variation with [Fe/H] easier to model.
Paper: Color–Magnitude Diagram of NGC 205 and Its RR Lyrae Variables
Authors: Ata Sarajedini
Figure caption: Hess diagrams highlighting the more prominent features visible in the WFC1 and WFC2 CMDs. The red points are the RR Lyrae variables in each chip.
Paper: Color–Magnitude Diagram of NGC 205 and Its RR Lyrae Variables
Authors: Ata Sarajedini
Figure caption: Color–magnitude diagrams showing the WFC1 (227,591 stars) and WFC2 (143,987 stars) photometry reduced and analyzed in the present study. The horizontal lines represent the location of the RGB tip as determined herein.
Paper: Color–Magnitude Diagram of NGC 205 and Its RR Lyrae Variables
Authors: Ata Sarajedini
Figure caption: Same as Figure 8 except that the RGB sequences from the DSEP theoretical isochrones are overplotted.
Paper: Color–Magnitude Diagram of NGC 205 and Its RR Lyrae Variables
Authors: Ata Sarajedini
Figure caption: The upper panel shows the F814W luminosity function of NGC 205 in the region of the RGB tip after combining the data in the WFC1 and WFC2 chips. The lower panel shows the results of applying the Sobel edge-detection algorithm to the luminosity function in search of the magnitude of the RGB tip shown by the vertical dashed line.
Paper: Color–Magnitude Diagram of NGC 205 and Its RR Lyrae Variables
Authors: Ata Sarajedini
Figure caption: The Bailey diagram for the RR Lyrae stars in NGC 205. The filled and open circles are from the WFC1 (246 RRL) and WFC2 (233 RRLs) chips, respectively.
Paper: Color–Magnitude Diagram of NGC 205 and Its RR Lyrae Variables
Authors: Ata Sarajedini
Figure caption: Sample light curves for ab-type RR Lyrae variables in NGC 205. Filled circles represent F814W magnitudes while the open circles are the F606W magnitudes.
Paper: Color–Magnitude Diagram of NGC 205 and Its RR Lyrae Variables
Authors: Ata Sarajedini
Figure caption: The metallicity-distribution function of NGC 205 derived from the color distribution of the RGB stars at M(F814W) = −2.8 ± 0.2 within the framework of the isochrone grid.
Paper: Color–Magnitude Diagram of NGC 205 and Its RR Lyrae Variables
Authors: Ata Sarajedini
Figure caption: Distance and reddening corrected CMD of the combined WFC1 and WFC2 photometry along with the T. M. Brown et al. (2005) cluster fiducials overplotted.
Paper: Mind the Gap. II. The Near-UV Fluxes of M Dwarfs
Authors: Wei-Chun Jao, 惟君 饒, Allison Youngblood
Figure caption: The GAGDR3 sample on the H-R diagram ((a) and (c)), MG vs. MNUV diagram (b), and MG vs. MFUV diagram (d). The orange dots represent the stars on the upper branch, and the blue dots are stars on the lower branch. The red and blue dashed lines represent the fitted distributions based on the clustering algorithm. The red lines on (a) and (c) are defined in Figure 1. The black dashed line in (b) indicates stars with MG > 7.0 from the PARSEC model with a 1 billion yr age. The arrows for 3×, 13×, and 25× represent the excess fluxes relative to the low-NUV states at MG = 8, 10, and 11, respectively. The bottom two plots are the same as the top two plots but for stars with detections in the FUV band. The two arrows in the lower right plot indicate the excess fluxes at MG = 8 and 10. The PARSEC model in the FUV is not shown here, because it is beyond the range of this plot. The NUV benchmark star, GJ 832, is shown as the black box.
Paper: Mind the Gap. II. The Near-UV Fluxes of M Dwarfs
Authors: Wei-Chun Jao, 惟君 饒, Allison Youngblood
Figure caption: Stars with Mg II indices on the H-R diagram (a), MG vs. MNUV diagram (b), and MG vs. Mg II index diagram (c). The stars from T. Pal et al. (2023) are shown with black dots. An additional 38 stars retrieved from MAST with the STIS-MAMA+G230L observing configuration are shown with brown dots. The red dots represent known members of the Hyades. The open boxes indicate stars without GALEX NUV photometry. In (c), the dark gray region indicates stars with positive indices of strong absorption wings and core Mg II emission, and the light gray region indicates negative indices of strong Mg II emission from the chromosphere. The red lines in (a) are defined in Figure 1, and the blue dots in (b) are the GAGDR3 sample.
