adsabs/AstroCLIMB huggingface dataset:
Paper: The Prevalence of Resonance Among Young, Close-in Planets
Authors: Fei Dai, Max Goldberg, Konstantin Batygin, Jennifer van Saders, Eugene Chiang, Nick Choksi, Rixin Li, Erik A. Petigura, Gregory J. Gilbert, Sarah C. Millholland, Yuan-Zhe Dai, Luke Bouma, Lauren M. Weiss, Joshua N. Winn
Figure caption: The observed deviation Δ for the resonant-chain systems with well-measured ages vs. the cumulative eccentricity damping, i.e., all terms in Equation (2) except the reduced tidal quality factor. The solid lines shows the theoretically predicted Δ at various reduced tidal quality factors. We have labeled each resonant-chain system with the radius of the planet that is expected to experience the strongest tides. TOI-1136 (700 Myr old; F. Dai et al. 2023) and AU Mic (20 Myr old; P. Plavchan et al. 2020) are still deep in resonances (Δ ∼ 0.1%), and the inferred reduced tidal quality factor is roughly 104–105, which is consistent with Uranus (e.g., S. R. A. Gomes & A. C. M. Correia 2024). However, HD 109833 (10–16 Myr old; M. L. Wood et al. 2023), TOI-2076 (200 Myr old; C. Hedges et al. 2021) are substantially far away from resonance (Δ ∼ 1%), such that the required reduced tidal quality factor ﹩{Q}_{p}^{{\prime} }\lt 10﹩ seems unphysical. Other processes such as disk e-damping (N. Choksi & E. Chiang 2020), disk turbulence (M. Goldberg & K. Batygin 2023), obliquity tides (S. Millholland & G. Laughlin 2019), and planetesimal scattering (S. Chatterjee & E. B. Ford 2015) should be included to explain the observed Δ distribution.
Paper: The Prevalence of Resonance Among Young, Close-in Planets
Authors: Fei Dai, Max Goldberg, Konstantin Batygin, Jennifer van Saders, Eugene Chiang, Nick Choksi, Rixin Li, Erik A. Petigura, Gregory J. Gilbert, Sarah C. Millholland, Yuan-Zhe Dai, Luke Bouma, Lauren M. Weiss, Joshua N. Winn
Figure caption: Orbital architectures of “young” multiplanet systems (<100 Myr old). Cluster members are labeled. Symbol sizes represent planet radii as indicated. Each near-resonant pair of planets is labeled by its resonance and the fractional deviation Δ from perfect period commensurability (Equation (1)). Colors indicate resonance order. Planet pairs situated within several percent of a period commensurability but that fall formally outside our Δ thresholds (Tables 1 and 2) are colored light gray (and not counted in our resonance incidence rates). Near-resonant configurations appear to dominate these young planetary systems, with 8 out of 10 pairs of neighboring planets falling within our Δ thresholds for resonance, and 6 out of 7 systems exhibiting at least one resonant pair so defined.
Paper: The Prevalence of Resonance Among Young, Close-in Planets
Authors: Fei Dai, Max Goldberg, Konstantin Batygin, Jennifer van Saders, Eugene Chiang, Nick Choksi, Rixin Li, Erik A. Petigura, Gregory J. Gilbert, Sarah C. Millholland, Yuan-Zhe Dai, Luke Bouma, Lauren M. Weiss, Joshua N. Winn
Figure caption: Top: the incidence of first-order resonant pairs (blue curve) and the incidence of planetary systems with at least one resonant pair (first- or second-order; orange curve) across three age bins: (1) “young” (<100 Myr), (2) “adolescent” (100–1000 Myr), and (3) “mature” (>1 Gyr). The young planetary systems abound in resonances, which appear to disintegrate over a timescale on the order of 100 Myr. The age bins have been offset for clarity. Bottom: cumulative distributions of Δ near first-order commensurability across different age groups. Data are plotted for all pairs, resonant and nonresonant; the red and black curves saturate at large Δ values not plotted. We see evidence of the Δ distribution broadening with time, in particular within the first 1 Gyr.
Paper: The Prevalence of Resonance Among Young, Close-in Planets
Authors: Fei Dai, Max Goldberg, Konstantin Batygin, Jennifer van Saders, Eugene Chiang, Nick Choksi, Rixin Li, Erik A. Petigura, Gregory J. Gilbert, Sarah C. Millholland, Yuan-Zhe Dai, Luke Bouma, Lauren M. Weiss, Joshua N. Winn
Figure caption: The orbital periods and radii of the innermost planets in multiplanet systems. The resonant chain systems (solid symbols representing systems with unbroken multiple resonant pairs) and generic multiplanet systems (gray circles) are shown separately. The bottom panel is the rotation period distribution of young stars in rho Ophiuchus (∼1 Myr old L. M. Rebull et al. 2018), which is still in the disk-hosting stage. If resonant chains are parked near the disk inner edges, the orbital period distribution of the innermost planets should trace the rotation period distribution of young stars. Indeed, almost all resonant chain systems have innermost planets <10 days, the same applies to the rotation periods of young stars. On the other hand, 25% ± 2% of generic multiplanet systems have their innermost planets between 10 and 100 days.
