adsabs/AstroCLIMB huggingface dataset:
Paper: Searching for GEMS: Confirmation of TOI-5573 b, a Cool, Saturn-like Planet Orbiting an M Dwarf 
Authors: Rachel B. Fernandes, Shubham Kanodia, Megan Delamer, Andrew Hotnisky, Te Han, Caleb I. Cañas, Jessica Libby-Roberts, Varghese Reji, Arvind F. Gupta, Jaime A. Alvarado-Montes, Chad F. Bender, Cullen H. Blake, William D. Cochran, Zoë L. de Beurs, Scott A. Diddams, Jiayin Dong, Mark E. Everett, Eric B. Ford, Samuel Halverson, Jesus Higuera, Henry A. Kobulnicky, Daniel M. Krolikowski, Alexander Larsen, Andrea S.J. Lin, Suvrath Mahadevan, Michael W. McElwain, Andrew Monson, Joe P. Ninan, Leonardo A. Paredes, Yatrik G. Patel, Paul Robertson, Gabrielle Ross, Arpita Roy, Christian Schwab, Gudmundur Stefansson, Daniel J. Stevens, Andrew M. Vanderburg, Jason Wright
Figure caption: Planet radius vs. mass for TOI-5573 b (highlighted by a green circle) alongside other GEMS with masses between 95 and 850 M⊕. The stellar effective temperature is color-coded for each planet, and for comparison, planets around FGK-type stars are displayed in gray with density contours at 0.3, 0.5, 0.8, 1.0, 1.2, and 1.5 g cm−3.
Paper: Searching for GEMS: Confirmation of TOI-5573 b, a Cool, Saturn-like Planet Orbiting an M Dwarf 
Authors: Rachel B. Fernandes, Shubham Kanodia, Megan Delamer, Andrew Hotnisky, Te Han, Caleb I. Cañas, Jessica Libby-Roberts, Varghese Reji, Arvind F. Gupta, Jaime A. Alvarado-Montes, Chad F. Bender, Cullen H. Blake, William D. Cochran, Zoë L. de Beurs, Scott A. Diddams, Jiayin Dong, Mark E. Everett, Eric B. Ford, Samuel Halverson, Jesus Higuera, Henry A. Kobulnicky, Daniel M. Krolikowski, Alexander Larsen, Andrea S.J. Lin, Suvrath Mahadevan, Michael W. McElwain, Andrew Monson, Joe P. Ninan, Leonardo A. Paredes, Yatrik G. Patel, Paul Robertson, Gabrielle Ross, Arpita Roy, Christian Schwab, Gudmundur Stefansson, Daniel J. Stevens, Andrew M. Vanderburg, Jason Wright
Figure caption: Stellar metallicity vs. planet density TOI-5573 b (highlighted by a green circle) alongside other GEMS, color-coded by planet radius, with planets around FGK-type stars are displayed in gray.
Paper: Searching for GEMS: Confirmation of TOI-5573 b, a Cool, Saturn-like Planet Orbiting an M Dwarf 
Authors: Rachel B. Fernandes, Shubham Kanodia, Megan Delamer, Andrew Hotnisky, Te Han, Caleb I. Cañas, Jessica Libby-Roberts, Varghese Reji, Arvind F. Gupta, Jaime A. Alvarado-Montes, Chad F. Bender, Cullen H. Blake, William D. Cochran, Zoë L. de Beurs, Scott A. Diddams, Jiayin Dong, Mark E. Everett, Eric B. Ford, Samuel Halverson, Jesus Higuera, Henry A. Kobulnicky, Daniel M. Krolikowski, Alexander Larsen, Andrea S.J. Lin, Suvrath Mahadevan, Michael W. McElwain, Andrew Monson, Joe P. Ninan, Leonardo A. Paredes, Yatrik G. Patel, Paul Robertson, Gabrielle Ross, Arpita Roy, Christian Schwab, Gudmundur Stefansson, Daniel J. Stevens, Andrew M. Vanderburg, Jason Wright
Figure caption: Equilibrium temperature vs. planet density TOI-5573 b (highlighted by a green circle) alongside other GEMS, with data points color-coded by planet radius, with planets around FGK-type stars are displayed in gray. There are notably no inflated hot Jupiters around M dwarfs.
