adsabs/AstroCLIMB huggingface dataset:
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). IX. A 27 Myr Extended Population of Lower Centaurus Crux with a Transiting Two-planet System
Authors: Mackenna L. Wood, Andrew W. Mann, Madyson G. Barber, Jonathan L. Bush, Adam L. Kraus, Benjamin M. Tofflemire, Andrew Vanderburg, Elisabeth R. Newton, Gregory A. Feiden, George Zhou, Luke G. Bouma, Samuel N. Quinn, David J. Armstrong, Ares Osborn, Vardan Adibekyan, Elisa Delgado Mena, Sergio G. Sousa, Jonathan Gagné, Matthew J. Fields, Reilly P. Milburn, Pa Chia Thao, Stephen P. Schmidt, Crystal L. Gnilka, Steve B. Howell, Nicholas M. Law, Carl Ziegler, César Briceño, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Joshua E. Schlieder, Hugh P. Osborn, Joseph D. Twicken, David R. Ciardi, Chelsea X. Huang
Figure caption: Phase-folded transits of HD 109833 b and HD 109833 c. The data are shown in yellow, with the 20 s cadence data from Sectors 38 and 39 binned to 2 m. Red points show all data binned together, and the black line shows the batman model using the results from the e = 0 MISTTBORN run.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). IX. A 27 Myr Extended Population of Lower Centaurus Crux with a Transiting Two-planet System
Authors: Mackenna L. Wood, Andrew W. Mann, Madyson G. Barber, Jonathan L. Bush, Adam L. Kraus, Benjamin M. Tofflemire, Andrew Vanderburg, Elisabeth R. Newton, Gregory A. Feiden, George Zhou, Luke G. Bouma, Samuel N. Quinn, David J. Armstrong, Ares Osborn, Vardan Adibekyan, Elisa Delgado Mena, Sergio G. Sousa, Jonathan Gagné, Matthew J. Fields, Reilly P. Milburn, Pa Chia Thao, Stephen P. Schmidt, Crystal L. Gnilka, Steve B. Howell, Nicholas M. Law, Carl Ziegler, César Briceño, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Joshua E. Schlieder, Hugh P. Osborn, Joseph D. Twicken, David R. Ciardi, Chelsea X. Huang
Figure caption: The posterior distribution of eccentricity resulting from the MISTTBORN fit, using a uniform prior distribution on e, and Gaussian prior on ρ * from our stellar parameters. Both planets are consistent with zero eccentricity.
Paper: The Orbital Architecture of Qatar-6: A Fully Aligned Three-body System?
Authors: Malena Rice, Songhu Wang, Konstantin Gerbig, Xian-Yu Wang, Fei Dai, Dakotah Tyler, Howard Isaacson, Andrew W. Howard
Figure caption: Gallery of 10 comparison systems with similar properties to Qatar-6, together with the normalized density of accepted orbital inclinations across all samples (bottom left). A total of 1000 accepted orbits, fit to Gaia DR3 astrometric constraints, are shown for each system. While we do find a tendency toward edge-on systems, the distribution of accepted orbits in our comparison sample is much broader than that of the Qatar-6 AB binary system.
Paper: The Orbital Architecture of Qatar-6: A Fully Aligned Three-body System?
Authors: Malena Rice, Songhu Wang, Konstantin Gerbig, Xian-Yu Wang, Fei Dai, Dakotah Tyler, Howard Isaacson, Andrew W. Howard
Figure caption: Posteriors from LOFTI fits to the Qatar-6 AB binary star system. The inclination (i) and longitude of ascending node (Ω) for the binary system are well constrained by Gaia DR3 astrometry. The median and 68% minimum credible interval for each parameter are each shown in gray and provided along the top of each panel.
Paper: The Orbital Architecture of Qatar-6: A Fully Aligned Three-body System?
