adsabs/AstroCLIMB huggingface dataset:
Paper: Accurate Photometry of Saturated Stars Using the Point-spread-function Wing Technique with Spitzer
Authors: Kate Y. L. Su, G. H. Rieke, M. Marengo, Everett Schlawin
Figure caption:                         (a) Radial flux ratio between Sirius and the star of interest with the name given on the upper left corner of each panel. For each row, the left panel is for channel 1 and the right panel for channel 2. Data points are shown as open, black squares with 1σ error bars, and the accumulative weighted average is shown with a solid red line. Blue dots show the data points that are used to compute the final flux ratio (i.e., having S/N greater than the cutoff threshold (20 in this case) and within ± 1σ of the average profile). (b) Similar to Figure 5(a) but for four additional stars. Note that data points that have S/N lower than the threshold (20 in this case) are not shown. (c) Similar to Figure 5(a) but for the rest of the stars.
Paper: Accurate Photometry of Saturated Stars Using the Point-spread-function Wing Technique with Spitzer
Authors: Kate Y. L. Su, G. H. Rieke, M. Marengo, Everett Schlawin
Figure caption: Radial profiles of all targets in the 3.6 μm (left panel) and 4.5 μm (right panel) bands, respectively. Different stars are plotted with different colors given on the plot. All radial profiles are self similar within 100″ (a dynamical range of ≳100 per star) while the profiles outside that range depart due to small background offsets. For the faintest target HD 165459, we also use various symbols to illustrate the signal-to-noise (S/N) ratio: solid black dots represent points with S/N ≥ 10, red circles for S/N ≥ 20, and blue circles for S/N ≥ 40.
Paper: The Transit Timing and Atmosphere of Hot Jupiter HAT-P-37b
Authors: Napaporn A-thano, Ing-Guey Jiang, Supachai Awiphan, Ronnakrit Rattanamala, Li-Hsin Su, Torik Hengpiya, Devesh P. Sariya, Li-Chin Yeh, A. A. Shlyapnikov, Mark A. Gorbachev, Alexey N. Rublevski, Vineet Kumar Mannaday, Parijat Thakur, D. K. Sahu, David Mkrtichian, Evgeny Griv
Figure caption:  O − C diagram and best-fitting models for HAT-P-37b with the data from Bakos et al. (2012; gray unfilled circles), Maciejewski et al. (2016; gray filled circles), Turner et al. (2017; blue unfilled circles), Wang et al. (2021; blue filled circles), Yang et al. (2021; red unfilled circles), and this work (red filled circles). The orange and green dotted lines present the timing residuals of the orbital decay and apsidal precession models, respectively.
Paper: The Transit Timing and Atmosphere of Hot Jupiter HAT-P-37b
Authors: Napaporn A-thano, Ing-Guey Jiang, Supachai Awiphan, Ronnakrit Rattanamala, Li-Hsin Su, Torik Hengpiya, Devesh P. Sariya, Li-Chin Yeh, A. A. Shlyapnikov, Mark A. Gorbachev, Alexey N. Rublevski, Vineet Kumar Mannaday, Parijat Thakur, D. K. Sahu, David Mkrtichian, Evgeny Griv
Figure caption: Searching for possible periodicity of TTVs of HAT-P-37b (a) GLS periodogram for timing residuals from Table 6. The dashed lines indicate the FAP levels. (b) O − C diagram and the best fit of sinusoidal variability from the frequency of the highest power peak, FAP = 0.02% (blue dotted line).
Paper: The Transit Timing and Atmosphere of Hot Jupiter HAT-P-37b
Authors: Napaporn A-thano, Ing-Guey Jiang, Supachai Awiphan, Ronnakrit Rattanamala, Li-Hsin Su, Torik Hengpiya, Devesh P. Sariya, Li-Chin Yeh, A. A. Shlyapnikov, Mark A. Gorbachev, Alexey N. Rublevski, Vineet Kumar Mannaday, Parijat Thakur, D. K. Sahu, David Mkrtichian, Evgeny Griv
Figure caption: Normalized flux as a function of phased-folded transit light curves of HAT-P-37b from our observations. The red and blue lines represent the best-fitting light curves model for R band and B band, respectively. The corresponding residuals with offsets 0.94 for R band and 0.92 for B band are shown below the light curves.