Paper: Resolving the Unresolved: Using NESSI to Search for Unresolved Companions in Low-mass Disk Wide Binaries
Authors: Zachary D. Hartman, Gerard van Belle, Sébastien Lépine, Mark E. Everett, Ilija Medan
Figure caption: Distribution of the projected physical separations for the 32 inner binaries that were detected in either our NESSI search, N. M. Law et al. (2010), or Gaia DR3 as resolved triples. The two vertical dashed lines represent the peaks of the separation distribution for solar-type stars at 51 au (black line, from D. Raghavan et al. 2010) and for M dwarfs at 20 au (blue line, from J. G. Winters et al. 2019). We note the small number statistics here and the need to find more of these close binaries in very wide systems to fill in this distribution.
Paper: Resolving the Unresolved: Using NESSI to Search for Unresolved Companions in Low-mass Disk Wide Binaries
Authors: Zachary D. Hartman, Gerard van Belle, Sébastien Lépine, Mark E. Everett, Ilija Medan
Figure caption: Color–magnitude diagram of our wide binary sample, with both the primary and secondary components shown. True wide binaries with no additional companions resolved by NESSI are marked by cyan circles, wide binaries containing a speckle-detected third companion are marked by red stars, and Gaia-resolved higher-order multiple systems are shown as gold triangles. For the higher-order multiples detected by speckle imaging, both the primary and secondary components are marked with stars, however only one may be a binary. For the Gaia-resolved triples, only the two components observed by NESSI are shown and some of these have speckle detections themselves. We also include the systems observed by N. M. Law et al. (2010) as blue circles (true wide binaries—no detected third component) and violet stars (higher-order multiples).
Paper: Resolving the Unresolved: Using NESSI to Search for Unresolved Companions in Low-mass Disk Wide Binaries
Authors: Zachary D. Hartman, Gerard van Belle, Sébastien Lépine, Mark E. Everett, Ilija Medan
Figure caption: Widest projected physical separations of the 50 systems in our sample plotted against distance to the primary component of the wide binary. Blue points show the location of systems which are true binaries according to NESSI and Gaia. Gold points indicate the systems which are higher-order multiples according to NESSI (stars), Gaia (triangles), and Simbad (squares). Red points and violet stars represent the same for the N. M. Law et al. (2010) sample. The red lines indicate the upper (3600″) and lower (2″) search radii of SUPERWIDE in this plot. The vertical black dashed line shows the median dividing line used in our analysis using only our NESSI results, while the vertical green dashed line represents the 4000 au upper selection used by N. M. Law et al. (2010).
Paper: Resolving the Unresolved: Using NESSI to Search for Unresolved Companions in Low-mass Disk Wide Binaries
Authors: Zachary D. Hartman, Gerard van Belle, Sébastien Lépine, Mark E. Everett, Ilija Medan
Figure caption: Data products produced from the speckle data reduction. Left: reconstructed image in the red filter (832 nm) for the target star (UCAC4706-053644). A binary is detected at 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩172 with a delta magnitude of 0.52. A ghost image at 180° is seen as well. This ghost image is not a third companion but is an artifact of the image reconstruction. The true companion is the brighter component to the lower left of the target star in the middle. Right: contrast curves for all of the observed targets in our sample. Blue lines highlight the contrast curves for the 562 nm filter, while red lines do the same for the 832 nm filter.
Paper: Deep Reinforcement Learning for Efficient Scheduling of Ground-based Astronomical Observations
Authors: Hai Cao, Shaoming Hu, Junju Du, Xu Chen, Shuqi Liu, Shuai Feng, Bo Zhang, Yuchen Jiang
Figure caption: Flow scheme of astronomical observation scheduling. Using the features derived from preprocessing the requirements as inputs, the pointer network generates the target’s probability distribution, and an observation plan is created by successively selecting targets.