Authors: Malena Rice, Songhu Wang, Konstantin Gerbig, Xian-Yu Wang, Fei Dai, Dakotah Tyler, Howard Isaacson, Andrew W. Howard
Figure caption: Maximum starting stellar obliquity at the time of protoplanetary disk dispersal, for a range of k 2/Q 10 values under the framework of dynamical tides. We consider the cases in which the true obliquity ψ is either within 1° of alignment (ψ = 1°) or set to ψ = 22°—the central value determined in Section 4.
Paper: Kepler-80 Revisited: Assessing the Participation of a Newly Discovered Planet in the Resonant Chain
Authors: D. Weisserman, J. C. Becker, A. Vanderburg
Figure caption: These histograms show the simulated libration amplitudes for the Kepler-80 three-body MMRs. For each of the four fits given in Table 1, 500 randomly selected draws were taken from the posterior and for each one, a numerical integration was run for 104 yr. From these integrations, the libration amplitude was computed. The vast majority of the draws from the posteriors show resonant libration for all three three-planet chains considered. Note that 3.8% of simulations from the fit including Kepler-80 g and with floating fit eccentricity exhibited nonresonant behavior in the g-c-b resonance, and were not included in the histograms shown here.
Paper: Kepler-80 Revisited: Assessing the Participation of a Newly Discovered Planet in the Resonant Chain
Authors: D. Weisserman, J. C. Becker, A. Vanderburg
Figure caption: These plots show the evolution of the resonant angles (given in degrees) for two draws from the unconstrained eccentricity posteriors (one with Kepler-80 g and one without Kepler-80 g) for a case where the planets are in a five-planet resonant chain. The evolution was computed by N-body simulation.
Paper: Kepler-80 Revisited: Assessing the Participation of a Newly Discovered Planet in the Resonant Chain
Authors: D. Weisserman, J. C. Becker, A. Vanderburg
Figure caption: These plots show the distribution of possible values for the masses of each planet under the four permutations of our fit assumptions.
Paper: Statistical Analysis of the Dearth of Super-eccentric Jupiters in the Kepler Sample
Authors: Jonathan M. Jackson, Rebekah I. Dawson, Billy Quarles, Jiayin Dong
Figure caption: Eccentricity vs. semimajor axis distribution of Jupiter-mass (>0.25 M Jup) confirmed planets orbiting main sequence stars (see Section 3 for exact cuts). Here 1 − e 2 is plotted on the y-axis to emphasize elliptical orbits. Hot Jupiters are plotted as red circles, moderately eccentric (0.2 < e < 0.6) Jupiters on tidal migration tracks are plotted as blue squares in the orange-shaded region, and more distant Jupiters (P > 10 days) are plotted as gray circles. Approximate periods shown on the upper axis are calculated assuming M * = 1 M ☉. The range of potential tidal migration tracks is outlined with dashed lines and two intervals of migration tracks, defined by 2.8 < P final < 5 and 5 < P final < 10 days, are delineated by the dotted line. The super-eccentric region (e > 0.9) within these tracks is shaded blue. The upper limit on the completeness of the Kepler sample (2 yr) is shown by the vertical purple line. Error bars have been removed for clarity, but see Dawson & Johnson (2018) Figure 4 for a similar plot with uncertainties included. Data taken from the NASA Exoplanet Archive on 2022 May 6 (NASA Exoplanet Science Institute 2020).
