adsabs/AstroCLIMB huggingface dataset:
Paper: Detection of H2O and CO2 in the Atmosphere of the Hot Super-Neptune WASP-166b with JWST
Authors: Andrew W. Mayo, Charles D. Fortenbach, Dana R. Louie, Courtney D. Dressing, Emma V. Turtelboom, Steven Giacalone, Caleb K. Harada
Figure caption: Posterior distributions of free parameters (corner plot) for PLATON Equilibrium Chemistry Case, E2. (Note: the “wfc_offset_transit” parameter is equivalent to δrel in our POSEIDON retrievals; we adjust the wavelength range for “wfc_offset_transit” from 1–1.7 μm (for HST WFC3) to 0.8–2.8 μm (for NIRISS SOSS)).
Paper: A VLBI Software Correlator for Fast Radio Transients
Authors: Calvin Leung, Shion Andrew, Kiyoshi W. Masui, Charanjot Brar, Tomas Cassanelli, Shami Chatterjee, Victoria Kaspi, Kholoud Khairy, Adam E. Lanman, Mattias Lazda, Juan Mena-Parra, Gavin Noble, Aaron B. Pearlman, Mubdi Rahman, Pranav Sanghavi, Vishwangi Shah
Figure caption: A realization-by-realization comparison of the signal power, noise power, and signal-to-noise ratio measured by each correlator variant (labeled SNR) as a function of the signal-to-noise measured by the basic correlator. The black lines denote equality between the basic and improved correlator variants. Each column shows a signal injected at a different fractional sample delay 0 ≤ d/(2N) ≤ 1. Each row within each column shows the impact of each correlator on the recovered signal and noise power, normalized to the basic correlator (see Section 5.3).
Paper: A VLBI Software Correlator for Fast Radio Transients
Authors: Calvin Leung, Shion Andrew, Kiyoshi W. Masui, Charanjot Brar, Tomas Cassanelli, Shami Chatterjee, Victoria Kaspi, Kholoud Khairy, Adam E. Lanman, Mattias Lazda, Juan Mena-Parra, Gavin Noble, Aaron B. Pearlman, Mubdi Rahman, Pranav Sanghavi, Vishwangi Shah
Figure caption: An example single-baseline localization of a Crab giant pulse. Left panel: a zoomed-out plot of various localization contours. A CHIME-only localization is plotted as a wide ellipse encompassing both statistical and systematic errors (light blue and red contours show the 2σ and 1σ uncertainty levels). The VLBI localization contour encompassing statistical errors only (shaded red and blue contours show the 20σ and 10σ uncertainty levels). Finally, we show the VLBI localization contour after taking into account the systematic uncertainty of στ = 2 ns in Equation (A1) (heavy red and blue lines show the 2σ and 1σ levels, respectively). This illustrates the relative sizes of contributions to the localization contour, which are typically dominated by systematic rather than statistical errors for single-pulse observations of typical brightnesses (see A. E. Lanman et al. (2024) for empirical characterization of our systematic localization errors for the CHIME-KKO baseline).