Paper: The Prevalence of Resonance Among Young, Close-in Planets
Authors: Fei Dai, Max Goldberg, Konstantin Batygin, Jennifer van Saders, Eugene Chiang, Nick Choksi, Rixin Li, Erik A. Petigura, Gregory J. Gilbert, Sarah C. Millholland, Yuan-Zhe Dai, Luke Bouma, Lauren M. Weiss, Joshua N. Winn
Figure caption: The incidence of first- and second-order resonant pairs increases with the observed planet multiplicity. For the first-order resonances, the incidence within systems of two detected planets is 9.1% ± 1.3% (43/470). It steadily increases to 15.7% ± 2.0% (53/338) for three-planet systems, 18.8% ± 2.9% (35/186) for four-planet systems, 19.0% ± 4.3% (16/84) for five-planet systems, and 57.5% ± 7.8% (23/40) for six-planet systems. We caution there is only one seven-planet system (TRAPPIST-1; M. Gillon et al. 2017; R. Luger et al. 2017) and one eight-planet system (Kepler-90; C. J. Shallue & A. Vanderburg 2018) in our sample. Both systems evince an abundance of resonances. The horizontal dotted lines represent the incidence of resonant pairs across all multiplanet systems, irrespective of age.
Paper: The Prevalence of Resonance Among Young, Close-in Planets
Authors: Fei Dai, Max Goldberg, Konstantin Batygin, Jennifer van Saders, Eugene Chiang, Nick Choksi, Rixin Li, Erik A. Petigura, Gregory J. Gilbert, Sarah C. Millholland, Yuan-Zhe Dai, Luke Bouma, Lauren M. Weiss, Joshua N. Winn
Figure caption: Same as Figure 5 but for the “adolescent” planetary systems, defined as having ages between 100 Myr and 1 Gyr. Cluster members are labeled. Six out of 16 systems have at least one pair of near-resonant planets, and 11 out of 29 neighboring pairs are near-resonant (as defined by our Δ criteria; see Tables 1 and 2). The near-resonant pair of planets in TOI-712 falls right on our Δ boundary but exhibits TTV variations suggesting strongly resonant interaction (data not shown).
Paper:  Yuti: A General-purpose Transit Simulator for Arbitrary Shaped Objects Orbiting Stars
Authors: Ushasi Bhowmick, Vikram Khaire
Figure caption: Transit of a Dyson disk, compared to the transit of a planet of the same dimensions and distance to the star. The top panel shows the light curves obtained for a planet as well as Dyson disk transits. All the systems have a size R pl = 0.1 R st and R orb = 2 R st. The bottom panel shows the residuals (Dyson disk–Planet transit). Column A shows a simple transit with no eccentricity or limb darkening. While the planet's transit is flat, the Dyson disk's transit shows an upward curvature during ingress and egress due to the change in the projection area. Column B adds limb darkening to the first transit, which diminishes the residual feature. Column C shows a transit with an eccentric orbit with the semimajor axis perpendicular to the line of sight. The Dyson Disk light curve shows significant asymmetry in ingress and egress due to the change of area of projection. Column D shows the same system with limb darkening. This results in a slightly diminished but still significant residual feature.
Paper:  Yuti: A General-purpose Transit Simulator for Arbitrary Shaped Objects Orbiting Stars
Authors: Ushasi Bhowmick, Vikram Khaire
Figure caption: Simulated heartbeat star systems in various configurations. Each panel is a configuration with a value of eccentricity, periapsis offset, and inclination (e, w, i). The radius ratio (r  s /r  p  = 0.8), semimajor axis (5r  p ), fluid Love number (1.5), and mass ratio (m  s /m  p  = 0.9) are the same for all of the configurations. Three cases are considered. Case A represents an ellipsoidal star with a spherical opaque companion (relative flux f = 0, cyan curve). Case B represents an ellipsoidal star with a spherical bright companion (f = 1 red curve). Case C considers an ellipsoidal star with an ellipsoidal bright companion (h  f  = 1, f = 1, pink curve). The top panels also show the ellc model (black dotted–dashed line), which coincides with the simulated light curves from Yuti. The bottom panels plot the residuals. Panels (I)–(V) represent heartbeat signatures at lower inclination that show no transit. Panel (VI) represents the highest inclination case which shows primary and secondary transits along with tidal deformation.
