adsabs/AstroCLIMB huggingface dataset:
Paper: The Chemical Composition of Extreme-velocity Stars 
Authors: Henrique Reggiani, Alexander P. Ji, Kevin C. Schlaufman, Anna Frebel, Lina Necib, Tyler Nelson, Keith Hawkins, Jhon Yana Galarza
Figure caption: Abundances of the iron-peak elements chromium, manganese, nickel, and zinc. We plot our HVSs as dark blue stars. We plot in yellow the abundances of metal-poor stars in the Milky Way outer halo from Cayrel et al. (2004) and Jacobson et al. (2015); in red we show abundances of inner halo stars from H. Reggiani et al. (2022, in preparation), Reggiani et al. (2017), and Nissen & Schuster (2010); we display the Bensby et al. (2010) bulge stars in orange; in light-blue we include stars from the dwarf spheroidal galaxies Carina, Sculptor, Fornax, and Sagittarius from Shetrone et al. (2003), Geisler et al. (2005), Monaco et al. (2005), and Letarte et al. (2010).
Paper: The Chemical Composition of Extreme-velocity Stars 
Authors: Henrique Reggiani, Alexander P. Ji, Kevin C. Schlaufman, Anna Frebel, Lina Necib, Tyler Nelson, Keith Hawkins, Jhon Yana Galarza
Figure caption: Total energy as a function of angular momentum. We separate our stars into two groups. In blue are our stars with [Mg/Fe] < 0.2 (more likely to be extragalactic) and in red stars with [Mg/Fe] > 0.2. The background gray data are galactic halo stars from Naidu et al. (2021, private communication). The colored ellipses are from Bonaca et al. (2021), based on the substructures identified in Naidu et al. (2020). We include Arjuna, Cetus, GSE, Helmi, Iitoi, Sequoia, Sgr, Thamnos, and Wukong (orange, black, brown, deep pink, green, blue, purple, red and indigo, respectively).
Paper: The Chemical Composition of Extreme-velocity Stars 
Authors: Henrique Reggiani, Alexander P. Ji, Kevin C. Schlaufman, Anna Frebel, Lina Necib, Tyler Nelson, Keith Hawkins, Jhon Yana Galarza
Figure caption: Abundances of the light odd-Z elements sodium, aluminum, potassium, and scandium. We plot our HVSs as dark blue stars. We plot in yellow the abundances of metal-poor stars in the Milky Way outer halo from Cayrel et al. (2004) and Jacobson et al. (2015); in red we show abundances of inner halo stars from H. Reggiani et al. (2022, in preparation), Reggiani et al. (2017), Nissen & Schuster (2010), and Fishlock et al. (2017); we display the Bensby et al. (2010) bulge stars in orange; in light-blue we include stars from the dwarf spheroidal galaxies Carina, Sculptor, Fornax, and Sagittarius from Shetrone et al. (2003), Geisler et al. (2005), Monaco et al. (2005), and Letarte et al. (2010).
Paper: The Chemical Composition of Extreme-velocity Stars 
Authors: Henrique Reggiani, Alexander P. Ji, Kevin C. Schlaufman, Anna Frebel, Lina Necib, Tyler Nelson, Keith Hawkins, Jhon Yana Galarza
Figure caption: Distance from the Galactic Plane as a function of eccentricity. Orange triangles are stars from the Galactic Halo, gray squares are Enceladus stars, and green stars are from the Nyx stream (Necib et al. 2020). We separate our stars into two groups. In blue are our stars with [Mg/Fe] < 0.2 (more likely to be extragalactic) and in red stars with [Mg/Fe] > 0.2. Notice how all the stars with deviating eccentricity have low [Mg/Fe] abundance.
