adsabs/AstroCLIMB huggingface dataset:
Paper: The Milky Way Bulge Extra-tidal Star Survey: BH 261 (AL 3)
Authors: Andrea Kunder, Zdenek Prudil, Kevin R. Covey, Joanne Hughes, Meridith Joyce, Iulia T. Simion, Rebekah Kuss, Carlos Campos, Christian I. Johnson, Catherine A. Pilachowski, Kristen A. Larson, Andreas J. Koch-Hansen, Tommaso Marchetti, Michael R. Rich, Evan Butler, William I. Clarkson, Michael Rivet, Kathryn Devine, A. Katherina Vivas, Gabriel I. Perren, Mario Soto, Erika Silva
Figure caption: Left: the heliocentric velocities of our targeted stars within 65′ of BH 261, with the tidal radius at r  t  = 5.′4 indicated by the solid gray line. The uncertainty in radial velocity is ∼4 km s−1, except for the horizontal branch stars, where the RV uncertainty is ∼9 km s−1. Large (green) stars represent the targeted RR Lyrae stars. The stars with SP_ACE metallicities, photometric metallicities, and radial velocities consistent with BH 261 are circled, and are potential extra-tidal stars belonging to BH 261. Right: a comparison between the photometric [Fe/H] and spectroscopic [Fe/H] for the stars with both photometric metallicities and radial velocities consistent with BH 261. The two red clump stars with spectroscopic [Fe/H] metallicities that are discrepant from the photometric ones also have T eff and log g values that suggest they are not red clump giants.
Paper: The Milky Way Bulge Extra-tidal Star Survey: BH 261 (AL 3)
Authors: Andrea Kunder, Zdenek Prudil, Kevin R. Covey, Joanne Hughes, Meridith Joyce, Iulia T. Simion, Rebekah Kuss, Carlos Campos, Christian I. Johnson, Catherine A. Pilachowski, Kristen A. Larson, Andreas J. Koch-Hansen, Tommaso Marchetti, Michael R. Rich, Evan Butler, William I. Clarkson, Michael Rivet, Kathryn Devine, A. Katherina Vivas, Gabriel I. Perren, Mario Soto, Erika Silva
Figure caption: The simulated tidal tails for BH 261 (gray), calculated with the cluster's best-fit parameters, are compared to the most promising BH 261 extra-tidal candidates presented here. The legend in the upper left corner indicates the length of time the cluster orbit is integrated forwards as well as the mass of BH 261 used in the simulation. The stream of the tidal debris has a narrow width when using a small GC mass (i.e., the mass inferred from its luminosity), and the simulated tidal tails occupy a greater area around the center of the cluster as a larger GC mass is used (i.e., the mass inferred from its velocity dispersion).
Paper: JWST-TST High Contrast: Asymmetries, Dust Populations, and Hints of a Collision in the β Pictoris Disk with NIRCam and MIRI
Authors: Isabel Rebollido, Christopher C. Stark, Jens Kammerer, Marshall D. Perrin, Kellen Lawson, Laurent Pueyo, Christine Chen, Dean Hines, Julien H. Girard, Kadin Worthen, Carl Ingerbretsen, Sarah Betti, Mark Clampin, David Golimowski, Kielan Hoch, Nikole K. Lewis, Cicero X. Lu, Roeland P. van der Marel, Emily Rickman, Sara Seager, Rémi Soummer, Jeff A. Valenti, Kimberly Ward-Duong, C. Matt Mountain
Figure caption: Synthetic 23 μm thermal emission image of a multicomponent sporadic dust production model with an ISM drag force, which broadly reproduces the shape, color, and flux of the cat’s tail (∼150 yr old), as well as the presence of additional arcs to the SW (∼150–200 yr old) and NE (≳1000 yr old), as marked in Figure 4. The left panel shows the projected view oriented the same as in Figure 4, and the right panel shows a face-on view looking down onto the disk from the NW.