Paper: Testing the Interaction between a Substellar Companion and a Debris Disk in the HR 2562 System
Authors: Stella Yimiao Zhang, Gaspard Duchêne, Robert J. De Rosa, Megan Ansdell, Quinn Konopacky, Thomas Esposito, Eugene Chiang, Malena Rice, Brenda Matthews, Paul Kalas, Bruce Macintosh, Franck Marchis, Stan Metchev, Jenny Patience, Julien Rameau, Kimberly Ward-Duong, Schuyler Wolff, Michael P. Fitzgerald, Vanessa P. Bailey, Travis S. Barman, Joanna Bulger, Christine H. Chen, Jeffrey K. Chilcotte, Tara Cotten, René Doyon, Katherine B. Follette, Benjamin L. Gerard, Stephen Goodsell, James R. Graham, Alexandra Z. Greenbaum, Pascale Hibon, Li-Wei Hung, Patrick Ingraham, Jérôme Maire, Mark S. Marley, Christian Marois, Maxwell A. Millar-Blanchaer, Eric L. Nielsen, Rebecca Oppenheimer, David W. Palmer, Marshall D. Perrin, Lisa A. Poyneer, Laurent Pueyo, Abhijith Rajan, Fredrik T. Rantakyrö, Jean-Baptiste Ruffio, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Inseok Song, Remi Soummer, Sandrine Thomas, Jason J. Wang, Sloane J. Wiktorowicz
Figure caption: Posterior distributions and associated covariances of the semimajor axis (a), periastron distance (r apo), eccentricity (e), and inclination (i) from an orbit fit with (red) and without (black) a prior probability on the inclination and position angle (Ω) derived from the ALMA disk fitting. Contours represent the 1σ, 2σ, and 3σ confidence levels. Limiting the orbit to a coplanar configuration removes the tail of extremely high-eccentricity orbits.
Paper: Testing the Interaction between a Substellar Companion and a Debris Disk in the HR 2562 System
Authors: Stella Yimiao Zhang, Gaspard Duchêne, Robert J. De Rosa, Megan Ansdell, Quinn Konopacky, Thomas Esposito, Eugene Chiang, Malena Rice, Brenda Matthews, Paul Kalas, Bruce Macintosh, Franck Marchis, Stan Metchev, Jenny Patience, Julien Rameau, Kimberly Ward-Duong, Schuyler Wolff, Michael P. Fitzgerald, Vanessa P. Bailey, Travis S. Barman, Joanna Bulger, Christine H. Chen, Jeffrey K. Chilcotte, Tara Cotten, René Doyon, Katherine B. Follette, Benjamin L. Gerard, Stephen Goodsell, James R. Graham, Alexandra Z. Greenbaum, Pascale Hibon, Li-Wei Hung, Patrick Ingraham, Jérôme Maire, Mark S. Marley, Christian Marois, Maxwell A. Millar-Blanchaer, Eric L. Nielsen, Rebecca Oppenheimer, David W. Palmer, Marshall D. Perrin, Lisa A. Poyneer, Laurent Pueyo, Abhijith Rajan, Fredrik T. Rantakyrö, Jean-Baptiste Ruffio, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Inseok Song, Remi Soummer, Sandrine Thomas, Jason J. Wang, Sloane J. Wiktorowicz
Figure caption: Left panel: ALMA data of the HR 2562 system at 870 μm. The (0,0) of the images correspond to R.A. = 102.°5, decl. = −60.°2; Right panel: a zoomed-in region of the center of the disk is shown in the top left corner. The black circle represents the center of the disk determined by 2D Gaussian fit, the red star represents the Gaia DR3 coordinates of the star HR 2562, and the blue circle represents the orbit-predicted location of the companion HR 2562 B on 2018 January 31st. The disk center and the star are well aligned, and the companion is close to the star as expected.
Paper: Testing the Interaction between a Substellar Companion and a Debris Disk in the HR 2562 System
Authors: Stella Yimiao Zhang, Gaspard Duchêne, Robert J. De Rosa, Megan Ansdell, Quinn Konopacky, Thomas Esposito, Eugene Chiang, Malena Rice, Brenda Matthews, Paul Kalas, Bruce Macintosh, Franck Marchis, Stan Metchev, Jenny Patience, Julien Rameau, Kimberly Ward-Duong, Schuyler Wolff, Michael P. Fitzgerald, Vanessa P. Bailey, Travis S. Barman, Joanna Bulger, Christine H. Chen, Jeffrey K. Chilcotte, Tara Cotten, René Doyon, Katherine B. Follette, Benjamin L. Gerard, Stephen Goodsell, James R. Graham, Alexandra Z. Greenbaum, Pascale Hibon, Li-Wei Hung, Patrick Ingraham, Jérôme Maire, Mark S. Marley, Christian Marois, Maxwell A. Millar-Blanchaer, Eric L. Nielsen, Rebecca Oppenheimer, David W. Palmer, Marshall D. Perrin, Lisa A. Poyneer, Laurent Pueyo, Abhijith Rajan, Fredrik T. Rantakyrö, Jean-Baptiste Ruffio, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Inseok Song, Remi Soummer, Sandrine Thomas, Jason J. Wang, Sloane J. Wiktorowicz
Figure caption: Posterior distributions and associated covariance of the orbital eccentricity (e), inclination (i), and companion mass (M 2) from a joint fit to the relative and absolute astrometry. Contours represent the 1σ, 2σ, and 3σ confidence intervals.
