adsabs/AstroCLIMB huggingface dataset:
Paper: The Epoch of Giant Planet Migration Planet Search Program. II. A Young Hot Jupiter Candidate around the AB Dor Member HS Psc 
Authors: Quang H. Tran, Brendan P. Bowler, William D. Cochran, Samuel Halverson, Suvrath Mahadevan, Joe P. Ninan, Paul Robertson, Guđmundur Stefánsson, Ryan C. Terrien
Figure caption: GLS periodograms of the spectral time series. Beginning with the top panel, the periodograms are calculated for the HPF RVs, the dLW activity indicator, the CRX, the Ca II IRT indices for the Ca II 1, 2, and 3 IRT emission lines, the RV residuals after subtracting the best-fit planetary model, and the spectral WF. The planet orbital period (P  b  = 3.99 days) and the stellar rotation period (P rot = 1.086 days) are highlighted in the blue and red vertical shaded regions, respectively. FAPs of 1% and 0.01%, calculated using the bootstrap method, are shown as orange dotted and dashed lines, respectively. There are five peaks above the FAP = 0.01% threshold in the periodogram of the RVs; these represent the nightly sampling alias (seen at 1.0 day in the bottom panel with the WF periodogram), the stellar rotation period, the orbital period, and likely aliases of the stellar rotation and orbital periods.
Paper: The Epoch of Giant Planet Migration Planet Search Program. II. A Young Hot Jupiter Candidate around the AB Dor Member HS Psc 
Authors: Quang H. Tran, Brendan P. Bowler, William D. Cochran, Samuel Halverson, Suvrath Mahadevan, Joe P. Ninan, Paul Robertson, Guđmundur Stefánsson, Ryan C. Terrien
Figure caption: Cross-validation tests for Model 2 (top) and Model 3 (bottom). Left: the best-fit joint Keplerian and GP models are plotted as solid black lines. The training and test RV data sets are displayed as purple points and black stars, respectively. The residuals between the models and both data sets are displayed on the bottom. Right: the distributions of RV residuals for the training and test data sets are plotted in purple and black, respectively. The range and structure of the residuals are consistent between the training and test sets, supporting the predictive power of the best-fit models and providing evidence against overfitting.
Paper: The Epoch of Giant Planet Migration Planet Search Program. II. A Young Hot Jupiter Candidate around the AB Dor Member HS Psc 
Authors: Quang H. Tran, Brendan P. Bowler, William D. Cochran, Samuel Halverson, Suvrath Mahadevan, Joe P. Ninan, Paul Robertson, Guđmundur Stefánsson, Ryan C. Terrien
Figure caption: The same plots as Figure 3 for the Model 1 (Keplerian-only) fits.
Paper: The Epoch of Giant Planet Migration Planet Search Program. II. A Young Hot Jupiter Candidate around the AB Dor Member HS Psc 
Authors: Quang H. Tran, Brendan P. Bowler, William D. Cochran, Samuel Halverson, Suvrath Mahadevan, Joe P. Ninan, Paul Robertson, Guđmundur Stefánsson, Ryan C. Terrien
Figure caption: The same plots as Figure 3 for the Model 2 (Keplerian and QP GP) fits.
Paper: The Solar Neighborhood LI: A Variability Survey of Nearby M Dwarfs with Planets from Months to Decades with TESS and the CTIO/SMARTS 0.9 m Telescope
Authors: Aman Kar, Todd J. Henry, Andrew A. Couperus, Eliot Halley Vrijmoet, Wei-Chun Jao
Figure caption: Top: TESS light curves of LHS 145 (left) and WD 0310–688 (right), two white dwarfs showing no significant photometric variations in fluxes from all four data processing methods (blue, green, red, purple; as defined in Figure 4). The unpopular without-polynomial line (purple) is similar to the with-polynomial line (red) and therefore is not visible in the plot. No systematics have been introduced in our application of unpopular, with or without the polynomial for nonvariable stars. Middle: TESS light curves of a fast-rotating 8.4 day Kepler target (left) and a fast-rotating MEarth target (right) with a known rotation period of 6.4 days where the exclusion of the polynomial component (purple) preserves the high-frequency rotation signal. Bottom: TESS light curves of a slow-rotating 28.1 day Kepler target (left) and a slow-rotating MEarth target (right) with a known rotation period of 91.7 days where the inclusion of the polynomial component (red) preserves the low-frequency rotation signal.
