adsabs/AstroCLIMB huggingface dataset:
Paper: A Blind Search for Transit Depth Variability with TESS
Authors: Gavin Wang, Néstor Espinoza
Figure caption: Same as Figure 12, but for nested ratio vs. host star mass. The best-fit linear model has slope (0.89 ± 4.93) × 10−2, again consistent with 0.
Paper: A Blind Search for Transit Depth Variability with TESS
Authors: Gavin Wang, Néstor Espinoza
Figure caption: Phased out-of-transit lightcurve for WASP-121b, binned to 2000 points. The best-fit sinusoidal model is overplotted in black.
Paper: High-resolution Imaging of a TESS Control Sample: Verifying a Deficit of Close-in Stellar Companions to Exoplanet Host Stars
Authors: Colin Littlefield, Steve B. Howell, David R. Ciardi, Kathryn V. Lester, Mark E. Everett, Elise Furlan, Rachel A. Matson, Sergio B. Fajardo-Acosta, Crystal L. Gnilka
Figure caption: Top: projected binary separations for the detected companions in the control sample compared against those of the Howell et al. (2021) and Lester et al. (2021) TOI stars whose values of ρ and Δmag place them outside the parameter space of the selection bias. A Kolomogorov–Smirnoff (K-S) test comparing these two distributions has a p-value of 0.07, indicating marginal statistical evidence of a difference. Bottom: as with the top panel, except that mass ratios are compared. The corresponding K-S test has a p-value of 0.2, indicating no statistically significant difference. In both panels we lift the restrictions on spectral type and ρ used in the simulations, so all 26 detected companions around control stars are included.
Paper: High-resolution Imaging of a TESS Control Sample: Verifying a Deficit of Close-in Stellar Companions to Exoplanet Host Stars
Authors: Colin Littlefield, Steve B. Howell, David R. Ciardi, Kathryn V. Lester, Mark E. Everett, Elise Furlan, Rachel A. Matson, Sergio B. Fajardo-Acosta, Crystal L. Gnilka
Figure caption: Two-dimensional histogram showing the predicted number of companions for FGK primaries at various combinations of ρ and Δmag. The color scale is logarithmic. The predictions are from Monte Carlo simulations that use Raghavan et al. (2010) field-binary statistics. The 20 control-star companions detected at 832 nm with separations under 1.″2 are also shown, revealing the conspicuous absence of detected companions at 0.″1 ≲ ρ ≲ 1.″2 and Δmag ≲3 (the region bounded with a thick dashed white line). The simulations predict no such deficit, which we show to be the result of a selection bias that prevented the observation of binaries in this parameter space.
Paper: High-resolution Imaging of a TESS Control Sample: Verifying a Deficit of Close-in Stellar Companions to Exoplanet Host Stars
Authors: Colin Littlefield, Steve B. Howell, David R. Ciardi, Kathryn V. Lester, Mark E. Everett, Elise Furlan, Rachel A. Matson, Sergio B. Fajardo-Acosta, Crystal L. Gnilka
Figure caption: The dependence of gaiaqflag on Δmag and ρ in companion-hosting TOI objects. Binaries with Δmag ≲ 3 and 0.″1 ≲ ρ ≲ 1.″2 (represented with a shaded region in both panels) disproportionately fail the Gaia quality test. As we discuss in the text, sources that fail the Gaia quality test will lack the parameters used to assemble our control sample, creating a powerful selection bias against binaries within this parameter space.
Paper: Spectroscopic Distance, Mass, and Age Estimations for APOGEE DR17
Authors: Alexander Stone-Martinez, Jon A. Holtzman, Julie Imig, Christian Nitschelm, Keivan G. Stassun, Joel R. Brownstein
Figure caption: Blue line in all plots shows the MAD of test stars vs. surface gravity for our model. Red shows the Gaia parallax uncertainty. Figure (a) shows just our model compared to the Gaia error, with the dashed lines showing the quartile of the absolute deviation. Figure (b) shows AstroNN’s (Leung & Bovy 2019) MAD and quartile ranges in green compared to Gaia and our model. Figure (c) shows the Bayesian NMSU distance MAD in black. The deviations reported here are the listed stellar distance from each method compared against the Gaia distances.
