adsabs/AstroCLIMB huggingface dataset:
Paper: Detailed Chemical Abundances of Stars in the Outskirts of the Tucana II Ultrafaint Dwarf Galaxy 
Authors: Anirudh Chiti, Anna Frebel, Alexander P. Ji, Mohammad K. Mardini, Xiaowei Ou, Joshua D. Simon, Helmut Jerjen, Dongwon Kim, John E. Norris
Figure caption: Sample regions of our Magellan/MIKE spectra covering the CH absorption band at ∼4311 Å (left panels), the Ba line region at 4554 Å (middle panels), and the Mg b region around 5170 Å (right panels). Tuc2-309, the most metal-rich ([Fe/H] = −1.93) star, is plotted in the top panels; TucII-306, with a metallicity of [Fe/H] = −3.26, is plotted in the middle panels; and TucII-305, the most metal-poor star ([Fe/H] = −3.59), is plotted in the bottom panels. Note the lack of a detectable Ba feature in these stars, supporting their classification as UFD members (see Section 4.3).
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). IX. A 27 Myr Extended Population of Lower Centaurus Crux with a Transiting Two-planet System
Authors: Mackenna L. Wood, Andrew W. Mann, Madyson G. Barber, Jonathan L. Bush, Adam L. Kraus, Benjamin M. Tofflemire, Andrew Vanderburg, Elisabeth R. Newton, Gregory A. Feiden, George Zhou, Luke G. Bouma, Samuel N. Quinn, David J. Armstrong, Ares Osborn, Vardan Adibekyan, Elisa Delgado Mena, Sergio G. Sousa, Jonathan Gagné, Matthew J. Fields, Reilly P. Milburn, Pa Chia Thao, Stephen P. Schmidt, Crystal L. Gnilka, Steve B. Howell, Nicholas M. Law, Carl Ziegler, César Briceño, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Joshua E. Schlieder, Hugh P. Osborn, Joseph D. Twicken, David R. Ciardi, Chelsea X. Huang
Figure caption: A comparison of the period–radius distribution of HD 109833 planets, other transiting planets from young associations (colored dots), and from the field (background contours). The young planets are colored according to their ages. Planets orbiting field stars are shown as density contours. HD 109833 b and HD 109833 c are shown as stars. Planet data is taken from Table 9 of Newton et al. (2022), with the addition of the young planets discovered by Zhou et al. (2022), Bouma et al. (2022), and Barber et al. (2022)
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). IX. A 27 Myr Extended Population of Lower Centaurus Crux with a Transiting Two-planet System
Authors: Mackenna L. Wood, Andrew W. Mann, Madyson G. Barber, Jonathan L. Bush, Adam L. Kraus, Benjamin M. Tofflemire, Andrew Vanderburg, Elisabeth R. Newton, Gregory A. Feiden, George Zhou, Luke G. Bouma, Samuel N. Quinn, David J. Armstrong, Ares Osborn, Vardan Adibekyan, Elisa Delgado Mena, Sergio G. Sousa, Jonathan Gagné, Matthew J. Fields, Reilly P. Milburn, Pa Chia Thao, Stephen P. Schmidt, Crystal L. Gnilka, Steve B. Howell, Nicholas M. Law, Carl Ziegler, César Briceño, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Joshua E. Schlieder, Hugh P. Osborn, Joseph D. Twicken, David R. Ciardi, Chelsea X. Huang
Figure caption: A TESS Sector 38 image colored by flux (see the color bar) on top of a DSS image (grayscale). Red circles indicate the two stars that could reproduce the transit signal for planet b, while orange indicates those that could reproduce c. The bright central star is HD 109833.
Paper: The Orbital Architecture of Qatar-6: A Fully Aligned Three-body System?
Authors: Malena Rice, Songhu Wang, Konstantin Gerbig, Xian-Yu Wang, Fei Dai, Dakotah Tyler, Howard Isaacson, Andrew W. Howard
Figure caption: Geometry of the Qatar-6 AB stellar system. We orient our schematic with north upward and east to the left. The position vector between the two stars (black) and the relative proper-motion vector (purple), scaled to demonstrate the geometry of the system, are nearly linear within the sky plane. Qatar-6 B is moving in a sky-projected direction γ = 179.°11 away from the primary, Qatar-6 A.