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. VI. Confirmation of a Long-period Giant Planet Discovered with a Single TESS Transit
Authors: Zahra Essack, Diana Dragomir, Paul A. Dalba, Matthew P. Battley, David R. Ciardi, Karen A. Collins, Steve B. Howell, Matias I. Jones, Stephen R. Kane, Eric E. Mamajek, Christopher R. Mann, Ismael Mireles, Dominic Oddo, Lauren A. Sgro, Keivan G. Stassun, Solene Ulmer-Moll, Cristilyn N. Watkins, Samuel W. Yee, Carl Ziegler, Allyson Bieryla, Ioannis Apergis, Khalid Barkaoui, Rafael Brahm, Edward M. Bryant, Thomas M. Esposito, Pedro Figueira, Benjamin J. Fulton, Samuel Gill, Andrew W. Howard, Howard Isaacson, Alicia Kendall, Nicholas Law, Michael B. Lund, Andrew W. Mann, Rachel A. Matson, Felipe Murgas, Enric Palle, Samuel N. Quinn, Alexandre Revol, Suman Saha, Richard P. Schwarz, Ramotholo Sefako, Avi Shporer, Ivan A. Strakhov, Steven Villanueva, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Pau Bosch-Cabot, Kevin I. Collins, Raquel Forés-Toribio, Fabian Rodriguez Frustagia, Eric Girardin, Ian J. Helm, Pablo Lewin, Jose A. Muñoz, Patrick Newman, Peter Plavchan, Gregor Srdoc, Chris Stockdale, Anaël Wünsche, Mario Billiani, Martin Davy, Alex Douvas, Keiichi Fukui, Bruno Guillet, Cory Ostrem, Michael Rushton, Angsar Schmidt, Andrea Finardi, Patrice Girard, Tateki Goto, Julien S. de Lambilly, Liouba Leroux, Fabrice Mortecrette, John W. Pickering, Michael Primm, Marc Ribot, Ethan Teng, Aad Verveen, Stefan Will, Mark Ziegler
Figure caption: SED of TOI-4465. Red symbols represent the observed photometric measurements, where the horizontal bars represent the effective width of the passband. Blue symbols are the model fluxes from the best-fit PHOENIX atmosphere model (black). The inset shows the absolute flux-calibrated Gaia spectrophotometry as a gray swathe overlaid on the model (black).
Paper: A VLBI Software Correlator for Fast Radio Transients
Authors: Calvin Leung, Shion Andrew, Kiyoshi W. Masui, Charanjot Brar, Tomas Cassanelli, Shami Chatterjee, Victoria Kaspi, Kholoud Khairy, Adam E. Lanman, Mattias Lazda, Juan Mena-Parra, Gavin Noble, Aaron B. Pearlman, Mubdi Rahman, Pranav Sanghavi, Vishwangi Shah
Figure caption: VLBI fringes on an FRB detected on the CHIME-ARO10 and CHIME-TONE baselines (left and right columns, respectively), whose lengths are representative of those of CHIME/FRB Outriggers. This tests our delay compensation algorithms. We show the initial fringes detected (blue) while pointing at an initial guess of the FRB’s position from the CHIME/FRB baseband pipeline, and the fringes after recorrelation to a refined position obtained using the method in Appendix A.1, demonstrating the convergence of our procedure.
Paper: A VLBI Software Correlator for Fast Radio Transients
Authors: Calvin Leung, Shion Andrew, Kiyoshi W. Masui, Charanjot Brar, Tomas Cassanelli, Shami Chatterjee, Victoria Kaspi, Kholoud Khairy, Adam E. Lanman, Mattias Lazda, Juan Mena-Parra, Gavin Noble, Aaron B. Pearlman, Mubdi Rahman, Pranav Sanghavi, Vishwangi Shah
Figure caption: A high-level description of the various stages of single-pulse localization. The solid arrows denote the various stages in our pipeline. First, an initial guess of the FRB’s initial position is computed, with subarcminute precision, from the CHIME/FRB beamformer (D. Michilli et al. 2021). This allows for fringes to be found, and a coarse localization within the synthesized beam refines the delay center. The data are recorrelated toward the new delay center, which improves the correlation signal-to-noise ratio.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. VI. Confirmation of a Long-period Giant Planet Discovered with a Single TESS Transit
