adsabs/AstroCLIMB huggingface dataset:
Paper: The TESS-Keck Survey. VIII. Confirmation of a Transiting Giant Planet on an Eccentric 261 Day Orbit with the Automated Planet Finder Telescope 
Authors: Paul A. Dalba, Stephen R. Kane, Diana Dragomir, Steven Villanueva, Karen A. Collins, Thomas Lee Jacobs, Daryll M. LaCourse, Robert Gagliano, Martti H. Kristiansen, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Andrew Vanderburg, Benjamin Fulton, Howard Isaacson, Judah Van Zandt, Andrew W. Howard, Daniel P. Thorngren, Steve B. Howell, Natalie M. Batalha, Ashley Chontos, Ian J. M. Crossfield, Courtney D. Dressing, Daniel Huber, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Aida Behmard, Corey Beard, Casey L. Brinkman, Steven Giacalone, Michelle L. Hill, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Alex S. Polanski, Malena Rice, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Paul Benni, Pat Boyce, Thomas M. Esposito, E. Girardin, Didier Laloum, Pablo Lewin, Christopher R. Mann, Franck Marchis, Richard P. Schwarz, Gregor Srdoc, Jana Steuer, Thirupathi Sivarani, Athira Unni, Nora L. Eisner, Tara Fetherolf, Zhexing Li, Xinyu Yao, Joshua Pepper, George R. Ricker, Roland Vanderspek, David W. Latham, S. Seager, Joshua N. Winn, Jon M. Jenkins, Christopher J. Burke, Jason D. Eastman, Michael B. Lund, David R. Rodriguez, Pamela Rowden, Eric B. Ting, Jesus Noel Villaseñor
Figure caption: Limiting magnitudes (Δm) for the nondetection of a neighboring star based on the speckle imaging from ‘Alopeke. The inset shows the speckle image at 832 nm.
Paper: Discovery of CWISE J052306.42−015355.4, an Extreme T Subdwarf Candidate
Authors: Hunter Brooks, J. Davy Kirkpatrick, Dan Caselden, Adam C. Schneider, Aaron M. Meisner, Jacqueline K. Faherty, S. L. Casewell, Marc J. Kuchner
Figure caption: Color−color diagram adapted from Figure 1 of Meisner et al. (2021) and Kirkpatrick et al. (2016). The gray box was described in Meisner et al. (2021) to contain all known esdTs and candidates; therefore, we call it the esdT box. The location of J0523−0153 (red circle) places it well within the esdT box. L dwarfs (blue downward triangles), T dwarfs (orange upward triangles), young L (purple diamonds), young T dwarfs (green squares), L subdwarfs (light blue circles), and T subdwarfs (pink stars) from the 20 pc L, T, and Y dwarf sample of Kirkpatrick et al. (2021a) are shown for comparison, as are the extreme T subdwarf candidates from the BYW papers (black crosses) of Schneider et al. (2020) and Meisner et al. (2021). WISEA J153429.75−104303.3 (Kirkpatrick et al. 2021b) has a large J − W2 color, falling at a J − W2 value that is too red for this graph. Both CWISEP J050521.29–591311.7 and CWISEP J090536.35+740009.1 from Meisner et al. 2020 are shown by maroon crosses. Objects in the esdT box are: 1: J0523−0153, 2: J0905+7400, 3: J0414−5854, 4: J2217−1454, 5: J0505−5913, 6: J1810−1010, and 7: J0738−6643 (all of these objects can be found in Table 2).
Paper: The Scorpion Planet Survey: Wide-orbit Giant Planets Around Young A-type Stars
Authors: Kevin Wagner, Dániel Apai, Markus Kasper, Melissa McClure, Massimo Robberto
Figure caption: Confirmed substellar companions among Sco-Cen A-type stars. These three objects span masses of ∼4–30 M Jup and separations of ∼15–100 au. The discoveries and initial analyses of HIP 75056Ab, HD 95086b, and HIP 65426b can be found in Wagner et al. (2020), Rameau et al. (2013), and Chauvin et al. (2017), respectively.