Paper: Confirmation of Water Absorption in the Thermal Emission Spectrum of the Hot Jupiter WASP-77Ab with HST/WFC3
Authors: Megan Mansfield, Lindsey Wiser, Kevin B. Stevenson, Peter Smith, Michael R. Line, Jacob L. Bean, Jonathan J. Fortney, Vivien Parmentier, Eliza M.-R. Kempton, Jacob Arcangeli, Jean-Michel Désert, Brian Kilpatrick, Laura Kreidberg, Matej Malik
Figure caption: HST water feature strength (﹩{S}_{{{\rm{H}}}_{2}{\rm{O}}}﹩) and dayside temperature (T day) of WASP-77Ab (bold, diamond point) in the context of all other planets observed between 1.1 and 1.7 μm with HST/WFC3 (colored, circular points; Mansfield et al. 2021; Fu et al. 2022). Both values are calculated following the descriptions in Mansfield et al. (2021). Positive/negative values of ﹩{S}_{{{\rm{H}}}_{2}{\rm{O}}}﹩ indicate features observed in absorption/emission, respectively, and a value of ﹩{S}_{{{\rm{H}}}_{2}{\rm{O}}}=0﹩ indicates a featureless, blackbody-like spectrum. The gray points and shaded region show predictions from the 1D model grid presented in Mansfield et al. (2021). WASP-77Ab has ﹩{S}_{{{\rm{H}}}_{2}{\rm{O}}}=0.157\pm 0.049﹩, indicating the presence of a strong water absorption feature in its spectrum. This value agrees with previously observed trends that planets below T day ≈ 2100 K tend to have absorption features due to noninverted T–P profiles, but that the scatter in water feature strengths for planets at similar temperatures suggests compositional differences in their atmospheres (Fortney et al. 2008; Parmentier et al. 2018; Mansfield et al. 2021).
Paper: Confirmation of Water Absorption in the Thermal Emission Spectrum of the Hot Jupiter WASP-77Ab with HST/WFC3
Authors: Megan Mansfield, Lindsey Wiser, Kevin B. Stevenson, Peter Smith, Michael R. Line, Jacob L. Bean, Jonathan J. Fortney, Vivien Parmentier, Eliza M.-R. Kempton, Jacob Arcangeli, Jean-Michel Désert, Brian Kilpatrick, Laura Kreidberg, Matej Malik
Figure caption: Atmospheric metallicity as a function of planet mass. Black points show solar system planet metallicities, which are based on measurements of [CH4/H] (Wong et al. 2004; Fletcher et al. 2009; Karkoschka & Tomasko 2011; Sromovsky et al. 2011). The black dashed line shows a fit to the solar system trend, but plateauing at 1 when the planet metallicity equals the stellar metallicity. Gray points show [H2O/H] for previously observed exoplanets (Welbanks et al. 2019). We additionally compare four measurements of the metallicity of WASP-77Ab: [M/H] from our grid retrieval described in Section 3.2 (red), [M/H] from the grid retrieval on the data with the bluest four points removed (orange, see Section 4.2), [H2O/H] from our free retrieval described in Section 3.1 (blue, lower limit only), and [C+O/H] from recent high-resolution observations with Gemini-S/IGRINS (green, Line et al. 2021).
Paper: Confirmation of Water Absorption in the Thermal Emission Spectrum of the Hot Jupiter WASP-77Ab with HST/WFC3
Authors: Megan Mansfield, Lindsey Wiser, Kevin B. Stevenson, Peter Smith, Michael R. Line, Jacob L. Bean, Jonathan J. Fortney, Vivien Parmentier, Eliza M.-R. Kempton, Jacob Arcangeli, Jean-Michel Désert, Brian Kilpatrick, Laura Kreidberg, Matej Malik
Figure caption: Comparison of our HST/WFC3 and Spitzer emission spectrum of WASP-77Ab (black points) with a fit of dayside emission from high-resolution Gemini-S/IGRINS observation (Line et al. 2021). The blue line and points show the median model fit to the IGRINS data, at full resolution and smoothed to the resolution of the WFC3 data, respectively. Red lines show 500 random draws from the posterior of the high-resolution fit smoothed to an R = 100.
