adsabs/AstroCLIMB huggingface dataset:
Paper: K2-79b and K2-222b: Mass Measurements of Two Small Exoplanets with Periods beyond 10 days that Overlap with Periodic Magnetic Activity Signals
Authors: Chantanelle Nava, Mercedes López-Morales, Annelies Mortier, Li Zeng, Helen A. C. Giles, Allyson Bieryla, Andrew Vanderburg, Lars A. Buchhave, Ennio Poretti, Steven H. Saar, Xavier Dumusque, David W. Latham, David Charbonneau, Mario Damasso, Aldo S. Bonomo, Christophe Lovis, Andrew Collier Cameron, Jason D. Eastman, Alessandro Sozzetti, Rosario Cosentino, Marco Pedani, Francesco Pepe, Emilio Molinari, Dimitar Sasselov, Michel Mayor, Manu Stalport, Luca Malavolta, Ken Rice, Christopher A. Watson, A. F. Martinez Fiorenzano, Luca Di Fabrizio
Figure caption: K2-79 GLS periodograms of HARPS-N RVs and activity indicators. The full RV set shows weak correlations with the contrast, cross-correlation function (CCF) area, and bisector inverse span (BIS). The season 1 (S1) RVs show no correlation with any activity indicators. The season 2 (S2) RVs show weak correlations with the contrast and CCF area, as well as a strong anticorrelation with the BIS. P  b  is the period of the known transiting exoplanet. The signal at P  b  could potentially be combined with an activity signal, based on the corresponding peaks with FAP ≈ 10% and ≈ 50% in the S2 BIS and contrast periodograms, respectively. At P  b , the seasonal RVs show a stronger signal in S1, but the seasonal-activity indicators show stronger signals in S2, particularly in contrast and BIS.
Paper: K2-79b and K2-222b: Mass Measurements of Two Small Exoplanets with Periods beyond 10 days that Overlap with Periodic Magnetic Activity Signals
Authors: Chantanelle Nava, Mercedes López-Morales, Annelies Mortier, Li Zeng, Helen A. C. Giles, Allyson Bieryla, Andrew Vanderburg, Lars A. Buchhave, Ennio Poretti, Steven H. Saar, Xavier Dumusque, David W. Latham, David Charbonneau, Mario Damasso, Aldo S. Bonomo, Christophe Lovis, Andrew Collier Cameron, Jason D. Eastman, Alessandro Sozzetti, Rosario Cosentino, Marco Pedani, Francesco Pepe, Emilio Molinari, Dimitar Sasselov, Michel Mayor, Manu Stalport, Luca Malavolta, Ken Rice, Christopher A. Watson, A. F. Martinez Fiorenzano, Luca Di Fabrizio
Figure caption: K2-222 GLS periodograms of HARPS-N RVs and activity indicators. The full RV set shows a moderate correlation with the contrast and a weak correlation with the CCF area.Pb  is the period of the known transiting exoplanet. The signal at Pb  could potentially be combined with an activity signal, based on the corresponding peak with FAP ≈ 10% in the contrast periodogram. At Pb , the seasonal RVs show a stronger signal in S1, but the seasonal-activity indicators show stronger signals in S2, particularly contrast. Pc?   is the period of a potential second companion object, and P act with FAP ≈ 1% is a signal we attribute to stellar activity because of the nearby peaks with FAP ≈ 10% in the FWHM periodograms. The signal at P act,1/2 with FAP ≈ 10% may also be related to activity, as it occurs at approximately one-half of P act and less than 1 day away from a peak with FAP < 50% in the contrast periodogram. The four prominent peaks surrounding the peak at P act,1/2 are aliases with the largest peak in the S2 window function. P  b  is the period of the known transiting exoplanet. The signal at P  b  could potentially be combined with an activity signal, based on the corresponding peak with FAP ≈ 10% in the contrast periodogram. At P  b , the seasonal RVs show a stronger signal in S1, but the seasonal-activity indicators show stronger signals in S2, particularly contrast. P  c? is the period of a potential second companion object, and P act with FAP≈1% is a signal we attribute to stellar activity because of the nearby peaks with FAP≈ 10% in the FWHM periodograms. The signal at P act,1/2 with FAP ≈ 10% may also be related to activity, as it occurs at approximately one-half of P act and less than 1 day away from a peak with FAP < 50% in the contrast periodogram. The four prominent peaks surrounding the peak at P act,1/2 are aliases with the largest peak in the S2 window function.
