adsabs/AstroCLIMB huggingface dataset:
Paper: ELemental abundances of Planets and brown dwarfs Imaged around Stars (ELPIS). I. Potential Metal Enrichment of the Exoplanet AF Lep b and a Novel Retrieval Approach for Cloudy Self-luminous Atmospheres
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Keith Hawkins, Catherine Manea, Jonathan J. Fortney, Caroline V. Morley, Andrew Skemer, Mark S. Marley, Brendan P. Bowler, Aarynn L. Carter, Kyle Franson, Zachary G. Maas, Christopher Sneden
Figure caption: Fitted orbits compared to the observed relative astrometry (top), the absolute astrometry (middle), and the host star’s relative RVs (bottom left). In each panel, we present the observed data (top) and residuals (bottom) as filled circles, and the best-fit orbital solution as black solid lines. Predictions of 1000 random orbits are color-coded by the dynamical mass of AF Lep b, estimated to be ﹩{2.7}_{-0.5}^{+0.6}﹩                      M Jup by our analysis.
Paper: ELemental abundances of Planets and brown dwarfs Imaged around Stars (ELPIS). I. Potential Metal Enrichment of the Exoplanet AF Lep b and a Novel Retrieval Approach for Cloudy Self-luminous Atmospheres
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Keith Hawkins, Catherine Manea, Jonathan J. Fortney, Caroline V. Morley, Andrew Skemer, Mark S. Marley, Brendan P. Bowler, Aarynn L. Carter, Kyle Franson, Zachary G. Maas, Christopher Sneden
Figure caption: Parameter posteriors for two modes of our derived orbital solution, corresponding to positive (red) and negative (blue) ΔRV b−A values at epoch J2024.0. The axes of Ω, ω ⋆, and λ ref,⋆ extend beyond the nominal range of [0°, 360°) so that each mode of the orbital solution does not split into multiple peaks due to the modulus of 360°.
Paper: Atmospheric Retrieval of L Dwarfs: Benchmarking Results and Characterizing the Young Planetary Mass Companion HD 106906 b in the Near-infrared
Authors: Arthur D. Adams, Michael R. Meyer, Alex R. Howe, Ben Burningham, Sebastian Daemgen, Jonathan Fortney, Mike Line, Mark Marley, Sascha P. Quanz, Kamen Todorov
Figure caption: Spectra and contribution functions of the retrieved forward model fits to data simulated from cloud-free forward models of an L dwarf. The forward model spectra (using the MLE parameter values) are in color, with the data in gray. The retrieved models are nearly identical and overlap nearly entirely. Immediately beneath the spectra are the contribution functions for the two principal carbon- and oxygen-bearing species; CO2 is included in the model used to generate the simulated data, but its contributions to the emission are well below those of H2O and CO. The deepest contours, outlined in solid colors, enclose the regions where the contribution function reaches >1% of the total contribution within the atmospheric column at a given wavelength bin. Each successive contour denotes 2 orders of magnitude smaller fractional contribution (here, 10−4 and 10−6). The faint gray lines in the J-band (leftmost) sections contribution plots denote the location of the cloud layer as retrieved by the cloudy model on the cloud-free data. The faintness of the lines denotes the low optical depth of the cloud layer, in contrast with the darker cloud contours as seen in the retrieval on cloudy simulated data (Figure 6).
Paper: Atmospheric Retrieval of L Dwarfs: Benchmarking Results and Characterizing the Young Planetary Mass Companion HD 106906 b in the Near-infrared
Authors: Arthur D. Adams, Michael R. Meyer, Alex R. Howe, Ben Burningham, Sebastian Daemgen, Jonathan Fortney, Mike Line, Mark Marley, Sascha P. Quanz, Kamen Todorov
Figure caption: Spectra and contribution functions of the retrieved forward model fits to data simulated from cloudy forward models of an L dwarf. The forward model spectra (using the MLE parameter values) are in color, with the data in gray. The retrieved models are nearly identical and overlap nearly entirely. Immediately beneath the spectra are the contribution functions for the three principal carbon- and oxygen-bearing species. The deepest contours, outlined in solid colors, enclose the regions where the contribution function reaches >1% of the total contribution within the atmospheric column at a given wavelength bin. Each successive contour denotes 2 orders of magnitude smaller fractional contribution (here, 10−4 and 10−6).