Paper: A Close-in Puffy Neptune with Hidden Friends: The Enigma of TOI 620
Authors: Michael A. Reefe, Rafael Luque, Eric Gaidos, Corey Beard, Peter P. Plavchan, Marion Cointepas, Bryson L. Cale, Enric Palle, Hannu Parviainen, Dax L. Feliz, Jason Eastman, Keivan Stassun, Jonathan Gagné, Jon M. Jenkins, Patricia T. Boyd, Richard C. Kidwell, Scott McDermott, Karen A. Collins, William Fong, Natalia Guerrero, Jose-Manuel Almenara-Villa, Jacob Bean, Charles A. Beichman, John Berberian, Allyson Bieryla, Xavier Bonfils, François Bouchy, Madison Brady, Edward M. Bryant, Luca Cacciapuoti, Caleb I. Cañas, David R. Ciardi, Kevin I. Collins, Ian J. M. Crossfield, Courtney D. Dressing, Philipp Eigmüller, Mohammed El Mufti, Emma Esparza-Borges, Akihiko Fukui, Peter Gao, Claire Geneser, Crystal L. Gnilka, Erica Gonzales, Arvind F. Gupta, Sam Halverson, Fred Hearty, Steve B. Howell, Jonathan Irwin, Shubham Kanodia, David Kasper, Takanori Kodama, Veselin Kostov, David W. Latham, Monika Lendl, Andrea Lin, John H. Livingston, Jack Lubin, Suvrath Mahadevan, Rachel Matson, Elisabeth Matthews, Felipe Murgas, Norio Narita, Patrick Newman, Joe Ninan, Ares Osborn, Samuel N. Quinn, Paul Robertson, Arpita Roy, Joshua Schlieder, Christian Schwab, Andreas Seifahrt, Gareth D. Smith, Ahmad Sohani, Guðmundur Stefánsson, Daniel Stevens, Julian Stürmer, Angelle Tanner, Ryan Terrien, Johanna Teske, David Vermilion, Sharon X. Wang, Justin Wittrock, Jason T. Wright, Mathias Zechmeister, Farzaneh Zohrabi
Figure caption: Kempton et al. (2018) metrics of signal-to-noise (S/N) for hypothetical observations of exoplanet atmospheres in transmission (during primary transit) and emission (during secondary eclipse) for a subset of TESS candidate or confirmed planets (TOIs) detected as of the end of 2021 September (NASA Exoplanet Archive, IPAC 2013; Akeson et al. 2013). Only planets smaller than Neptune, with T eq < 1300 K, and that are predicted to impart a Doppler RV signal K > 3 m s−1 are shown. Planet masses are estimated from the Chen & Kipping (2016) mass–radius relation and are thus only preliminary. The points’ sizes are scaled with planet radius and the colors are keyed to T eq. Increased metric means higher S/N, and the dashed lines indicate the boundary above and to the right of which systems are suitable for JWST observations (Kempton et al. 2018). Candidate planet TOI 620.01 is presented by its Exoplanet Archive–based value (filled point), and by a value/lower limit based on revised star and planet properties presented in this work (open gray point and arrow).
Paper: A Close-in Puffy Neptune with Hidden Friends: The Enigma of TOI 620
Authors: Michael A. Reefe, Rafael Luque, Eric Gaidos, Corey Beard, Peter P. Plavchan, Marion Cointepas, Bryson L. Cale, Enric Palle, Hannu Parviainen, Dax L. Feliz, Jason Eastman, Keivan Stassun, Jonathan Gagné, Jon M. Jenkins, Patricia T. Boyd, Richard C. Kidwell, Scott McDermott, Karen A. Collins, William Fong, Natalia Guerrero, Jose-Manuel Almenara-Villa, Jacob Bean, Charles A. Beichman, John Berberian, Allyson Bieryla, Xavier Bonfils, François Bouchy, Madison Brady, Edward M. Bryant, Luca Cacciapuoti, Caleb I. Cañas, David R. Ciardi, Kevin I. Collins, Ian