Paper: Exciting Mutual Inclination in Planetary Systems with a Distant Stellar Companion: The Case of Kepler-108
Authors: Wenrui Xu, Daniel Fabrycky
Figure caption: An example of capturing into a first-order ivection resonance. The primary and the binary are both 1M ⊙ stars, on circular orbit with a  B  ≈ 200 au and I  B  = 120° initially. The two planets have masses m 1 = 10M ⊕ and m 2 = 10M Jup and periods P 1 = 1 yr and P 2 = 3.7 yr, respectively, with initially circular and coplanar orbits. The binary migrates outward at a timescale of 40 Myr, increasing ﹩| \dot{{\rm{\Omega }}}| /{n}_{B}﹩. The system is captured into a first-order ivection resonance at ∼10 Myr. Once captured, the resonant angle librates around π, and the mutual inclination keeps increasing; meanwhile, the eccentricities of both planets remain small. The orange dashed curve in the top panel shows an analytic prediction of mutual inclination evolution based on the Hamiltonian in Equation (10). Both the location of the resonance and the inclination evolution after resonance capture agree well with the numerical result up to I ∼ 30°.
Paper: Exciting Mutual Inclination in Planetary Systems with a Distant Stellar Companion: The Case of Kepler-108
Authors: Wenrui Xu, Daniel Fabrycky
Figure caption: Estimates of the critical migration timescale T crit and the ratio between T prec and P  B , evaluated for first-order ivection resonance (top-left panel; e  B  = 0), second-order ivection resonance (top-right panel; e  B  = 0), and eccentric ivection resonance (bottom-left panel; e  B  = 0.95). The gray dashed lines mark P  B /P prec = 1 and 2.
Paper: Exciting Mutual Inclination in Planetary Systems with a Distant Stellar Companion: The Case of Kepler-108
Authors: Wenrui Xu, Daniel Fabrycky
Figure caption: A simulation that reproduces the orbital configuration of Kepler-108 from initially coplanar planets. The dashed lines in the top-left, middle-left, middle-right, and bottom-right panels show observed system parameters, with the 1σ observational uncertainty of eccentricity (middle left) and inclination (top left) marked by shades. The mutual inclination is excited due to capturing into an eccentric ivection resonance with an e  B  = 0.95, I  B  = 45°, and P  B  = 7000 yr binary. The system leaves the resonance (at t ∼ 4.5 Myr) probably due to encountering a 2:7 MMR. The initial eccentricities are due to a passage through 1:2 MMR at t < 0. The eccentricities are further excited when passing a 1:3 MMR at ≈1.8 Myr and after the ivection resonance is disrupted by the 2:7 MMR. The final eccentricities and mutual inclination are consistent with observation. See Section 4 for more discussion of this simulation.
Paper: Exciting Mutual Inclination in Planetary Systems with a Distant Stellar Companion: The Case of Kepler-108
Authors: Wenrui Xu, Daniel Fabrycky
Figure caption: Estimates for the nodal precession timescale P prec and binary period P  B  of systems with known external binary companion. Color marks whether the system hosts multiple observed planets, and marker shape corresponds to detection method. The gray dashed line marks P prec = P  B .
Paper: Exciting Mutual Inclination in Planetary Systems with a Distant Stellar Companion: The Case of Kepler-108
Authors: Wenrui Xu, Daniel Fabrycky
Figure caption: Disruption of ivection resonance due to crossing an eviction resonance, when extending the simulation shown in Figure 3. The top-right and bottom-right panels show the resonant angle of ivection resonance and eviction resonance, respectively. After encountering the eviction resonance, the mutual inclination ceases to increase.
Paper: Exciting Mutual Inclination in Planetary Systems with a Distant Stellar Companion: The Case of Kepler-108
Authors: Wenrui Xu, Daniel Fabrycky
Figure caption: The distribution of (estimated) P  B /P prec for systems with a single observed planet and with multiple observed planets. A gap appears for single-planet systems at 0–0.5 dex (see analysis of the statistical significance in Appendix C). If the gap is not a coincidence due to the small sample size, this will suggest that ivection/evection resonance may play an important role in the formation and evolution of exoplanetary systems with binary companions.
Paper: Exciting Mutual Inclination in Planetary Systems with a Distant Stellar Companion: The Case of Kepler-108
Authors: Wenrui Xu, Daniel Fabrycky
Figure caption: The distribution of (estimated) P  B /P prec for observed system (gray histogram), estimated distribution of P  B /P prec assuming there is no gap (blue line; obtained by smearing the observation, see the text for details), and p ≤ for each bin (orange dots; see definition of p ≤ in the text). Smaller p ≤ means more significant inconsistency with the gap-less distribution.