Authors: Zahra Essack, Diana Dragomir, Paul A. Dalba, Matthew P. Battley, David R. Ciardi, Karen A. Collins, Steve B. Howell, Matias I. Jones, Stephen R. Kane, Eric E. Mamajek, Christopher R. Mann, Ismael Mireles, Dominic Oddo, Lauren A. Sgro, Keivan G. Stassun, Solene Ulmer-Moll, Cristilyn N. Watkins, Samuel W. Yee, Carl Ziegler, Allyson Bieryla, Ioannis Apergis, Khalid Barkaoui, Rafael Brahm, Edward M. Bryant, Thomas M. Esposito, Pedro Figueira, Benjamin J. Fulton, Samuel Gill, Andrew W. Howard, Howard Isaacson, Alicia Kendall, Nicholas Law, Michael B. Lund, Andrew W. Mann, Rachel A. Matson, Felipe Murgas, Enric Palle, Samuel N. Quinn, Alexandre Revol, Suman Saha, Richard P. Schwarz, Ramotholo Sefako, Avi Shporer, Ivan A. Strakhov, Steven Villanueva, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Pau Bosch-Cabot, Kevin I. Collins, Raquel Forés-Toribio, Fabian Rodriguez Frustagia, Eric Girardin, Ian J. Helm, Pablo Lewin, Jose A. Muñoz, Patrick Newman, Peter Plavchan, Gregor Srdoc, Chris Stockdale, Anaël Wünsche, Mario Billiani, Martin Davy, Alex Douvas, Keiichi Fukui, Bruno Guillet, Cory Ostrem, Michael Rushton, Angsar Schmidt, Andrea Finardi, Patrice Girard, Tateki Goto, Julien S. de Lambilly, Liouba Leroux, Fabrice Mortecrette, John W. Pickering, Michael Primm, Marc Ribot, Ethan Teng, Aad Verveen, Stefan Will, Mark Ziegler
Figure caption: Gemini North ‘Alopeke 5σ speckle imaging contrast curves in the 562 nm filter (blue line) and 832 nm filter (red line) as a function of the angular separation out to 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩2. The inset shows the reconstructed 832 nm image of TOI-4465 with a 1″ scale bar. TOI-4465 was found to have no close companions from the diffraction limit out to 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩2 to within the contrast levels achieved.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. VI. Confirmation of a Long-period Giant Planet Discovered with a Single TESS Transit
Authors: Zahra Essack, Diana Dragomir, Paul A. Dalba, Matthew P. Battley, David R. Ciardi, Karen A. Collins, Steve B. Howell, Matias I. Jones, Stephen R. Kane, Eric E. Mamajek, Christopher R. Mann, Ismael Mireles, Dominic Oddo, Lauren A. Sgro, Keivan G. Stassun, Solene Ulmer-Moll, Cristilyn N. Watkins, Samuel W. Yee, Carl Ziegler, Allyson Bieryla, Ioannis Apergis, Khalid Barkaoui, Rafael Brahm, Edward M. Bryant, Thomas M. Esposito, Pedro Figueira, Benjamin J. Fulton, Samuel Gill, Andrew W. Howard, Howard Isaacson, Alicia Kendall, Nicholas Law, Michael B. Lund, Andrew W. Mann, Rachel A. Matson, Felipe Murgas, Enric Palle, Samuel N. Quinn, Alexandre Revol, Suman Saha, Richard P. Schwarz, Ramotholo Sefako, Avi Shporer, Ivan A. Strakhov, Steven Villanueva, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Pau Bosch-Cabot, Kevin I. Collins, Raquel Forés-Toribio, Fabian Rodriguez Frustagia, Eric Girardin, Ian J. Helm, Pablo Lewin, Jose A. Muñoz, Patrick Newman, Peter Plavchan, Gregor Srdoc, Chris Stockdale, Anaël Wünsche, Mario Billiani, Martin Davy, Alex Douvas, Keiichi Fukui, Bruno Guillet, Cory Ostrem, Michael Rushton, Angsar Schmidt, Andrea Finardi, Patrice Girard, Tateki Goto, Julien S. de Lambilly, Liouba Leroux, Fabrice Mortecrette, John W. Pickering, Michael Primm, Marc Ribot, Ethan Teng, Aad Verveen, Stefan Will, Mark Ziegler
