adsabs/AstroCLIMB huggingface dataset:
Paper: The DESI Survey Validation: Results from Visual Inspection of the Quasar Survey Spectra
Authors: David M. Alexander, Tamara M. Davis, E. Chaussidon, V. A. Fawcett, Alma X. Gonzalez-Morales, Ting-Wen Lan, Christophe Yèche, S. Ahlen, J. N. Aguilar, E. Armengaud, S. Bailey, D. Brooks, Z. Cai, R. Canning, A. Carr, S. Chabanier, Marie-Claude Cousinou, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, A. C. Edge, S. Eftekharzadeh, K. Fanning, James Farr, A. Font-Ribera, J. Garcia-Bellido, Lehman Garrison, E. Gaztañaga, Satya Gontcho A Gontcho, C. Gordon, Stefany Guadalupe Medellin Gonzalez, J. Guy, Hiram K. Herrera-Alcantar, L. Jiang, S. Juneau, N. G. Karaçaylı, R. Kehoe, T. Kisner, A. Kovács, M. Landriau, Michael E. Levi, C. Magneville, P. Martini, Aaron M. Meisner, M. Mezcua, R. Miquel, P. Montero Camacho, J. Moustakas, Andrea Muñoz-Gutiérrez, Adam D. Myers, S. Nadathur, L. Napolitano, J. D. Nie, N. Palanque-Delabrouille, Z. Pan, W. J. Percival, I. Pérez-Ràfols, C. Poppett, F. Prada, César Ramírez-Pérez, C. Ravoux, D. J. Rosario, M. Schubnell, Gregory Tarlé, M. Walther, B. Weiner, S. Youles, Zhimin Zhou, H. Zou, Siwei Zou
Figure caption: Median composites of high-quality Redrock-identified QSOs (blue) and visually confirmed galaxies (green) from the deep-field VI of the QSO survey. These composite spectra are normalized over rest-frame 5100–5200 Å for visualization purposes. The inset plot is focused around 2600–3000 Å and 3600–4000 Å to highlight the lack of AGN features (left) and the prominent stellar absorption features (right) in comparison to the QSO composite. The vertical lines indicate several key emission (dashed line) and absorption (dotted line) features.
Paper: An Orbit-flip Mechanism by Eccentric Lidov–Kozai Effect with Stellar Oblateness
Authors: Yue Wang, 悦 王, Tao Fu, 韬 伏
Figure caption: Minimum flipping inclination due to the ELK effect. Each curve marks the minimum i 0 that induces flips for the given value of ε Oct and different values of κ Ob. Below each curve none of the orbits flip, and above it some orbits do. These curves are obtained by numerically integrating Equations (9) and (10) initialized with e 0 = 0.01, ω 0 = 0, and Ω0 = π, scanning through the values of i 0 from 0 to π/2 to determine the minimum i 0 that allows flips. We did not scan the initial Ω0, because according to the phase space structure at e 0 ∼ 0, the lower limit of flipping i 0 is determined at Ω0 = π. At this initial e 0, orbit flips occur in the region dominated by the ELK effect. These curves are symmetric about i 0 = 90°, and only the parts below 90° are depicted.
Paper: An Orbit-flip Mechanism by Eccentric Lidov–Kozai Effect with Stellar Oblateness
Authors: Yue Wang, 悦 王, Tao Fu, 韬 伏
Figure caption: Minimum flipping inclination due to the ELK–J 2 effect. These curves are drawn following a similar approach as in Figure 11, but setting initial e 0 = 0.82 and Ω0 = 0 (ω 0 = 0). This picture captures orbit flips mostly due to the ELK–J 2 effect, as indicated by Figure 10. However, note that the curves in this figure do not represent the minimum flipping i 0 for all initial Ω0, because at low values of κ Ob flips due to the ELK effect with libration islands centered at Ω0 = π generally determine a lower minimum flipping i 0. However, at high values of κ Ob, when the ELK effect has been almost entirely suppressed, the initial Ω0 = 0 gives the exact minimum values.
Paper: An Orbit-flip Mechanism by Eccentric Lidov–Kozai Effect with Stellar Oblateness
Authors: Yue Wang, 悦 王, Tao Fu, 韬 伏
Figure caption: Numerical results: orbit-flipping regions in the ﹩\left({e}_{0},{i}_{0}\right)﹩ space for systems with κ Ob = 0, 10−4, 10−3, and 0.03, respectively. The initial conditions are indicated in these plots. The total integration time is 500t LK for each trajectory.