Paper: Testing the Interaction between a Substellar Companion and a Debris Disk in the HR 2562 System
Authors: Stella Yimiao Zhang, Gaspard Duchêne, Robert J. De Rosa, Megan Ansdell, Quinn Konopacky, Thomas Esposito, Eugene Chiang, Malena Rice, Brenda Matthews, Paul Kalas, Bruce Macintosh, Franck Marchis, Stan Metchev, Jenny Patience, Julien Rameau, Kimberly Ward-Duong, Schuyler Wolff, Michael P. Fitzgerald, Vanessa P. Bailey, Travis S. Barman, Joanna Bulger, Christine H. Chen, Jeffrey K. Chilcotte, Tara Cotten, René Doyon, Katherine B. Follette, Benjamin L. Gerard, Stephen Goodsell, James R. Graham, Alexandra Z. Greenbaum, Pascale Hibon, Li-Wei Hung, Patrick Ingraham, Jérôme Maire, Mark S. Marley, Christian Marois, Maxwell A. Millar-Blanchaer, Eric L. Nielsen, Rebecca Oppenheimer, David W. Palmer, Marshall D. Perrin, Lisa A. Poyneer, Laurent Pueyo, Abhijith Rajan, Fredrik T. Rantakyrö, Jean-Baptiste Ruffio, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Inseok Song, Remi Soummer, Sandrine Thomas, Jason J. Wang, Sloane J. Wiktorowicz
Figure caption: 870 μm brightness profile along the disk major axis. The yellow shade indicates the 1σ uncertainty as determined from the surrounding background areas. The dashed line represent a horizontally reflected brightness profile about the location of the star.
Paper: Testing the Interaction between a Substellar Companion and a Debris Disk in the HR 2562 System
Authors: Stella Yimiao Zhang, Gaspard Duchêne, Robert J. De Rosa, Megan Ansdell, Quinn Konopacky, Thomas Esposito, Eugene Chiang, Malena Rice, Brenda Matthews, Paul Kalas, Bruce Macintosh, Franck Marchis, Stan Metchev, Jenny Patience, Julien Rameau, Kimberly Ward-Duong, Schuyler Wolff, Michael P. Fitzgerald, Vanessa P. Bailey, Travis S. Barman, Joanna Bulger, Christine H. Chen, Jeffrey K. Chilcotte, Tara Cotten, René Doyon, Katherine B. Follette, Benjamin L. Gerard, Stephen Goodsell, James R. Graham, Alexandra Z. Greenbaum, Pascale Hibon, Li-Wei Hung, Patrick Ingraham, Jérôme Maire, Mark S. Marley, Christian Marois, Maxwell A. Millar-Blanchaer, Eric L. Nielsen, Rebecca Oppenheimer, David W. Palmer, Marshall D. Perrin, Lisa A. Poyneer, Laurent Pueyo, Abhijith Rajan, Fredrik T. Rantakyrö, Jean-Baptiste Ruffio, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Inseok Song, Remi Soummer, Sandrine Thomas, Jason J. Wang, Sloane J. Wiktorowicz
Figure caption: The GPI PSF estimated from the four satellite spots (left column), the BKA forward model (second column), the GPI images of HR 2562 B (third column), and the residuals (fourth column) for each observation. The color scales are different for each data set and are denoted by the color bar on the right. The KLIP parameters used for each reduction are given in Table 1.