Paper: Exciting Mutual Inclination in Planetary Systems with a Distant Stellar Companion: The Case of Kepler-108
Authors: Wenrui Xu, Daniel Fabrycky
Figure caption: Contour of the Hamiltonians (Equations (10) and (17)) in (x,y) phase space (see definition in Equation (11)), at different η values. Top panel: Hamiltonian for first-order ivection resonance and eccentric ivection resonance given in Equation (10). A bifurcation occurs at η = 1.5. The Hamiltonian is similar to that of a first-order MMR. Bottom panel: Hamiltonian for second-order ivection resonance given in Equation (17). Two bifurcations occur at η = 0 and 1. The Hamiltonian is similar to that of a second-order MMR. Stable and unstable fixed points are marked by red dots and crosses, respectively. When the system is captured into resonance, it should librate around the leftmost fixed point for the Hamiltonian in the top panels, and the top or bottom fixed point (with equal probability) for the Hamiltonian in the bottom panels.
Paper: Exciting Mutual Inclination in Planetary Systems with a Distant Stellar Companion: The Case of Kepler-108
Authors: Wenrui Xu, Daniel Fabrycky
Figure caption: Disruption of ivection resonance due to crossing an MMR. The setup is similar to that of Figures 3 and 4, except that the binary orbit is fixed and the outer planet migrates inward. After encountering the 1:3 MMR, the eccentricities of both planets increase significantly, and the inner planet is eventually ejected at 9.3 Myr.
Paper: Exciting Mutual Inclination in Planetary Systems with a Distant Stellar Companion: The Case of Kepler-108
Authors: Wenrui Xu, Daniel Fabrycky
Figure caption: Probability of capture as a function of the initial inclination I (in units of I 0) and the parameter d η/d τ (which is proportional to the migration rate). Left panel: first-order ivection resonance and eccentric ivection resonance (given by the Hamiltonian in Equation (10)). Right panel: second-order ivection resonance (given by the Hamiltonian in Equation (17)). Contours of 10%, 30%, and 90% capture probability are plotted for reference.
Paper: The Transit Timing and Atmosphere of Hot Jupiter HAT-P-37b
Authors: Napaporn A-thano, Ing-Guey Jiang, Supachai Awiphan, Ronnakrit Rattanamala, Li-Hsin Su, Torik Hengpiya, Devesh P. Sariya, Li-Chin Yeh, A. A. Shlyapnikov, Mark A. Gorbachev, Alexey N. Rublevski, Vineet Kumar Mannaday, Parijat Thakur, D. K. Sahu, David Mkrtichian, Evgeny Griv
Figure caption: Upper-mass limit of the perturbing planet in the HAT-P-37 system. The upper-mass limit for TTV amplitudes of 50, 100, and 150 s are shown in blue dashed–dotted, green dashed, and red solid lines, respectively. The best ﹩{\rm{\Delta }}{\chi }_{\mathrm{red}}^{2}﹩ within a 0.05 period ratio bin is presented by the black dotted line. The contours represent the best ﹩{\rm{\Delta }}{\chi }_{\mathrm{red}}^{2}﹩ between the best TTV model and the best linear model. The unstable orbit region is shown by the black shaded region. The right vertical dashed line displays the orbital period of HAT-P-37b. The black vertical lines show 2:1, 3:2, 1:2, 1:3, and 1:4 orbital period resonance from left to right, respectively.