Paper: An Orbit-flip Mechanism by Eccentric Lidov–Kozai Effect with Stellar Oblateness
Authors: Yue Wang, 悦 王, Tao Fu, 韬 伏
Figure caption: Poincaré surfaces of section at different levels of energy constant presented in the ﹩\left({\rm{\Omega }},\cos i\right)﹩ plane for a system specified by κ Ob = 0.1, ε Oct = 0.03. Only the trajectories associated with orbit flips are recorded. The sections in the upper and lower panels are defined by ﹩\omega =0,\dot{\omega }\gt 0﹩ and ﹩\omega =0,\dot{\omega }\lt 0﹩, respectively. In each panel, the green dots characterize the boundaries of the libration islands that allow orbit flips, and ﹩{\rm{\Delta }}\cos i﹩ represents the size of the islands.
Paper: An Orbit-flip Mechanism by Eccentric Lidov–Kozai Effect with Stellar Oblateness
Authors: Yue Wang, 悦 王, Tao Fu, 韬 伏
Figure caption: Analytical results: orbit-flipping boundaries in the entire (e 0, i 0) space for a system with κ Ob = 0.1, κ Oct = 0.03 obtained by exploiting the Poincaré surfaces of section. The dominant two regions are designated as I and II, respectively. (Note: although the Poincaré surface of section is based on numerical integrations of the secular equations, we would like to refer to the results acquired in this manner as “analytical” to distinguish them from the numerical exploration in the whole phase space.)
Paper: An Orbit-flip Mechanism by Eccentric Lidov–Kozai Effect with Stellar Oblateness
Authors: Yue Wang, 悦 王, Tao Fu, 韬 伏
Figure caption: Geometry of the angular momentum vectors of the inner system. The total angular momentum  L  in is conserved when the outer perturber is ignored. θ 0 and θ 1 are the angles of  L  0 and  L  1 with respect to  L  in.
Paper: An Orbit-flip Mechanism by Eccentric Lidov–Kozai Effect with Stellar Oblateness
Authors: Yue Wang, 悦 王, Tao Fu, 韬 伏
Figure caption: Numerical results: flipping orbits in the entire ﹩\left({e}_{0},{i}_{0}\right)﹩ space obtained by numerical integrations of Equations (A5)–(A10). The initial ω is ω 0 = 0, and Ω0 is set for several cases as indicated in the figure. The total integration time is 500t Lk for each trajectory.
Paper: An Orbit-flip Mechanism by Eccentric Lidov–Kozai Effect with Stellar Oblateness
Authors: Yue Wang, 悦 王, Tao Fu, 韬 伏
Figure caption: Reproduction of the last panel of Figure 10 for misaligned configurations. The stellar obliquity is ϑ = 10° (upper) and ϑ = 40° (lower), respectively.
Paper: An Orbit-flip Mechanism by Eccentric Lidov–Kozai Effect with Stellar Oblateness
Authors: Yue Wang, 悦 王, Tao Fu, 韬 伏
Figure caption: Variations of θ 0 and θ 1 with the mass of the inner planet.