Paper: Atmospheric Retrieval of L Dwarfs: Benchmarking Results and Characterizing the Young Planetary Mass Companion HD 106906 b in the Near-infrared
Authors: Arthur D. Adams, Michael R. Meyer, Alex R. Howe, Ben Burningham, Sebastian Daemgen, Jonathan Fortney, Mike Line, Mark Marley, Sascha P. Quanz, Kamen Todorov
Figure caption: Single-parameter (1D) and parameter vs. parameter (2D) posterior distributions of cloud parameters from the samples in the cloudy forward model fit to data simulated from a cloud-free forward model of an L dwarf (see Section 4). The cloud opacity is modeled as a power law in wavelength, as described in Section 3.3. The median value and 68% confidence interval of each parameter are shown at the top of each column; the full list of median, interval range, and MLE values is shown in Table 4. As there is no cloud opacity in the simulated data, the model can adapt its cloud opacity in several ways to effectively remove its influence on the resulting emission spectrum. The first is to turn the reference optical depth ﹩\tau \left({\lambda }_{0}\right)﹩ to a very low value (≪1); the second is to introduce significant opacity ﹩\tau \left({\lambda }_{0}\right)\gtrsim 1﹩ but to place the cloud deep into the atmosphere, below where the majority of the thermal emission originates in the spectrum (i.e., below the photosphere).
Paper: Atmospheric Retrieval of L Dwarfs: Benchmarking Results and Characterizing the Young Planetary Mass Companion HD 106906 b in the Near-infrared
Authors: Arthur D. Adams, Michael R. Meyer, Alex R. Howe, Ben Burningham, Sebastian Daemgen, Jonathan Fortney, Mike Line, Mark Marley, Sascha P. Quanz, Kamen Todorov
Figure caption: The vertical temperature–pressure profiles of the retrieved forward model fits to data simulated from cloud-free forward models of an L dwarf. We show the MLE, median, and 95% confidence interval of the retrieved T–P profiles, with the true profile overplotted.
Paper: Atmospheric Retrieval of L Dwarfs: Benchmarking Results and Characterizing the Young Planetary Mass Companion HD 106906 b in the Near-infrared
Authors: Arthur D. Adams, Michael R. Meyer, Alex R. Howe, Ben Burningham, Sebastian Daemgen, Jonathan Fortney, Mike Line, Mark Marley, Sascha P. Quanz, Kamen Todorov
Figure caption: Single-parameter (1D) and parameter vs. parameter (2D) posterior distributions of gas parameters from the samples in the cloudy (red) and cloud-free (blue) forward model fit to data simulated from a cloud-free forward model of an L dwarf (see Section 4). The cloud opacity is modeled as a power law in wavelength, as described in Section 3.3. The median value and 68% confidence interval of each parameter are shown at the top of each column; the full list of median, interval range, and MLE values is shown in Table 4.
Paper: Atmospheric Retrieval of L Dwarfs: Benchmarking Results and Characterizing the Young Planetary Mass Companion HD 106906 b in the Near-infrared
Authors: Arthur D. Adams, Michael R. Meyer, Alex R. Howe, Ben Burningham, Sebastian Daemgen, Jonathan Fortney, Mike Line, Mark Marley, Sascha P. Quanz, Kamen Todorov
Figure caption: The vertical temperature–pressure profiles of the retrieved forward model fits to data simulated from cloudy forward models of an L dwarf. We show the MLE, median, and 95% confidence interval of the retrieved T–P profiles, with the true profile overplotted.
Paper: Atmospheric Retrieval of L Dwarfs: Benchmarking Results and Characterizing the Young Planetary Mass Companion HD 106906 b in the Near-infrared
Authors: Arthur D. Adams, Michael R. Meyer, Alex R. Howe, Ben Burningham, Sebastian Daemgen, Jonathan Fortney, Mike Line, Mark Marley, Sascha P. Quanz, Kamen Todorov
Figure caption: A selection of parameters of the retrieved forward model fits to data simulated from cloud-free forward models of an L dwarf, shown as 1D and 2D histograms in a corner plot of the retrieved posterior distributions. The median value and 68% confidence interval of each parameter are shown at the top of each column; the full list of median, interval range, and MLE values is shown in Table 4.