Paper: JWST-TST High Contrast: Asymmetries, Dust Populations, and Hints of a Collision in the β Pictoris Disk with NIRCam and MIRI
Authors: Isabel Rebollido, Christopher C. Stark, Jens Kammerer, Marshall D. Perrin, Kellen Lawson, Laurent Pueyo, Christine Chen, Dean Hines, Julien H. Girard, Kadin Worthen, Carl Ingerbretsen, Sarah Betti, Mark Clampin, David Golimowski, Kielan Hoch, Nikole K. Lewis, Cicero X. Lu, Roeland P. van der Marel, Emily Rickman, Sara Seager, Rémi Soummer, Jeff A. Valenti, Kimberly Ward-Duong, C. Matt Mountain
Figure caption: Numerical experiment validating the deconvolution method used. Top row: the ground-truth synthetic disk image (left) and the corresponding PSF-convolved image as described in Appendix A. Middle row: the results for standard R-L deconvolution (left), and the R-L variant that considers coronagraphic transmission (right). All images are shown with a logarithmic stretch and a 12″ × 6″ field of view. Bottom panel: the ratio of radial surface brightness measurements for each of the images of the upper panel with those of the ground truth. Surface brightness measurements are made using 1 pixel wide rectangular apertures that extend to the edge of the field of view. Measurements shown are for the right side of the disk, but values for the left side are comparable. The R-L variant for coronagraphy does far better at correctly reconstructing the disk surface brightness within the inner arcsecond.
Paper: JWST-TST High Contrast: Asymmetries, Dust Populations, and Hints of a Collision in the β Pictoris Disk with NIRCam and MIRI
Authors: Isabel Rebollido, Christopher C. Stark, Jens Kammerer, Marshall D. Perrin, Kellen Lawson, Laurent Pueyo, Christine Chen, Dean Hines, Julien H. Girard, Kadin Worthen, Carl Ingerbretsen, Sarah Betti, Mark Clampin, David Golimowski, Kielan Hoch, Nikole K. Lewis, Cicero X. Lu, Roeland P. van der Marel, Emily Rickman, Sara Seager, Rémi Soummer, Jeff A. Valenti, Kimberly Ward-Duong, C. Matt Mountain
Figure caption: SEDs for identical disks with porous (blue) and nonporous (orange) organic refractory material. Porosity reduces the scattered light by a factor ∼300 and increases the mid-infrared flux by a factor ∼100. A secondary disk and cat’s tail composed of porous organic refractory material would appear faint in scattered light and bright in the mid-infrared, potentially explaining the relative absence of these features in scattered light as well as the varying best-fit compositions appearing in the literature.
Paper: JWST-TST High Contrast: Asymmetries, Dust Populations, and Hints of a Collision in the β Pictoris Disk with NIRCam and MIRI
Authors: Isabel Rebollido, Christopher C. Stark, Jens Kammerer, Marshall D. Perrin, Kellen Lawson, Laurent Pueyo, Christine Chen, Dean Hines, Julien H. Girard, Kadin Worthen, Carl Ingerbretsen, Sarah Betti, Mark Clampin, David Golimowski, Kielan Hoch, Nikole K. Lewis, Cicero X. Lu, Roeland P. van der Marel, Emily Rickman, Sara Seager, Rémi Soummer, Jeff A. Valenti, Kimberly Ward-Duong, C. Matt Mountain
Figure caption: Same as Figure 20 but for MIRI filters. Instead of a single fit for the secondary disk, in this case we fitted the NE and SW separately, and further divided the SW side in two sections: (1) base of the cat’s tail and (2) tip of the cat’s tail. The fields of view are slightly different for F1550C (24″) vs. MIRI (30″), leading to different spatial coverages.