Paper:  Yuti: A General-purpose Transit Simulator for Arbitrary Shaped Objects Orbiting Stars
Authors: Ushasi Bhowmick, Vikram Khaire
Figure caption: Transit of weird objects. The left-hand panel imagines a Dyson sphere in partial construction, causing gaps between the Dyson disks. The size of individual panels is 0.157 R st at a distance of 2 R st, which corresponds to 40 panels at the equatorial circumference. Away from the equator, the orbits and sizes are scaled according to the latitude in order to maintain 40 panels in any circumference. A total of 100 panels are placed in this incomplete Dyson swarm. The bottom left-hand panel shows the resulting transit light curve, which shows a highly asymmetric and distorted geometry. The right-hand panel shows a transit of a hypothetical polar ring. The ring is made of 41 panels, each of size 0.153 R st at a distance of 2 R st. The bottom right-hand panel shows the resulting transit, which is very similar to a planet transit with half the orbital period.
Paper:  Yuti: A General-purpose Transit Simulator for Arbitrary Shaped Objects Orbiting Stars
Authors: Ushasi Bhowmick, Vikram Khaire
Figure caption: Convergence of Monte Carlo simulation. The top panel shows the variation of Monte Carlo noise with changing frame resolution with a fixed sampling resolution of 105. The rms error flattens out to a fixed value of 3.12 × 10−4. The middle panel shows the variation of Monte Carlo noise with sampling resolution, for a fixed frame resolution of 500. The plot is linear in the log–log scale, as represented by the best-fit line (y = mx + c). The slope of this line is m = −0.5, which is characteristic of a Monte Carlo distribution. The bottom panel shows the Monte Carlo resolution required to simulate a system with a given transit depth at a required confidence level. Each of the solid lines represents a certain confidence level.
Paper:  Yuti: A General-purpose Transit Simulator for Arbitrary Shaped Objects Orbiting Stars
Authors: Ushasi Bhowmick, Vikram Khaire
Figure caption: Comparison of the simulation from Yuti with the standard model for a transiting exoplanet around a limb-darkened star. Simulated parameters are: R pl = 0.12 R st, R orb = 2 R st, u 1 = 0.3 and u 2 = 0.2. The top panel shows the simulation and the analytical model (overlapping) of K. Mandel & E. Agol (2002). The bottom panel plots the residuals (simulation - model) arising due to Monte Carlo noise. The residuals are less than 0.5% of the transit depth.
Paper:  Yuti: A General-purpose Transit Simulator for Arbitrary Shaped Objects Orbiting Stars
Authors: Ushasi Bhowmick, Vikram Khaire
Figure caption: Exocomet simulation for candidate KIC: 3542116 Dip 1268. The top panel shows a schematic of the simulation geometry. The comet size has been exaggerated for visual clarity. The middle panel shows the light curve of KIC 3542116 and the simulated comet model. The bottom panel shows the residuals (data simulation). The fitted parameters are given.
Paper:  Yuti: A General-purpose Transit Simulator for Arbitrary Shaped Objects Orbiting Stars
Authors: Ushasi Bhowmick, Vikram Khaire
Figure caption: Trappist-1 simulated light curve. The total phase duration is equal to one orbit of Trappist-1h. The top panel shows one frame of the simulation, with the seven planets. The size of the planets has been scaled up and distances have been scaled down for clarity. The planets have been color-coded by their orbital distance. The bottom panel shows the simulated light curve. The simulated light curve is for the realistic system.
Paper:  Yuti: A General-purpose Transit Simulator for Arbitrary Shaped Objects Orbiting Stars
Authors: Ushasi Bhowmick, Vikram Khaire
Figure caption: Simulated light curves for WASP-103b. The top panel shows phase folded transits from CHEOPS (gray), the ellc light curve with appropriate parameters, and the simulated light curve from Yuti. The middle panel shows the residuals from the observation (data-ellc), whereas the last panel shows the residuals between the simulation and ellc.
Paper:  Yuti: A General-purpose Transit Simulator for Arbitrary Shaped Objects Orbiting Stars
Authors: Ushasi Bhowmick, Vikram Khaire
Figure caption: A schematic showing the orbital configuration of a Dyson disk. The top panel shows five orientations of a flat circular 2D structure along the orbit. The size of the structure is 0.3 R st at a distance of 2 R st. The bottom panel shows the resulting transit.