Paper: Deep Reinforcement Learning for Efficient Scheduling of Ground-based Astronomical Observations
Authors: Hai Cao, Shaoming Hu, Junju Du, Xu Chen, Shuqi Liu, Shuai Feng, Bo Zhang, Yuchen Jiang
Figure caption: The decoder comprises an LSTM module, two dense layers, and a learnable parameters set. The LSTM takes the outputs of the encoder as input to form a hybrid context to capture the sequence states. The outputs of the two dense layers are added, and the sum is sent to the learnable parameters block. After adding the result with the logarithmic mask, the softmax layer calculates the probability distribution of unscheduled targets.
Paper: Deep Reinforcement Learning for Efficient Scheduling of Ground-based Astronomical Observations
Authors: Hai Cao, Shaoming Hu, Junju Du, Xu Chen, Shuqi Liu, Shuai Feng, Bo Zhang, Yuchen Jiang
Figure caption: The encoder comprises two structurally enhanced transformer layers. Embedded static and dynamic features are concatenated and then fed to the encoder. The transformer layers recursively encode the features with the attention mask and previous outputs.
Paper: Resolving the Unresolved: Using NESSI to Search for Unresolved Companions in Low-mass Disk Wide Binaries
Authors: Zachary D. Hartman, Gerard van Belle, Sébastien Lépine, Mark E. Everett, Ilija Medan
Figure caption: Higher-order multiplicity fraction as a function of widest projected physical separation in the combined sample of N. M. Law et al. (2010) and our NESSI observations. The final bin at 105 contains only two systems, and therefore its value is questionable. We do not see evidence of increasing higher-order multiplicity at increasing physical separations.
Paper: Detailed Analysis of Six Contact Binaries and their Possible Origin
Authors: Somayeh Soomandar, Lorne Nelson, Joshua Aiken
Figure caption: Evolution of potential progenitor binaries for contact binary systems in the orbital period–age (Porb−t) plane. The solid lines show the evolution of primordial binaries that have initial masses of 1.0 and 0.8 M⊙ and the dashed lines correspond to initial masses of 2.0 and 1.8 M⊙. The black, blue, and red curves correspond to cases for which β = 0 (conservative mass transfer), 0.5, and 1 (completely nonconservative mass transfer), respectively. The initial orbital periods are either 1 or 3 days (as can be inferred from the graph). The black, blue, and red stars denote the endpoints at which the tracks produce a contact binary. Note that the red triangle corresponds to a ZACV with an initial period of 51 days. The other red-dashed vertical line leads to the creation of another ZACV containing a Helium White Dwarf with a period of 131 days. Depending on the initial conditions, LTCB systems, intermediate temperature contact binaries (ITCB) systems, or β Lyrae binaries can be produced. Note that two insets are used to delineate the Porbs of the LTCB and ITCB systems.
Paper: Detailed Analysis of Six Contact Binaries and their Possible Origin
Authors: Somayeh Soomandar, Lorne Nelson, Joshua Aiken
Figure caption: Left panel: diagram of the orbital angular momentum vs. total mass of the binary systems. Right panel: the position of the contact binary components in the M−L plane.
Paper: Detailed Analysis of Six Contact Binaries and their Possible Origin
Authors: Somayeh Soomandar, Lorne Nelson, Joshua Aiken
Figure caption: Schematic diagram of the two types of eclipsing binaries. Note that the dotted–dashed line corresponds to a component that is being eclipsed.