Paper: Spectroscopic Distance, Mass, and Age Estimations for APOGEE DR17
Authors: Alexander Stone-Martinez, Jon A. Holtzman, Julie Imig, Christian Nitschelm, Keivan G. Stassun, Joel R. Brownstein
Figure caption: Model fractional error vs. cluster distance for cluster stars. Blue points show the average predicted distance to each cluster. The error bars show the standard deviation of the scatter in distance predictions for stars in each cluster around the mean distance. Scatter of the cluster distance averages is printed for each distance method. Panel (a) shows our model results, panel (b) shows AstroNN (Leung & Bovy 2019), and panel (c) shows NMSU distances. STD of the cluster distance average (orange points) is printed for each plot.
Paper: Spectroscopic Distance, Mass, and Age Estimations for APOGEE DR17
Authors: Alexander Stone-Martinez, Jon A. Holtzman, Julie Imig, Christian Nitschelm, Keivan G. Stassun, Joel R. Brownstein
Figure caption: (a) Residual plot showing dwarf stars over Gaia distance. Red line indicates the 0.13 cutoff threshold (b) Kiel diagram, showing where binary stars live.
Paper: Spectroscopic Distance, Mass, and Age Estimations for APOGEE DR17
Authors: Alexander Stone-Martinez, Jon A. Holtzman, Julie Imig, Christian Nitschelm, Keivan G. Stassun, Joel R. Brownstein
Figure caption: Density plots showing the Kiel and metallicity diagrams and for the full data set ((a) and (c)) and for the training set after the 15% distance uncertainty cutoff ((b) and (d)). Color scale is logarithmic.
Paper: Spectroscopic Distance, Mass, and Age Estimations for APOGEE DR17
Authors: Alexander Stone-Martinez, Jon A. Holtzman, Julie Imig, Christian Nitschelm, Keivan G. Stassun, Joel R. Brownstein
Figure caption: HR diagram showing stars with added cluster distances shown in green (a) Coverage of log g and metallicity parameter space showing stars with added cluster distances shown in green (b).
Paper: Characterization of High-polarization Stars and Blazars with DIPOL-1 at Sierra Nevada Observatory
Authors: J. Otero-Santos, V. Piirola, J. Escudero Pedrosa, I. Agudo, D. Morcuende, A. Sota, V. Casanova, F. J. Aceituno, P. Santos-Sanz
Figure caption: Modulation curve example for the λ/2 plate rotation, averaged from 128 × 2 s exposures of the zero-polarization star HD 219623, in terms of the normalized flux differences (F  o  − F  e )/(F  o  + F  e ). Error bars are smaller than the plotting symbol. The curve shows a Fourier fit with up to fourth harmonics included. The amplitude corresponds to the ∼4% instrumental polarization produced by the Nasmyth mirror (M3). The power in the harmonics 1–3 is negligible (smaller by a factor >200 compared with that in the fourth). The difference in the transmission coefficients of the o- and e-beams is automatically calibrated out in the reduction procedure.
Paper: Characterization of High-polarization Stars and Blazars with DIPOL-1 at Sierra Nevada Observatory
Authors: J. Otero-Santos, V. Piirola, J. Escudero Pedrosa, I. Agudo, D. Morcuende, A. Sota, V. Casanova, F. J. Aceituno, P. Santos-Sanz
Figure caption: Scheme of the DIPOL-1 polarimeter. A rotatable superachromatic λ/2 retarder plate modulates the relative intensities of the two polarized beams produced by the calcite crystal, with an amount proportional to the degree of linear polarization of the incoming radiation. The fluxes of the two polarized stellar images are recorded with a highly sensitive cooled CMOS detector.
Paper: Characterization of High-polarization Stars and Blazars with DIPOL-1 at Sierra Nevada Observatory
Authors: J. Otero-Santos, V. Piirola, J. Escudero Pedrosa, I. Agudo, D. Morcuende, A. Sota, V. Casanova, F. J. Aceituno, P. Santos-Sanz
Figure caption: Polarization degree errors with respect to the exposure time of each image of the 128 image observing cycle. Different markers and colors symbolize different magnitude values.
Paper: Characterization of High-polarization Stars and Blazars with DIPOL-1 at Sierra Nevada Observatory
Authors: J. Otero-Santos, V. Piirola, J. Escudero Pedrosa, I. Agudo, D. Morcuende, A. Sota, V. Casanova, F. J. Aceituno, P. Santos-Sanz
Figure caption: Raw image of the blazar S4 0954+65 observed by DIPOL-1. The white rectangle corresponds to the subfield saved and used in the polarimetry analysis. A slight amount of coma is due to telescope optics misalignment at the time of the observation. Flat-field features are enhanced by a high contrast.