Figure caption: SOAR speckle imaging observations of TOI-4465. The contrast curve (5σ sensitivity limits) and autocorrelation functions (inset) are shown. No additional sources were detected within 3″ of TOI-4465.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. VI. Confirmation of a Long-period Giant Planet Discovered with a Single TESS Transit
Authors: Zahra Essack, Diana Dragomir, Paul A. Dalba, Matthew P. Battley, David R. Ciardi, Karen A. Collins, Steve B. Howell, Matias I. Jones, Stephen R. Kane, Eric E. Mamajek, Christopher R. Mann, Ismael Mireles, Dominic Oddo, Lauren A. Sgro, Keivan G. Stassun, Solene Ulmer-Moll, Cristilyn N. Watkins, Samuel W. Yee, Carl Ziegler, Allyson Bieryla, Ioannis Apergis, Khalid Barkaoui, Rafael Brahm, Edward M. Bryant, Thomas M. Esposito, Pedro Figueira, Benjamin J. Fulton, Samuel Gill, Andrew W. Howard, Howard Isaacson, Alicia Kendall, Nicholas Law, Michael B. Lund, Andrew W. Mann, Rachel A. Matson, Felipe Murgas, Enric Palle, Samuel N. Quinn, Alexandre Revol, Suman Saha, Richard P. Schwarz, Ramotholo Sefako, Avi Shporer, Ivan A. Strakhov, Steven Villanueva, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Pau Bosch-Cabot, Kevin I. Collins, Raquel Forés-Toribio, Fabian Rodriguez Frustagia, Eric Girardin, Ian J. Helm, Pablo Lewin, Jose A. Muñoz, Patrick Newman, Peter Plavchan, Gregor Srdoc, Chris Stockdale, Anaël Wünsche, Mario Billiani, Martin Davy, Alex Douvas, Keiichi Fukui, Bruno Guillet, Cory Ostrem, Michael Rushton, Angsar Schmidt, Andrea Finardi, Patrice Girard, Tateki Goto, Julien S. de Lambilly, Liouba Leroux, Fabrice Mortecrette, John W. Pickering, Michael Primm, Marc Ribot, Ethan Teng, Aad Verveen, Stefan Will, Mark Ziegler
Figure caption: SAI speckle imaging observations of TOI-4465. The contrast curve (5σ sensitivity limits) and autocorrelation functions (inset) are shown.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. VI. Confirmation of a Long-period Giant Planet Discovered with a Single TESS Transit
Authors: Zahra Essack, Diana Dragomir, Paul A. Dalba, Matthew P. Battley, David R. Ciardi, Karen A. Collins, Steve B. Howell, Matias I. Jones, Stephen R. Kane, Eric E. Mamajek, Christopher R. Mann, Ismael Mireles, Dominic Oddo, Lauren A. Sgro, Keivan G. Stassun, Solene Ulmer-Moll, Cristilyn N. Watkins, Samuel W. Yee, Carl Ziegler, Allyson Bieryla, Ioannis Apergis, Khalid Barkaoui, Rafael Brahm, Edward M. Bryant, Thomas M. Esposito, Pedro Figueira, Benjamin J. Fulton, Samuel Gill, Andrew W. Howard, Howard Isaacson, Alicia Kendall, Nicholas Law, Michael B. Lund, Andrew W. Mann, Rachel A. Matson, Felipe Murgas, Enric Palle, Samuel N. Quinn, Alexandre Revol, Suman Saha, Richard P. Schwarz, Ramotholo Sefako, Avi Shporer, Ivan A. Strakhov, Steven Villanueva, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Pau Bosch-Cabot, Kevin I. Collins, Raquel Forés-Toribio, Fabian Rodriguez Frustagia, Eric Girardin, Ian J. Helm, Pablo Lewin, Jose A. Muñoz, Patrick Newman, Peter Plavchan, Gregor Srdoc, Chris Stockdale, Anaël Wünsche, Mario Billiani, Martin Davy, Alex Douvas, Keiichi Fukui, Bruno Guillet, Cory Ostrem, Michael Rushton, Angsar Schmidt, Andrea Finardi, Patrice Girard, Tateki Goto, Julien S. de Lambilly, Liouba Leroux, Fabrice Mortecrette, John W. Pickering, Michael Primm, Marc Ribot, Ethan Teng, Aad Verveen, Stefan Will, Mark Ziegler