Paper: A 16 Myr Super-Neptune in Upper Centaurus Lupus and a Preliminary Survey of Transiting Planets in Sco-Cen with TESS
Authors: Sydney Vach, George Zhou, Andrew W. Mann, Madyson G. Barber, Tyler R. Fairnington, Chelsea X. Huang, James G. Rogers, Luke G. Bouma, Joachim Krüger, Duncan Wright, Annabelle E. Niblett, Jack M. Nelson, Samuel N. Quinn, David W. Latham, Allyson Bieryla, Karen A. Collins, Michelle Kunimoto, Cristilyn N. Watkins, Richard P. Schwarz, Kevin I. Collins, Ramotholo Sefako, Keith Horne, Steve B. Howell, Catherine A. Clark, Colin Littlefield, Jessie L. Christiansen, Zahra Essack, Joshua N. Winn
Figure caption: Galactic coordinates (l,  b) of literature Sco-Cen (gray) members (see K. L. Luhman 2022, and references within). TIC 88785435 (red star) is a member of the classically defined UCL subpopulation. S. Ratzenböck et al. (2023b) identified TIC 88785435 as a high-confidence candidate member of the kinematically distinct ϕ Lup substructure (salmon circles) primarily within UCL. ϕ Lup candidate members outlined in black are rotationally and photometrically validated members of the Sco-Cen population (L. M. Rebull et al. 2018, 2022).
Paper: A 16 Myr Super-Neptune in Upper Centaurus Lupus and a Preliminary Survey of Transiting Planets in Sco-Cen with TESS
Authors: Sydney Vach, George Zhou, Andrew W. Mann, Madyson G. Barber, Tyler R. Fairnington, Chelsea X. Huang, James G. Rogers, Luke G. Bouma, Joachim Krüger, Duncan Wright, Annabelle E. Niblett, Jack M. Nelson, Samuel N. Quinn, David W. Latham, Allyson Bieryla, Karen A. Collins, Michelle Kunimoto, Cristilyn N. Watkins, Richard P. Schwarz, Kevin I. Collins, Ramotholo Sefako, Keith Horne, Steve B. Howell, Catherine A. Clark, Colin Littlefield, Jessie L. Christiansen, Zahra Essack, Joshua N. Winn
Figure caption: Top three panels: TESS FFI light curves (gray) for TIC 88785435 across Sectors 11, 38, and 65. We model the stellar activity using a spline fit and the transits are modeled with batman using our best-fit parameters from our global model (purple). The transits of TIC 88785435b are marked by purple triangles. Bottom two panels: phase-folded TESS transit and best-fit model of the super-Neptune, TIC 88785435b, and the model residuals.
Paper: A 16 Myr Super-Neptune in Upper Centaurus Lupus and a Preliminary Survey of Transiting Planets in Sco-Cen with TESS
Authors: Sydney Vach, George Zhou, Andrew W. Mann, Madyson G. Barber, Tyler R. Fairnington, Chelsea X. Huang, James G. Rogers, Luke G. Bouma, Joachim Krüger, Duncan Wright, Annabelle E. Niblett, Jack M. Nelson, Samuel N. Quinn, David W. Latham, Allyson Bieryla, Karen A. Collins, Michelle Kunimoto, Cristilyn N. Watkins, Richard P. Schwarz, Kevin I. Collins, Ramotholo Sefako, Keith Horne, Steve B. Howell, Catherine A. Clark, Colin Littlefield, Jessie L. Christiansen, Zahra Essack, Joshua N. Winn
Figure caption: Stellar rotation period as a function of effective temperature for TIC 88785435 (red star) from the TESS light curves. We plot UCL/LCC members with rotation periods presented in L. M. Rebull et al. (2022; gray squares). The subset of stars identified as candidate members of the ϕ Lup subpopulations are highlighted by the salmon circles.
