adsabs/AstroCLIMB huggingface dataset:
Paper: Revised Stellar Parameters for V471 Tau, A Post-common Envelope Binary in the Hyades
Authors: Philip S. Muirhead, Jason Nordhaus, Maria R. Drout
Figure caption: Radius vs. mass for white dwarfs and the white-dwarf component of V471 Tau. Small circles show measurements from the Sloan Digital Sky Survey (Tremblay et al. 2011). The square indicates our measurement for the mass and radius of the main-sequence star, and the circle indicates a previous measurement from the literature (O’Brien et al. 2001).
Paper: Revised Stellar Parameters for V471 Tau, A Post-common Envelope Binary in the Hyades
Authors: Philip S. Muirhead, Jason Nordhaus, Maria R. Drout
Figure caption: Same as Figure 4 but for parameters of interest that were derived from the fitted parameters.
Paper: The James Webb Space Telescope Absolute Flux Calibration. I. Program Design and Calibrator Stars
Authors: Karl D. Gordon, Ralph Bohlin, G. C. Sloan, George Rieke, Kevin Volk, Martha Boyer, James Muzerolle, Everett Schlawin, Susana E. Deustua, Dean C. Hines, Kathleen E. Kraemer, Susan E. Mullally, Kate Y. L. Su
Figure caption: The spectra of all the calibration stars compared to the instrumental sensitivities. The spectra are plotted in Rayleigh–Jeans units. The calibration min/max ranges for the NIRISS/FGS, NIRSpec, and MIRI instrument modes are plotted as vertical lines. The wavelengths of the sensitivities of some of the modes have been shifted to minimize overlap.
Paper: The James Webb Space Telescope Absolute Flux Calibration. I. Program Design and Calibrator Stars
Authors: Karl D. Gordon, Ralph Bohlin, G. C. Sloan, George Rieke, Kevin Volk, Martha Boyer, James Muzerolle, Everett Schlawin, Susana E. Deustua, Dean C. Hines, Kathleen E. Kraemer, Susan E. Mullally, Kate Y. L. Su
Figure caption: The spectra of all the calibration stars compared to the instrumental sensitivities. The spectra are plotted in Rayleigh–Jeans units. The calibration min/max ranges for the NIRCam instrument modes are plotted as vertical lines. The wavelengths of the sensitivities of some of the modes have been shifted to minimize overlap.
Paper: The James Webb Space Telescope Absolute Flux Calibration. I. Program Design and Calibrator Stars
Authors: Karl D. Gordon, Ralph Bohlin, G. C. Sloan, George Rieke, Kevin Volk, Martha Boyer, James Muzerolle, Everett Schlawin, Susana E. Deustua, Dean C. Hines, Kathleen E. Kraemer, Susan E. Mullally, Kate Y. L. Su
Figure caption: Example spectra for each of the three types of stars included in our sample are plotted in Rayleigh–Jeans units. The spectra are shown at spectral resolving powers of 3000 and 150 as these match the approximate maximum and minimum spectral resolving powers of JWST spectroscopy. For reference, the highest-resolution model spectra available are shown.
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: Markov Chain Monte Carlo (MCMC) corner plot of our joint ground and space-based transit model MCMC for TOI 620. Plots along the diagonal show one-dimensional histograms of the posterior distributions of each parameter. Off-diagonal plots show the covariance between each model parameter. Note that ﹩\mathrm{chord}=\sqrt{{(1-{R}_{P}/{R}_{* })}^{2}-{b}^{2}}﹩ and L 2 = sign(V  c /V  e  − 1)L (see Eastman et al. 2019). Not all model parameters that were varied are shown in this corner plot. Namely, we do not show the detrending parameters of each data set, linear and quadratic limb-darkening coefficients from each wavelength band, R *, R *,SED, T eff, T eff,SED, [Fe/H]0, ﹩\mathrm{log}{M}_{* }/{M}_{\odot }﹩, M  P , R  P /R *, and ﹩\mathrm{log}P﹩. The posteriors not shown are well behaved, and there is no strong covariance between any of them except the linear and quadratic limb-darkening coefficients, which show anticorrelation, and the metallicity and initial metallicity, which show strong correlation. All MCMC corner plots presented in this paper are generated using corner.py (Foreman-Mackey 2016).