Paper: The Orbital Architecture of Qatar-6: A Fully Aligned Three-body System?
Authors: Malena Rice, Songhu Wang, Konstantin Gerbig, Xian-Yu Wang, Fei Dai, Dakotah Tyler, Howard Isaacson, Andrew W. Howard
Figure caption: Keck/HIRES observations from the UT 5/30/22 transit of Qatar-6 A b, with the best-fitting RM model, corresponding to λ = 0.°1 ± 2.°6, overplotted. The associated residuals from the best-fitting model are provided below.
Paper: The Orbital Architecture of Qatar-6: A Fully Aligned Three-body System?
Authors: Malena Rice, Songhu Wang, Konstantin Gerbig, Xian-Yu Wang, Fei Dai, Dakotah Tyler, Howard Isaacson, Andrew W. Howard
Figure caption: Selection of 1000 accepted orbits from the posterior of LOFTI orbit fits to the Qatar-6 AB stellar system. All accepted orbits have nearly edge-on inclinations, with ﹩{i}_{B}={90.17}_{-1.06}^{+1.07\circ} ﹩. Here the R.A. and decl. of the primary star have been centered at (0,0).
Paper: The Orbital Architecture of Qatar-6: A Fully Aligned Three-body System?
Authors: Malena Rice, Songhu Wang, Konstantin Gerbig, Xian-Yu Wang, Fei Dai, Dakotah Tyler, Howard Isaacson, Andrew W. Howard
Figure caption: SAP light curve for Qatar-6 A with transits masked. The star shows significant rotational modulations with a periodicity of P * = 12.962 ± 0.015 days based on a GLS analysis.
Paper: Statistical Analysis of the Dearth of Super-eccentric Jupiters in the Kepler Sample
Authors: Jonathan M. Jackson, Rebekah I. Dawson, Billy Quarles, Jiayin Dong
Figure caption: Expected 2D posterior for orbital period P vs. ρ circ/ρ * of super-eccentric Jupiters. The 45 observed candidates in our sample are overplotted with blue/red bars for planet candidates with/without companions. If the observations matched the prediction, we would expect to see approximately four candidates in the high-probability density region.
Paper: Statistical Analysis of the Dearth of Super-eccentric Jupiters in the Kepler Sample
Authors: Jonathan M. Jackson, Rebekah I. Dawson, Billy Quarles, Jiayin Dong
Figure caption: Top: histogram depicting the relative probability distribution of the predicted mean number of super-eccentric Jupiters in P final interval 1 (red, dotted), interval 2 (blue, dashed), and combined (black). Bottom: histogram depicting the relative probability distribution of the expected number of observed super-eccentric Jupiters, created by sampling from the above distribution of Poisson means.
Paper: Statistical Analysis of the Dearth of Super-eccentric Jupiters in the Kepler Sample
Authors: Jonathan M. Jackson, Rebekah I. Dawson, Billy Quarles, Jiayin Dong
Figure caption: Eccentricity vs. semimajor axis of the 5 planet candidates with the greatest probability of being super-eccentric Jupiters (blue shaded region). From left to right, these are KOI-1193.01, KOI-211.01, KOI-2689.01, KOI3801.01, and Kepler-1746 b. The error bars represent the 68% confidence interval for each candidate’s eccentricity. Three of these confidence intervals cross into the super-eccentric region of parameter space. Shaded regions and deliminator lines are the same as in Figure 1.