Paper: JWST-TST High Contrast: Asymmetries, Dust Populations, and Hints of a Collision in the β Pictoris Disk with NIRCam and MIRI
Authors: Isabel Rebollido, Christopher C. Stark, Jens Kammerer, Marshall D. Perrin, Kellen Lawson, Laurent Pueyo, Christine Chen, Dean Hines, Julien H. Girard, Kadin Worthen, Carl Ingerbretsen, Sarah Betti, Mark Clampin, David Golimowski, Kielan Hoch, Nikole K. Lewis, Cicero X. Lu, Roeland P. van der Marel, Emily Rickman, Sara Seager, Rémi Soummer, Jeff A. Valenti, Kimberly Ward-Duong, C. Matt Mountain
Figure caption: Synthetic 23 μm thermal emission image of a two-component model without external forcing, as proposed in Section 5.2, consistent of a quasi–steady-state secondary disk and a single 150 yr old collisional event. This reproduces the shape of the cat’s tail, with exception to the crook near the tip. The left panel shows the projected view oriented the same as Figure 4, and the right panel shows a face-on view looking down onto the disk from the NW.
Paper: JWST-TST High Contrast: Asymmetries, Dust Populations, and Hints of a Collision in the β Pictoris Disk with NIRCam and MIRI
Authors: Isabel Rebollido, Christopher C. Stark, Jens Kammerer, Marshall D. Perrin, Kellen Lawson, Laurent Pueyo, Christine Chen, Dean Hines, Julien H. Girard, Kadin Worthen, Carl Ingerbretsen, Sarah Betti, Mark Clampin, David Golimowski, Kielan Hoch, Nikole K. Lewis, Cicero X. Lu, Roeland P. van der Marel, Emily Rickman, Sara Seager, Rémi Soummer, Jeff A. Valenti, Kimberly Ward-Duong, C. Matt Mountain
Figure caption: Left: F2300C flux as a function of apparent separation measured along the main disk’s midplane, as well as the measured and modeled cat’s tail. Right: color (F1550C/F2300 flux ratio) of the components. Our model with porous organic refractory grains largely reproduces the flux and color over the length of the cat’s tail.
Paper: JWST-TST High Contrast: Asymmetries, Dust Populations, and Hints of a Collision in the β Pictoris Disk with NIRCam and MIRI
Authors: Isabel Rebollido, Christopher C. Stark, Jens Kammerer, Marshall D. Perrin, Kellen Lawson, Laurent Pueyo, Christine Chen, Dean Hines, Julien H. Girard, Kadin Worthen, Carl Ingerbretsen, Sarah Betti, Mark Clampin, David Golimowski, Kielan Hoch, Nikole K. Lewis, Cicero X. Lu, Roeland P. van der Marel, Emily Rickman, Sara Seager, Rémi Soummer, Jeff A. Valenti, Kimberly Ward-Duong, C. Matt Mountain
Figure caption: Fitting of the location of the secondary disk in the NIRCam short and long filters, using a multicomponent fit following the approach of Golimowski et al. (2006), their Figure 9. The shaded areas show the data used in the fit, to avoid those with large errors in the determination of the main disk (i.e., low S/N of the detection).
Paper: JWST/NIRCam Transmission Spectroscopy of the Nearby Sub-Earth GJ 341b
Authors: James Kirk, Kevin B. Stevenson, Guangwei Fu, Jacob Lustig-Yaeger, Sarah E. Moran, Sarah Peacock, Munazza K. Alam, Natasha E. Batalha, Katherine A. Bennett, Junellie Gonzalez-Quiles, Mercedes López-Morales, Joshua D. Lothringer, Ryan J. MacDonald, E. M. May, L. C. Mayorga, Zafar Rustamkulov, David K. Sing, Kristin S. Sotzen, Jeff A. Valenti, Hannah R. Wakeford
Figure caption: The M-dwarf cosmic shoreline (Zahnle & Catling 2017) plotted in escape velocity–instellation space. Planets that sit below the shoreline (gray line) are more likely to have atmospheres and those above are less likely. The targets in our program are GJ 341b (this paper), LHS 475b (Lustig-Yaeger et al. 2023a), GJ 486b (Moran et al. 2023), GJ 1132b (May et al. 2023), and TRAPPIST-1h (Z. Rustamkulov & S. Peacock et al. 2024, in preparation). We include the other TRAPPIST-1 planets for reference.