Paper: A 20 Second Cadence View of Solar-type Stars and Their Planets with TESS: Asteroseismology of Solar Analogs and a Recharacterization of π Men c
Authors: Daniel Huber, Timothy R. White, Travis S. Metcalfe, Ashley Chontos, Michael M. Fausnaugh, Cynthia S. K. Ho, Vincent Van Eylen, Warrick H. Ball, Sarbani Basu, Timothy R. Bedding, Othman Benomar, Diego Bossini, Sylvain Breton, Derek L. Buzasi, Tiago L. Campante, William J. Chaplin, Jørgen Christensen-Dalsgaard, Margarida S. Cunha, Morgan Deal, Rafael A. García, Antonio García Muñoz, Charlotte Gehan, Lucía González-Cuesta, Chen Jiang, Cenk Kayhan, Hans Kjeldsen, Mia S. Lundkvist, Stéphane Mathis, Savita Mathur, Mário J. P. F. G. Monteiro, Benard Nsamba, Jia Mian Joel Ong, Erika Pakštienė, Aldo M. Serenelli, Victor Silva Aguirre, Keivan G. Stassun, Dennis Stello, Sissel Norgaard Stilling, Mark Lykke Winther, Tao Wu, Thomas Barclay, Tansu Daylan, Maximilian N. Günther, J. J. Hermes, Jon M. Jenkins, David W. Latham, Alan M. Levine, George R. Ricker, Sara Seager, Avi Shporer, Joseph D. Twicken, Roland K. Vanderspek, Joshua N. Winn
Figure caption: Planet radius versus orbital period for Kepler exoplanets orbiting asteroseismic host stars from Van Eylen et al. (2018a). The shaded area shows the best-fit model for the radius gap as a function of orbital period from Van Eylen et al. (2018a). The rectangle covers published radii (including 1σ uncertainties) for π Men c in the literature. The triangle marks the position of π Men c from our analysis, with the error bar being smaller than the symbol size.
Paper: Discovery of CWISE J052306.42−015355.4, an Extreme T Subdwarf Candidate
Authors: Hunter Brooks, J. Davy Kirkpatrick, Dan Caselden, Adam C. Schneider, Aaron M. Meisner, Jacqueline K. Faherty, S. L. Casewell, Marc J. Kuchner
Figure caption: The movement of J0523−0153 from WISE in 2010 through NEOWISE in 2019. The green circle shows the position of J0523−0153 in 2010, and the red circle shows it in 2019.
Paper: Discovery of CWISE J052306.42−015355.4, an Extreme T Subdwarf Candidate
Authors: Hunter Brooks, J. Davy Kirkpatrick, Dan Caselden, Adam C. Schneider, Aaron M. Meisner, Jacqueline K. Faherty, S. L. Casewell, Marc J. Kuchner
Figure caption: VISTA Hemisphere Survey (DR6) J-band image is on the left alongside the WISE W2-band image on the right. Both figures show the same patch of sky at the same scale, which is indicated on the right-hand panel. The purple circle is J0523−0153 and the blue circle is a nearby object that can be used as a reference.
Paper: Scanning Disk Rings and Winds in CO at 0.01–10 au: A High-resolution M-band Spectroscopy Survey with IRTF-iSHELL
Authors: Andrea Banzatti, Kirsten M. Abernathy, Sean Brittain, Arthur D. Bosman, Klaus M. Pontoppidan, Adwin Boogert, Stanley Jensen, John Carr, Joan Najita, Sierra Grant, Rocio M. Sigler, Michael A. Sanchez, Joshua Kern, John T. Rayner
Figure caption: Comparison between inner dust and CO gas radii for the iSHELL (left) and CRIRES (right) surveys. The samples are ordered from bottom to top by the measured CO v2/v1 ratio (right axis with upper limits in parentheses, displaying the measured value for BC in triangular lines). The names of disks with evidence for an inner dust cavity from the infrared index n 13–30 > 0 are marked in bold italics. R NIR is the measured inner dust radius from H- or K-band interferometry with the Very Large Telescope Interferometer (VLTI; Lazareff et al. 2017; Gravity Collaboration et al. 2019; 9; The GRAVITY Collaboration et al. 2021). R subl is an empirical estimate of R NIR as a function of the stellar luminosity based on data collected in Marcos-Arenal et al. (2021); see Appendix D. R 10% and R 50% are estimates of the CO emitting radius from the HW10% and HWHM as explained in Section 4.8. Error bars (thin lines) are dominated by the uncertainty in disk inclinations. R mm,cav reports the approximate size of an inner dust cavity from spatially resolved millimeter interferometry (Huang et al. 2018; Pinilla et al. 2018; Francis & van der Marel 2020).