Paper: Statistical Analysis of the Dearth of Super-eccentric Jupiters in the Kepler Sample
Authors: Jonathan M. Jackson, Rebekah I. Dawson, Billy Quarles, Jiayin Dong
Figure caption: Top: histogram depicting the relative probability distribution of the expected number of super-eccentric Jupiters from our prediction in Section 2 (identical to bottom panel of Figure 2). Bottom: histogram depicting the relative probability distribution of super-eccentric Jupiters observed in the Kepler sample. The clear difference between these distributions demonstrates that the observations deviate from the prediction.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). IX. A 27 Myr Extended Population of Lower Centaurus Crux with a Transiting Two-planet System
Authors: Mackenna L. Wood, Andrew W. Mann, Madyson G. Barber, Jonathan L. Bush, Adam L. Kraus, Benjamin M. Tofflemire, Andrew Vanderburg, Elisabeth R. Newton, Gregory A. Feiden, George Zhou, Luke G. Bouma, Samuel N. Quinn, David J. Armstrong, Ares Osborn, Vardan Adibekyan, Elisa Delgado Mena, Sergio G. Sousa, Jonathan Gagné, Matthew J. Fields, Reilly P. Milburn, Pa Chia Thao, Stephen P. Schmidt, Crystal L. Gnilka, Steve B. Howell, Nicholas M. Law, Carl Ziegler, César Briceño, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Joshua E. Schlieder, Hugh P. Osborn, Joseph D. Twicken, David R. Ciardi, Chelsea X. Huang
Figure caption: A CMD showing each step of the membership search. The top panel shows the results of Comove, and the cuts made on those results to make a tight core membership. The second panel shows the results of BANYAN Σ and the subsequent cut on CMD position to remove old interlopers and stars with poor color measurements. Candidates that survived this cut are colored by their kinematic membership probability. The bottom panel shows the final membership list, colored by membership probability. Stars with Gaia RUWE > 1.2, possible binaries, are marked as small squares, and form a binary sequence above the main association. Four DSEP magnetic isochrones (Feiden 2016), showing 10, 20, 30, and 40 Myr, are plotted alongside the sequence. In the top two panels, the zero-age main sequence is shown as a black line, derived empirically by Pecaut & Mamajek (2013).
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). IX. A 27 Myr Extended Population of Lower Centaurus Crux with a Transiting Two-planet System
Authors: Mackenna L. Wood, Andrew W. Mann, Madyson G. Barber, Jonathan L. Bush, Adam L. Kraus, Benjamin M. Tofflemire, Andrew Vanderburg, Elisabeth R. Newton, Gregory A. Feiden, George Zhou, Luke G. Bouma, Samuel N. Quinn, David J. Armstrong, Ares Osborn, Vardan Adibekyan, Elisa Delgado Mena, Sergio G. Sousa, Jonathan Gagné, Matthew J. Fields, Reilly P. Milburn, Pa Chia Thao, Stephen P. Schmidt, Crystal L. Gnilka, Steve B. Howell, Nicholas M. Law, Carl Ziegler, César Briceño, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Joshua E. Schlieder, Hugh P. Osborn, Joseph D. Twicken, David R. Ciardi, Chelsea X. Huang
Figure caption: Rotation periods of candidate members of MELANGE-4 as a function of Gaia B  P  − R  P  color. We compare the color–period sequence of candidate members to the younger (∼10 Myr) population of Upper Scorpius (Rebull et al. 2018) and older (45–60 Myr) populations of Carina (CAR), Columba (COL), Tucana-Horologium (THA), and μ Tau (Gagné et al. 2020). As expected, the MELANGE-4 sequence shows more coherence than the sequence of the younger Upper Scorpius. The low-mass candidates rotate slower than those in the 45–60 Myr populations, indicating a younger population that will spin up as they contract onto the main sequence. The high-mass candidates are a mix of still rapidly rotating stars and stars that have begun to spin down.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). IX. A 27 Myr Extended Population of Lower Centaurus Crux with a Transiting Two-planet System