Paper: JWST/NIRCam Transmission Spectroscopy of the Nearby Sub-Earth GJ 341b
Authors: James Kirk, Kevin B. Stevenson, Guangwei Fu, Jacob Lustig-Yaeger, Sarah E. Moran, Sarah Peacock, Munazza K. Alam, Natasha E. Batalha, Katherine A. Bennett, Junellie Gonzalez-Quiles, Mercedes López-Morales, Joshua D. Lothringer, Ryan J. MacDonald, E. M. May, L. C. Mayorga, Zafar Rustamkulov, David K. Sing, Kristin S. Sotzen, Jeff A. Valenti, Hannah R. Wakeford
Figure caption: Comparison of retrieval results on data reduced by the Eureka!, Tiberius, and Tswift pipelines, respectively (rows of subplots). For each reduction’s retrieval, the median spectral fit is shown in the left panel, the 1D marginalized CO2 posterior is shown in the middle panel, and the 1D marginalized O3 posterior is shown in the right panel. Although either CO2 or O3 are weakly detected in retrievals of the Tiberius and Tswift spectra, respectively (the Eureka! result is unconstrained), these findings are incompatible with one another. Thus, relatively small differences in the reductions can cause comparatively large changes in the subsequent physical interpretation, including spurious molecular detections.
Paper: JWST/NIRCam Transmission Spectroscopy of the Nearby Sub-Earth GJ 341b
Authors: James Kirk, Kevin B. Stevenson, Guangwei Fu, Jacob Lustig-Yaeger, Sarah E. Moran, Sarah Peacock, Munazza K. Alam, Natasha E. Batalha, Katherine A. Bennett, Junellie Gonzalez-Quiles, Mercedes López-Morales, Joshua D. Lothringer, Ryan J. MacDonald, E. M. May, L. C. Mayorga, Zafar Rustamkulov, David K. Sing, Kristin S. Sotzen, Jeff A. Valenti, Hannah R. Wakeford
Figure caption: Atmospheric forward models compared to the Eureka! reduction from JWST/NIRCam. Because of the planet’s small size and low equilibrium temperature, only hydrogen-dominated or methane atmospheres are strongly ruled out or disfavored by the data. Atmospheres of water, carbon dioxide, or an opaque haze layer—or no atmosphere—are all statistically consistent with the data to within ∼1σ across all three reductions.
Paper: JWST/NIRCam Transmission Spectroscopy of the Nearby Sub-Earth GJ 341b
Authors: James Kirk, Kevin B. Stevenson, Guangwei Fu, Jacob Lustig-Yaeger, Sarah E. Moran, Sarah Peacock, Munazza K. Alam, Natasha E. Batalha, Katherine A. Bennett, Junellie Gonzalez-Quiles, Mercedes López-Morales, Joshua D. Lothringer, Ryan J. MacDonald, E. M. May, L. C. Mayorga, Zafar Rustamkulov, David K. Sing, Kristin S. Sotzen, Jeff A. Valenti, Hannah R. Wakeford
Figure caption: Atmospheric retrieval posteriors (lower-left corner pairs) and range of spectral fits (upper right) from our coadded NIRCam observations of GJ 341b reduced with Eureka!. A subset of model parameters and covariances are shown, with H2O, CH4, and CO not displayed (nor constrained) for clarity. Analogous results are shown for the Tiberius and Tswift data-reduction pipelines in Figures 17 and 18, respectively.