J. M. Crossfield, Courtney D. Dressing, Philipp Eigmüller, Mohammed El Mufti, Emma Esparza-Borges, Akihiko Fukui, Peter Gao, Claire Geneser, Crystal L. Gnilka, Erica Gonzales, Arvind F. Gupta, Sam Halverson, Fred Hearty, Steve B. Howell, Jonathan Irwin, Shubham Kanodia, David Kasper, Takanori Kodama, Veselin Kostov, David W. Latham, Monika Lendl, Andrea Lin, John H. Livingston, Jack Lubin, Suvrath Mahadevan, Rachel Matson, Elisabeth Matthews, Felipe Murgas, Norio Narita, Patrick Newman, Joe Ninan, Ares Osborn, Samuel N. Quinn, Paul Robertson, Arpita Roy, Joshua Schlieder, Christian Schwab, Andreas Seifahrt, Gareth D. Smith, Ahmad Sohani, Guðmundur Stefánsson, Daniel Stevens, Julian Stürmer, Angelle Tanner, Ryan Terrien, Johanna Teske, David Vermilion, Sharon X. Wang, Justin Wittrock, Jason T. Wright, Mathias Zechmeister, Farzaneh Zohrabi
Figure caption: Lomb–Scargle periodograms (left panels) of TESS Sectors 8 (top) and 35 (bottom) photometry, showing peaks corresponding to plausible stellar rotation at 4.45 and 8.93 days, respectively. The horizontal green line is the power corresponding to a false alarm probability of 0.1%, and the vertical dotted lines mark the half-orbit and thruster firing (momentum dump) intervals of TESS where systematics are expected. The normalized light curves phased using these peak periods are shown in the right panels.
Paper: A Close-in Puffy Neptune with Hidden Friends: The Enigma of TOI 620
Authors: Michael A. Reefe, Rafael Luque, Eric Gaidos, Corey Beard, Peter P. Plavchan, Marion Cointepas, Bryson L. Cale, Enric Palle, Hannu Parviainen, Dax L. Feliz, Jason Eastman, Keivan Stassun, Jonathan Gagné, Jon M. Jenkins, Patricia T. Boyd, Richard C. Kidwell, Scott McDermott, Karen A. Collins, William Fong, Natalia Guerrero, Jose-Manuel Almenara-Villa, Jacob Bean, Charles A. Beichman, John Berberian, Allyson Bieryla, Xavier Bonfils, François Bouchy, Madison Brady, Edward M. Bryant, Luca Cacciapuoti, Caleb I. Cañas, David R. Ciardi, Kevin I. Collins, Ian J. M. Crossfield, Courtney D. Dressing, Philipp Eigmüller, Mohammed El Mufti, Emma Esparza-Borges, Akihiko Fukui, Peter Gao, Claire Geneser, Crystal L. Gnilka, Erica Gonzales, Arvind F. Gupta, Sam Halverson, Fred Hearty, Steve B. Howell, Jonathan Irwin, Shubham Kanodia, David Kasper, Takanori Kodama, Veselin Kostov, David W. Latham, Monika Lendl, Andrea Lin, John H. Livingston, Jack Lubin, Suvrath Mahadevan, Rachel Matson, Elisabeth Matthews, Felipe Murgas, Norio Narita, Patrick Newman, Joe Ninan, Ares Osborn, Samuel N. Quinn, Paul Robertson, Arpita Roy, Joshua Schlieder, Christian Schwab, Andreas Seifahrt, Gareth D. Smith, Ahmad Sohani, Guðmundur Stefánsson, Daniel Stevens, Julian Stürmer, Angelle Tanner, Ryan Terrien, Johanna Teske, David Vermilion, Sharon X. Wang, Justin Wittrock, Jason T. Wright, Mathias Zechmeister, Farzaneh Zohrabi
Figure caption: TESS target pixel file (TPF) data from Sector 8 (left) and Sector 35 (right) for TOI 620, created with tpfplotter (Aller et al. 2020). The pixels shown outlined in orange were the ones used to extract the light curve, while point sources from the Gaia DR2 catalog are labeled in red, with sizes in accordance to their relative magnitude from the target star.