Paper: The DESI Survey Validation: Results from Visual Inspection of the Quasar Survey Spectra
Authors: David M. Alexander, Tamara M. Davis, E. Chaussidon, V. A. Fawcett, Alma X. Gonzalez-Morales, Ting-Wen Lan, Christophe Yèche, S. Ahlen, J. N. Aguilar, E. Armengaud, S. Bailey, D. Brooks, Z. Cai, R. Canning, A. Carr, S. Chabanier, Marie-Claude Cousinou, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, A. C. Edge, S. Eftekharzadeh, K. Fanning, James Farr, A. Font-Ribera, J. Garcia-Bellido, Lehman Garrison, E. Gaztañaga, Satya Gontcho A Gontcho, C. Gordon, Stefany Guadalupe Medellin Gonzalez, J. Guy, Hiram K. Herrera-Alcantar, L. Jiang, S. Juneau, N. G. Karaçaylı, R. Kehoe, T. Kisner, A. Kovács, M. Landriau, Michael E. Levi, C. Magneville, P. Martini, Aaron M. Meisner, M. Mezcua, R. Miquel, P. Montero Camacho, J. Moustakas, Andrea Muñoz-Gutiérrez, Adam D. Myers, S. Nadathur, L. Napolitano, J. D. Nie, N. Palanque-Delabrouille, Z. Pan, W. J. Percival, I. Pérez-Ràfols, C. Poppett, F. Prada, César Ramírez-Pérez, C. Ravoux, D. J. Rosario, M. Schubnell, Gregory Tarlé, M. Walther, B. Weiner, S. Youles, Zhimin Zhou, H. Zou, Siwei Zou
Figure caption: Example DESI spectra illustrating the different VI quality classes (left) and thumbnail images (18″ × 18″) centered on each target (right). Salient information for each target is plotted at the top of each spectrum including the VI quality flag. For each target both an unsmoothed (gray) and smoothed (black) spectrum are plotted along with the associated error spectrum (orange) and the overlapping wavelength ranges for the three different spectral arms (pale pink shaded regions). The most prominent emission lines identified in the two high-quality spectra (with VI quality flags of 3 and 4) are highlighted using blue vertical dashed lines as well as the potential identification of a single emission line ([O II] at z = 1.261) for the VI quality flag 2 target. We note that these visually inspected spectra were obtained with 10x longer exposures than those used in the main DESI survey.
Paper: The DESI Survey Validation: Results from Visual Inspection of the Quasar Survey Spectra
Authors: David M. Alexander, Tamara M. Davis, E. Chaussidon, V. A. Fawcett, Alma X. Gonzalez-Morales, Ting-Wen Lan, Christophe Yèche, S. Ahlen, J. N. Aguilar, E. Armengaud, S. Bailey, D. Brooks, Z. Cai, R. Canning, A. Carr, S. Chabanier, Marie-Claude Cousinou, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, A. C. Edge, S. Eftekharzadeh, K. Fanning, James Farr, A. Font-Ribera, J. Garcia-Bellido, Lehman Garrison, E. Gaztañaga, Satya Gontcho A Gontcho, C. Gordon, Stefany Guadalupe Medellin Gonzalez, J. Guy, Hiram K. Herrera-Alcantar, L. Jiang, S. Juneau, N. G. Karaçaylı, R. Kehoe, T. Kisner, A. Kovács, M. Landriau, Michael E. Levi, C. Magneville, P. Martini, Aaron M. Meisner, M. Mezcua, R. Miquel, P. Montero Camacho, J. Moustakas, Andrea Muñoz-Gutiérrez, Adam D. Myers, S. Nadathur, L. Napolitano, J. D. Nie, N. Palanque-Delabrouille, Z. Pan, W. J. Percival, I. Pérez-Ràfols, C. Poppett, F. Prada, César Ramírez-Pérez, C. Ravoux, D. J. Rosario, M. Schubnell, Gregory Tarlé, M. Walther, B. Weiner, S. Youles, Zhimin Zhou, H. Zou, Siwei Zou
Figure caption: Distribution of (left) VI quality flags and (right) high-quality VI redshifts for the deep-field VI (top) and missed QSOs in the sparse VI (bottom). Targets meeting the SV1 and main selection are indicated in pale and dark gray, respectively. The dashed line indicates the threshold required for a high-quality redshift (VI ≥2.5).