Paper: Revisiting the Transit Timing and Atmosphere Characterization of the Neptune-mass Planet HAT-P-26 b
Authors: Napaporn A-thano, Supachai Awiphan, Ing-Guey Jiang, Eamonn Kerins, Akshay Priyadarshi, Iain McDonald, Yogesh C. Joshi, Thansuda Chulikorn, Joshua J. C. Hayes, Stephen Charles, Chung-Kai Huang, Ronnakrit Rattanamala, Li-Chin Yeh, Vik S Dhillon
Figure caption: Normalized rms plots for all ground-based residual light curves from both our observations and existing data fit as a function of the number of points per bin. The observation data are shown in ﹩g^{\prime} ﹩ (blue), ﹩r^{\prime} ﹩ (yellow), R (orange), ﹩i^{\prime} ﹩ (red), I (dark red), and ﹩z^{\prime} ﹩ (brown).
Paper: Revisiting the Transit Timing and Atmosphere Characterization of the Neptune-mass Planet HAT-P-26 b
Authors: Napaporn A-thano, Supachai Awiphan, Ing-Guey Jiang, Eamonn Kerins, Akshay Priyadarshi, Iain McDonald, Yogesh C. Joshi, Thansuda Chulikorn, Joshua J. C. Hayes, Stephen Charles, Chung-Kai Huang, Ronnakrit Rattanamala, Li-Chin Yeh, Vik S Dhillon
Figure caption: Normalized, phased-folded HAT-P-26 b transit light curves from HST/WFC3, reduced using the Iraclis package (dots). Three sets of observations are shown, with the light curves and TransitFit models in the left-hand panels, and the corresponding residual differences in the right-hand panels. The top-left, top-right, and bottom pairs of panels respectively show the G141 grism observations from 2016 March 12, the G141 grism observations from 2016 May 02, and the G102 prism observations from 2016 October 16. The light curves and the residuals have arbitrary offsets for clarity.
Paper: Revisiting the Transit Timing and Atmosphere Characterization of the Neptune-mass Planet HAT-P-26 b
Authors: Napaporn A-thano, Supachai Awiphan, Ing-Guey Jiang, Eamonn Kerins, Akshay Priyadarshi, Iain McDonald, Yogesh C. Joshi, Thansuda Chulikorn, Joshua J. C. Hayes, Stephen Charles, Chung-Kai Huang, Ronnakrit Rattanamala, Li-Chin Yeh, Vik S Dhillon
Figure caption: Normalized rms plots for the HST residual light curves fit as a function of the number of points per bin. The observations from HST/WFC3 G102 and HST/WFC3 G141 are shown in green and red, respectively.
Paper: Revisiting the Transit Timing and Atmosphere Characterization of the Neptune-mass Planet HAT-P-26 b
Authors: Napaporn A-thano, Supachai Awiphan, Ing-Guey Jiang, Eamonn Kerins, Akshay Priyadarshi, Iain McDonald, Yogesh C. Joshi, Thansuda Chulikorn, Joshua J. C. Hayes, Stephen Charles, Chung-Kai Huang, Ronnakrit Rattanamala, Li-Chin Yeh, Vik S Dhillon
Figure caption: Left panels: normalized, phased-folded HAT-P-26 b transit light curves observed using the SPEARNET telescope network (gray dots) with the best-fitting model from TransitFit (solid lines). The red dots show the light curves binned into 5 minute intervals. Right panels: the corresponding residual light curves after the models are subtracted. Both the light curves and the residuals have arbitrary vertical offsets for clarity.
Paper: Revisiting the Transit Timing and Atmosphere Characterization of the Neptune-mass Planet HAT-P-26 b
Authors: Napaporn A-thano, Supachai Awiphan, Ing-Guey Jiang, Eamonn Kerins, Akshay Priyadarshi, Iain McDonald, Yogesh C. Joshi, Thansuda Chulikorn, Joshua J. C. Hayes, Stephen Charles, Chung-Kai Huang, Ronnakrit Rattanamala, Li-Chin Yeh, Vik S Dhillon
Figure caption: The locations and sizes of the telescopes in SPEARNET.