Figure caption: Results of the juliet joint fit to LCOGT, NGTS, and NEOSSat photometry. Top: transit observations of the respective instruments phase-folded to the period of TOI-4465 b. The black curve is the best-fit juliet transit model, and the 68% confidence interval is represented by the gray shaded region. Binned data points with error bars are shown for clarity (white circles). The LCOGT data are binned in 45-minute intervals, the NGTS data are binned in 10-minute intervals, and the NEOSSat data are binned in 4-minute intervals. Bottom: residuals after the data have been subtracted from the best-fit model.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. VI. Confirmation of a Long-period Giant Planet Discovered with a Single TESS Transit
Authors: Zahra Essack, Diana Dragomir, Paul A. Dalba, Matthew P. Battley, David R. Ciardi, Karen A. Collins, Steve B. Howell, Matias I. Jones, Stephen R. Kane, Eric E. Mamajek, Christopher R. Mann, Ismael Mireles, Dominic Oddo, Lauren A. Sgro, Keivan G. Stassun, Solene Ulmer-Moll, Cristilyn N. Watkins, Samuel W. Yee, Carl Ziegler, Allyson Bieryla, Ioannis Apergis, Khalid Barkaoui, Rafael Brahm, Edward M. Bryant, Thomas M. Esposito, Pedro Figueira, Benjamin J. Fulton, Samuel Gill, Andrew W. Howard, Howard Isaacson, Alicia Kendall, Nicholas Law, Michael B. Lund, Andrew W. Mann, Rachel A. Matson, Felipe Murgas, Enric Palle, Samuel N. Quinn, Alexandre Revol, Suman Saha, Richard P. Schwarz, Ramotholo Sefako, Avi Shporer, Ivan A. Strakhov, Steven Villanueva, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Pau Bosch-Cabot, Kevin I. Collins, Raquel Forés-Toribio, Fabian Rodriguez Frustagia, Eric Girardin, Ian J. Helm, Pablo Lewin, Jose A. Muñoz, Patrick Newman, Peter Plavchan, Gregor Srdoc, Chris Stockdale, Anaël Wünsche, Mario Billiani, Martin Davy, Alex Douvas, Keiichi Fukui, Bruno Guillet, Cory Ostrem, Michael Rushton, Angsar Schmidt, Andrea Finardi, Patrice Girard, Tateki Goto, Julien S. de Lambilly, Liouba Leroux, Fabrice Mortecrette, John W. Pickering, Michael Primm, Marc Ribot, Ethan Teng, Aad Verveen, Stefan Will, Mark Ziegler
Figure caption: Mass–radius diagram for confirmed giant planets (Rp > 0.2RJ, Mp < 13MJ) with measured mass and radius uncertainties below 20%. Planets are colored according to their average equilibrium temperature (calculated assuming zero albedo and efficient heat redistribution). Left: mass–radius diagram with curves of constant bulk densities ranging from 0.1 g cm−3 (dark blue) to 6.2 g cm−3 (yellow). Right: mass–radius diagram with composition curves from theoretical models in J. J. Fortney et al. (2007). From bottom curve to top: 100% silicates (light orange), 100% H2O (dark orange), 10% H/He atmosphere (magenta), 50% H/He (purple), and 100% H/He (dark blue). TOI-4465 b has a bulk density of 3.73 g cm−3 and is one of very few known giant planets that are large, massive, dense, and temperate.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. VI. Confirmation of a Long-period Giant Planet Discovered with a Single TESS Transit
Authors: Zahra Essack, Diana Dragomir, Paul A. Dalba, Matthew P. Battley, David R. Ciardi, Karen A. Collins, Steve B. Howell, Matias I. Jones, Stephen R. Kane, Eric E. Mamajek, Christopher R. Mann, Ismael Mireles, Dominic Oddo, Lauren A. Sgro, Keivan G. Stassun, Solene Ulmer-Moll, Cristilyn N. Watkins, Samuel W. Yee, Carl Ziegler, Allyson Bieryla, Ioannis Apergis, Khalid Barkaoui, Rafael Brahm, Edward M. Bryant, Thomas M. Esposito, Pedro Figueira, Benjamin J. Fulton, Samuel Gill, Andrew W. Howard, Howard Isaacson, Alicia Kendall, Nicholas Law, Michael B. Lund, Andrew W. Mann, Rachel A. Matson, Felipe Murgas, Enric Palle, Samuel N. Quinn, Alexandre Revol, Suman Saha, Richard