Paper: The Solar Neighborhood LI: A Variability Survey of Nearby M Dwarfs with Planets from Months to Decades with TESS and the CTIO/SMARTS 0.9 m Telescope
Authors: Aman Kar, Todd J. Henry, Andrew A. Couperus, Eliot Halley Vrijmoet, Wei-Chun Jao
Figure caption: L 98–59 TESS light curve from Sector 12 over 27.4 days. The raw/SAP (blue) fluxes, processed/PDCSAP (green) fluxes, and the unpopular fluxes are overlaid with (red) and without (purple) the inclusion of the polynomial component, respectively. The zero y-axis is defined the same as Figure 3. Note that the rotational modulation of the star is evident in the raw data, eliminated in the PDCSAP reduction, effectively lost in the unpopular reduction without the polynomial, but clear in the unpopular reduction with the polynomial applied. For comparison, σ and IDR values for variability over the 27 days are given for each reduction in the lower left. “P” in the legend refers to polynomial.
Paper: The Solar Neighborhood LI: A Variability Survey of Nearby M Dwarfs with Planets from Months to Decades with TESS and the CTIO/SMARTS 0.9 m Telescope
Authors: Aman Kar, Todd J. Henry, Andrew A. Couperus, Eliot Halley Vrijmoet, Wei-Chun Jao
Figure caption: Panels illustrating three different types of blending in TESS, categorized as major (LHS 1748, top row), minor (Proxima Centauri, middle row), and no (GJ 1061, bottom row) blending. Left column: images from the CTIO/SMARTS 0.9 m telescope that are ∼3′ on each side (0.″401 pixel−1 plate scale) in which the ATLAS stars are circled in green. Middle column: TPFs of the ATLAS stars (indicated with a white “X” and labeled “1” in each panel) from TESS. We overlay two apertures for the given target. The white aperture comes from the default SPOC pipeline. Shown in red is our custom rectangular aperture, drawn for the unpopular package to resemble the white SPOC aperture closely, as can be seen by the overplots of these two semitransparent apertures. With tpfplotter, we identify contaminants in the red aperture. The filled red circles designate Gaia DR3 sources in the field where the radius of the circle is scaled to the ΔG ( Δm scale shown in each panel) value of the source itself. Right column: the TESS light curves of the ATLAS stars extracted in the same way as in Figure 4.
Paper: The Solar Neighborhood LI: A Variability Survey of Nearby M Dwarfs with Planets from Months to Decades with TESS and the CTIO/SMARTS 0.9 m Telescope
Authors: Aman Kar, Todd J. Henry, Andrew A. Couperus, Eliot Halley Vrijmoet, Wei-Chun Jao
Figure caption: Light curves of the 32 ATLAS targets obtained using data from the CTIO/SMARTS 0.9 m telescope. Plots are ordered by R.A. from left to right and top to bottom. Blue, green, and orange points represent observations taken in filter V , R, and I , respectively. IDR measurements are reported from all the light curves in Table 1. Each data point represents the nightly mean of observations, typically taken within a window of 30 minutes. The zero y-axis value corresponds to the median magnitude of each system.(The data used to create this figure are available.)