Paper: Revisiting the Transit Timing and Atmosphere Characterization of the Neptune-mass Planet HAT-P-26 b
Authors: Napaporn A-thano, Supachai Awiphan, Ing-Guey Jiang, Eamonn Kerins, Akshay Priyadarshi, Iain McDonald, Yogesh C. Joshi, Thansuda Chulikorn, Joshua J. C. Hayes, Stephen Charles, Chung-Kai Huang, Ronnakrit Rattanamala, Li-Chin Yeh, Vik S Dhillon
Figure caption: Normalized, phased-folded HAT-P-26 b transit light curves from TESS (gray dots, left panels) with the best-fitting model from TransitFit (solid lines). Their corresponding residuals are shown in the right panels. The light curves and the residuals have arbitrary offsets for clarity.
Paper: A Solution to Continuous RFI in Narrowband Radio SETI with FAST: The MultiBeam Point-source Scanning Strategy
Authors: Bo-Lun Huang, Zhen-Zhao Tao, Tong-Jie Zhang
Figure caption: Waterfall plots of the OTBs from a simulated MBPS observation with a slew rate of 6″ s−1. The colored bar indicates the power with arbitrary units. (a) Waterfall plot of a high-S/N signal in the five OTBs during the whole observation. (b) Same as (a) but with a lower S/N. (c) Waterfall plot of the lower-S/N signal in the five OTWs. (d) Same as (c), but the central frequencies of beams 2, 1, 5, and 14 are subtracted by the frequency drifts during the corresponding gaps between OTWs.
Paper: TOI-4010: A System of Three Large Short-period Planets with a Massive Long-period Companion
Authors: Michelle Kunimoto, Andrew Vanderburg, Chelsea X. Huang, M. Ryleigh Davis, Laura Affer, Andrew Collier Cameron, David Charbonneau, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martnez Fiorenzano, Adriano Ghedina, R. D. Haywood, Florian Lienhard, Mercedes López-Morales, Michel Mayor, Francesco Pepe, Matteo Pinamonti, Ennio Poretti, Jesús Maldonado, Ken Rice, Alessandro Sozzetti, Thomas G. Wilson, Stéphane Udry, Jay Baptista, Khalid Barkaoui, Juliette Becker, Paul Benni, Allyson Bieryla, Pau Bosch-Cabot, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Elise Evans, Trent J. Dupuy, Maria V. Goliguzova, Pere Guerra, Adam Kraus, Jack J. Lissauer, Daniel Huber, Felipe Murgas, Enric Palle, Samuel N. Quinn, Boris S. Safonov, Richard P. Schwarz, Avi Shporer, Keivan G. Stassun, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Roland Vanderspek, Joshua Winn, Zahra Essack, Hannah M. Lewis, Mark E. Rose
Figure caption: Mass–radius diagram for planets with density known to better than 50% precision (﹩{\sigma }_{{\rho }_{p}}/{\rho }_{p}\lt 0.5﹩), plotted alongside the three transiting, short-period TOI-4010. Planets are colored by equilibrium temperature, which we recalculated assuming an albedo of 0 for uniformity. Mass–radius curves from Zeng et al. (2018) assuming 1000 K surface temperature for Earth-like rocky cores with no atmosphere or 0.1%, 1%, and 2% H2 envelopes by mass are overlaid in green, along with water-rich cores with 0.1%, 0.3%, and 1% H2 envelopes by mass (blue) and a pure rock composition (red).