Paper: Testing the Interaction between a Substellar Companion and a Debris Disk in the HR 2562 System
Authors: Stella Yimiao Zhang, Gaspard Duchêne, Robert J. De Rosa, Megan Ansdell, Quinn Konopacky, Thomas Esposito, Eugene Chiang, Malena Rice, Brenda Matthews, Paul Kalas, Bruce Macintosh, Franck Marchis, Stan Metchev, Jenny Patience, Julien Rameau, Kimberly Ward-Duong, Schuyler Wolff, Michael P. Fitzgerald, Vanessa P. Bailey, Travis S. Barman, Joanna Bulger, Christine H. Chen, Jeffrey K. Chilcotte, Tara Cotten, René Doyon, Katherine B. Follette, Benjamin L. Gerard, Stephen Goodsell, James R. Graham, Alexandra Z. Greenbaum, Pascale Hibon, Li-Wei Hung, Patrick Ingraham, Jérôme Maire, Mark S. Marley, Christian Marois, Maxwell A. Millar-Blanchaer, Eric L. Nielsen, Rebecca Oppenheimer, David W. Palmer, Marshall D. Perrin, Lisa A. Poyneer, Laurent Pueyo, Abhijith Rajan, Fredrik T. Rantakyrö, Jean-Baptiste Ruffio, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Inseok Song, Remi Soummer, Sandrine Thomas, Jason J. Wang, Sloane J. Wiktorowicz
Figure caption: Normalized joint prior probability on the orbital inclination i and position angle Ω estimated using a Gaussian KDE for the coplanar scenario (main panel). Solid contours are spaced in 0.2 dex increments from −1.8 to −0.2; the inner dashed contour is at −0.01. Marginalized distributions are shown in the top and right panels for the posterior distribution estimated from the ALMA data (black solid histogram, Section 4) and for the prior distribution used in the orbit fit (red dashed histogram).
Paper: Testing the Interaction between a Substellar Companion and a Debris Disk in the HR 2562 System
Authors: Stella Yimiao Zhang, Gaspard Duchêne, Robert J. De Rosa, Megan Ansdell, Quinn Konopacky, Thomas Esposito, Eugene Chiang, Malena Rice, Brenda Matthews, Paul Kalas, Bruce Macintosh, Franck Marchis, Stan Metchev, Jenny Patience, Julien Rameau, Kimberly Ward-Duong, Schuyler Wolff, Michael P. Fitzgerald, Vanessa P. Bailey, Travis S. Barman, Joanna Bulger, Christine H. Chen, Jeffrey K. Chilcotte, Tara Cotten, René Doyon, Katherine B. Follette, Benjamin L. Gerard, Stephen Goodsell, James R. Graham, Alexandra Z. Greenbaum, Pascale Hibon, Li-Wei Hung, Patrick Ingraham, Jérôme Maire, Mark S. Marley, Christian Marois, Maxwell A. Millar-Blanchaer, Eric L. Nielsen, Rebecca Oppenheimer, David W. Palmer, Marshall D. Perrin, Lisa A. Poyneer, Laurent Pueyo, Abhijith Rajan, Fredrik T. Rantakyrö, Jean-Baptiste Ruffio, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Inseok Song, Remi Soummer, Sandrine Thomas, Jason J. Wang, Sloane J. Wiktorowicz
Figure caption: (left panel) Relative astrometry of HR 2562 B relative to HR 2562 from GPI (red) and SPHERE (blue). The location of the host star is indicated by the orange cross. Two hundred orbits drawn from the MCMC analysis (black curves) are also shown. (right panel) Offset between HR 2562 and the companion, and the residual compared with the median orbit, in the R.A. (top) and decl. (bottom) directions.