Paper: JWST/NIRCam Transmission Spectroscopy of the Nearby Sub-Earth GJ 341b
Authors: James Kirk, Kevin B. Stevenson, Guangwei Fu, Jacob Lustig-Yaeger, Sarah E. Moran, Sarah Peacock, Munazza K. Alam, Natasha E. Batalha, Katherine A. Bennett, Junellie Gonzalez-Quiles, Mercedes López-Morales, Joshua D. Lothringer, Ryan J. MacDonald, E. M. May, L. C. Mayorga, Zafar Rustamkulov, David K. Sing, Kristin S. Sotzen, Jeff A. Valenti, Hannah R. Wakeford
Figure caption: The light curves and best-fit models resulting from the Tiberius pipeline. The columns show, from left to right: transit 1, transit 2, and transit 3. The rows show, from top to bottom: (1) the white light curve and residuals, (2) the spectroscopic light curves, (3) the best-fit models to the spectroscopic light curves, (4) the residuals from the spectroscopic light-curve fitting. The vertical band at the left-hand edge of the panels in rows 2–4 correspond to the 600 integrations that were masked during the spectroscopic light-curve fitting stage.
Paper: JWST/NIRCam Transmission Spectroscopy of the Nearby Sub-Earth GJ 341b
Authors: James Kirk, Kevin B. Stevenson, Guangwei Fu, Jacob Lustig-Yaeger, Sarah E. Moran, Sarah Peacock, Munazza K. Alam, Natasha E. Batalha, Katherine A. Bennett, Junellie Gonzalez-Quiles, Mercedes López-Morales, Joshua D. Lothringer, Ryan J. MacDonald, E. M. May, L. C. Mayorga, Zafar Rustamkulov, David K. Sing, Kristin S. Sotzen, Jeff A. Valenti, Hannah R. Wakeford
Figure caption: The light curves and best-fit models resulting from the Tswift pipeline. The columns show, from left to right: transit 1, transit 2, and transit 3. The rows show, from top to bottom: (1) the white light curve and residuals, (2) the spectroscopic light curves, (3) the best-fit models to the spectroscopic light curves, (4) the residuals from the spectroscopic light-curve fitting.
Paper: JWST/NIRCam Transmission Spectroscopy of the Nearby Sub-Earth GJ 341b
Authors: James Kirk, Kevin B. Stevenson, Guangwei Fu, Jacob Lustig-Yaeger, Sarah E. Moran, Sarah Peacock, Munazza K. Alam, Natasha E. Batalha, Katherine A. Bennett, Junellie Gonzalez-Quiles, Mercedes López-Morales, Joshua D. Lothringer, Ryan J. MacDonald, E. M. May, L. C. Mayorga, Zafar Rustamkulov, David K. Sing, Kristin S. Sotzen, Jeff A. Valenti, Hannah R. Wakeford
Figure caption: The transmission spectra for visit 1 (blue), visit 2 (orange), and visit 3 (green) as measured by Tiberius (top panel), Eureka! (middle panel), and Tswift (bottom panel).
Paper: JWST/NIRCam Transmission Spectroscopy of the Nearby Sub-Earth GJ 341b
Authors: James Kirk, Kevin B. Stevenson, Guangwei Fu, Jacob Lustig-Yaeger, Sarah E. Moran, Sarah Peacock, Munazza K. Alam, Natasha E. Batalha, Katherine A. Bennett, Junellie Gonzalez-Quiles, Mercedes López-Morales, Joshua D. Lothringer, Ryan J. MacDonald, E. M. May, L. C. Mayorga, Zafar Rustamkulov, David K. Sing, Kristin S. Sotzen, Jeff A. Valenti, Hannah R. Wakeford
Figure caption: Atmospheric forward models compared to the Tiberius reduction from JWST/NIRCam.
Paper: JWST/NIRCam Transmission Spectroscopy of the Nearby Sub-Earth GJ 341b
Authors: James Kirk, Kevin B. Stevenson, Guangwei Fu, Jacob Lustig-Yaeger, Sarah E. Moran, Sarah Peacock, Munazza K. Alam, Natasha E. Batalha, Katherine A. Bennett, Junellie Gonzalez-Quiles, Mercedes López-Morales, Joshua D. Lothringer, Ryan J. MacDonald, E. M. May, L. C. Mayorga, Zafar Rustamkulov, David K. Sing, Kristin S. Sotzen, Jeff A. Valenti, Hannah R. Wakeford
Figure caption: Atmospheric forward models compared to the Tswift reduction from JWST/NIRCam.