Paper: K2-79b and K2-222b: Mass Measurements of Two Small Exoplanets with Periods beyond 10 days that Overlap with Periodic Magnetic Activity Signals
Authors: Chantanelle Nava, Mercedes López-Morales, Annelies Mortier, Li Zeng, Helen A. C. Giles, Allyson Bieryla, Andrew Vanderburg, Lars A. Buchhave, Ennio Poretti, Steven H. Saar, Xavier Dumusque, David W. Latham, David Charbonneau, Mario Damasso, Aldo S. Bonomo, Christophe Lovis, Andrew Collier Cameron, Jason D. Eastman, Alessandro Sozzetti, Rosario Cosentino, Marco Pedani, Francesco Pepe, Emilio Molinari, Dimitar Sasselov, Michel Mayor, Manu Stalport, Luca Malavolta, Ken Rice, Christopher A. Watson, A. F. Martinez Fiorenzano, Luca Di Fabrizio
Figure caption: Phase-folded K2-79 LC (cyan points) with the fit-posterior transit model overplotted (green line).
Paper: K2-79b and K2-222b: Mass Measurements of Two Small Exoplanets with Periods beyond 10 days that Overlap with Periodic Magnetic Activity Signals
Authors: Chantanelle Nava, Mercedes López-Morales, Annelies Mortier, Li Zeng, Helen A. C. Giles, Allyson Bieryla, Andrew Vanderburg, Lars A. Buchhave, Ennio Poretti, Steven H. Saar, Xavier Dumusque, David W. Latham, David Charbonneau, Mario Damasso, Aldo S. Bonomo, Christophe Lovis, Andrew Collier Cameron, Jason D. Eastman, Alessandro Sozzetti, Rosario Cosentino, Marco Pedani, Francesco Pepe, Emilio Molinari, Dimitar Sasselov, Michel Mayor, Manu Stalport, Luca Malavolta, Ken Rice, Christopher A. Watson, A. F. Martinez Fiorenzano, Luca Di Fabrizio
Figure caption: Phase-folded K2-222 LC (cyan points) with the fit-posterior model overplotted (green line).
Paper: K2-79b and K2-222b: Mass Measurements of Two Small Exoplanets with Periods beyond 10 days that Overlap with Periodic Magnetic Activity Signals
Authors: Chantanelle Nava, Mercedes López-Morales, Annelies Mortier, Li Zeng, Helen A. C. Giles, Allyson Bieryla, Andrew Vanderburg, Lars A. Buchhave, Ennio Poretti, Steven H. Saar, Xavier Dumusque, David W. Latham, David Charbonneau, Mario Damasso, Aldo S. Bonomo, Christophe Lovis, Andrew Collier Cameron, Jason D. Eastman, Alessandro Sozzetti, Rosario Cosentino, Marco Pedani, Francesco Pepe, Emilio Molinari, Dimitar Sasselov, Michel Mayor, Manu Stalport, Luca Malavolta, Ken Rice, Christopher A. Watson, A. F. Martinez Fiorenzano, Luca Di Fabrizio
Figure caption: Phase-folded K2-79b RV curve (purple points, orange error bar) with the fit-posterior model overplotted (black line). The binned RVs (teal), spaced equally in phase (binsize = 1/Nbins) and averaged over phase and RV, were not used in any fits.