Paper: Validation of TOI-1221 b: A Warm Sub-Neptune Exhibiting Transit Timing Variations around a Sun-like Star
Authors: Christopher Mann, David Lafreniére, Diana Dragomir, Samuel N. Quinn, Thiam-Guan Tan, Karen A. Collins, Steve B. Howell, Carl Ziegler, Andrew W. Mann, Keivan G. Stassun, Martti H. Kristiansen, Hugh Osborn, Tabetha Boyajian, Nora Eisner, Coel Hellier, George R. Ricker, Roland Vanderspek, David W. Latham, S. Seager, Joshua N. Winn, Jon M. Jenkins, Jesus Noel Villaseñor, Brian McLean, Pamela Rowden, Guillermo Torres, Douglas A. Caldwell, Kevin I. Collins, Richard P. Schwarz
Figure caption: Individual transit midpoint posteriors for each transit in our data set. In each plot, the orange region corresponds to the 68% highest-posterior-density region, and the blue line shows where the best-fitting linear ephemeris would predict the midpoint to fall. Gray dashed curves show the Gaussian prior placed on these midpoint timings.
Paper: Validation of TOI-1221 b: A Warm Sub-Neptune Exhibiting Transit Timing Variations around a Sun-like Star
Authors: Christopher Mann, David Lafreniére, Diana Dragomir, Samuel N. Quinn, Thiam-Guan Tan, Karen A. Collins, Steve B. Howell, Carl Ziegler, Andrew W. Mann, Keivan G. Stassun, Martti H. Kristiansen, Hugh Osborn, Tabetha Boyajian, Nora Eisner, Coel Hellier, George R. Ricker, Roland Vanderspek, David W. Latham, S. Seager, Joshua N. Winn, Jon M. Jenkins, Jesus Noel Villaseñor, Brian McLean, Pamela Rowden, Guillermo Torres, Douglas A. Caldwell, Kevin I. Collins, Richard P. Schwarz
Figure caption: Top: midpoint timing distributions from Figure 6 plotted across time. The width of the blue region indicates the posterior probability distribution. The purple curves show sinusoid fits to 1000 random draws of these distributions. The timings display a sinusoidal variation suggestive of systematic TTVs. Bottom: distributions of the amplitude and periodicity from fitting 105 random draws. A zero-amplitude line (i.e., fixed-period ephemeris) is disfavored at 5.7σ.
Paper: Validation of TOI-1221 b: A Warm Sub-Neptune Exhibiting Transit Timing Variations around a Sun-like Star
Authors: Christopher Mann, David Lafreniére, Diana Dragomir, Samuel N. Quinn, Thiam-Guan Tan, Karen A. Collins, Steve B. Howell, Carl Ziegler, Andrew W. Mann, Keivan G. Stassun, Martti H. Kristiansen, Hugh Osborn, Tabetha Boyajian, Nora Eisner, Coel Hellier, George R. Ricker, Roland Vanderspek, David W. Latham, S. Seager, Joshua N. Winn, Jon M. Jenkins, Jesus Noel Villaseñor, Brian McLean, Pamela Rowden, Guillermo Torres, Douglas A. Caldwell, Kevin I. Collins, Richard P. Schwarz
Figure caption: First row: sector-by-sector PDCSAP flux, normalized to within-sector median. Purple bars indicate where transits were detected, orange bars indicate where expected transits fell in observing gaps. Rows 2 and 3: zoomed plot of each of the six caught transits. The TESS data were taken at a cadence of 2 minutes and are shown binned to 60 minute intervals with cyan points. The displayed transit model is described in Sections 3 and 4. Orange vertical lines show the predicted midpoints given a fixed-period ephemeris. Dashed black lines indicate the fitted midpoints, showing TTVs described in Section 3.4.