Authors: Mackenna L. Wood, Andrew W. Mann, Madyson G. Barber, Jonathan L. Bush, Adam L. Kraus, Benjamin M. Tofflemire, Andrew Vanderburg, Elisabeth R. Newton, Gregory A. Feiden, George Zhou, Luke G. Bouma, Samuel N. Quinn, David J. Armstrong, Ares Osborn, Vardan Adibekyan, Elisa Delgado Mena, Sergio G. Sousa, Jonathan Gagné, Matthew J. Fields, Reilly P. Milburn, Pa Chia Thao, Stephen P. Schmidt, Crystal L. Gnilka, Steve B. Howell, Nicholas M. Law, Carl Ziegler, César Briceño, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Joshua E. Schlieder, Hugh P. Osborn, Joseph D. Twicken, David R. Ciardi, Chelsea X. Huang
Figure caption: The results of Comove. HD 109833 and neighbors within 30 pc and 2 km s−1, are shown in X-, Y-, and Z-coordinates. The size of the points corresponds inversely to their distance from HD 109833, and the color with the velocity difference, so that the largest points are closest to HD 109833, and the darkest points are most similar in velocity. Stars with Gaia renormalized unit weight error (RUWE) ≥ 1.2 are represented with squares. The velocity differences of binary stars are poor indicators of membership, due to velocity from binary motion. Circles are used to represent stars with Gaia RUWE < 1.2.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). IX. A 27 Myr Extended Population of Lower Centaurus Crux with a Transiting Two-planet System
Authors: Mackenna L. Wood, Andrew W. Mann, Madyson G. Barber, Jonathan L. Bush, Adam L. Kraus, Benjamin M. Tofflemire, Andrew Vanderburg, Elisabeth R. Newton, Gregory A. Feiden, George Zhou, Luke G. Bouma, Samuel N. Quinn, David J. Armstrong, Ares Osborn, Vardan Adibekyan, Elisa Delgado Mena, Sergio G. Sousa, Jonathan Gagné, Matthew J. Fields, Reilly P. Milburn, Pa Chia Thao, Stephen P. Schmidt, Crystal L. Gnilka, Steve B. Howell, Nicholas M. Law, Carl Ziegler, César Briceño, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Joshua E. Schlieder, Hugh P. Osborn, Joseph D. Twicken, David R. Ciardi, Chelsea X. Huang
Figure caption: The spatial and velocity spreads of MELANGE-4, the nearby LCC subpopulations, and Carina. The top row shows the galactic position (X, Y, and Z) for each population, and the bottom row shows the velocities (U, V, and W). The membership candidates for MELANGE-4 are shown in turquoise, and high-probability (>99%) members of LCC-A, LCC-B, LCC-C, and Carina are shown in red, orange, yellow, and purple, respectively. The position of HD 109833 is marked with a turquoise star.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). IX. A 27 Myr Extended Population of Lower Centaurus Crux with a Transiting Two-planet System
Authors: Mackenna L. Wood, Andrew W. Mann, Madyson G. Barber, Jonathan L. Bush, Adam L. Kraus, Benjamin M. Tofflemire, Andrew Vanderburg, Elisabeth R. Newton, Gregory A. Feiden, George Zhou, Luke G. Bouma, Samuel N. Quinn, David J. Armstrong, Ares Osborn, Vardan Adibekyan, Elisa Delgado Mena, Sergio G. Sousa, Jonathan Gagné, Matthew J. Fields, Reilly P. Milburn, Pa Chia Thao, Stephen P. Schmidt, Crystal L. Gnilka, Steve B. Howell, Nicholas M. Law, Carl Ziegler, César Briceño, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Joshua E. Schlieder, Hugh P. Osborn, Joseph D. Twicken, David R. Ciardi, Chelsea X. Huang
Figure caption: Lithium measurements for MELANGE-4. (Left) Fraction of initial Li abundance as a function of absolute K magnitude, overplotted with DSEP magnetic isochrones (Feiden 2016). EWs of association members were converted to Li/Li0 using the curve of growth from Zapatero Osorio et al. (2002). The transparency of the points corresponds to their kinetic membership probability from BANYAN Σ, such that the most likely interlopers are the faintest. (Right) Comparison of MELANGE-4 Li sequence and Li sequences of known associations. For members of each association, Li EWs are shown as a function of Gaia Bp − Rp. EWs of MELANGE-4 members marked with downward triangles are upper limits. The transparency of the points corresponds to their kinetic membership probability from BANYAN Σ, such that the most likely interlopers are the faintest. Li measurements of MELANGE-4 members are supplemented with an additional five measurements from Mamajek et al. (2002), Torres et al. (2006), and Pecaut & Mamajek (2016). The Li measurements of β Pic members are taken from Shkolnik et al. (2017), measurements of ϵ Chamaeleontis members from Murphy et al. (2013), and measurements for Tuc-Hor from da Silva et al. (2009) and Kraus et al. (2014).