P. Schwarz, Ramotholo Sefako, Avi Shporer, Ivan A. Strakhov, Steven Villanueva, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Pau Bosch-Cabot, Kevin I. Collins, Raquel Forés-Toribio, Fabian Rodriguez Frustagia, Eric Girardin, Ian J. Helm, Pablo Lewin, Jose A. Muñoz, Patrick Newman, Peter Plavchan, Gregor Srdoc, Chris Stockdale, Anaël Wünsche, Mario Billiani, Martin Davy, Alex Douvas, Keiichi Fukui, Bruno Guillet, Cory Ostrem, Michael Rushton, Angsar Schmidt, Andrea Finardi, Patrice Girard, Tateki Goto, Julien S. de Lambilly, Liouba Leroux, Fabrice Mortecrette, John W. Pickering, Michael Primm, Marc Ribot, Ethan Teng, Aad Verveen, Stefan Will, Mark Ziegler
Figure caption: Period–mass plot for confirmed giant planets (Rp > 0.2RJ, Mp < 13MJ) with measured mass and radius uncertainties below 20%. Planets are colored according to their orbital eccentricity. Planets at longer orbital periods generally trend toward higher eccentricities. TOI-4465 b’s eccentricity is comparatively mild for its mass and period.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. VI. Confirmation of a Long-period Giant Planet Discovered with a Single TESS Transit
Authors: Zahra Essack, Diana Dragomir, Paul A. Dalba, Matthew P. Battley, David R. Ciardi, Karen A. Collins, Steve B. Howell, Matias I. Jones, Stephen R. Kane, Eric E. Mamajek, Christopher R. Mann, Ismael Mireles, Dominic Oddo, Lauren A. Sgro, Keivan G. Stassun, Solene Ulmer-Moll, Cristilyn N. Watkins, Samuel W. Yee, Carl Ziegler, Allyson Bieryla, Ioannis Apergis, Khalid Barkaoui, Rafael Brahm, Edward M. Bryant, Thomas M. Esposito, Pedro Figueira, Benjamin J. Fulton, Samuel Gill, Andrew W. Howard, Howard Isaacson, Alicia Kendall, Nicholas Law, Michael B. Lund, Andrew W. Mann, Rachel A. Matson, Felipe Murgas, Enric Palle, Samuel N. Quinn, Alexandre Revol, Suman Saha, Richard P. Schwarz, Ramotholo Sefako, Avi Shporer, Ivan A. Strakhov, Steven Villanueva, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Pau Bosch-Cabot, Kevin I. Collins, Raquel Forés-Toribio, Fabian Rodriguez Frustagia, Eric Girardin, Ian J. Helm, Pablo Lewin, Jose A. Muñoz, Patrick Newman, Peter Plavchan, Gregor Srdoc, Chris Stockdale, Anaël Wünsche, Mario Billiani, Martin Davy, Alex Douvas, Keiichi Fukui, Bruno Guillet, Cory Ostrem, Michael Rushton, Angsar Schmidt, Andrea Finardi, Patrice Girard, Tateki Goto, Julien S. de Lambilly, Liouba Leroux, Fabrice Mortecrette, John W. Pickering, Michael Primm, Marc Ribot, Ethan Teng, Aad Verveen, Stefan Will, Mark Ziegler
Figure caption: TESS light curves of TOI-4465. Top: detrended, normalized, and flattened Sector 40 FFI light curve. Light-gray points are the TESS 10-minute cadence flux measurements; dark-gray points are the same data binned into 2.5 hr intervals. The single transit occurred at 2459395.1256 BJD. Middle: zoomed-in view of the transit event, along with the best-fit transit model (red). Gray points are 10-minute cadence measurements. Bottom: residuals after the data have been subtracted from the best-fit model. Residuals are binned into 50-minute intervals.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. VI. Confirmation of a Long-period Giant Planet Discovered with a Single TESS Transit