Paper: A Transiting, Temperate Mini-Neptune Orbiting the M Dwarf TOI-1759 Unveiled by TESS
Authors: Néstor Espinoza, Enric Pallé, Jonas Kemmer, Rafael Luque, José  A. Caballero, Carlos Cifuentes, Enrique Herrero, Víctor J. Sánchez Béjar, Stephan Stock, Karan Molaverdikhani, Giuseppe Morello, Diana Kossakowski, Martin Schlecker, Pedro J. Amado, Paz Bluhm, Miriam Cortés-Contreras, Thomas Henning, Laura Kreidberg, Martin Kürster, Marina Lafarga, Nicolas Lodieu, Juan Carlos Morales, Mahmoudreza Oshagh, Vera M. Passegger, Alexey Pavlov, Andreas Quirrenbach, Sabine Reffert, Ansgar Reiners, Ignasi Ribas, Eloy Rodríguez, Cristina Rodríguez López, Andreas Schweitzer, Trifon Trifonov, Priyanka Chaturvedi, Stefan Dreizler, Sandra V. Jeffers, Adrian Kaminski, María José López-González, Jorge Lillo-Box, David Montes, Grzegorz Nowak, Santos Pedraz, Siegfried Vanaverbeke, Maria R. Zapatero Osorio, Mathias Zechmeister, Karen A. Collins, Eric Girardin, Pere Guerra, Ramon Naves, Ian J. M. Crossfield, Elisabeth C. Matthews, Steve B. Howell, David R. Ciardi, Erica Gonzales, Rachel A. Matson, Charles A. Beichman, Joshua E. Schlieder, Thomas Barclay, Michael Vezie, Jesus Noel Villaseñor, Tansu Daylan, Ismael Mireies, Diana Dragomir, Joseph D. Twicken, Jon Jenkins, Joshua N. Winn, David Latham, George Ricker, Sara Seager
Figure caption: TESS target pixel files (TPFs) for TOI-1759 from the different sectors from which data were gathered with the mission (Sector 16, left; 17, center; 24, right). TOI-1759 is marked with a white cross on top of a red point and is numbered 1. Smaller numbered red points are the closest stars to the target (drawn from Gaia) with Gaia magnitude differences with the target of ∣ΔG∣ < 6 mag. Contamination is not a problem for TOI-1759, as most nearby targets are very faint. The plot is made using tpfplotter (Aller et al. 2020).
Paper: The Transit Timing and Atmosphere of Hot Jupiter HAT-P-37b
Authors: Napaporn A-thano, Ing-Guey Jiang, Supachai Awiphan, Ronnakrit Rattanamala, Li-Hsin Su, Torik Hengpiya, Devesh P. Sariya, Li-Chin Yeh, A. A. Shlyapnikov, Mark A. Gorbachev, Alexey N. Rublevski, Vineet Kumar Mannaday, Parijat Thakur, D. K. Sahu, David Mkrtichian, Evgeny Griv
Figure caption: The best-fit transmission spectrum of HAT-P-37b with synthetic models generated from PLATON retrieval (top) and the bandpass filters: B, V, R, r, and i band (from left to right; bottom).
Paper: The Transit Timing and Atmosphere of Hot Jupiter HAT-P-37b
Authors: Napaporn A-thano, Ing-Guey Jiang, Supachai Awiphan, Ronnakrit Rattanamala, Li-Hsin Su, Torik Hengpiya, Devesh P. Sariya, Li-Chin Yeh, A. A. Shlyapnikov, Mark A. Gorbachev, Alexey N. Rublevski, Vineet Kumar Mannaday, Parijat Thakur, D. K. Sahu, David Mkrtichian, Evgeny Griv
Figure caption: Posterior probability distributions from PLATON retrieval for HAT-P-37b of wavelength range 390–779 nm (including B filter).
Paper: The Transit Timing and Atmosphere of Hot Jupiter HAT-P-37b
Authors: Napaporn A-thano, Ing-Guey Jiang, Supachai Awiphan, Ronnakrit Rattanamala, Li-Hsin Su, Torik Hengpiya, Devesh P. Sariya, Li-Chin Yeh, A. A. Shlyapnikov, Mark A. Gorbachev, Alexey N. Rublevski, Vineet Kumar Mannaday, Parijat Thakur, D. K. Sahu, David Mkrtichian, Evgeny Griv
Figure caption: Posterior probability distributions from PLATON retrieval for HAT-P-37b of wavelength range 501–779 nm (without B filter).
Paper: The Transit Timing and Atmosphere of Hot Jupiter HAT-P-37b
Authors: Napaporn A-thano, Ing-Guey Jiang, Supachai Awiphan, Ronnakrit Rattanamala, Li-Hsin Su, Torik Hengpiya, Devesh P. Sariya, Li-Chin Yeh, A. A. Shlyapnikov, Mark A. Gorbachev, Alexey N. Rublevski, Vineet Kumar Mannaday, Parijat Thakur, D. K. Sahu, David Mkrtichian, Evgeny Griv
Figure caption: Posterior probability distribution of the constant-period model MCMC fitting parameters.
Paper: The Transit Timing and Atmosphere of Hot Jupiter HAT-P-37b
Authors: Napaporn A-thano, Ing-Guey Jiang, Supachai Awiphan, Ronnakrit Rattanamala, Li-Hsin Su, Torik Hengpiya, Devesh P. Sariya, Li-Chin Yeh, A. A. Shlyapnikov, Mark A. Gorbachev, Alexey N. Rublevski, Vineet Kumar Mannaday, Parijat Thakur, D. K. Sahu, David Mkrtichian, Evgeny Griv
Figure caption: Posterior probability distribution of the apsidal precession model MCMC fitting parameters.