Paper: TOI-4010: A System of Three Large Short-period Planets with a Massive Long-period Companion
Authors: Michelle Kunimoto, Andrew Vanderburg, Chelsea X. Huang, M. Ryleigh Davis, Laura Affer, Andrew Collier Cameron, David Charbonneau, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martnez Fiorenzano, Adriano Ghedina, R. D. Haywood, Florian Lienhard, Mercedes López-Morales, Michel Mayor, Francesco Pepe, Matteo Pinamonti, Ennio Poretti, Jesús Maldonado, Ken Rice, Alessandro Sozzetti, Thomas G. Wilson, Stéphane Udry, Jay Baptista, Khalid Barkaoui, Juliette Becker, Paul Benni, Allyson Bieryla, Pau Bosch-Cabot, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Elise Evans, Trent J. Dupuy, Maria V. Goliguzova, Pere Guerra, Adam Kraus, Jack J. Lissauer, Daniel Huber, Felipe Murgas, Enric Palle, Samuel N. Quinn, Boris S. Safonov, Richard P. Schwarz, Avi Shporer, Keivan G. Stassun, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Roland Vanderspek, Joshua Winn, Zahra Essack, Hannah M. Lewis, Mark E. Rose
Figure caption: Mass–metallicity diagram for sub-Saturn-sized planets (R  p  = 4–8 R ⊕) from Figure 12, including TOI-4010c and d. This population shows a tentative positive correlation between mass and host-star metallicity. TOI-4010 d is one of the most massive sub-Saturns discovered in a multiplanet system. TOI-4010 follows the general trend of more massive sub-Saturns orbiting higher-metallicity stars.
Paper: TOI-4010: A System of Three Large Short-period Planets with a Massive Long-period Companion
Authors: Michelle Kunimoto, Andrew Vanderburg, Chelsea X. Huang, M. Ryleigh Davis, Laura Affer, Andrew Collier Cameron, David Charbonneau, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martnez Fiorenzano, Adriano Ghedina, R. D. Haywood, Florian Lienhard, Mercedes López-Morales, Michel Mayor, Francesco Pepe, Matteo Pinamonti, Ennio Poretti, Jesús Maldonado, Ken Rice, Alessandro Sozzetti, Thomas G. Wilson, Stéphane Udry, Jay Baptista, Khalid Barkaoui, Juliette Becker, Paul Benni, Allyson Bieryla, Pau Bosch-Cabot, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Elise Evans, Trent J. Dupuy, Maria V. Goliguzova, Pere Guerra, Adam Kraus, Jack J. Lissauer, Daniel Huber, Felipe Murgas, Enric Palle, Samuel N. Quinn, Boris S. Safonov, Richard P. Schwarz, Avi Shporer, Keivan G. Stassun, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Roland Vanderspek, Joshua Winn, Zahra Essack, Hannah M. Lewis, Mark E. Rose
Figure caption: Period–radius diagram for the planets shown in Figure 12, with planets colored by insolation flux. TOI-4010 b lies in the sparsely populated region of short-period, intermediate-sized planets known as the hot-Neptune desert. The edges of the desert are roughly indicated by the black dashed lines.
Paper: TOI-4010: A System of Three Large Short-period Planets with a Massive Long-period Companion
Authors: Michelle Kunimoto, Andrew Vanderburg, Chelsea X. Huang, M. Ryleigh Davis, Laura Affer, Andrew Collier Cameron, David Charbonneau, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martnez Fiorenzano, Adriano Ghedina, R. D. Haywood, Florian Lienhard, Mercedes López-Morales, Michel Mayor, Francesco Pepe, Matteo Pinamonti, Ennio Poretti, Jesús Maldonado, Ken Rice, Alessandro Sozzetti, Thomas G. Wilson, Stéphane Udry, Jay Baptista, Khalid Barkaoui, Juliette Becker, Paul Benni, Allyson Bieryla, Pau Bosch-Cabot, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Elise Evans, Trent J. Dupuy, Maria V. Goliguzova, Pere Guerra, Adam Kraus, Jack J. Lissauer, Daniel Huber, Felipe Murgas, Enric Palle, Samuel N. Quinn, Boris S. Safonov, Richard P. Schwarz, Avi Shporer, Keivan G. Stassun, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Roland Vanderspek, Joshua Winn, Zahra Essack, Hannah M. Lewis, Mark E. Rose
Figure caption: Histograms of the distributions of all fit parameters from the four-planet, joint transit + RV fit. The parameters fitted for TOI-4010 b, c, d, and e are shown in blue, orange, green, and purple, respectively.