Paper: The DESI Survey Validation: Results from Visual Inspection of the Quasar Survey Spectra
Authors: David M. Alexander, Tamara M. Davis, E. Chaussidon, V. A. Fawcett, Alma X. Gonzalez-Morales, Ting-Wen Lan, Christophe Yèche, S. Ahlen, J. N. Aguilar, E. Armengaud, S. Bailey, D. Brooks, Z. Cai, R. Canning, A. Carr, S. Chabanier, Marie-Claude Cousinou, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, A. C. Edge, S. Eftekharzadeh, K. Fanning, James Farr, A. Font-Ribera, J. Garcia-Bellido, Lehman Garrison, E. Gaztañaga, Satya Gontcho A Gontcho, C. Gordon, Stefany Guadalupe Medellin Gonzalez, J. Guy, Hiram K. Herrera-Alcantar, L. Jiang, S. Juneau, N. G. Karaçaylı, R. Kehoe, T. Kisner, A. Kovács, M. Landriau, Michael E. Levi, C. Magneville, P. Martini, Aaron M. Meisner, M. Mezcua, R. Miquel, P. Montero Camacho, J. Moustakas, Andrea Muñoz-Gutiérrez, Adam D. Myers, S. Nadathur, L. Napolitano, J. D. Nie, N. Palanque-Delabrouille, Z. Pan, W. J. Percival, I. Pérez-Ràfols, C. Poppett, F. Prada, César Ramírez-Pérez, C. Ravoux, D. J. Rosario, M. Schubnell, Gregory Tarlé, M. Walther, B. Weiner, S. Youles, Zhimin Zhou, H. Zou, Siwei Zou
Figure caption: Venn diagrams showing (top) the overlap between the missed QSO sample, the Mg II absorption systems, and the targets with nonrepeatable redshifts and (bottom) the overlap in the selection of missed QSOs between the three afterburner selections across the sparse VI fields.
Paper: The DESI Survey Validation: Results from Visual Inspection of the Quasar Survey Spectra
Authors: David M. Alexander, Tamara M. Davis, E. Chaussidon, V. A. Fawcett, Alma X. Gonzalez-Morales, Ting-Wen Lan, Christophe Yèche, S. Ahlen, J. N. Aguilar, E. Armengaud, S. Bailey, D. Brooks, Z. Cai, R. Canning, A. Carr, S. Chabanier, Marie-Claude Cousinou, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, A. C. Edge, S. Eftekharzadeh, K. Fanning, James Farr, A. Font-Ribera, J. Garcia-Bellido, Lehman Garrison, E. Gaztañaga, Satya Gontcho A Gontcho, C. Gordon, Stefany Guadalupe Medellin Gonzalez, J. Guy, Hiram K. Herrera-Alcantar, L. Jiang, S. Juneau, N. G. Karaçaylı, R. Kehoe, T. Kisner, A. Kovács, M. Landriau, Michael E. Levi, C. Magneville, P. Martini, Aaron M. Meisner, M. Mezcua, R. Miquel, P. Montero Camacho, J. Moustakas, Andrea Muñoz-Gutiérrez, Adam D. Myers, S. Nadathur, L. Napolitano, J. D. Nie, N. Palanque-Delabrouille, Z. Pan, W. J. Percival, I. Pérez-Ràfols, C. Poppett, F. Prada, César Ramírez-Pérez, C. Ravoux, D. J. Rosario, M. Schubnell, Gregory Tarlé, M. Walther, B. Weiner, S. Youles, Zhimin Zhou, H. Zou, Siwei Zou
Figure caption: Pie chart showing the distribution of high-quality optical spectral classifications and low-quality spectra from the deep-field VI for targets meeting the SV1 (top) and main (bottom) target selections.
Paper: An Orbit-flip Mechanism by Eccentric Lidov–Kozai Effect with Stellar Oblateness
Authors: Yue Wang, 悦 王, Tao Fu, 韬 伏
Figure caption: An example of an orbit flip by the ELK–J 2 effect (left column, red) and comparison to an orbit flip by the ELK effect (right column, green). The blue trajectory in the left column is the numerical integration of the full equations of motion, Equation (A1). In this paper, a fourth- and fifth-order Runge–Kutta method with adaptive step size is used to numerically solve the equations. The two cases of the left and right columns have similar system parameters except the stellar oblateness J 2, and similar initial conditions except Ω0. The system parameters are m 0 = 2 M ⊙, R 0 = 3 R ⊙, J 2 = 10−3 (J 2 = 0 for the right column), m Per = 50 M J, the particle’s mass m ≪ m Per, a = 0.61 au, a Per = 20 au, and e Per = 0.79. With these parameters, the characteristic parameters of the system are κ Ob ≃ 0.1775 (κ Ob = 0 for the right column) and ε Oct ≃ 0.0393. The initial conditions of the particle are set as i = 74°, e = 0.87, ω = 0°, and Ω = 0° (180°) for the left (right) column. The total integration time is 1.96  Myr (∼100t LK). It shows a good agreement between the full equations of motion and the secular model of the octupole-level approximation.