Paper: The Transit Timing and Atmosphere of Hot Jupiter HAT-P-37b
Authors: Napaporn A-thano, Ing-Guey Jiang, Supachai Awiphan, Ronnakrit Rattanamala, Li-Hsin Su, Torik Hengpiya, Devesh P. Sariya, Li-Chin Yeh, A. A. Shlyapnikov, Mark A. Gorbachev, Alexey N. Rublevski, Vineet Kumar Mannaday, Parijat Thakur, D. K. Sahu, David Mkrtichian, Evgeny Griv
Figure caption: Posterior probability distribution of the orbital decay model MCMC fitting parameters.
Paper: A Transiting, Temperate Mini-Neptune Orbiting the M Dwarf TOI-1759 Unveiled by TESS
Authors: Néstor Espinoza, Enric Pallé, Jonas Kemmer, Rafael Luque, José  A. Caballero, Carlos Cifuentes, Enrique Herrero, Víctor J. Sánchez Béjar, Stephan Stock, Karan Molaverdikhani, Giuseppe Morello, Diana Kossakowski, Martin Schlecker, Pedro J. Amado, Paz Bluhm, Miriam Cortés-Contreras, Thomas Henning, Laura Kreidberg, Martin Kürster, Marina Lafarga, Nicolas Lodieu, Juan Carlos Morales, Mahmoudreza Oshagh, Vera M. Passegger, Alexey Pavlov, Andreas Quirrenbach, Sabine Reffert, Ansgar Reiners, Ignasi Ribas, Eloy Rodríguez, Cristina Rodríguez López, Andreas Schweitzer, Trifon Trifonov, Priyanka Chaturvedi, Stefan Dreizler, Sandra V. Jeffers, Adrian Kaminski, María José López-González, Jorge Lillo-Box, David Montes, Grzegorz Nowak, Santos Pedraz, Siegfried Vanaverbeke, Maria R. Zapatero Osorio, Mathias Zechmeister, Karen A. Collins, Eric Girardin, Pere Guerra, Ramon Naves, Ian J. M. Crossfield, Elisabeth C. Matthews, Steve B. Howell, David R. Ciardi, Erica Gonzales, Rachel A. Matson, Charles A. Beichman, Joshua E. Schlieder, Thomas Barclay, Michael Vezie, Jesus Noel Villaseñor, Tansu Daylan, Ismael Mireies, Diana Dragomir, Joseph D. Twicken, Jon Jenkins, Joshua N. Winn, David Latham, George Ricker, Sara Seager
Figure caption: Properties of TOI-1759 b as compared to previously small, known exoplanets with a measured mass and radius. (a) Mass−radius diagram of all known small (R  p  < 4 R ⊕) exoplanets with T eq < 1000 K (gray) and TOI-1759 b (blue). The mass–radius models are from Zeng et al. (2016) and show 100% Fe (gray), an Earth-like composition (32.5% Fe, 67.5% MgSiO3 by mass; brown), a 50% Earth-like and 50% water-by-mass composition (blue), and Earth-like composition models with 2% and 5% H2 on top of it (green). Water-rich models with 2% and 5% H2 on top (i.e., Neptune-like compositions) are not shown, but would be indistinguishable from the green models in this panel given the size of the error bars. (b) Equilibrium temperature (assuming zero albedo) vs. radius diagram for the same cuts made for panel (a), showing the location of TESS planets (white markers), non-TESS planets (white transparent markers), planets that have previously been characterized via transmission spectroscopy with WFC3 on the Hubble Space Telescope (HST; red markers) and TOI-1759 b (blue). The size of the markers represents the value of the transmission spectroscopy metric (TSM; Kempton et al. 2018); the gray band shows the proposed region of hazy exoplanets by Yu et al. (2021; see text for discussion).