Paper: The Solar Neighborhood LI: A Variability Survey of Nearby M Dwarfs with Planets from Months to Decades with TESS and the CTIO/SMARTS 0.9 m Telescope
Authors: Aman Kar, Todd J. Henry, Andrew A. Couperus, Eliot Halley Vrijmoet, Wei-Chun Jao
Figure caption: Left: simulated light curve of a star with a 42 day rotation period and a semiamplitude of 20 mmag over a baseline of 27.4 days. Each simulated y-value (blue) is plotted along the y − Z sine curve (cyan; see Equation (1)). The zero y-axis value corresponds to the median magnitude of the light curve. Right: a histogram of the simulated light curve is given with the median value represented with a black vertical line, highlighting the 50th percentile of the distribution. The interdecile range (IDR; red horizontal arrows) used in this paper ranges from the 90th percentile to the 10th percentile (red vertical lines), and better represents the overall range of variability in this example.
Paper: The Solar Neighborhood LI: A Variability Survey of Nearby M Dwarfs with Planets from Months to Decades with TESS and the CTIO/SMARTS 0.9 m Telescope
Authors: Aman Kar, Todd J. Henry, Andrew A. Couperus, Eliot Halley Vrijmoet, Wei-Chun Jao
Figure caption: TESS light curves from selected four consecutive sectors for L 98–59, an intermediate variable in the ATLAS sample. Light curves using the three reductions (blue, green, and red) are as defined in Figure 4. The IDR value for each sector is given in the legend for the three reductions, but these sectors are not stitched together. Instead, we report the average IDR value in Table 1 when multiple sectors like these are available.
Paper: The Solar Neighborhood LI: A Variability Survey of Nearby M Dwarfs with Planets from Months to Decades with TESS and the CTIO/SMARTS 0.9 m Telescope
Authors: Aman Kar, Todd J. Henry, Andrew A. Couperus, Eliot Halley Vrijmoet, Wei-Chun Jao
Figure caption: TESS light curves for the two most variable stars in the ATLAS sample: GJ 317 (left) and L 34–26 (right). Light curves are shown from reductions with the colors as defined in Figure 4. Note the different y-scale for L 34–26 and the purple color of the unpopular flux, which is a result of excluding the polynomial component due to the obvious fast-rotation signal that is present in the data.
Paper: The Solar Neighborhood LI: A Variability Survey of Nearby M Dwarfs with Planets from Months to Decades with TESS and the CTIO/SMARTS 0.9 m Telescope
Authors: Aman Kar, Todd J. Henry, Andrew A. Couperus, Eliot Halley Vrijmoet, Wei-Chun Jao
Figure caption: TESS light curves for the two least-variable stars in the ATLAS sample: GJ 357 (left) and GJ 1061 (right). Light curves are shown from reductions with the colors as defined in Figure 4.
Paper: The Solar Neighborhood LI: A Variability Survey of Nearby M Dwarfs with Planets from Months to Decades with TESS and the CTIO/SMARTS 0.9 m Telescope
Authors: Aman Kar, Todd J. Henry, Andrew A. Couperus, Eliot Halley Vrijmoet, Wei-Chun Jao
Figure caption: H-R diagram highlighting the 32 ATLAS exoplanet hosts (red) plotted with the RECONS 25 pc sample (gray) and M dwarfs (blue), with limits in M  V  and V − K set as described in Section 3.