Paper: A 16 Myr Super-Neptune in Upper Centaurus Lupus and a Preliminary Survey of Transiting Planets in Sco-Cen with TESS
Authors: Sydney Vach, George Zhou, Andrew W. Mann, Madyson G. Barber, Tyler R. Fairnington, Chelsea X. Huang, James G. Rogers, Luke G. Bouma, Joachim Krüger, Duncan Wright, Annabelle E. Niblett, Jack M. Nelson, Samuel N. Quinn, David W. Latham, Allyson Bieryla, Karen A. Collins, Michelle Kunimoto, Cristilyn N. Watkins, Richard P. Schwarz, Kevin I. Collins, Ramotholo Sefako, Keith Horne, Steve B. Howell, Catherine A. Clark, Colin Littlefield, Jessie L. Christiansen, Zahra Essack, Joshua N. Winn
Figure caption: Gemini South 8 m blue (562 nm) and red (832 nm) arm diffraction limited images and 5σ contrast curves of TIC 88785435. No companions were found within detection limits.
Paper: A 16 Myr Super-Neptune in Upper Centaurus Lupus and a Preliminary Survey of Transiting Planets in Sco-Cen with TESS
Authors: Sydney Vach, George Zhou, Andrew W. Mann, Madyson G. Barber, Tyler R. Fairnington, Chelsea X. Huang, James G. Rogers, Luke G. Bouma, Joachim Krüger, Duncan Wright, Annabelle E. Niblett, Jack M. Nelson, Samuel N. Quinn, David W. Latham, Allyson Bieryla, Karen A. Collins, Michelle Kunimoto, Cristilyn N. Watkins, Richard P. Schwarz, Kevin I. Collins, Ramotholo Sefako, Keith Horne, Steve B. Howell, Catherine A. Clark, Colin Littlefield, Jessie L. Christiansen, Zahra Essack, Joshua N. Winn
Figure caption: Phase-folded ground-based transit observations of TIC 88785435b (gray, binned in purple). Overlaid are our best-fit transit models via batman for each observation.
Paper: A Pair of Dynamically Interacting Sub-Neptunes around TOI-6054
Authors: Maxwell A. Kroft, Thomas G. Beatty, Ian J. M. Crossfield, Joseph R. Livesey, Juliette Becker, Jacob K. Luhn, Paul Robertson, Allyson Bieryla, David R. Ciardi, Catherine A. Clark, Maria V. Goliguzova, Steve B. Howell, Jack J. Lissauer, Colin Littlefield, Michael B. Lund, Boris S. Safonov, Joseph M. Akana Murphy, Natalie M. Batalha, Malik Bossett, Jonathan Brande, Tansu Daylan, Courtney Dressing, Anna Gagnebin, Daniel Huber, Howard Isaacson, Stephen R. Kane, Laura Kreidberg, David W. Latham, Rafael Luque, Alex S. Polanski, Pranav H. Premnath, Maleah Rhem, Claire J. Rogers, Emma V. Turtelboom
Figure caption: Simulated transmission spectra and NIRCam observations of TOI-6054b for a range of possible atmospheric metallicities (Section 5.3). Based on the mass of the planet, we expect the M/H = 100× solar metallicity to be the most likely scenario. The simulated data points are for a pair of NIRCam observations of the system: one using F322W2+DHS and one using F444W+DHS. These observations would be able to strongly differentiate between a low-mean-molecular-weight and a high-mean-molecular-weight atmosphere on TOI-6054b at >10σ. Also marked with the vertical dashed line is the location of the He triplet near 1083 nm. Based on our equivalent-width estimates in Section 5.1, TOI-6054b’s transit depth will be roughly 550 ppm at these wavelengths if the planet is losing its atmosphere. This would be readily observable in a single transit observation using NIRCam DHS.