Paper: K2-79b and K2-222b: Mass Measurements of Two Small Exoplanets with Periods beyond 10 days that Overlap with Periodic Magnetic Activity Signals
Authors: Chantanelle Nava, Mercedes López-Morales, Annelies Mortier, Li Zeng, Helen A. C. Giles, Allyson Bieryla, Andrew Vanderburg, Lars A. Buchhave, Ennio Poretti, Steven H. Saar, Xavier Dumusque, David W. Latham, David Charbonneau, Mario Damasso, Aldo S. Bonomo, Christophe Lovis, Andrew Collier Cameron, Jason D. Eastman, Alessandro Sozzetti, Rosario Cosentino, Marco Pedani, Francesco Pepe, Emilio Molinari, Dimitar Sasselov, Michel Mayor, Manu Stalport, Luca Malavolta, Ken Rice, Christopher A. Watson, A. F. Martinez Fiorenzano, Luca Di Fabrizio
Figure caption: Phase-folded K2-222b RV curve (purple points, orange error bar) with the one-planet fit-posterior model overplotted (black line). The binned RVs (teal), spaced equally in phase and averaged over phase and RV, were not used in any fits.
Paper: K2-79b and K2-222b: Mass Measurements of Two Small Exoplanets with Periods beyond 10 days that Overlap with Periodic Magnetic Activity Signals
Authors: Chantanelle Nava, Mercedes López-Morales, Annelies Mortier, Li Zeng, Helen A. C. Giles, Allyson Bieryla, Andrew Vanderburg, Lars A. Buchhave, Ennio Poretti, Steven H. Saar, Xavier Dumusque, David W. Latham, David Charbonneau, Mario Damasso, Aldo S. Bonomo, Christophe Lovis, Andrew Collier Cameron, Jason D. Eastman, Alessandro Sozzetti, Rosario Cosentino, Marco Pedani, Francesco Pepe, Emilio Molinari, Dimitar Sasselov, Michel Mayor, Manu Stalport, Luca Malavolta, Ken Rice, Christopher A. Watson, A. F. Martinez Fiorenzano, Luca Di Fabrizio
Figure caption: Phase-folded K2-222b (left) and candidate second companion (right) RVs (purple points, orange error bar) with the two-planet fit-posterior model overplotted (black line). The binned RVs (teal), spaced equally in phase and averaged over phase and RV, were not used in any fits.
Paper: K2-79b and K2-222b: Mass Measurements of Two Small Exoplanets with Periods beyond 10 days that Overlap with Periodic Magnetic Activity Signals
Authors: Chantanelle Nava, Mercedes López-Morales, Annelies Mortier, Li Zeng, Helen A. C. Giles, Allyson Bieryla, Andrew Vanderburg, Lars A. Buchhave, Ennio Poretti, Steven H. Saar, Xavier Dumusque, David W. Latham, David Charbonneau, Mario Damasso, Aldo S. Bonomo, Christophe Lovis, Andrew Collier Cameron, Jason D. Eastman, Alessandro Sozzetti, Rosario Cosentino, Marco Pedani, Francesco Pepe, Emilio Molinari, Dimitar Sasselov, Michel Mayor, Manu Stalport, Luca Malavolta, Ken Rice, Christopher A. Watson, A. F. Martinez Fiorenzano, Luca Di Fabrizio
Figure caption: The scatter plot (left) shows the placements of K2-79b and K2-222b in mass–radius space among other confirmed small exoplanets (colored points) with T eq between 300 and 3000 K, 1σ mass errors less than 50%, 1σ radius errors less than 20%, and orbiting stars with radii between 0.6 R ⊙ and 2.0 R ⊙ (NASA Exoplanet Archive). Uranus (U) and Neptune (N) are indicated by gray dots. The red curve represents Fe-metal compositions of 100% iron, the orange curve represents pure silicates (MgSiO3) composition, and the blue curve represents pure H2O compositions. The contours above the blue curve depict different values of the z parameter discussed in Section 7, which characterizes both the amount and the temperature of the added envelope (Section 7; Zeng et al., 2021 (accepted)). The two sets of contours between the three colored curves represent equally spaced mass-proportions of the two compositions they lie between. The histogram (top right) shows the distribution of ζ values, also discussed in Section 7, for the same population of planets in the scatter plot, with K2-79b and K2-222b shown in blue. The histogram shows clearly a bimodal distribution, with the first peak (ζ ∼ 1) corresponding to purely rocky compositions, while the second peak (ζ ∼ 1.4) is consistent with ice-dominated compositions. The histogram also shows a potential trimodal distribution, with the third peak (ζ ∼ 2.1–2.4) consistent with Neptune-like planets. K2-222b is consistent with the second peak, and K2-79b is consistent with the third peak. The ternary plot (bottom left) shows how ζ relates to various potential exoplanet compositions (Zeng et al., 2021 (accepted)). The solid diagonal lines are contours of ζ, which range from slightly less than 0.9 in one extreme (pure-Fe metals) to slightly more than 1.4 in the other extreme (pure ices). The dashed straight line is a fixed ratio of Fe metals/silicates, which is a theoretical prediction from maximum collision stripping models.