Paper: Mind the Gap. II. The Near-UV Fluxes of M Dwarfs
Authors: Wei-Chun Jao, 惟君 饒, Allison Youngblood
Figure caption: Distributions of stars from GAGDR3 (blue dots) and A. C. Schneider & E. L. Shkolnik (2018) on the H-R diagram ((a) and (c)) and the MG vs. MNUV diagram ((b) and (d)). Single young and field stars from A. C. Schneider & E. L. Shkolnik (2018) are shown with the red and black dots, respectively. The red lines are defined in Figure 1. The stars in GAGDR3 identified as potential members of young moving groups using the BANYAN tool are shown with the orange dots in the bottom two plots.
Paper: Mind the Gap. II. The Near-UV Fluxes of M Dwarfs
Authors: Wei-Chun Jao, 惟君 饒, Allison Youngblood
Figure caption: Spectral comparisons between stars on different branches. The left column compares spectra for GJ163 and 2MA0417+1454, and the right column compares those for GJ699 and 2MA0358+1237. Top: the spectra are calibrated to a distance of 10 pc, with the red spectra shifted upward relative to the blue spectra for better visual comparison. The short blue spectra magnify the Fe II forests from the fainter comparison stars. Key features such as Si II, Fe II, and Mg I lines are marked with ticks. The strong emission at 2800 Å is the Mg II doublets. The black dashed lines indicate the GALEX NUV bandpass, with its filter effective area labeled on the right side of the top two plots. Middle: spectral differences for each pair, convolved with the GALEX NUV bandpass. Bottom: cumulative percentage of flux from the middle plots.
Paper: Mind the Gap. II. The Near-UV Fluxes of M Dwarfs
Authors: Wei-Chun Jao, 惟君 饒, Allison Youngblood
Figure caption: Flaring M dwarfs in the NUV band on various diagrams: the H-R diagram (a), MNUV vs. MG (b), ﹩\mathrm{log}{E}_{\mathrm{flaring}}﹩ vs. MGG (c), and ﹩\mathrm{log}﹩E vs. distance (d). The red and blue dots show stars with and without detectable NUV flaring in P. Rekhi et al. (2023), respectively. Most of the NUV flaring stars in P. Rekhi et al. (2023) are on neither of the two branches. The orange and black dots represent the stars in R. R. Paudel et al. (2024) on the lower and upper branches, respectively. The open circles highlight stars with detected NUV flares in R. R. Paudel et al. (2024). Because multiple flares are reported in R. R. Paudel et al. (2024) for a given star, the largest and smallest flares are connected by a black line in (c). The stars from R. R. Paudel et al. (2024) without detected NUV flares are shown with arrows marked at their MG magnitudes in (c) and at their distances in (d).
Paper: Mind the Gap. II. The Near-UV Fluxes of M Dwarfs
Authors: Wei-Chun Jao, 惟君 饒, Allison Youngblood
Figure caption: Distributions of stars with rotation period measurements from the Kepler K2 Campaigns in T. Reinhold & S. Hekker (2020) and from nearby stars in E. R. Newton et al. (2017). The left plot shows their distributions on the H-R diagram, and the right plot shows their distributions on the MG vs. MNUV plot. The black and red dots indicate slow and fast rotators, respectively. The definitions of “fast” and “slow” rotators are relative to the critical period (Pcrit) discussed in W.-C. Jao et al. (2023). The red lines on the left plot are defined in Figure 1.
Paper: Mind the Gap. II. The Near-UV Fluxes of M Dwarfs
Authors: Wei-Chun Jao, 惟君 饒, Allison Youngblood
Figure caption: Distribution of Hα activity from M dwarfs in the MEarth, CARMENES, and LAMOST surveys. The left plot shows their distributions on the H-R diagram, and the right plot shows their distributions on the MG vs. MNUV plot. The two populations of Hα activity mimic the two branches in the right plot. We note that because of the various selection biases from these surveys, the distributions do not indicate the completeness of the nearby M dwarfs on these two plots. The red lines on the left plot are defined in Figure 1.
Paper: Mind the Gap. II. The Near-UV Fluxes of M Dwarfs
Authors: Wei-Chun Jao, 惟君 饒, Allison Youngblood
Figure caption: This four-panel figure demonstrates that the NUV − RP color shift identified by C. Cifuentes et al. (2020) at G − J ~ 2.5 is not at the interior transition based on the GAGDR3 sample. The top two panels show the distributions of stars in NUV − RP vs. G − J and MG vs. MNUV plots. We also approximately separate the stars into the upper branch (orange dots) and lower branch (blue dots), using the line later discussed in Section 7 and Table 2. The bottom two panels highlight stars with G − J between 2.6 and 2.4 mag at the color shift or close to the M2 type. The red dots represent stars within the main-sequence gap, which is marked by the red rectangular box.