Paper: An Orbit-flip Mechanism by Eccentric Lidov–Kozai Effect with Stellar Oblateness
Authors: Yue Wang, 悦 王, Tao Fu, 韬 伏
Figure caption: Phase portraits of a system with κ Ob = 0.1775 at the quadrupole-level dynamics. From the upper panel, (A) j z = 0.259, (B) j z = 0.136, and (C) j z = 0.105, respectively. The green and red curves are separatrices of the librating (in black) and circulating cycles (in yellow). There are four types of quadrupole-level cycle: librating and circulating LK cycles, and librating and circulating LK–J 2 cycles.
Paper: An Orbit-flip Mechanism by Eccentric Lidov–Kozai Effect with Stellar Oblateness
Authors: Yue Wang, 悦 王, Tao Fu, 韬 伏
Figure caption: Evolution of j z and trajectories in the ﹩\left(e,\,i\right)﹩ space for the triple systems presented in Figure 2. The left column represents the ELK–J 2 effect and the right column represents the ELK case, corresponding to the left and right columns of Figure 2, respectively. The black curves in the lower two planes are contour lines of ﹩{j}_{{\rm{z}}}=\sqrt{1-{e}^{2}}\cos i﹩.
Paper: An Orbit-flip Mechanism by Eccentric Lidov–Kozai Effect with Stellar Oblateness
Authors: Yue Wang, 悦 王, Tao Fu, 韬 伏
Figure caption: Orbit flips in the ﹩\left({\omega }_{0},\,{e}_{0}\right)﹩ space for the system presented in Figure 2 (κ Ob ≈ 0.1775, ε Oct ≈ 0.0393) by numerical simulations. For each grid, the initial Ω is Ω0 = 0 and the initial i is given by j z,0 = 0.105 and 0.05 for the left and right panels, respectively. The initial conditions that lead to orbit flips are marked by red.
Paper: An Orbit-flip Mechanism by Eccentric Lidov–Kozai Effect with Stellar Oblateness
Authors: Yue Wang, 悦 王, Tao Fu, 韬 伏
Figure caption: Contours of the energy constant, ﹩{\psi }^{\ast }\approx 16\psi /(15{\psi }_{0})﹩, in the ﹩\left(e,\cos i\right)﹩ plane with ω = 0 for a system with κ Ob = 0.1. For clarity, we adopt a different abscissa scale for the e > 0.9 areas.
Paper: An Orbit-flip Mechanism by Eccentric Lidov–Kozai Effect with Stellar Oblateness
Authors: Yue Wang, 悦 王, Tao Fu, 韬 伏
Figure caption: Geometry of the hierarchical three-body system. An oblate center star is orbited by a massless inner planet and a massive exterior perturber. The perturber’s orbit pole and the stellar spin are assumed to be aligned.
Paper: A Census of the TW Hya Association with Gaia 
Authors: K. L. Luhman
Figure caption:                       ﹩{M}_{{G}_{\mathrm{RP}}}﹩ vs. G BP − G RP and G − G RP for the bona fide members of TWA compiled by Gagné et al. (2017; top) and the adopted members from this work (bottom). Three stars that appear below the sequence in G BP − G RP are labeled with their TWA numbers. Each CMD includes a fit to the single-star sequence of the Pleiades (red line; Luhman 2023). The spectral types that correspond to the colors of young stars are indicated in the top CMDs (Luhman 2022a).
Paper: A Census of the TW Hya Association with Gaia 
Authors: K. L. Luhman
Figure caption: Galactic Cartesian coordinates and UVW velocities for adopted members of TWA from this work. The most discrepant measurements of UVW are labeled with the TWA numbers. The V and W velocities of Gaia DR3 3567379121431731328 are also marked. Its membership is discussed in Section 2.3.
Paper: A Census of the TW Hya Association with Gaia 
Authors: K. L. Luhman
Figure caption: Proper motion offsets vs. equatorial coordinates for the bona fide members of TWA compiled by Gagné et al. (2017; top) and the adopted members from this work (bottom). Outliers are labeled with their TWA numbers. TWA 4A is beyond the boundaries of the diagrams on the right.
Paper: A Census of the TW Hya Association with Gaia 
Authors: K. L. Luhman
Figure caption: Example of a GMOS spectrum of a candidate member of TWA (Gaia DR3 5401389770971149568), which is displayed at a resolution of 13 Å.(The data used to create this figure are available.)