Paper: Characterization of High-polarization Stars and Blazars with DIPOL-1 at Sierra Nevada Observatory
Authors: J. Otero-Santos, V. Piirola, J. Escudero Pedrosa, I. Agudo, D. Morcuende, A. Sota, V. Casanova, F. J. Aceituno, P. Santos-Sanz
Figure caption: Left: DIPOL-1 polarimeter with its CMOS camera on the T90. Right: T90 telescope. Credit: IAA-CSIC.
Paper: The First Photometric Analysis of Two Low-mass-ratio Contact Binary Systems in TESS Survey
Authors: Qiyuan Cheng, Jianping Xiong, Xu Ding, Kaifan Ji, Jiao Li, Chao Liu, Jiangdan Li, Jingxiao Luo, Xin Lyu, Zhanwen Han, Xuefei Chen
Figure caption: Comparison of our sample with low-mass ratio samples from CSS (Christopoulou et al. 2022) and individually studied W UMa samples (Latković et al. 2021) on the mass–radius (panel (a)) and mass–luminosity (panel (b)) diagrams. The black lines are the zero age main sequence with different metallicities (Z). The dashed line, solid line, and dashed dotted line represent the ZAMS with Z = 0.01, Z = 0.02, and Z = 0.03, respectively. The orange line represents the terminal age main sequence. The gray solid and open circles are the primary stars and secondary stars of the compiled samples (W Uma catalog and the 30 new low-mass ratio contact binaries from CSS; Latković et al. 2021). The red symbols represent the TIC 55007847 and the blue symbols represent TIC 63597006. The solid symbols and the open symbols represent the primary stars and the secondary stars, respectively. The different symbols represent the masses obtained from different methods, i.e the triangles, the rectangles, and pentagons are the mass from Equation (16), the method of Poro et al. (2022), and the Equation (17).
Paper: The First Photometric Analysis of Two Low-mass-ratio Contact Binary Systems in TESS Survey
Authors: Qiyuan Cheng, Jianping Xiong, Xu Ding, Kaifan Ji, Jiao Li, Chao Liu, Jiangdan Li, Jingxiao Luo, Xin Lyu, Zhanwen Han, Xuefei Chen
Figure caption: This figure shows the merger status of TIC 55007847 and TIC 63597006 when we use the different dimensionless gyration radii. According to Poro et al. (2022), the k 2 ranges from 0.06 to 0.205. We set ﹩{k}_{1}^{2}=0.06﹩ (fully radiative) in panel (a). The ﹩{k}_{1}^{2}﹩ is 0.1325 (a midstatus) in panel (b), and the ﹩{k}_{1}^{2}﹩ is 0.205 (fully convective) in panel (c). In each panel, the bottom stars are the status of ﹩{k}_{2}^{2}=0.06﹩ and the top stars are the ﹩{k}_{2}^{2}=0.205﹩. The red stars are the TIC 55007847 and the blue stars are the TIC 63597006. Moreover, when M > 1.4 solar mass, k 1 can be regarded as a constant value of 0.18, for our targets. The panel (d) shows the different merger statuses for ﹩{k}_{2}^{2}=0.06﹩, ﹩{k}_{2}^{2}=0.1325﹩ and ﹩{k}_{2}^{2}=0.205﹩.
Paper: The First Photometric Analysis of Two Low-mass-ratio Contact Binary Systems in TESS Survey
Authors: Qiyuan Cheng, Jianping Xiong, Xu Ding, Kaifan Ji, Jiao Li, Chao Liu, Jiangdan Li, Jingxiao Luo, Xin Lyu, Zhanwen Han, Xuefei Chen
Figure caption: The O − C diagram for the object TIC 63597006. Panel (a) shows the result from the Lomb–Scargle method (P 0 = 0.7005181 day), while panel (b) is for the corrected period (P = 0.7008995 day). We see an obvious periodic signal in the panel (b) which could be caused by the orbital motion from the third body or the magnetic activities. The green solid line shows the result of LTTE and the orange solid line shows the sine function fitting. They represent the affection of the third body and magnetic activities, respectively.
Paper: The First Photometric Analysis of Two Low-mass-ratio Contact Binary Systems in TESS Survey
Authors: Qiyuan Cheng, Jianping Xiong, Xu Ding, Kaifan Ji, Jiao Li, Chao Liu, Jiangdan Li, Jingxiao Luo, Xin Lyu, Zhanwen Han, Xuefei Chen
Figure caption: The SED of TIC 63597006. We use data from SkyMapper (U V R), Gaia DR2 (BP G RP), Gaia EDR3 (BP G RP), 2MASS (J H K), and WISE (W1 W2). The error bars are smaller than the symbols’ sizes.