Paper: Direct-imaging Discovery of a Substellar Companion Orbiting the Accelerating Variable Star HIP 39017
Authors: Taylor L. Tobin, Thayne Currie, Yiting Li, Jeffrey Chilcote, Timothy D. Brandt, Brianna Lacy, Masayuki Kuzuhara, Maria Vincent, Mona El Morsy, Vincent Deo, Jonathan P. Williams, Olivier Guyon, Julien Lozi, Sebastien Vievard, Nour Skaf, Kyohoon Ahn, Tyler Groff, N. Jeremy Kasdin, Taichi Uyama, Motohide Tamura, Aidan Gibbs, Briley L. Lewis, Rachel Bowens-Rubin, Maïssa Salama, Qier An, Minghan Chen
Figure caption: Mass evolution isochrones for 0.12 and 0.7 Gyr objects given by several different hot-start evolutionary models. The positions of HIP 39017 b are highlighted with yellow and cyan points along the substellar isoage evolutionary tracks. With an estimated bolometric luminosity of −4.6 ± 0.2 dex, the predicted masses at ages of 0.12 and 0.7 Gyr have median values of ﹩{13.8}_{-1.6}^{+1.3}\,{M}_{J}﹩ and ﹩{38.2}_{-5.2}^{+7.9}\,{M}_{J}﹩, respectively. The mass uncertainties were estimated by adding the dispersion across the considered evolutionary tracks and the luminosity-related mass uncertainty in quadrature. We adopt 0.7 Gyr/﹩{38.2}_{-5.2}^{+7.9}\,{M}_{J}﹩ as the upper age/mass limit. The final conservative upper mass limit from evolutionary models is then 46 M  J . We adopt 0.12 Gyr/﹩{13.8}_{-1.6}^{+1.3}\,{M}_{J}﹩—the closest grid value to 115 Myr—as a more realistic characterization for HIP 39017 b. We note that a younger age than 115 Myr may indicate an even lower-mass planetary companion as suggested by evolutionary model predictions.
Paper: Direct-imaging Discovery of a Substellar Companion Orbiting the Accelerating Variable Star HIP 39017
Authors: Taylor L. Tobin, Thayne Currie, Yiting Li, Jeffrey Chilcote, Timothy D. Brandt, Brianna Lacy, Masayuki Kuzuhara, Maria Vincent, Mona El Morsy, Vincent Deo, Jonathan P. Williams, Olivier Guyon, Julien Lozi, Sebastien Vievard, Nour Skaf, Kyohoon Ahn, Tyler Groff, N. Jeremy Kasdin, Taichi Uyama, Motohide Tamura, Aidan Gibbs, Briley L. Lewis, Rachel Bowens-Rubin, Maïssa Salama, Qier An, Minghan Chen
Figure caption: The fits results of the Lacy/Burrows models (Currie et al. 2023b) to the 2022 December SCExAO/CHARIS spectrum and the NIRC2 ﹩L^{\prime} ﹩ photometric point of HIP 39017 b. Top: ﹩{\chi }_{\nu }^{2}﹩ fits for each available model spectrum as a function of T eff and ﹩\mathrm{log}g﹩ as above. Cloud parameterization is labeled for each subfigure (AE, AEE, or E, as well as modal dust size, in microns), with “rCH4” indicating grids derived with reduced methane. Bottom: six of the Lacy/Burrows model spectra, smoothed to R = 50 at 2.65 μm and overplotted on the observed HIP 39017 b spectrum used for fitting. The legend gives the T eff, ﹩\mathrm{log}g﹩, cloud prescription, whether they have reduced CH4, and its ﹩{\chi }_{\nu }^{2}﹩ fit to the observations. The first four spectra shown are the four Lacy/Burrows spectra with the lowest ﹩{\chi }_{\nu }^{2}﹩, while the last two are those with the lowest ﹩{\chi }_{\nu }^{2}﹩ of the remaining two cloud prescription/methane abundance grids.
Paper: Direct-imaging Discovery of a Substellar Companion Orbiting the Accelerating Variable Star HIP 39017
Authors: Taylor L. Tobin, Thayne Currie, Yiting Li, Jeffrey Chilcote, Timothy D. Brandt, Brianna Lacy, Masayuki Kuzuhara, Maria Vincent, Mona El Morsy, Vincent Deo, Jonathan P. Williams, Olivier Guyon, Julien Lozi, Sebastien Vievard, Nour Skaf, Kyohoon Ahn, Tyler Groff, N. Jeremy Kasdin, Taichi Uyama, Motohide Tamura, Aidan Gibbs, Briley L. Lewis, Rachel Bowens-Rubin, Maïssa Salama, Qier An, Minghan Chen
Figure caption: The Sonora Bobcat (Marley et al. 2021) fit results to the HIP 39017 b spectrum using the 2022 December CHARIS data set and the Keck/NIRC2 ﹩L^{\prime} ﹩ photometric point. Left: map of the ﹩{\chi }_{\nu }^{2}﹩ as a function of model ﹩\mathrm{log}g﹩ and T eff for Sonora Bobcat models with solar metallicity and C/O. The best-fit Sonora Bobcat model is marked with the black diamond, with 1, 2, and 3σ contours around the minimum. Right: the best-fit model spectrum (smoothed to R = 50 at 2.65 μm) for each C/O value provided in the Sonora Bobcat model grid overplotted with the HIP 39017 b observations. The legend denotes the T eff, ﹩\mathrm{log}g﹩, C/O, and ﹩{\chi }_{\nu }^{2}﹩ for each model spectrum shown. Note: Sonora Bobcat spectra with C/O = {0.5, 1.5} are only available with ﹩\mathrm{log}g=5.0﹩.