Paper: K2-79b and K2-222b: Mass Measurements of Two Small Exoplanets with Periods beyond 10 days that Overlap with Periodic Magnetic Activity Signals
Authors: Chantanelle Nava, Mercedes López-Morales, Annelies Mortier, Li Zeng, Helen A. C. Giles, Allyson Bieryla, Andrew Vanderburg, Lars A. Buchhave, Ennio Poretti, Steven H. Saar, Xavier Dumusque, David W. Latham, David Charbonneau, Mario Damasso, Aldo S. Bonomo, Christophe Lovis, Andrew Collier Cameron, Jason D. Eastman, Alessandro Sozzetti, Rosario Cosentino, Marco Pedani, Francesco Pepe, Emilio Molinari, Dimitar Sasselov, Michel Mayor, Manu Stalport, Luca Malavolta, Ken Rice, Christopher A. Watson, A. F. Martinez Fiorenzano, Luca Di Fabrizio
Figure caption: Corner plot showing posterior distributions of hyper-parameters from the successful K2-79 Radvel Markov Chain Monte Carlo fits including a stellar activity signal modeled with quasiperiodic GP regression. The Radvel hyper-parameters 1–4 represent A, τ, P quasi, and η. The ≈24 day P quasi signal is consistent with that returned by the LC ACFs, as well as close in value to the largest peaks in the LC periodogram, P rot,Noyes, and the ﹩{P}_{\mathrm{rot},\max }﹩ calculated from ﹩v\,\sin \,i﹩. The second smaller peak that shows up in the posterior at 12–13 days and the 11 day peak in the BIS periodogram both sit near the first harmonic of the 24 day signal. We therefore estimate that K2-79 has a P rot in the range 21–26 days.
Paper: K2-79b and K2-222b: Mass Measurements of Two Small Exoplanets with Periods beyond 10 days that Overlap with Periodic Magnetic Activity Signals
Authors: Chantanelle Nava, Mercedes López-Morales, Annelies Mortier, Li Zeng, Helen A. C. Giles, Allyson Bieryla, Andrew Vanderburg, Lars A. Buchhave, Ennio Poretti, Steven H. Saar, Xavier Dumusque, David W. Latham, David Charbonneau, Mario Damasso, Aldo S. Bonomo, Christophe Lovis, Andrew Collier Cameron, Jason D. Eastman, Alessandro Sozzetti, Rosario Cosentino, Marco Pedani, Francesco Pepe, Emilio Molinari, Dimitar Sasselov, Michel Mayor, Manu Stalport, Luca Malavolta, Ken Rice, Christopher A. Watson, A. F. Martinez Fiorenzano, Luca Di Fabrizio
Figure caption: Corner plot showing posterior distributions of hyper-parameters from one of the successful K2-222 Radvel Markov Chain Monte Carlo fits including a stellar activity signal modeled with quasiperiodic GP regression. The Radvel hyper-parameters 1–4 represent A, τ, P quasi, and η. We only show the corner plot for the fit utilizing all RVs because that from the fit to only S1 RVs contains no notable differences. The ≈4 day P quasi signal returned for K2-222 is consistent with the first harmonics of the estimated P rot,Noyes and the ≈8 day peaks in the RV and FWHM periodograms. While we believe ≈8 days is the most likely rotation period of this star, estimates of P rot for K2-222 have varied greatly for certain methods, and we are less confident in this estimate than that for K2-79.
Paper: Dynamical Mass of the Exoplanet Host Star HR 8799
Authors: Aldo G. Sepulveda, Brendan P. Bowler
Figure caption: NIRC2 3 μm observation of HR 8799. The left panel shows the processed (PSF-subtracted) image, revealing HR 8799 b, c, d. Planet e is not detected at a significant level in this data set. The right panel shows the corresponding S/N map. North is up, and east is to the left.