Paper: The First Photometric Analysis of Two Low-mass-ratio Contact Binary Systems in TESS Survey
Authors: Qiyuan Cheng, Jianping Xiong, Xu Ding, Kaifan Ji, Jiao Li, Chao Liu, Jiangdan Li, Jingxiao Luo, Xin Lyu, Zhanwen Han, Xuefei Chen
Figure caption: The photometric result of TIC 63597006. Blue dots are the photometric data from the TESS survey, and the orange solid line is the fitting result. The photometric data do not show an obvious O’Connell effect. Therefore, the model does not include the parameters of a starspot. According to the previous result, TIC 63597006 is a three-bodies system. So, we add a third light fraction to our model.
Paper: The First Photometric Analysis of Two Low-mass-ratio Contact Binary Systems in TESS Survey
Authors: Qiyuan Cheng, Jianping Xiong, Xu Ding, Kaifan Ji, Jiao Li, Chao Liu, Jiangdan Li, Jingxiao Luo, Xin Lyu, Zhanwen Han, Xuefei Chen
Figure caption: The Hertzsprung–Russell diagram of TIC 55007847 and TIC 63597006. The red star is the TIC 55007847. The blue star is the TIC 63597006. The gray dots represent the stars selected from Gaia DR3 using the selection method presented by Lindegren et al. (2018), which have a distance of less than 100 pc.
Paper: The First Photometric Analysis of Two Low-mass-ratio Contact Binary Systems in TESS Survey
Authors: Qiyuan Cheng, Jianping Xiong, Xu Ding, Kaifan Ji, Jiao Li, Chao Liu, Jiangdan Li, Jingxiao Luo, Xin Lyu, Zhanwen Han, Xuefei Chen
Figure caption: The O − C diagram for the object TIC 55007847. Panel (a) shows the result from the Lomb–Scargle method (P 0 = 0.6113643 day), while panel (b) is for the corrected period (P = 0.6117108 day).
Paper: The First Photometric Analysis of Two Low-mass-ratio Contact Binary Systems in TESS Survey
Authors: Qiyuan Cheng, Jianping Xiong, Xu Ding, Kaifan Ji, Jiao Li, Chao Liu, Jiangdan Li, Jingxiao Luo, Xin Lyu, Zhanwen Han, Xuefei Chen
Figure caption: Light curve for the object TIC 55007847. Blue dots are the photometric data from TESS survey, and the orange solid line is the photometric solution. The two red dash line shows the O’Conell effect on the light curve.
Paper: The Active Asteroids Citizen Science Program: Overview and First Results
Authors: Colin Orion Chandler, Chadwick A. Trujillo, William J. Oldroyd, Jay K. Kueny, William A. Burris, Henry H. Hsieh, Jarod A. DeSpain, Nima Sedaghat, Scott S. Sheppard, Kennedy A. Farrell, David E. Trilling, Annika Gustafsson, Mark Jesus Mendoza Magbanua, Michele T. Mazzucato, Milton K. D. Bosch, Tiffany Shaw-Diaz, Virgilio Gonano, Al Lamperti, José A. da Silva Campos, Brian L. Goodwin, Ivan A. Terentev, Charles J. A. Dukes, Sam Deen
Figure caption: Minor planets with activity discoveries resulting from the Active Asteroids project. (a)–(f) are active asteroids and MBC candidates; (g) is an active Centaur; (h)–(l) are active QHAs; (m)–(t) are JFCs. In all panels the object is at center, north is up and east is left, and the FOV is 126″ × 126″. The antisolar (yellow filled arrow) and anti-motion (black arrow with red border) directions as projected on sky are shown in the top-left corner of each image.