Paper: Direct-imaging Discovery of a Substellar Companion Orbiting the Accelerating Variable Star HIP 39017
Authors: Taylor L. Tobin, Thayne Currie, Yiting Li, Jeffrey Chilcote, Timothy D. Brandt, Brianna Lacy, Masayuki Kuzuhara, Maria Vincent, Mona El Morsy, Vincent Deo, Jonathan P. Williams, Olivier Guyon, Julien Lozi, Sebastien Vievard, Nour Skaf, Kyohoon Ahn, Tyler Groff, N. Jeremy Kasdin, Taichi Uyama, Motohide Tamura, Aidan Gibbs, Briley L. Lewis, Rachel Bowens-Rubin, Maïssa Salama, Qier An, Minghan Chen
Figure caption: Weighted MCMC orbital posteriors using a uniform, informative range of [0, 46] M  J  on the companion mass. This is a result from downsampling the original fit to the relative astrometry from direct imaging presented in Table 2 (left panel) and stellar absolute astrometry in R.A. and decl. from the HGCA eDR3 (right two panels). The red data points in the left panel are relative astrometry data driven by direct-imaging observations, while the two data points in cyan and orange in the right panels denote proper-motion measurements from the cross-calibrated Hipparcos and Gaia eDR3 catalogs.
Paper: Direct-imaging Discovery of a Substellar Companion Orbiting the Accelerating Variable Star HIP 39017
Authors: Taylor L. Tobin, Thayne Currie, Yiting Li, Jeffrey Chilcote, Timothy D. Brandt, Brianna Lacy, Masayuki Kuzuhara, Maria Vincent, Mona El Morsy, Vincent Deo, Jonathan P. Williams, Olivier Guyon, Julien Lozi, Sebastien Vievard, Nour Skaf, Kyohoon Ahn, Tyler Groff, N. Jeremy Kasdin, Taichi Uyama, Motohide Tamura, Aidan Gibbs, Briley L. Lewis, Rachel Bowens-Rubin, Maïssa Salama, Qier An, Minghan Chen
Figure caption: Left: CHARIS spectrum of the wider-separation point source shown to be a background star (green) with a Kurucz model atmosphere corresponding to a K2–K3 star overplotted (magenta). Right: proper-motion analysis showing that this point source’s astrometry is consistent with the motion expected for a background star. The dashed line connects the object’s position in the first detected epoch to its predicted position in the 2023 Keck/NIRC2 data if it is a background star, a prediction that matches the observations within errors (upper-right green dot).
Paper: Direct-imaging Discovery of a Substellar Companion Orbiting the Accelerating Variable Star HIP 39017
Authors: Taylor L. Tobin, Thayne Currie, Yiting Li, Jeffrey Chilcote, Timothy D. Brandt, Brianna Lacy, Masayuki Kuzuhara, Maria Vincent, Mona El Morsy, Vincent Deo, Jonathan P. Williams, Olivier Guyon, Julien Lozi, Sebastien Vievard, Nour Skaf, Kyohoon Ahn, Tyler Groff, N. Jeremy Kasdin, Taichi Uyama, Motohide Tamura, Aidan Gibbs, Briley L. Lewis, Rachel Bowens-Rubin, Maïssa Salama, Qier An, Minghan Chen
Figure caption: Posterior distributions of selected parameters from a joint fit with unweighted companion mass posteriors and using the full data sets of relative astrometry from direct imaging and complementary absolute astrometry from the HGCA. The contours show 1, 2, and 3σ contour levels at 68%, 95%, and 99.7% confidence levels.