Paper: Validation of TOI-1221 b: A Warm Sub-Neptune Exhibiting Transit Timing Variations around a Sun-like Star
Authors: Christopher Mann, David Lafreniére, Diana Dragomir, Samuel N. Quinn, Thiam-Guan Tan, Karen A. Collins, Steve B. Howell, Carl Ziegler, Andrew W. Mann, Keivan G. Stassun, Martti H. Kristiansen, Hugh Osborn, Tabetha Boyajian, Nora Eisner, Coel Hellier, George R. Ricker, Roland Vanderspek, David W. Latham, S. Seager, Joshua N. Winn, Jon M. Jenkins, Jesus Noel Villaseñor, Brian McLean, Pamela Rowden, Guillermo Torres, Douglas A. Caldwell, Kevin I. Collins, Richard P. Schwarz
Figure caption: Light curves from the two LCOGT observations. Cyan points are binned to 15 minute intervals. The predicted timings come from the fixed-period ephemeris of previous TESS data. The transit duration is long enough to require observing from two separate longitudes to detect both ingress and egress. Like in Figure 1, the central orange and black lines indicate the midpoint timing expected by a fixed-period model or fitted by an agnostic model allowing TTVs, respectively.
Paper: Validation of TOI-1221 b: A Warm Sub-Neptune Exhibiting Transit Timing Variations around a Sun-like Star
Authors: Christopher Mann, David Lafreniére, Diana Dragomir, Samuel N. Quinn, Thiam-Guan Tan, Karen A. Collins, Steve B. Howell, Carl Ziegler, Andrew W. Mann, Keivan G. Stassun, Martti H. Kristiansen, Hugh Osborn, Tabetha Boyajian, Nora Eisner, Coel Hellier, George R. Ricker, Roland Vanderspek, David W. Latham, S. Seager, Joshua N. Winn, Jon M. Jenkins, Jesus Noel Villaseñor, Brian McLean, Pamela Rowden, Guillermo Torres, Douglas A. Caldwell, Kevin I. Collins, Richard P. Schwarz
Figure caption: Contrast achieved via speckle imaging from SOAR (top) and Gemini-S/Zorro (bottom) for TOI-1221. Neither measurement detects any neighboring sources within the limits of their sensitivities (5σ).
Paper: Validation of TOI-1221 b: A Warm Sub-Neptune Exhibiting Transit Timing Variations around a Sun-like Star
Authors: Christopher Mann, David Lafreniére, Diana Dragomir, Samuel N. Quinn, Thiam-Guan Tan, Karen A. Collins, Steve B. Howell, Carl Ziegler, Andrew W. Mann, Keivan G. Stassun, Martti H. Kristiansen, Hugh Osborn, Tabetha Boyajian, Nora Eisner, Coel Hellier, George R. Ricker, Roland Vanderspek, David W. Latham, S. Seager, Joshua N. Winn, Jon M. Jenkins, Jesus Noel Villaseñor, Brian McLean, Pamela Rowden, Guillermo Torres, Douglas A. Caldwell, Kevin I. Collins, Richard P. Schwarz
Figure caption: A 5′ field of view from PEST centered on the target (center object, ID #6). An example TESS aperture is overlaid in the same scale (cyan). Identifier numbers come from a brightness-ordered list of Gaia stars (red × points) in the area. Given TESS's pixel size and PSF width, it is typical to check for NEBs within 2.′5 of the target (orange circle). NEB check results for detectable neighboring stars are displayed in Table 1.
Paper: Validation of TOI-1221 b: A Warm Sub-Neptune Exhibiting Transit Timing Variations around a Sun-like Star
Authors: Christopher Mann, David Lafreniére, Diana Dragomir, Samuel N. Quinn, Thiam-Guan Tan, Karen A. Collins, Steve B. Howell, Carl Ziegler, Andrew W. Mann, Keivan G. Stassun, Martti H. Kristiansen, Hugh Osborn, Tabetha Boyajian, Nora Eisner, Coel Hellier, George R. Ricker, Roland Vanderspek, David W. Latham, S. Seager, Joshua N. Winn, Jon M. Jenkins, Jesus Noel Villaseñor, Brian McLean, Pamela Rowden, Guillermo Torres, Douglas A. Caldwell, Kevin I. Collins, Richard P. Schwarz
Figure caption: Spectral energy distribution of TOI-1221. Red symbols represent the observed photometric measurements with the horizontal bars representing the effective width of the bandpass. Blue symbols are the model fluxes from the best-fit Kurucz atmosphere model (black).