Paper: Dynamical Mass of the Exoplanet Host Star HR 8799
Authors: Aldo G. Sepulveda, Brendan P. Bowler
Figure caption: Cutouts showing our negative PSF injection strategy for astrometry and relative photometry. The unsaturated image of HR 8799 (left) is used as a PSF model. After optimizing the model position and amplitude, planets b, c, and d (top) are removed from the final processed image (bottom) while preserving the underlying noise structure.
Paper: Dynamical Mass of the Exoplanet Host Star HR 8799
Authors: Aldo G. Sepulveda, Brendan P. Bowler
Figure caption: Relative astrometry used in this study as a function of time. The best-fitting linear models for ρ(t) and θ(t) are used to estimate the error inflation and calculate the respective ﹩{\chi }_{\nu }^{2}﹩ values. Raw uncertainties are denoted in red. Position angles have an additional systematic uncertainty term added in quadrature (see Section 3.1), denoted in blue along with corresponding revised linear regression. Uncertainties associated with the separation measurements are left unchanged because the reduced ﹩{\chi }_{\nu }^{2}﹩ value of a linear fit to the raw values is <1.0 for all four planets.
Paper: Dynamical Mass of the Exoplanet Host Star HR 8799
Authors: Aldo G. Sepulveda, Brendan P. Bowler
Figure caption: Orbit fits for HR 8799 b, c, d, and e using orbitize!. Each panel shows 150 orbits drawn from the converged MCMC chains as described in Section 3.2 together with the measured astrometry. For each planet, the left panel displays the orbits as they appear on-sky, and the right panels compare the same orbits to the astrometry.
Paper: Dynamical Mass of the Exoplanet Host Star HR 8799
Authors: Aldo G. Sepulveda, Brendan P. Bowler
Figure caption: Posterior probability distributions for the total mass of HR 8799 based on orbit fitting for each individual planet, as described in Section 3.2. Dark blue regions represent the 68% HCI, and light blue regions represent the 95% HCI. Median values are denoted with a black bar.
Paper: Dynamical Mass of the Exoplanet Host Star HR 8799
Authors: Aldo G. Sepulveda, Brendan P. Bowler
Figure caption: Graphical representation of our Bayesian framework to derive the joint dynamical mass posterior distribution for HR 8799. P(M ⋆∣b, c, d, e) represents the final joint constraint on the dynamical mass of HR 8799 given the astrometry of all four planets and without any assumptions about coplanarity, stability, or orbital resonances. This example uses a uniform prior for P(M ⋆).
Paper: Dynamical Mass of the Exoplanet Host Star HR 8799
Authors: Aldo G. Sepulveda, Brendan P. Bowler
Figure caption: Top row: MESA isomass tracks used to construct the age distributions of HR 8799. The thickness and color of each track is proportional to the probability density of the joint dynamical mass posterior distribution of HR 8799 at that model value. The solid black and gray lines denote the evolutionary track corresponding to the median value of our dynamical mass posterior. It is shown in black for the pre-main-sequence phase of evolution and then becomes gray for the post-main-sequence phase. Similarly, the dashed black and gray lines correspond to the 68% HCI. Each column of panels corresponds to a different metallicity from [Fe/H] = −0.5 to +0.25 dex. The orange ellipse represents the measurement and 1, 2, and 3σ uncertainties of L ⋆ and T eff for HR 8799. Middle row: The inferred age distributions of HR 8799 following the method described in Section 5.1. Bottom row: Corresponding hot-start masses for the planets derived directly from the age distribution and planet luminosities.
Paper: Dynamical Mass of the Exoplanet Host Star HR 8799
Authors: Aldo G. Sepulveda, Brendan P. Bowler
Figure caption: Summary of the MCMC orbit-fitting results for a uniform prior on the stellar host mass.
Paper: Dynamical Mass of the Exoplanet Host Star HR 8799
Authors: Aldo G. Sepulveda, Brendan P. Bowler
Figure caption: Same as Figure 8 but for the low-eccentricity scenario described in Section 4.1.