Paper: Direct-imaging Discovery of a Substellar Companion Orbiting the Accelerating Variable Star HIP 39017
Authors: Taylor L. Tobin, Thayne Currie, Yiting Li, Jeffrey Chilcote, Timothy D. Brandt, Brianna Lacy, Masayuki Kuzuhara, Maria Vincent, Mona El Morsy, Vincent Deo, Jonathan P. Williams, Olivier Guyon, Julien Lozi, Sebastien Vievard, Nour Skaf, Kyohoon Ahn, Tyler Groff, N. Jeremy Kasdin, Taichi Uyama, Motohide Tamura, Aidan Gibbs, Briley L. Lewis, Rachel Bowens-Rubin, Maïssa Salama, Qier An, Minghan Chen
Figure caption: Top: proper-motion analysis for HIP 39017 b compared to the motion of a background star with zero proper motion. Bottom: proper-motion analysis for a synthesized Besancon population compared to the 1, 3, and 5σ contours for background stars needed to match HIP 39017 b’s relative astrometry.
Paper: Direct-imaging Discovery of a Substellar Companion Orbiting the Accelerating Variable Star HIP 39017
Authors: Taylor L. Tobin, Thayne Currie, Yiting Li, Jeffrey Chilcote, Timothy D. Brandt, Brianna Lacy, Masayuki Kuzuhara, Maria Vincent, Mona El Morsy, Vincent Deo, Jonathan P. Williams, Olivier Guyon, Julien Lozi, Sebastien Vievard, Nour Skaf, Kyohoon Ahn, Tyler Groff, N. Jeremy Kasdin, Taichi Uyama, Motohide Tamura, Aidan Gibbs, Briley L. Lewis, Rachel Bowens-Rubin, Maïssa Salama, Qier An, Minghan Chen
Figure caption: Same as Figure 11 but employing a uniform, informative cutoff of 0–46 M Jup on the companion mass posteriors by downsampling the original posteriors in Figure 11.
Paper: Direct-imaging Discovery of a Substellar Companion Orbiting the Accelerating Variable Star HIP 39017
Authors: Taylor L. Tobin, Thayne Currie, Yiting Li, Jeffrey Chilcote, Timothy D. Brandt, Brianna Lacy, Masayuki Kuzuhara, Maria Vincent, Mona El Morsy, Vincent Deo, Jonathan P. Williams, Olivier Guyon, Julien Lozi, Sebastien Vievard, Nour Skaf, Kyohoon Ahn, Tyler Groff, N. Jeremy Kasdin, Taichi Uyama, Motohide Tamura, Aidan Gibbs, Briley L. Lewis, Rachel Bowens-Rubin, Maïssa Salama, Qier An, Minghan Chen
Figure caption: Detections of a wider-separation point source around HIP 39017 with Keck/NIRC2 (left and right panels) and SCExAO/CHARIS (middle panel).