Paper: TOI-4010: A System of Three Large Short-period Planets with a Massive Long-period Companion
Authors: Michelle Kunimoto, Andrew Vanderburg, Chelsea X. Huang, M. Ryleigh Davis, Laura Affer, Andrew Collier Cameron, David Charbonneau, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martnez Fiorenzano, Adriano Ghedina, R. D. Haywood, Florian Lienhard, Mercedes López-Morales, Michel Mayor, Francesco Pepe, Matteo Pinamonti, Ennio Poretti, Jesús Maldonado, Ken Rice, Alessandro Sozzetti, Thomas G. Wilson, Stéphane Udry, Jay Baptista, Khalid Barkaoui, Juliette Becker, Paul Benni, Allyson Bieryla, Pau Bosch-Cabot, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Elise Evans, Trent J. Dupuy, Maria V. Goliguzova, Pere Guerra, Adam Kraus, Jack J. Lissauer, Daniel Huber, Felipe Murgas, Enric Palle, Samuel N. Quinn, Boris S. Safonov, Richard P. Schwarz, Avi Shporer, Keivan G. Stassun, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Roland Vanderspek, Joshua Winn, Zahra Essack, Hannah M. Lewis, Mark E. Rose
Figure caption: Orbits of the transiting planets of TOI-4010 assuming the median values provided in Table 4.
Paper: TOI-4010: A System of Three Large Short-period Planets with a Massive Long-period Companion
Authors: Michelle Kunimoto, Andrew Vanderburg, Chelsea X. Huang, M. Ryleigh Davis, Laura Affer, Andrew Collier Cameron, David Charbonneau, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martnez Fiorenzano, Adriano Ghedina, R. D. Haywood, Florian Lienhard, Mercedes López-Morales, Michel Mayor, Francesco Pepe, Matteo Pinamonti, Ennio Poretti, Jesús Maldonado, Ken Rice, Alessandro Sozzetti, Thomas G. Wilson, Stéphane Udry, Jay Baptista, Khalid Barkaoui, Juliette Becker, Paul Benni, Allyson Bieryla, Pau Bosch-Cabot, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Elise Evans, Trent J. Dupuy, Maria V. Goliguzova, Pere Guerra, Adam Kraus, Jack J. Lissauer, Daniel Huber, Felipe Murgas, Enric Palle, Samuel N. Quinn, Boris S. Safonov, Richard P. Schwarz, Avi Shporer, Keivan G. Stassun, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Roland Vanderspek, Joshua Winn, Zahra Essack, Hannah M. Lewis, Mark E. Rose
Figure caption: Plots of the final joint transit + RV model fits, with residuals after subtracting the median models provided in the lower panel of each phase diagram. Black points show observations with offsets subtracted and jitter terms added in quadrature with uncertainties, while colored circles represent binned data. Solid colored lines represent median model values, while shaded regions cover 16th to 84th percentiles. The transit (left) and RV (right) phase diagrams for each planet are shown in each row. In each planet’s phase diagram, the best-fit models for the other three planets have been subtracted from the data.
Paper: TOI-4010: A System of Three Large Short-period Planets with a Massive Long-period Companion
Authors: Michelle Kunimoto, Andrew Vanderburg, Chelsea X. Huang, M. Ryleigh Davis, Laura Affer, Andrew Collier Cameron, David Charbonneau, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martnez Fiorenzano, Adriano Ghedina, R. D. Haywood, Florian Lienhard, Mercedes López-Morales, Michel Mayor, Francesco Pepe, Matteo Pinamonti, Ennio Poretti, Jesús Maldonado, Ken Rice, Alessandro Sozzetti, Thomas G. Wilson, Stéphane Udry, Jay Baptista, Khalid Barkaoui, Juliette Becker, Paul Benni, Allyson Bieryla, Pau Bosch-Cabot, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Elise Evans, Trent J. Dupuy, Maria V. Goliguzova, Pere Guerra, Adam Kraus, Jack J. Lissauer, Daniel Huber, Felipe Murgas, Enric Palle, Samuel N. Quinn, Boris S. Safonov, Richard P. Schwarz, Avi Shporer, Keivan G. Stassun, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Roland Vanderspek, Joshua Winn, Zahra Essack, Hannah M. Lewis, Mark E. Rose
Figure caption: Contrast curves from Keck II/NIRC2 AO analysis in the K  p  band (blue), Keck II/NIRC2 NRM analysis in the K  p  band (orange), Keck II/NIRC2 AO analysis in the K  s  band (green), and SAI/Speckle analysis in the I band (red). No companions bright enough to contaminate the TESS photometry or cause a false positive were detected.