Paper: A Pair of Dynamically Interacting Sub-Neptunes around TOI-6054
Authors: Maxwell A. Kroft, Thomas G. Beatty, Ian J. M. Crossfield, Joseph R. Livesey, Juliette Becker, Jacob K. Luhn, Paul Robertson, Allyson Bieryla, David R. Ciardi, Catherine A. Clark, Maria V. Goliguzova, Steve B. Howell, Jack J. Lissauer, Colin Littlefield, Michael B. Lund, Boris S. Safonov, Joseph M. Akana Murphy, Natalie M. Batalha, Malik Bossett, Jonathan Brande, Tansu Daylan, Courtney Dressing, Anna Gagnebin, Daniel Huber, Howard Isaacson, Stephen R. Kane, Laura Kreidberg, David W. Latham, Rafael Luque, Alex S. Polanski, Pranav H. Premnath, Maleah Rhem, Claire J. Rogers, Emma V. Turtelboom
Figure caption: Left column: BIS or stellar activity indices vs. RV. The data are shown in black and the best-fit bootstrapped linear regression model is shown in green with a 1σ envelope. The best-fit slope and its uncertainties are printed at the top of each plot. Right column: Lomb–Scargle periodograms, with the orbital frequencies of TOI-6054b and TOI-6054c shown in blue and purple, respectively. The 1% false alarm value is in red. The top row is the BIS, the middle row is the S-index, and the bottom row is the Hα index.
Paper: A Pair of Dynamically Interacting Sub-Neptunes around TOI-6054
Authors: Maxwell A. Kroft, Thomas G. Beatty, Ian J. M. Crossfield, Joseph R. Livesey, Juliette Becker, Jacob K. Luhn, Paul Robertson, Allyson Bieryla, David R. Ciardi, Catherine A. Clark, Maria V. Goliguzova, Steve B. Howell, Jack J. Lissauer, Colin Littlefield, Michael B. Lund, Boris S. Safonov, Joseph M. Akana Murphy, Natalie M. Batalha, Malik Bossett, Jonathan Brande, Tansu Daylan, Courtney Dressing, Anna Gagnebin, Daniel Huber, Howard Isaacson, Stephen R. Kane, Laura Kreidberg, David W. Latham, Rafael Luque, Alex S. Polanski, Pranav H. Premnath, Maleah Rhem, Claire J. Rogers, Emma V. Turtelboom
Figure caption: Top: density plot of the resonant argument given at the top of the plot vs. simulation time, with the color scale showing the number of simulations in each bin. The initial ∼800 yr settling phase is marked with a black vertical line. Bottom: density plot of the difference between the arguments of periastron of the two planets vs. simulation time, with the color scale showing the number of simulations in each bin. The diffusion period is marked in this plot as well.
Paper: A Pair of Dynamically Interacting Sub-Neptunes around TOI-6054
Authors: Maxwell A. Kroft, Thomas G. Beatty, Ian J. M. Crossfield, Joseph R. Livesey, Juliette Becker, Jacob K. Luhn, Paul Robertson, Allyson Bieryla, David R. Ciardi, Catherine A. Clark, Maria V. Goliguzova, Steve B. Howell, Jack J. Lissauer, Colin Littlefield, Michael B. Lund, Boris S. Safonov, Joseph M. Akana Murphy, Natalie M. Batalha, Malik Bossett, Jonathan Brande, Tansu Daylan, Courtney Dressing, Anna Gagnebin, Daniel Huber, Howard Isaacson, Stephen R. Kane, Laura Kreidberg, David W. Latham, Rafael Luque, Alex S. Polanski, Pranav H. Premnath, Maleah Rhem, Claire J. Rogers, Emma V. Turtelboom
Figure caption: Mass–radius diagram of confirmed exoplanets from the NASA Exoplanet Archive smaller than 4R⊕ and less massive than 15M⊕ (black dots). We filter these for planets with ≤20% mass uncertainties and ≤10% radius uncertainties. TOI-6054b and TOI-6054c are overplotted in blue and purple, respectively. Mass–radius curves for water-world planets at 40% and 60% H2O mass fractions, rocky worlds with a 2% H/He envelope mass fraction and an Earth-like core composition, and pure silicate rocky worlds are plotted in blue, green, and brown, respectively. See Section 4.3 for the details of these curves.