Paper: A Secular Solar System Resonance that Disrupts the Dominant Cycle in Earth’s Orbital Eccentricity (g 2 − g 5): Implications for Astrochronology
Authors: Richard E. Zeebe, Margriet L. Lantink
Figure caption: Examples of Mercury’s orbital eccentricity and resonant angle θ 12. (a) Mercury’s orbital eccentricity in solutions R01 and R07. The lighter foreground colors represent filter magnitudes (﹩| {z}_{M}^{* }| ﹩, see Section 2.5). (b), (c) Resonant angle ﹩{\theta }_{12}=({\varpi }_{1}^{* }-{\varpi }_{2}^{* })+({{\rm{\Omega }}}_{1}^{* }-{{\rm{\Omega }}}_{2}^{* })﹩ associated with σ 12 = (g 1 − g 2) + (s 1 − s 2) (see Section 2.5 for calculation). θ 12 is intentionally shown over a 16π range for clarity (at 2π range, lines connect and appear as areas/patches). (b) θ 12 in R01 circulates throughout; σ 12-resonance intervals are absent. (c) θ 12 in R07 circulates but also librates during σ 12-resonance intervals (oscillation around a constant value, see e.g., plateau at about −1.25 to −1.5 Gyr in (c)). Solutions exhibiting θ 12-circulation and libration were usually associated with intervals of slightly elevated eccentricity in Mercury’s orbit.
Paper: A Secular Solar System Resonance that Disrupts the Dominant Cycle in Earth’s Orbital Eccentricity (g 2 − g 5): Implications for Astrochronology
Authors: Richard E. Zeebe, Margriet L. Lantink
Figure caption: Climatic precession ﹩\bar{p}=e\sin \bar{\omega }﹩, where ﹩\bar{\omega }﹩ is the longitude of perihelion measured from the moving equinox (for details and code, see Zeebe 2022, github.com/rezeebe/snvec, www2.hawaii.edu/~zeebe/Astro.html, and Section 2.3). (a) ﹩\bar{p}﹩ in the recent past (last 1 Myr), nearly identical in all solutions. Panels (b, c) display examples of ﹩\bar{p}﹩ based on orbital solutions during σ 12-resonance intervals. Note the different lunisolar precession frequencies (carrier frequency) in the past owing to the Earth–Moon system’s evolution. (b) ﹩\bar{p}﹩ based on solution R28 over a 1 Myr interval centered at t = −1450 Myr. The amplitude modulation (AM) pattern fundamentally differs from (a). (c) ﹩\bar{p}﹩ based on R06 over a 1 Myr interval centered at t = −1180 Myr. In addition to an altered AM pattern, the total amplitude is reduced compared to (a).
Paper: A Secular Solar System Resonance that Disrupts the Dominant Cycle in Earth’s Orbital Eccentricity (g 2 − g 5): Implications for Astrochronology
Authors: Richard E. Zeebe, Margriet L. Lantink
Figure caption: Fast Fourier transform (FFT ﹩={ \mathcal F }(\bar{p})﹩) of climatic precession ﹩\bar{p}=e\sin \bar{\omega }﹩ over 6 Myr intervals. Frequencies in arcsec yr −1 = ″ yr −1. Note different lunisolar precession frequency Ψ in the past owing to the Earth–Moon system’s evolution (for details and code, see Zeebe 2022), github.com/rezeebe/snvec, www2.hawaii.edu/~zeebe/Astro.html, and Section 2.3). Top: standard spectrum in the recent past centered at t = −3 Myr (nearly identical in all solutions). Bottom: spectrum based on solution R06 centered at t = −1180 Myr. Note the split and reduced power of Ψ + g 2 in bottom vs. top panel (red circles).
Paper: A Secular Solar System Resonance that Disrupts the Dominant Cycle in Earth’s Orbital Eccentricity (g 2 − g 5): Implications for Astrochronology
Authors: Richard E. Zeebe, Margriet L. Lantink
Figure caption: Schematic illustration of (a) g and (b) s modes (see text).
Paper: A Secular Solar System Resonance that Disrupts the Dominant Cycle in Earth’s Orbital Eccentricity (g 2 − g 5): Implications for Astrochronology
Authors: Richard E. Zeebe, Margriet L. Lantink
Figure caption: Period of g 25 = (g 2 − g 5) from our ensemble integrations. Solutions including σ 12-resonance intervals (∼40%) are highlighted in color, the remaining solutions are displayed in gray. Importantly, the weak/absent LEC is critical, not the actual shift in the period, which would be unidentifiable in a stratigraphic record due to the low power in (g 2 − g 5).