Paper: Dynamical Mass of the Exoplanet Host Star HR 8799
Authors: Aldo G. Sepulveda, Brendan P. Bowler
Figure caption: Same as Figure 4 but for the low-eccentricity scenario described in Section 4.1.
Paper: Dynamical Mass of the Exoplanet Host Star HR 8799
Authors: Aldo G. Sepulveda, Brendan P. Bowler
Figure caption: Same as Figure 7 but using the dynamical mass with an informed Gaussian prior of 1.47 ± 0.30 M ⊙ for the stellar mass.
Paper: Dynamical Mass of the Exoplanet Host Star HR 8799
Authors: Aldo G. Sepulveda, Brendan P. Bowler
Figure caption: Same as Figure 7 but using the dynamical mass with a uniform prior and low eccentricities.
Paper: Dynamical Mass of the Exoplanet Host Star HR 8799
Authors: Aldo G. Sepulveda, Brendan P. Bowler
Figure caption: Same as Figure 7 but using the dynamical mass with an informed Gaussian prior of 1.47 ± 0.30 M ⊙ for the stellar mass and low eccentricities.
Paper: Validation of 13 Hot and Potentially Terrestrial TESS Planets
Authors: Steven Giacalone, Courtney D. Dressing, Christina Hedges, Veselin B. Kostov, Karen A. Collins, Eric L. N. Jensen, Daniel A. Yahalomi, Allyson Bieryla, David R. Ciardi, Steve B. Howell, Jorge Lillo-Box, Khalid Barkaoui, Jennifer G. Winters, Elisabeth Matthews, John H. Livingston, Samuel N. Quinn, Boris S. Safonov, Charles Cadieux, E. Furlan, Ian J. M. Crossfield, Avi M. Mandell, Emily A. Gilbert, Ethan Kruse, Elisa V. Quintana, George R. Ricker, S. Seager, Joshua N. Winn, Jon M. Jenkins, Britt Duffy Adkins, David Baker, Thomas Barclay, David Barrado, Natalie M. Batalha, Alexander A. Belinski, Zouhair Benkhaldoun, Lars A. Buchhave, Luca Cacciapuoti, David Charbonneau, Ashley Chontos, Jessie L. Christiansen, Ryan Cloutier, Kevin I. Collins, Dennis M. Conti, Neil Cutting, Scott Dixon, René Doyon, Mohammed El Mufti, Emma Esparza-Borges, Zahra Essack, Akihiko Fukui, Tianjun Gan, Kaz Gary, Mourad Ghachoui, Michaël Gillon, Eric Girardin, Ana Glidden, Erica J. Gonzales, Pere Guerra, Elliott P. Horch, Krzysztof G. Hełminiak, Andrew W. Howard, Daniel Huber, Jonathan M. Irwin, Giovanni Isopi, Emmanuël Jehin, Taiki Kagetani, Stephen R. Kane, Kiyoe Kawauchi, John F. Kielkopf, Pablo Lewin, Lindy Luker, Michael B. Lund, Franco Mallia, Shude Mao, Bob Massey, Rachel A. Matson, Ismael Mireles, Mayuko Mori, Felipe Murgas, Norio Narita, Tanner O'Dwyer, Erik A. Petigura, Alex S. Polanski, Francisco J. Pozuelos, Enric Palle, Hannu Parviainen, Peter P. Plavchan, Howard M. Relles, Paul Robertson, Mark E. Rose, Pamela Rowden, Arpita Roy, Arjun B. Savel, Joshua E. Schlieder, Chloe Schnaible, Richard P. Schwarz, Ramatholo Sefako, Aleksandra Selezneva, Brett Skinner, Chris Stockdale, Ivan A. Strakhov, Thiam-Guan Tan, Guillermo Torres, René Tronsgaard, Joseph D. Twicken, David Vermilion, Ian A. Waite, Bradley Walter, Gavin Wang, Carl Ziegler, Yujie Zou
Figure caption: Phase-folded TESS data and best-fit transit models for each TOI. The parameters associated with these fits are shown in Table 3. The TESS data are purged of 5σ outliers and binned for clarity.