Paper: A Pair of Dynamically Interacting Sub-Neptunes around TOI-6054
Authors: Maxwell A. Kroft, Thomas G. Beatty, Ian J. M. Crossfield, Joseph R. Livesey, Juliette Becker, Jacob K. Luhn, Paul Robertson, Allyson Bieryla, David R. Ciardi, Catherine A. Clark, Maria V. Goliguzova, Steve B. Howell, Jack J. Lissauer, Colin Littlefield, Michael B. Lund, Boris S. Safonov, Joseph M. Akana Murphy, Natalie M. Batalha, Malik Bossett, Jonathan Brande, Tansu Daylan, Courtney Dressing, Anna Gagnebin, Daniel Huber, Howard Isaacson, Stephen R. Kane, Laura Kreidberg, David W. Latham, Rafael Luque, Alex S. Polanski, Pranav H. Premnath, Maleah Rhem, Claire J. Rogers, Emma V. Turtelboom
Figure caption: Rp vs. Sinc for the California-Kepler Survey planets from B. J. Fulton & E. A. Petigura (2018) are plotted in black. The background color map is a weighted kernel density estimation of these planets showing relative occurrence rates as defined in that work. The blue dashed lines mark off the sub-Neptune desert defined in M. S. Lundkvist et al. (2016). TOI-6054b and c are overplotted with error bars in blue and purple, respectively. The blue and purple dots with arrows depict the estimated ZAMS Sinc for TOI-6054b and c, respectively, and their increase as the host star has evolved.
Paper: A Pair of Dynamically Interacting Sub-Neptunes around TOI-6054
Authors: Maxwell A. Kroft, Thomas G. Beatty, Ian J. M. Crossfield, Joseph R. Livesey, Juliette Becker, Jacob K. Luhn, Paul Robertson, Allyson Bieryla, David R. Ciardi, Catherine A. Clark, Maria V. Goliguzova, Steve B. Howell, Jack J. Lissauer, Colin Littlefield, Michael B. Lund, Boris S. Safonov, Joseph M. Akana Murphy, Natalie M. Batalha, Malik Bossett, Jonathan Brande, Tansu Daylan, Courtney Dressing, Anna Gagnebin, Daniel Huber, Howard Isaacson, Stephen R. Kane, Laura Kreidberg, David W. Latham, Rafael Luque, Alex S. Polanski, Pranav H. Premnath, Maleah Rhem, Claire J. Rogers, Emma V. Turtelboom
Figure caption: Corner plot of the posterior distributions of all fitted parameters in our joint fit described in Section 3.3. Parameters labeled with a “b” correspond to TOI-6054b, and those with a “c” correspond to TOI-6054c. Light-curve fitting parameters specific to Sectors 19 and 59 are labeled with “S19” and “S59,” respectively. The median values and 1σ uncertainties for these parameters are reported in Table 3.
Paper: Binary Star Orbits. VI. The Interferometric-spectroscopic Binary 73 Leo
Authors: Brian D. Mason, R. Elizabeth M. Griffin, R. T. Zavala, Christian A. Hummel, Haley M. Hurowitz, Jonathan L. Hurowitz, William I. Hartkopf, Ellyn K. Baines, Stephen J. Williams, Rachel A. Matson
Figure caption: As for Figure 6, but comparing the two stars in the Hδ region. The spectrum of ψ Boo has been scaled down by 10%. A weak addition to the depth of Hδ is discernible in 73 Leo and may be attributable to the presence of a faint F-type companion star.
Paper: Binary Star Orbits. VI. The Interferometric-spectroscopic Binary 73 Leo
Authors: Brian D. Mason, R. Elizabeth M. Griffin, R. T. Zavala, Christian A. Hummel, Haley M. Hurowitz, Jonathan L. Hurowitz, William I. Hartkopf, Ellyn K. Baines, Stephen J. Williams, Rachel A. Matson
Figure caption: As for Figure 6, but comparing the two stars in the near-UV. The spectrum of ψ Boo has been scaled down by 14%. A small amount of additional absorption is evident in 73 Leo in three places: in the cores of Ca II H and K, and in the core of the Balmer line at λ 3889 Å.