Authors: Zahra Essack, Diana Dragomir, Paul A. Dalba, Matthew P. Battley, David R. Ciardi, Karen A. Collins, Steve B. Howell, Matias I. Jones, Stephen R. Kane, Eric E. Mamajek, Christopher R. Mann, Ismael Mireles, Dominic Oddo, Lauren A. Sgro, Keivan G. Stassun, Solene Ulmer-Moll, Cristilyn N. Watkins, Samuel W. Yee, Carl Ziegler, Allyson Bieryla, Ioannis Apergis, Khalid Barkaoui, Rafael Brahm, Edward M. Bryant, Thomas M. Esposito, Pedro Figueira, Benjamin J. Fulton, Samuel Gill, Andrew W. Howard, Howard Isaacson, Alicia Kendall, Nicholas Law, Michael B. Lund, Andrew W. Mann, Rachel A. Matson, Felipe Murgas, Enric Palle, Samuel N. Quinn, Alexandre Revol, Suman Saha, Richard P. Schwarz, Ramotholo Sefako, Avi Shporer, Ivan A. Strakhov, Steven Villanueva, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Pau Bosch-Cabot, Kevin I. Collins, Raquel Forés-Toribio, Fabian Rodriguez Frustagia, Eric Girardin, Ian J. Helm, Pablo Lewin, Jose A. Muñoz, Patrick Newman, Peter Plavchan, Gregor Srdoc, Chris Stockdale, Anaël Wünsche, Mario Billiani, Martin Davy, Alex Douvas, Keiichi Fukui, Bruno Guillet, Cory Ostrem, Michael Rushton, Angsar Schmidt, Andrea Finardi, Patrice Girard, Tateki Goto, Julien S. de Lambilly, Liouba Leroux, Fabrice Mortecrette, John W. Pickering, Michael Primm, Marc Ribot, Ethan Teng, Aad Verveen, Stefan Will, Mark Ziegler
Figure caption: Results of the juliet joint fit to the APF, CHIRON, and TRES RVs. Top: APF (blue points), CHIRON (green points), and TRES (orange points) RVs over time, and full best-fit juliet model (black curve). Middle: phase-folded RV measurements from APF, CHIRON, and TRES. The black curve is the best-fit juliet RV model. Error bars are the quadrature sum of the individual instrument internal uncertainties and the RV jitter estimate from the juliet fit. The best-fit RV semiamplitude and orbital eccentricity are ﹩K=277.1{9}_{-1.90}^{+2.37}\,{\rm{m}}\,{{\rm{s}}}^{-1}﹩ and e = 0.24 ± 0.01, respectively. Bottom: RV residuals after the data have been subtracted from the best-fit model.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. VI. Confirmation of a Long-period Giant Planet Discovered with a Single TESS Transit
Authors: Zahra Essack, Diana Dragomir, Paul A. Dalba, Matthew P. Battley, David R. Ciardi, Karen A. Collins, Steve B. Howell, Matias I. Jones, Stephen R. Kane, Eric E. Mamajek, Christopher R. Mann, Ismael Mireles, Dominic Oddo, Lauren A. Sgro, Keivan G. Stassun, Solene Ulmer-Moll, Cristilyn N. Watkins, Samuel W. Yee, Carl Ziegler, Allyson Bieryla, Ioannis Apergis, Khalid Barkaoui, Rafael Brahm, Edward M. Bryant, Thomas M. Esposito, Pedro Figueira, Benjamin J. Fulton, Samuel Gill, Andrew W. Howard, Howard Isaacson, Alicia Kendall, Nicholas Law, Michael B. Lund, Andrew W. Mann, Rachel A. Matson, Felipe Murgas, Enric Palle, Samuel N. Quinn, Alexandre Revol, Suman Saha, Richard P. Schwarz, Ramotholo Sefako, Avi Shporer, Ivan A. Strakhov, Steven Villanueva, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Pau Bosch-Cabot, Kevin I. Collins, Raquel Forés-Toribio, Fabian Rodriguez Frustagia, Eric Girardin, Ian J. Helm, Pablo Lewin, Jose A. Muñoz, Patrick Newman, Peter Plavchan, Gregor Srdoc, Chris Stockdale, Anaël Wünsche, Mario Billiani, Martin Davy, Alex Douvas, Keiichi Fukui, Bruno Guillet, Cory Ostrem, Michael Rushton, Angsar Schmidt, Andrea Finardi, Patrice Girard, Tateki Goto, Julien S. de Lambilly, Liouba Leroux, Fabrice Mortecrette, John W. Pickering, Michael Primm, Marc Ribot, Ethan Teng, Aad Verveen, Stefan Will, Mark Ziegler
Figure caption: Period–radius plot for confirmed giant planets (Rp > 0.2RJ, Mp < 13MJ) with measured mass and radius uncertainties below 20%. Planets are colored according to their mass. TOI-4465 b has the largest radius among giant planets with P > 100 days and is the second most massive planet with Rp > 1.2RJ and P > 10 days.