Paper: A Close-in Puffy Neptune with Hidden Friends: The Enigma of TOI 620
Authors: Michael A. Reefe, Rafael Luque, Eric Gaidos, Corey Beard, Peter P. Plavchan, Marion Cointepas, Bryson L. Cale, Enric Palle, Hannu Parviainen, Dax L. Feliz, Jason Eastman, Keivan Stassun, Jonathan Gagné, Jon M. Jenkins, Patricia T. Boyd, Richard C. Kidwell, Scott McDermott, Karen A. Collins, William Fong, Natalia Guerrero, Jose-Manuel Almenara-Villa, Jacob Bean, Charles A. Beichman, John Berberian, Allyson Bieryla, Xavier Bonfils, François Bouchy, Madison Brady, Edward M. Bryant, Luca Cacciapuoti, Caleb I. Cañas, David R. Ciardi, Kevin I. Collins, Ian J. M. Crossfield, Courtney D. Dressing, Philipp Eigmüller, Mohammed El Mufti, Emma Esparza-Borges, Akihiko Fukui, Peter Gao, Claire Geneser, Crystal L. Gnilka, Erica Gonzales, Arvind F. Gupta, Sam Halverson, Fred Hearty, Steve B. Howell, Jonathan Irwin, Shubham Kanodia, David Kasper, Takanori Kodama, Veselin Kostov, David W. Latham, Monika Lendl, Andrea Lin, John H. Livingston, Jack Lubin, Suvrath Mahadevan, Rachel Matson, Elisabeth Matthews, Felipe Murgas, Norio Narita, Patrick Newman, Joe Ninan, Ares Osborn, Samuel N. Quinn, Paul Robertson, Arpita Roy, Joshua Schlieder, Christian Schwab, Andreas Seifahrt, Gareth D. Smith, Ahmad Sohani, Guðmundur Stefánsson, Daniel Stevens, Julian Stürmer, Angelle Tanner, Ryan Terrien, Johanna Teske, David Vermilion, Sharon X. Wang, Justin Wittrock, Jason T. Wright, Mathias Zechmeister, Farzaneh Zohrabi
Figure caption: Plots of angular separation vs. the change in magnitude, Δm, from each of our high-contrast imaging observations. The width of the NIRI, NIRC2, and ShaneAO curves indicates the range of uncertainty for each curve. The 5σ sensitivity curves for NIRI and NIRC2 achieve excellent sensitivity to resolve stellar companions, and do not identify any such companions in the field of view.
Paper: A Close-in Puffy Neptune with Hidden Friends: The Enigma of TOI 620
Authors: Michael A. Reefe, Rafael Luque, Eric Gaidos, Corey Beard, Peter P. Plavchan, Marion Cointepas, Bryson L. Cale, Enric Palle, Hannu Parviainen, Dax L. Feliz, Jason Eastman, Keivan Stassun, Jonathan Gagné, Jon M. Jenkins, Patricia T. Boyd, Richard C. Kidwell, Scott McDermott, Karen A. Collins, William Fong, Natalia Guerrero, Jose-Manuel Almenara-Villa, Jacob Bean, Charles A. Beichman, John Berberian, Allyson Bieryla, Xavier Bonfils, François Bouchy, Madison Brady, Edward M. Bryant, Luca Cacciapuoti, Caleb I. Cañas, David R. Ciardi, Kevin I. Collins, Ian J. M. Crossfield, Courtney D. Dressing, Philipp Eigmüller, Mohammed El Mufti, Emma Esparza-Borges, Akihiko Fukui, Peter Gao, Claire Geneser, Crystal L. Gnilka, Erica Gonzales, Arvind F. Gupta, Sam Halverson, Fred Hearty, Steve B. Howell, Jonathan Irwin, Shubham Kanodia, David Kasper, Takanori Kodama, Veselin Kostov, David W. Latham, Monika Lendl, Andrea Lin, John H. Livingston, Jack Lubin, Suvrath Mahadevan, Rachel Matson, Elisabeth Matthews, Felipe Murgas, Norio Narita, Patrick Newman, Joe Ninan, Ares Osborn, Samuel N. Quinn, Paul Robertson, Arpita Roy, Joshua Schlieder, Christian Schwab, Andreas Seifahrt, Gareth D. Smith, Ahmad Sohani, Guðmundur Stefánsson, Daniel Stevens, Julian Stürmer, Angelle Tanner, Ryan Terrien, Johanna Teske, David Vermilion, Sharon X. Wang, Justin Wittrock, Jason T. Wright, Mathias Zechmeister, Farzaneh Zohrabi
Figure caption: Spectral energy distribution fit of flux as a function of wavelength for TOI 620. Blue points are the best-fit values, and red points are the corresponding model values and errors.