Paper: The Active Asteroids Citizen Science Program: Overview and First Results
Authors: Colin Orion Chandler, Chadwick A. Trujillo, William J. Oldroyd, Jay K. Kueny, William A. Burris, Henry H. Hsieh, Jarod A. DeSpain, Nima Sedaghat, Scott S. Sheppard, Kennedy A. Farrell, David E. Trilling, Annika Gustafsson, Mark Jesus Mendoza Magbanua, Michele T. Mazzucato, Milton K. D. Bosch, Tiffany Shaw-Diaz, Virgilio Gonano, Al Lamperti, José A. da Silva Campos, Brian L. Goodwin, Ivan A. Terentev, Charles J. A. Dukes, Sam Deen
Figure caption: This UT 2014 March 28 DECam thumbnail image of active asteroid (62412) 2000 SY178 (at center) received a score of 0.35 via our analysis system (Section 4), below the 0.473 threshold needed to qualify as an activity candidate. The faint tail seen oriented toward a position angle (PA) ∼150° north through east (roughly 7 o’clock) extends beyond the edge of the image. The image FOV is 126″ × 126″, with north up and east left, and an overlaid green reticle as shown to Active Asteroids volunteers. DECam image from Prop. ID 2014A-0479, PI: Sheppard, observer S. Sheppard.
Paper: The Active Asteroids Citizen Science Program: Overview and First Results
Authors: Colin Orion Chandler, Chadwick A. Trujillo, William J. Oldroyd, Jay K. Kueny, William A. Burris, Henry H. Hsieh, Jarod A. DeSpain, Nima Sedaghat, Scott S. Sheppard, Kennedy A. Farrell, David E. Trilling, Annika Gustafsson, Mark Jesus Mendoza Magbanua, Michele T. Mazzucato, Milton K. D. Bosch, Tiffany Shaw-Diaz, Virgilio Gonano, Al Lamperti, José A. da Silva Campos, Brian L. Goodwin, Ivan A. Terentev, Charles J. A. Dukes, Sam Deen
Figure caption: Example orbits of objects representing different dynamical classes, as seen in the Jupiter corotating reference frame. In all frames the Sun (star marker) is at the center, Jupiter (orange marker) is at the right, and the object is indicated by blue markers. All axes are in units of au. (a) Main-belt asteroid and MBC 133P/Elst-Pizarro. (b) Centaur (2060) Chiron. (c) Jupiter-family comet (JFC) 67P/Churyumov-Gerasimenko. (d) (153) Hilda. (e) Quasi-Hilda object (QHO) 282P. (f) Nonperiodic comet C/2020 PV6 (Pan-STARRS).
Paper: The Active Asteroids Citizen Science Program: Overview and First Results
Authors: Colin Orion Chandler, Chadwick A. Trujillo, William J. Oldroyd, Jay K. Kueny, William A. Burris, Henry H. Hsieh, Jarod A. DeSpain, Nima Sedaghat, Scott S. Sheppard, Kennedy A. Farrell, David E. Trilling, Annika Gustafsson, Mark Jesus Mendoza Magbanua, Michele T. Mazzucato, Milton K. D. Bosch, Tiffany Shaw-Diaz, Virgilio Gonano, Al Lamperti, José A. da Silva Campos, Brian L. Goodwin, Ivan A. Terentev, Charles J. A. Dukes, Sam Deen
Figure caption: Jupiter corotating frame plots for the objects presented in this work. In all panels, the Sun (star marker) is at the center, with Jupiter and the minor planet indicated by orange and blue markers, respectively. All axes are in units of au. Acronyms: active asteroid (AA), Jupiter-family comet (JFC), main-belt comet (MBC), and quasi-Hilda comet (QHC).
Paper: The Active Asteroids Citizen Science Program: Overview and First Results
Authors: Colin Orion Chandler, Chadwick A. Trujillo, William J. Oldroyd, Jay K. Kueny, William A. Burris, Henry H. Hsieh, Jarod A. DeSpain, Nima Sedaghat, Scott S. Sheppard, Kennedy A. Farrell, David E. Trilling, Annika Gustafsson, Mark Jesus Mendoza Magbanua, Michele T. Mazzucato, Milton K. D. Bosch, Tiffany Shaw-Diaz, Virgilio Gonano, Al Lamperti, José A. da Silva Campos, Brian L. Goodwin, Ivan A. Terentev, Charles J. A. Dukes, Sam Deen
Figure caption: The weight for the first 1000 images for 10 unique, randomly selected users (numbered by markers 0–9) who classified between 1000 and 10,000 images. Each number represents 20 images classified, and scores are cumulative.