Paper: Dynamical Mass of the Ophiuchus Intermediate-mass Stellar System S1 with DYNAMO-VLBA
Authors: Jazmín Ordóñez-Toro, Sergio A. Dzib, Laurent Loinard, Gisela Ortiz-León, Marina A. Kounkel, Josep M. Masqué, S.-N. X. Medina, Phillip A. B. Galli, Trent J. Dupuy, Luis F. Rodríguez, Luis H. Quiroga-Nuñez
Figure caption: Orbital solution of S1. Top panel: stellar orbits relative to the central of mass (black cross). The orbits from best fit for S1A (red) and S1B (blue) are accompanied by a subset of 100 orbit pairs (light red for S1A, and gray for S1B) to show the range of solutions allowed by the errors in our fit. The subset of orbits shown corresponds to the best 100 of 5000 orbits generated by randomly obtaining orbital parameters from normal distributions with mean values equal to the values obtained from our best fit and with standard deviations equal to their errors. The measured positions of S1A (red squares) and S1B (blue circles) after correction of parallax and proper motions are also shown. The position errors are on the order of 0.1 mas, barely seen at the plot scale. Bottom panel: stellar relative positions and orbital fit model of S1. The blue dots indicate the relative positions of S1B with respect to S1A, and the error bars consider the position errors of both components, which are added in quadrature. The dashed black line traces the line of nodes from the model, and the black cross indicates the position of the primary. The measured positions of S1B obtained from infrared observations reported in Richichi et al. (1994) and Cheetham et al. (2015) are also plotted as red triangles. These infrared positions are listed in Table 4.
Paper: Dynamical Mass of the Ophiuchus Intermediate-mass Stellar System S1 with DYNAMO-VLBA
Authors: Jazmín Ordóñez-Toro, Sergio A. Dzib, Laurent Loinard, Gisela Ortiz-León, Marina A. Kounkel, Josep M. Masqué, S.-N. X. Medina, Phillip A. B. Galli, Trent J. Dupuy, Luis F. Rodríguez, Luis H. Quiroga-Nuñez
Figure caption: Spectral energy distribution of S1A. The data points (black squares) are taken from VizieR (see Table 6), while the fits (color lines) are based on the extinction curves of Rieke et al. (1989) and Fitzpatrick (1999; see text). The figure also includes residual plots for each model (bottom panels).
Paper: Dynamical Mass of the Ophiuchus Intermediate-mass Stellar System S1 with DYNAMO-VLBA
Authors: Jazmín Ordóñez-Toro, Sergio A. Dzib, Laurent Loinard, Gisela Ortiz-León, Marina A. Kounkel, Josep M. Masqué, S.-N. X. Medina, Phillip A. B. Galli, Trent J. Dupuy, Luis F. Rodríguez, Luis H. Quiroga-Nuñez
Figure caption: Final radio images of S1 at 4.5 GHz corresponding to each epoch observed during the DYNAMO-VLBA project. The intensity background images are clipped to intensities between –0.1 and 0.6 mJy beam−1. The contour levels are at –4, 4, 6, 10, 15, 30, and 60 times the noise levels of the images, listed in Table 1. The images are centered on the measured position of S1A, the primary component of the S1 binary system as listed in Table 1 and shown in the top left corner of each plot. The white ellipse in the bottom left corner of each plot represents the synthesized beam of the corresponding observed epoch.
Paper: Dynamical Mass of the Ophiuchus Intermediate-mass Stellar System S1 with DYNAMO-VLBA
Authors: Jazmín Ordóñez-Toro, Sergio A. Dzib, Laurent Loinard, Gisela Ortiz-León, Marina A. Kounkel, Josep M. Masqué, S.-N. X. Medina, Phillip A. B. Galli, Trent J. Dupuy, Luis F. Rodríguez, Luis H. Quiroga-Nuñez
Figure caption: Flux as a function of orbital phase for S1A (top) and S1B (bottom) at 5 GHz (blue dots) and 8 GHz (red squares). For S1A, the bins (gray boxes) show the mean and standard deviation values of fluxes in widths of 0.2 in the orbital phase. For S1B, the green arrows indicate the flux 3σ rms upper limits when the source is not detected. The error bars are shown and are sometimes smaller than the marker size.