Paper: A Close-in Puffy Neptune with Hidden Friends: The Enigma of TOI 620
Authors: Michael A. Reefe, Rafael Luque, Eric Gaidos, Corey Beard, Peter P. Plavchan, Marion Cointepas, Bryson L. Cale, Enric Palle, Hannu Parviainen, Dax L. Feliz, Jason Eastman, Keivan Stassun, Jonathan Gagné, Jon M. Jenkins, Patricia T. Boyd, Richard C. Kidwell, Scott McDermott, Karen A. Collins, William Fong, Natalia Guerrero, Jose-Manuel Almenara-Villa, Jacob Bean, Charles A. Beichman, John Berberian, Allyson Bieryla, Xavier Bonfils, François Bouchy, Madison Brady, Edward M. Bryant, Luca Cacciapuoti, Caleb I. Cañas, David R. Ciardi, Kevin I. Collins, Ian J. M. Crossfield, Courtney D. Dressing, Philipp Eigmüller, Mohammed El Mufti, Emma Esparza-Borges, Akihiko Fukui, Peter Gao, Claire Geneser, Crystal L. Gnilka, Erica Gonzales, Arvind F. Gupta, Sam Halverson, Fred Hearty, Steve B. Howell, Jonathan Irwin, Shubham Kanodia, David Kasper, Takanori Kodama, Veselin Kostov, David W. Latham, Monika Lendl, Andrea Lin, John H. Livingston, Jack Lubin, Suvrath Mahadevan, Rachel Matson, Elisabeth Matthews, Felipe Murgas, Norio Narita, Patrick Newman, Joe Ninan, Ares Osborn, Samuel N. Quinn, Paul Robertson, Arpita Roy, Joshua Schlieder, Christian Schwab, Andreas Seifahrt, Gareth D. Smith, Ahmad Sohani, Guðmundur Stefánsson, Daniel Stevens, Julian Stürmer, Angelle Tanner, Ryan Terrien, Johanna Teske, David Vermilion, Sharon X. Wang, Justin Wittrock, Jason T. Wright, Mathias Zechmeister, Farzaneh Zohrabi
Figure caption: The TESS PDC-SAP light curve of TOI 620 from Sector 8 (top) and Sector 35 (bottom) plotted as a function of time. The times of transit for TOI 620 b are indicated with blue triangles. Data gaps during sectors are due to data downlinks, momentum dumps, and other data artifacts and systematics such as scattered light. The best-fit cubic spline polynomial is shown in pink, and is fitted to the data with the transits of TOI 620 b masked out. Any interpolation in the data-dump regions are thrown out. The yellow shaded regions show the predicted transit windows for TOI 620 c from our two-planet MCMC analysis, showing no obvious presence of a more massive transiting companion to TOI 620 b (see Section 6.1.3)
Paper: A Close-in Puffy Neptune with Hidden Friends: The Enigma of TOI 620
Authors: Michael A. Reefe, Rafael Luque, Eric Gaidos, Corey Beard, Peter P. Plavchan, Marion Cointepas, Bryson L. Cale, Enric Palle, Hannu Parviainen, Dax L. Feliz, Jason Eastman, Keivan Stassun, Jonathan Gagné, Jon M. Jenkins, Patricia T. Boyd, Richard C. Kidwell, Scott McDermott, Karen A. Collins, William Fong, Natalia Guerrero, Jose-Manuel Almenara-Villa, Jacob Bean, Charles A. Beichman, John Berberian, Allyson Bieryla, Xavier Bonfils, François Bouchy, Madison Brady, Edward M. Bryant, Luca Cacciapuoti, Caleb I. Cañas, David R. Ciardi, Kevin I. Collins, Ian J. M. Crossfield, Courtney D. Dressing, Philipp Eigmüller, Mohammed El Mufti, Emma Esparza-Borges, Akihiko Fukui, Peter Gao, Claire Geneser, Crystal L. Gnilka, Erica Gonzales, Arvind F. Gupta, Sam Halverson, Fred Hearty, Steve B. Howell, Jonathan