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). IX. A 27 Myr Extended Population of Lower Centaurus Crux with a Transiting Two-planet System
Authors: Mackenna L. Wood, Andrew W. Mann, Madyson G. Barber, Jonathan L. Bush, Adam L. Kraus, Benjamin M. Tofflemire, Andrew Vanderburg, Elisabeth R. Newton, Gregory A. Feiden, George Zhou, Luke G. Bouma, Samuel N. Quinn, David J. Armstrong, Ares Osborn, Vardan Adibekyan, Elisa Delgado Mena, Sergio G. Sousa, Jonathan Gagné, Matthew J. Fields, Reilly P. Milburn, Pa Chia Thao, Stephen P. Schmidt, Crystal L. Gnilka, Steve B. Howell, Nicholas M. Law, Carl Ziegler, César Briceño, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Joshua E. Schlieder, Hugh P. Osborn, Joseph D. Twicken, David R. Ciardi, Chelsea X. Huang
Figure caption: The lithium-depletion boundary (LDB) of MELANGE-4. Shown is the color (J − K) and absolute magnitude (K  s ) of members of MELANGE-4. Observed stars with EW(Li) > 300 mÅ are shown as colored dots, and stars with EW(Li) < 300 mÅ as red X’s. Candidate association members that were not observed are shown as gray dots. Orange and yellow lines show the predicted 20 and 30 Myr 99% LDBs using the DSEP magnetic models with two different solar abundances. The 30 Myr GS98 line has been moved up by 0.03 magnitudes to increase visibility. The solid black lines through the brightest M-dwarf with Li absorption, and the faintest likely member without Li absorption show the edges of the boundary region.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). IX. A 27 Myr Extended Population of Lower Centaurus Crux with a Transiting Two-planet System
Authors: Mackenna L. Wood, Andrew W. Mann, Madyson G. Barber, Jonathan L. Bush, Adam L. Kraus, Benjamin M. Tofflemire, Andrew Vanderburg, Elisabeth R. Newton, Gregory A. Feiden, George Zhou, Luke G. Bouma, Samuel N. Quinn, David J. Armstrong, Ares Osborn, Vardan Adibekyan, Elisa Delgado Mena, Sergio G. Sousa, Jonathan Gagné, Matthew J. Fields, Reilly P. Milburn, Pa Chia Thao, Stephen P. Schmidt, Crystal L. Gnilka, Steve B. Howell, Nicholas M. Law, Carl Ziegler, César Briceño, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Joshua E. Schlieder, Hugh P. Osborn, Joseph D. Twicken, David R. Ciardi, Chelsea X. Huang
Figure caption: Corner plots of the MISTTBORN results for TOI-1097b (left) and TOI-1097c (right), with eccentricity locked to e = 0. Posterior distributions are shown as 2D contour plots, with levels corresponding to 1σ, 2σ, and 3σ, and as histograms with the 16th and 84th percentiles marked with dashed lines. Distributions are mostly Gaussian, with the exception of ρ *, which has a long tail toward a less-massive stellar host. The distribution of ρ * is shown on both plots, but only a single value is explored in the fit.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). IX. A 27 Myr Extended Population of Lower Centaurus Crux with a Transiting Two-planet System
Authors: Mackenna L. Wood, Andrew W. Mann, Madyson G. Barber, Jonathan L. Bush, Adam L. Kraus, Benjamin M. Tofflemire, Andrew Vanderburg, Elisabeth R. Newton, Gregory A. Feiden, George Zhou, Luke G. Bouma, Samuel N. Quinn, David J. Armstrong, Ares Osborn, Vardan Adibekyan, Elisa Delgado Mena, Sergio G. Sousa, Jonathan Gagné, Matthew J. Fields, Reilly P. Milburn, Pa Chia Thao, Stephen P. Schmidt, Crystal L. Gnilka, Steve B. Howell, Nicholas M. Law, Carl Ziegler, César Briceño, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Joshua E. Schlieder, Hugh P. Osborn, Joseph D. Twicken, David R. Ciardi, Chelsea X. Huang