Paper: A Transiting, Temperate Mini-Neptune Orbiting the M Dwarf TOI-1759 Unveiled by TESS
Authors: Néstor Espinoza, Enric Pallé, Jonas Kemmer, Rafael Luque, José  A. Caballero, Carlos Cifuentes, Enrique Herrero, Víctor J. Sánchez Béjar, Stephan Stock, Karan Molaverdikhani, Giuseppe Morello, Diana Kossakowski, Martin Schlecker, Pedro J. Amado, Paz Bluhm, Miriam Cortés-Contreras, Thomas Henning, Laura Kreidberg, Martin Kürster, Marina Lafarga, Nicolas Lodieu, Juan Carlos Morales, Mahmoudreza Oshagh, Vera M. Passegger, Alexey Pavlov, Andreas Quirrenbach, Sabine Reffert, Ansgar Reiners, Ignasi Ribas, Eloy Rodríguez, Cristina Rodríguez López, Andreas Schweitzer, Trifon Trifonov, Priyanka Chaturvedi, Stefan Dreizler, Sandra V. Jeffers, Adrian Kaminski, María José López-González, Jorge Lillo-Box, David Montes, Grzegorz Nowak, Santos Pedraz, Siegfried Vanaverbeke, Maria R. Zapatero Osorio, Mathias Zechmeister, Karen A. Collins, Eric Girardin, Pere Guerra, Ramon Naves, Ian J. M. Crossfield, Elisabeth C. Matthews, Steve B. Howell, David R. Ciardi, Erica Gonzales, Rachel A. Matson, Charles A. Beichman, Joshua E. Schlieder, Thomas Barclay, Michael Vezie, Jesus Noel Villaseñor, Tansu Daylan, Ismael Mireies, Diana Dragomir, Joseph D. Twicken, Jon Jenkins, Joshua N. Winn, David Latham, George Ricker, Sara Seager
Figure caption: CARMENES radial-velocity follow-up of TOI-1759. (a) Our CARMENES radial-velocity campaign (white points with black error bars; first point corresponding to 2,459,054.56851) had a total duration of about 6 months, over which we were able to detect both a radial-velocity variation at 18.85 days, along with a long-term signal here modeled as a GP. The blue line with transparent bands around it indicate our full (GP + planetary) median signal, along with its 68%, 95%, and 99% credibility intervals, respectively. (b) Phase-folded radial-velocity curve at the period of the transiting exoplanet TOI-1759 b (P = 18.85 days; gray points, binned data points covering about 2 days plotted as white points with black error bars). The semiamplitude we obtain for this signal is 3.64 ± 0.50 m s−1.
Paper: A Transiting, Temperate Mini-Neptune Orbiting the M Dwarf TOI-1759 Unveiled by TESS
Authors: Néstor Espinoza, Enric Pallé, Jonas Kemmer, Rafael Luque, José  A. Caballero, Carlos Cifuentes, Enrique Herrero, Víctor J. Sánchez Béjar, Stephan Stock, Karan Molaverdikhani, Giuseppe Morello, Diana Kossakowski, Martin Schlecker, Pedro J. Amado, Paz Bluhm, Miriam Cortés-Contreras, Thomas Henning, Laura Kreidberg, Martin Kürster, Marina Lafarga, Nicolas Lodieu, Juan Carlos Morales, Mahmoudreza Oshagh, Vera M. Passegger, Alexey Pavlov, Andreas Quirrenbach, Sabine Reffert, Ansgar Reiners, Ignasi Ribas, Eloy Rodríguez, Cristina Rodríguez López, Andreas Schweitzer, Trifon Trifonov, Priyanka Chaturvedi, Stefan Dreizler, Sandra V. Jeffers, Adrian Kaminski, María José López-González, Jorge Lillo-Box, David Montes, Grzegorz Nowak, Santos Pedraz, Siegfried Vanaverbeke, Maria R. Zapatero Osorio, Mathias Zechmeister, Karen A. Collins, Eric Girardin, Pere Guerra, Ramon Naves, Ian J. M. Crossfield, Elisabeth C. Matthews, Steve B. Howell, David R. Ciardi, Erica Gonzales, Rachel A. Matson, Charles A. Beichman, Joshua E. Schlieder, Thomas Barclay, Michael Vezie, Jesus Noel Villaseñor, Tansu Daylan, Ismael Mireies, Diana Dragomir, Joseph D. Twicken, Jon Jenkins, Joshua N. Winn, David Latham, George Ricker, Sara Seager
Figure caption: Generalized Lomb−Scargle (GLS) periodograms of the CARMENES radial-velocity data after subtracting different models. The power at each frequency corresponds to the one defined in Zechmeister & Kürster (2009; ZK in the labels above). The period of the transiting planet, P = 18.85 days, is marked by the red solid line and the stellar rotation period, P ≈ 80 days, and its first harmonic are shown with the blue solid and dashed lines, respectively. Further, the additional present long-term periodicity with P ≈ 270 days is marked by the yellow solid line. The horizontal dashed gray lines show the analytical false-alarm probabilities (FAP) of 10%, 1%, and 0.1%. The top panel corresponds to the mean-subtracted CARMENES radial-velocity data set.