Paper: The PFS View of TOI-677 b: A Spin–Orbit Aligned Warm Jupiter in a Dynamically Hot System 
Authors: Qingru Hu, Malena Rice, Xian-Yu Wang, Songhu Wang, Avi Shporer, Johanna K. Teske, Samuel W. Yee, R. Paul Butler, Stephen Shectman, Jeffrey D. Crane, Karen A. Collins, Kevin I. Collins
Figure caption: Distribution of measured ﹩\left|\lambda \right|﹩ values for hot and warm Jupiters (M p ≥ 0.4 M  J ) in single-star systems as a function of orbital separation a/R ⋆. The vertical dashed gray line marks the rough boundary a/R ⋆ = 11 between hot and warm Jupiters. The systems with hot stars (T eff ≥ 6100 K) are shown as red-edged points, while those with cool stars (T eff < 6100 K) are shown as blue-edged points. The face colors of the points display the orbital eccentricity of the planet, and systems with e > 0.3 are marked as triangles. The updated measurement of TOI-677 b from this work is labeled in the figure.
Paper: The PFS View of TOI-677 b: A Spin–Orbit Aligned Warm Jupiter in a Dynamically Hot System 
Authors: Qingru Hu, Malena Rice, Xian-Yu Wang, Songhu Wang, Avi Shporer, Johanna K. Teske, Samuel W. Yee, R. Paul Butler, Stephen Shectman, Jeffrey D. Crane, Karen A. Collins, Kevin I. Collins
Figure caption: Phase-folded light curves of TESS, SSMKO, Las Cumbres Observatory (LCO) 1 m, and LCO 0.4 m data, with the overplotted best-fit models from our combined fit shown as red dashed lines. The corresponding parameters are listed in Table 4.
Paper: The PFS View of TOI-677 b: A Spin–Orbit Aligned Warm Jupiter in a Dynamically Hot System 
Authors: Qingru Hu, Malena Rice, Xian-Yu Wang, Songhu Wang, Avi Shporer, Johanna K. Teske, Samuel W. Yee, R. Paul Butler, Stephen Shectman, Jeffrey D. Crane, Karen A. Collins, Kevin I. Collins
Figure caption: In-transit RVs and the best-fit models for our PFS, ESPRESSO, and combined data sets, with results corresponding to the three models described in Table 4. The orange and green points label the PFS and ESPRESSO data, respectively. The PFS model is shown as a black dashed line, and the ESPRESSO model is shown as a brown dashed line. Quadratic limb-darkening coefficients were modeled separately for PFS and ESPRESSO as listed in Table 4, so there are two overplotted model curves in the right panel. The RV baseline is subtracted from the RVs, and jitter terms have been added in quadrature to the RV uncertainties.
Paper: The PFS View of TOI-677 b: A Spin–Orbit Aligned Warm Jupiter in a Dynamically Hot System 
Authors: Qingru Hu, Malena Rice, Xian-Yu Wang, Songhu Wang, Avi Shporer, Johanna K. Teske, Samuel W. Yee, R. Paul Butler, Stephen Shectman, Jeffrey D. Crane, Karen A. Collins, Kevin I. Collins
Figure caption: The Kozaipy simulation results for different starting mutual inclinations i mut;0 using the initial conditions listed in Table 5 except that the eccentricity of the inner planet is set to nearly zero (e p ≈ 0). The mutual inclination oscillation is shown in red, while the eccentricity oscillation is in blue. The blue dashed lines show when the eccentricity oscillation reaches the currently observed value for TOI-677 b, and the red dashed lines demarcate the mutual inclinations at those times.
Paper: A Self-consistent Data-driven Model for Determining Stellar Parameters from Optical and Near-infrared Spectra
Authors: Logan Sizemore, Diego Llanes, Marina Kounkel, Brian Hutchinson, Keivan G. Stassun, Vedant Chandra
Figure caption: Comparison between the derived parameters from APOGEE Net and BOSS Net (including both BOSS and LAMOST spectra) of the sames sources, using the withheld test sample not used in training.
Paper: A Self-consistent Data-driven Model for Determining Stellar Parameters from Optical and Near-infrared Spectra
Authors: Logan Sizemore, Diego Llanes, Marina Kounkel, Brian Hutchinson, Keivan G. Stassun, Vedant Chandra
Figure caption: Top: sample of labels used to train APOGEE Net. Bottom: predicted parameters for SDSS I-IV DR18 and for SDSS-V APOGEE data.
Paper: A Blind Search for Transit Depth Variability with TESS
Authors: Gavin Wang, Néstor Espinoza
Figure caption: Radius–period distribution for planets in our sample, color-coded by number of transits. The majority of planets in our sample are hot Jupiters with period less than 10 days and radius ∼10–20 R ⊕. A small number of roughly Earth-sized planets are also present.