Paper: Dynamical Mass of the Ophiuchus Intermediate-mass Stellar System S1 with DYNAMO-VLBA
Authors: Jazmín Ordóñez-Toro, Sergio A. Dzib, Laurent Loinard, Gisela Ortiz-León, Marina A. Kounkel, Josep M. Masqué, S.-N. X. Medina, Phillip A. B. Galli, Trent J. Dupuy, Luis F. Rodríguez, Luis H. Quiroga-Nuñez
Figure caption: Measured positions of S1A (red dots) and S1B (blue dots) shown as offsets from the position of S1A in the first detected epoch used in the present paper (2005 June 24; see Table 1). The red and blue curves show the best fits, described in the text, to the positions of S1A and S1B, respectively.
Paper: Dynamical Mass of the Ophiuchus Intermediate-mass Stellar System S1 with DYNAMO-VLBA
Authors: Jazmín Ordóñez-Toro, Sergio A. Dzib, Laurent Loinard, Gisela Ortiz-León, Marina A. Kounkel, Josep M. Masqué, S.-N. X. Medina, Phillip A. B. Galli, Trent J. Dupuy, Luis F. Rodríguez, Luis H. Quiroga-Nuñez
Figure caption: Relative positions and orbital fit model. The green stars indicate the expected positions of S1B in undetected epochs. Orbital phases (ϕ) are indicated with vertical black lines and labeled accordingly.
Paper: ABYSS. II. Identification of Young Stars in Optical SDSS Spectra and Their Properties
Authors: Serat Saad, Kaitlyn Lane, Marina Kounkel, Keivan G. Stassun, Ricardo López-Valdivia, Jinyoung Serena Kim, Karla Peña Ramírez, Guy S. Stringfellow, Carlos G. Román-Zúñiga, Jesús Hernández, Scott J. Wolk, Lynne A. Hillenbrand
Figure caption: Li I distribution as a function of T eff across different age bins. Yellow dots show the raw data, black squares show the median Li I EqW in 0.1 dex T eff bins, and the black error bars show the 16–84 percentile scatter. The gray error bar shows the typical uncertainty in the individual measurements. The red dashed line shows the relationship of Li I as a function of T eff and age from Jeffries et al. (2023), and the blue solid line shows the polynomial fit presented in Equation (2).
Paper: ABYSS. II. Identification of Young Stars in Optical SDSS Spectra and Their Properties
Authors: Serat Saad, Kaitlyn Lane, Marina Kounkel, Keivan G. Stassun, Ricardo López-Valdivia, Jinyoung Serena Kim, Karla Peña Ramírez, Guy S. Stringfellow, Carlos G. Román-Zúñiga, Jesús Hernández, Scott J. Wolk, Lynne A. Hillenbrand
Figure caption: Comparison of Li I measurements reported here to those from Gaia-ESO spectra from Binks et al. (2022), color coded by the T eff of the star. The black line shows the best fit between the two.
Paper: ABYSS. II. Identification of Young Stars in Optical SDSS Spectra and Their Properties
Authors: Serat Saad, Kaitlyn Lane, Marina Kounkel, Keivan G. Stassun, Ricardo López-Valdivia, Jinyoung Serena Kim, Karla Peña Ramírez, Guy S. Stringfellow, Carlos G. Román-Zúñiga, Jesús Hernández, Scott J. Wolk, Lynne A. Hillenbrand
Figure caption: Ratio between the typical scatter in Li I in each age and T eff bin, and the typical uncertainty in Li I measurements in that bin. The black line shows the fitted average across all age ranges.