Paper: A Census of the TW Hya Association with Gaia 
Authors: K. L. Luhman
Figure caption: Galactic Cartesian coordinates and UVW velocities for the bona fide members of TWA compiled by Gagné et al. (2017). The most discrepant measurements of UVW are labeled with the TWA numbers.
Paper: A Census of the TW Hya Association with Gaia 
Authors: K. L. Luhman
Figure caption: Histogram of offsets in ﹩{M}_{{G}_{\mathrm{RP}}}﹩ from the median CMD sequence for UCL/LCC for low-mass stars in TWA (Figure 2). Negative values correspond to brighter magnitudes and younger ages.
Paper: A Census of the TW Hya Association with Gaia 
Authors: K. L. Luhman
Figure caption: IR color excesses for adopted members of TWA. The boundaries used for assigning disk classes are shown in the bottom diagram (red solid lines).
Paper: A Census of the TW Hya Association with Gaia 
Authors: K. L. Luhman
Figure caption: IR colors vs. spectral type for adopted members of TWA. In each diagram, the tight sequence of blue colors corresponds to stellar photospheres. The thresholds used for identifying color excesses from disks are indicated (red solid lines; Luhman 2022b).
Paper: A Census of the TW Hya Association with Gaia 
Authors: K. L. Luhman
Figure caption: Histogram of spectral types for adopted members of TWA.
Paper: TOI 560: Two Transiting Planets Orbiting a K Dwarf Validated with iSHELL, PFS, and HIRES RVs
Authors: Mohammed El Mufti, Peter P. Plavchan, Howard Isaacson, Bryson L. Cale, Dax L. Feliz, Michael A. Reefe, Coel Hellier, Keivan Stassun, Jason Eastman, Alex Polanski, Ian J. M. Crossfield, Eric Gaidos, Veselin Kostov, Justin M. Wittrock, Joel Villaseñor, Joshua E. Schlieder, Luke G. Bouma, Kevin I. Collins, Farzaneh Zohrabi, Rena A. Lee, Ahmad Sohani, John Berberian, David Vermilion, Patrick Newman, Claire Geneser, Angelle Tanner, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Lea A. Hirsch, Rae Holcomb, Jack Lubin, Andrew Mayo, Teo Močnik, Joseph M. Akana Murphy, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Christopher Stockdale, Karen Collins, Ryan Cloutier, Howard Relles, Thiam-Guan Tan, Nicholas J Scott, Zach Hartman, Elisabeth Matthews, David R. Ciardi, Erica Gonzales, Rachel A. Matson, Charles Beichman, Allyson Bieryla, E. Furlan, Crystal L. Gnilka, Steve B. Howell, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Markus Rabus, Marshall C. Johnson, Jessie Christiansen, Laura Kreidberg, David Anthony Berardo, Drake Deming, Varoujan Gorjian, Farisa Y. Morales, Björn Benneke, Diana Dragomir, Robert A. Wittenmyer, Sarah Ballard, Brendan P. Bowler, Jonathan Horner, John Kielkopf, Huigen Liu, Avi Shporer, C. G. Tinney, Hui Zhang, Duncan J. Wright, Brett C. Addison, Matthew W. Mengel, Jack Okumura
Figure caption: A series of GLS periodograms examining the signals in our TOI 560 RV time-series as described in the text including iSHELL, HIRES, and PFS. The top panel is a periodogram of the RVs after subtracting a stellar activity model fit. The middle panel additionally subtracts a model fit for TOI 560 b and stellar activity to search for a second planet, and the bottom panel subtracts a model fit for both TOI 560 b and c and stellar activity to search for a third planet. The periods of b and c are marked with dashed black and orange vertical lines and also the rotation period, one-half of it, and one-third of it are marked with dashed red, blue, and green vertical lines, respectively, in each panel. The bootstrap FAPs of 1% and 10% were marked with cyan horizontal dashed lines. Note, it remains challenging to find nontransiting RV planets at orbital periods near the stellar-rotation period or one of its prominent integer fraction aliases (e.g., 1/2, 1/3), as the GP stellar activity model could potentially “absorb” such a Keplerian signature (Vanderburg et al. 2016; Kossakowski et al. 2022).