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: Fits of our spectral binary model of the iSHELL iteration 10 stellar template in the 10% flux-ratio-limited case. The blue line is the iteration 10 stellar template (see Section A), the orange line is the combined final flux model, the purple and brown lines are the individual fluxes from the primary and secondary, respectively, and the green and red lines are the residuals from the single-star and double-star fits, respectively, with rms displayed. The wavelength range shown corresponds to echelle order 15 on the iSHELL spectrograph. An example stellar spectral absorption line at 2306 nm that is missing from the BT-Settl models is readily apparent. Note, in the stellar rest frame, the telluric absorption feature residuals from all of our 379 iSHELL spectra sampled at a range of barycenter velocities are decoherent and not contributing significantly to the observed residuals.
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: Transit data and models for each filter used in the EXOFASTv2 analysis of TOI 620. Filters shown, from top left to bottom right, are J, R, I, B, ﹩g^{\prime} ﹩, ﹩r^{\prime} ﹩, ﹩i^{\prime} ﹩, ﹩z^{\prime} ﹩, and TESS. In each filter’s plot, the top plot shows the combined transit data from all observations in that filter, phased to the period of the planet (5.09887 days), with each line showing the median transit model for the circum-primary (red), circum-secondary (green), and hierarchical eclipsing binary (HEB, blue) cases. The dilutions in the circum-secondary and HEB scenarios were allowed to independently vary in each bandpass and converge on unphysical values, as shown in Figure 15. The bottom plots show the residuals for the circum-primary model only.
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: rms Gaia photocenter shift, in units of milliarcseconds, expected for an unresolved binary with a given separation and Gaia contrast ratio that produce an asymmetric point-spread function. The per-observation centroid measurement error for TOI 620 is 0.3 mas and the photocenter rms would exceed this (and RUWE would be ≳1.4) in the red shaded region. The blue and magenta curves are the 5σ detection contrast ratio limits on any companion from our Keck II/NIRC2 and Gemini-N/NIRI AO imaging.
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: One-dimensional model parameter posterior histograms and model parameter covariances for T eff of the host [H], T eff of the contaminant [C], impact parameter, and host stellar density against the planet-to-star radius ratio (top) and flux contamination (middle) from a secondary star. Bottom: the corrected or “true” exoplanet radius as a function of the flux contamination from a secondary.
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: A historical Digitized Sky Survey (DSS) image of the TOI 620 system in 1954, in the DSS red band, where the current location of TOI 620 is circled in yellow. The diameter of the circle is ≈11″, or ∼half the size of a TESS pixel. It is visibly clear that no stars would be in the background of TOI 620's current position. The star to the lower right of its current position is the aforementioned TIC 296739889 at a separation of 9.″2, with a T-mag contrast of 7. Its close separation indicates its light would be blended with TOI 620's in the TESS aperture.
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: Markov Chain Monte Carlo corner plot of our spectral binary analysis of the iSHELL iteration 10 stellar template. Plots along the diagonal show one-dimensional histograms of the posterior distributions of each parameter. Off-diagonal plots show the covariance between each model parameter. The posterior distributions are bisected to show a zoom of each of the two individual posterior peaks on the left and right corner plots, showing that they are centralized maxima and are not edge solutions in our model parameter space.
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: Limits on the separation and contrast ratio of a potential companion detected by Gaia (and RVs). The color map linearly represents the posterior probability of a companion in the separation–companion mass plane, as ascertained by Monte Carlo calculations. The left panel assumes a uniform prior on companion mass, while the right panel uses a log-normal prior centered on 1 Jupiter mass and with a standard deviation of 0.6 dex.
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: Reconstructed images from Zorro (top left: 562 nm, bottom left: 832 nm), NIRI (top middle), NIRC2 (bottom middle), and ShaneAO (top right: J, bottom right: Ks ) which appear single to the limit of each instrument’s resolution.
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 mass–radius diagram for all exoplanets with provided radii and masses from the NASA Exoplanet Archive. TOI 620 b’s 5σ upper limit is plotted in pink with an arrow and dashed line. The arrow extends back down to the median mass from our MCMC chains. The blue line traces the Chen & Kipping (2016) relation. This plot demonstrates that TOI 620 is among some of the lowest-density Neptune-sized planets known.