Paper: JWST-TST High Contrast: Living on the Wedge, or, NIRCam Bar Coronagraphy Reveals CO2 in the HR 8799 and 51 Eri Exoplanets’ Atmospheres
Authors: William O. Balmer, Jens Kammerer, Laurent Pueyo, Marshall D. Perrin, Julien H. Girard, Jarron M. Leisenring, Kellen Lawson, Henry Dennen, Roeland P. van der Marel, Charles A. Beichman, Geoffrey Bryden, Jorge Llop-Sayson, Jeff A. Valenti, Joshua D. Lothringer, Nikole K. Lewis, Mathilde Mâlin, Isabel Rebollido, Emily Rickman, Kielan K. W. Hoch, Rémi Soummer, Mark Clampin, C. Matt Mountain
Figure caption: Visual orbit parameters and dynamical masses of the 51 Eri system, from our orbital analysis (Section 4.2) using orbitize!. Parameters with respect to 51 Eri b are denoted with subscript “1,” and parameters with respect to 51 Eri A are denoted with subscript “0.” Complex correlations between the parameters describing the visual orbit are apparent, as in previous orbit fits (A. L. Maire et al. 2019; R. J. De Rosa et al. 2020; T. J. Dupuy et al. 2022); the updated measurement from JWST/NIRCam confirms the preference for high-eccentricity solutions (e = 0.58) and a moderate semimajor axis (a = 9.34 au) that was found in those works. The inclusion of absolute astrometry from the HGCA provides an upper limit on the planet’s mass, Mb < 9.0 MJ at 3σ.
Paper: JWST-TST High Contrast: Living on the Wedge, or, NIRCam Bar Coronagraphy Reveals CO2 in the HR 8799 and 51 Eri Exoplanets’ Atmospheres
Authors: William O. Balmer, Jens Kammerer, Laurent Pueyo, Marshall D. Perrin, Julien H. Girard, Jarron M. Leisenring, Kellen Lawson, Henry Dennen, Roeland P. van der Marel, Charles A. Beichman, Geoffrey Bryden, Jorge Llop-Sayson, Jeff A. Valenti, Joshua D. Lothringer, Nikole K. Lewis, Mathilde Mâlin, Isabel Rebollido, Emily Rickman, Kielan K. W. Hoch, Rémi Soummer, Mark Clampin, C. Matt Mountain
Figure caption: LWB/narrow observations of all four HR 8799 planets (SW filters as blue hexagons, LW filters as gold hexagons) compared to petitRADTRANS models that were fit to previously available observations, primarily ground-based spectroscopy and photometry (shown in Figure 6), from E. Nasedkin et al. (2024). A random model has been chosen to highlight in black, and synthesized photometry from this model for each NIRCam filter is shown as an open hexagon; all other models from the exhaustive retrieval analysis are plotted in light purple. Some of the retrieval models are consistent with some of the NIRCam photometry, but many are not, especially at shorter wavelengths near the K band. This could be due to the absolute flux calibration of the ground-based spectra; see discussion in Section 4.1.
Paper: JWST-TST High Contrast: Living on the Wedge, or, NIRCam Bar Coronagraphy Reveals CO2 in the HR 8799 and 51 Eri Exoplanets’ Atmospheres
Authors: William O. Balmer, Jens Kammerer, Laurent Pueyo, Marshall D. Perrin, Julien H. Girard, Jarron M. Leisenring, Kellen Lawson, Henry Dennen, Roeland P. van der Marel, Charles A. Beichman, Geoffrey Bryden, Jorge Llop-Sayson, Jeff A. Valenti, Joshua D. Lothringer, Nikole K. Lewis, Mathilde Mâlin, Isabel Rebollido, Emily Rickman, Kielan K. W. Hoch, Rémi Soummer, Mark Clampin, C. Matt Mountain
Figure caption: Deconvolution of the F410M image of HR 8799 (Figure 4) using webbpsf model PSFs, as described in Appendix B. Left panel: deconvolved result, Right panel: top, smoothed by a Gaussian with an FWHM of 1 pixel. The deconvolution, which has accounted for the spatially dependent off-axis coronagraphic PSF as well as the coronagraph transmission function captures the intrinsic luminosity difference between the four planets in this filter (see also the calibrated photometry in Table 2).