Figure caption: Comparison of the PARSEC isochrones to high-probability members of MELANGE-4 (circles). Stars are shaded by their outlier probability, as determined by the mixture model fit. Outliers are not necessarily nonmembers. The red star shows the planet host (HD 109833). The green lines are 100 random draws from the MCMC using the PARSEC isochrones and fit reddening. The inset shows the region around HD 109833 and representative-age model predictions.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). IX. A 27 Myr Extended Population of Lower Centaurus Crux with a Transiting Two-planet System
Authors: Mackenna L. Wood, Andrew W. Mann, Madyson G. Barber, Jonathan L. Bush, Adam L. Kraus, Benjamin M. Tofflemire, Andrew Vanderburg, Elisabeth R. Newton, Gregory A. Feiden, George Zhou, Luke G. Bouma, Samuel N. Quinn, David J. Armstrong, Ares Osborn, Vardan Adibekyan, Elisa Delgado Mena, Sergio G. Sousa, Jonathan Gagné, Matthew J. Fields, Reilly P. Milburn, Pa Chia Thao, Stephen P. Schmidt, Crystal L. Gnilka, Steve B. Howell, Nicholas M. Law, Carl Ziegler, César Briceño, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Joshua E. Schlieder, Hugh P. Osborn, Joseph D. Twicken, David R. Ciardi, Chelsea X. Huang
Figure caption: TESS light curves for Sectors (from top to bottom) 11, 12, 38, and 39. Data for each sector is shown as gray dots, and binned values are shown as black dots. The blue line indicates the model GP fit to the data with uncertainties (shaded region). The times of the transits are marked with dashed and dotted vertical lines for planets (b) and (c), respectively.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). IX. A 27 Myr Extended Population of Lower Centaurus Crux with a Transiting Two-planet System
Authors: Mackenna L. Wood, Andrew W. Mann, Madyson G. Barber, Jonathan L. Bush, Adam L. Kraus, Benjamin M. Tofflemire, Andrew Vanderburg, Elisabeth R. Newton, Gregory A. Feiden, George Zhou, Luke G. Bouma, Samuel N. Quinn, David J. Armstrong, Ares Osborn, Vardan Adibekyan, Elisa Delgado Mena, Sergio G. Sousa, Jonathan Gagné, Matthew J. Fields, Reilly P. Milburn, Pa Chia Thao, Stephen P. Schmidt, Crystal L. Gnilka, Steve B. Howell, Nicholas M. Law, Carl Ziegler, César Briceño, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Joshua E. Schlieder, Hugh P. Osborn, Joseph D. Twicken, David R. Ciardi, Chelsea X. Huang
Figure caption: Best-fit template spectrum (G1V; black) and synthetic photometry (green) compared to the observed photometry of HD 109833 (red). Errors on observed photometry are shown as vertical errors, while horizontal errors indicate the approximate width of the filter. BT-SETTL models (blue) were used to fill in regions of high telluric absorption or beyond the template range. The bottom panel shows the photometric residual in units of standard deviations.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). IX. A 27 Myr Extended Population of Lower Centaurus Crux with a Transiting Two-planet System
Authors: Mackenna L. Wood, Andrew W. Mann, Madyson G. Barber, Jonathan L. Bush, Adam L. Kraus, Benjamin M. Tofflemire, Andrew Vanderburg, Elisabeth R. Newton, Gregory A. Feiden, George Zhou, Luke G. Bouma, Samuel N. Quinn, David J. Armstrong, Ares Osborn, Vardan Adibekyan, Elisa Delgado Mena, Sergio G. Sousa, Jonathan Gagné, Matthew J. Fields, Reilly P. Milburn, Pa Chia Thao, Stephen P. Schmidt, Crystal L. Gnilka, Steve B. Howell, Nicholas M. Law, Carl Ziegler, César Briceño, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Joshua E. Schlieder, Hugh P. Osborn, Joseph D. Twicken, David R. Ciardi, Chelsea X. Huang
Figure caption: Spectra of all association members with measured Li absorption, overplotted with a Li free M-dwarf template (gray; Bochanski et al. 2007). The location of the Li line, 6707.8 Å, is marked with a dashed black line. Two of these stars, TIC 68515382 (light green) and TIC 256168939 (light orange), have EW(Li) < 300  mÅ, and thus are not fully Li-depleted.