Irwin, Shubham Kanodia, David Kasper, Takanori Kodama, Veselin Kostov, David W. Latham, Monika Lendl, Andrea Lin, John H. Livingston, Jack Lubin, Suvrath Mahadevan, Rachel Matson, Elisabeth Matthews, Felipe Murgas, Norio Narita, Patrick Newman, Joe Ninan, Ares Osborn, Samuel N. Quinn, Paul Robertson, Arpita Roy, Joshua Schlieder, Christian Schwab, Andreas Seifahrt, Gareth D. Smith, Ahmad Sohani, Guðmundur Stefánsson, Daniel Stevens, Julian Stürmer, Angelle Tanner, Ryan Terrien, Johanna Teske, David Vermilion, Sharon X. Wang, Justin Wittrock, Jason T. Wright, Mathias Zechmeister, Farzaneh Zohrabi
Figure caption: Our Markov Chain Monte Carlo dilution priors (red) vs. posteriors of the secondary for the circum-secondary model (green) and the hierarchical eclipsing binary (HEB, blue) model. We see a prior distribution that decreases with wavelength as expected for flux contamination from a hotter primary star, whereas the posteriors are mostly flat and become inconsistent at short and long wavelengths.
Paper: A Close-in Puffy Neptune with Hidden Friends: The Enigma of TOI 620
Authors: Michael A. Reefe, Rafael Luque, Eric Gaidos, Corey Beard, Peter P. Plavchan, Marion Cointepas, Bryson L. Cale, Enric Palle, Hannu Parviainen, Dax L. Feliz, Jason Eastman, Keivan Stassun, Jonathan Gagné, Jon M. Jenkins, Patricia T. Boyd, Richard C. Kidwell, Scott McDermott, Karen A. Collins, William Fong, Natalia Guerrero, Jose-Manuel Almenara-Villa, Jacob Bean, Charles A. Beichman, John Berberian, Allyson Bieryla, Xavier Bonfils, François Bouchy, Madison Brady, Edward M. Bryant, Luca Cacciapuoti, Caleb I. Cañas, David R. Ciardi, Kevin I. Collins, Ian J. M. Crossfield, Courtney D. Dressing, Philipp Eigmüller, Mohammed El Mufti, Emma Esparza-Borges, Akihiko Fukui, Peter Gao, Claire Geneser, Crystal L. Gnilka, Erica Gonzales, Arvind F. Gupta, Sam Halverson, Fred Hearty, Steve B. Howell, Jonathan Irwin, Shubham Kanodia, David Kasper, Takanori Kodama, Veselin Kostov, David W. Latham, Monika Lendl, Andrea Lin, John H. Livingston, Jack Lubin, Suvrath Mahadevan, Rachel Matson, Elisabeth Matthews, Felipe Murgas, Norio Narita, Patrick Newman, Joe Ninan, Ares Osborn, Samuel N. Quinn, Paul Robertson, Arpita Roy, Joshua Schlieder, Christian Schwab, Andreas Seifahrt, Gareth D. Smith, Ahmad Sohani, Guðmundur Stefánsson, Daniel Stevens, Julian Stürmer, Angelle Tanner, Ryan Terrien, Johanna Teske, David Vermilion, Sharon X. Wang, Justin Wittrock, Jason T. Wright, Mathias Zechmeister, Farzaneh Zohrabi
Figure caption: Full unphased RV time series as a function of time, with the black dashed lines representing our one-planet and two-planet (Section 6.1.3) MAP models with the linear trend. The top plot shows the RVs for each instrument and error bars over the full time baseline of observations, while the bottom plot shows the residuals (data − model). The one- and two-planet models have slightly different (<2 m s−1) RV offsets (γ) for each data set, as enumerated in Tables 8 and 11, respectively, but only the one-planet RV offsets are applied to the data as shown for clarity.