Paper: KIC 6362386: An Eclipsing Binary with γ Doradus–type Pulsations and Starspots
Authors: Mengqi Jin, Jianning Fu, Xiaobin Zhang, Weikai Zong, Jiaxin Wang, Xiaoyu Ma, Keyu Xing, Haotian Wang
Figure caption: The phase-folded light curves of KIC 6362386 from the photometry. The top, middle, and bottom panels stands for the data from Kepler LC quarters, SC quarters, and TESS sectors, respectively.
Paper: KIC 6362386: An Eclipsing Binary with γ Doradus–type Pulsations and Starspots
Authors: Mengqi Jin, Jianning Fu, Xiaobin Zhang, Weikai Zong, Jiaxin Wang, Xiaoyu Ma, Keyu Xing, Haotian Wang
Figure caption: The RV curve of KIC 6362386. The red dashed line represents the best-fit curve resulting from the fitting process.
Paper: KIC 6362386: An Eclipsing Binary with γ Doradus–type Pulsations and Starspots
Authors: Mengqi Jin, Jianning Fu, Xiaobin Zhang, Weikai Zong, Jiaxin Wang, Xiaoyu Ma, Keyu Xing, Haotian Wang
Figure caption: The distribution of SNR of a total of 146 spectra.
Paper: KIC 6362386: An Eclipsing Binary with γ Doradus–type Pulsations and Starspots
Authors: Mengqi Jin, Jianning Fu, Xiaobin Zhang, Weikai Zong, Jiaxin Wang, Xiaoyu Ma, Keyu Xing, Haotian Wang
Figure caption: Three examples of MRS for KIC 6362386.
Paper: KIC 6362386: An Eclipsing Binary with γ Doradus–type Pulsations and Starspots
Authors: Mengqi Jin, Jianning Fu, Xiaobin Zhang, Weikai Zong, Jiaxin Wang, Xiaoyu Ma, Keyu Xing, Haotian Wang
Figure caption: The light curve of KIC 6362386 observed by Kepler and TESS. The top, middle, and bottom panels show the light curves of data of all LC quarters, all SC quarters observed by Kepler, and all sectors observed by TESS, respectively.
Paper: KIC 6362386: An Eclipsing Binary with γ Doradus–type Pulsations and Starspots
Authors: Mengqi Jin, Jianning Fu, Xiaobin Zhang, Weikai Zong, Jiaxin Wang, Xiaoyu Ma, Keyu Xing, Haotian Wang
Figure caption: An example of the Kepler TPF file of KIC 6362386. The red squares stands for the aperture selected for photometry.
Paper: KIC 6362386: An Eclipsing Binary with γ Doradus–type Pulsations and Starspots
Authors: Mengqi Jin, Jianning Fu, Xiaobin Zhang, Weikai Zong, Jiaxin Wang, Xiaoyu Ma, Keyu Xing, Haotian Wang
Figure caption: An example of the TESS FFI file of KIC 6362386. The red squares stands for the aperture selected for photometry.
Paper: KIC 6362386: An Eclipsing Binary with γ Doradus–type Pulsations and Starspots
Authors: Mengqi Jin, Jianning Fu, Xiaobin Zhang, Weikai Zong, Jiaxin Wang, Xiaoyu Ma, Keyu Xing, Haotian Wang
Figure caption: The O – C diagram for KIC 6362386. The red line shows the fitting for the O – C diagram. The outliers shown as the gray crosses are excluded in the fitting progress.
Paper: KIC 6362386: An Eclipsing Binary with γ Doradus–type Pulsations and Starspots
Authors: Mengqi Jin, Jianning Fu, Xiaobin Zhang, Weikai Zong, Jiaxin Wang, Xiaoyu Ma, Keyu Xing, Haotian Wang
Figure caption: The corner diagram of the RV curve fitting.
Paper: Detection of High-frequency Pulsation in WR 135: Investigation of Stellar Wind Dynamics
Authors: Subhajit Kar, Ramkrishna Das, Blesson Mathew, Tapas Baug, Avijit Mandal
Figure caption: Normalized lightcurves of WR 135 with 10 minute cadence derived from FFIs observed in Sector 41, 54, and 55.
Paper: Detection of High-frequency Pulsation in WR 135: Investigation of Stellar Wind Dynamics
Authors: Subhajit Kar, Ramkrishna Das, Blesson Mathew, Tapas Baug, Avijit Mandal
Figure caption: Line profile of C III λ5696 (left panel) and C IV λλ5802-12 (right panel) in the spectroscopic time-series dataset from CFHT (see Table 2).
Paper: Detection of High-frequency Pulsation in WR 135: Investigation of Stellar Wind Dynamics
Authors: Subhajit Kar, Ramkrishna Das, Blesson Mathew, Tapas Baug, Avijit Mandal
Figure caption: Comparison among the mean-flux (in magenta), mean-Rosseland (in green), and electron-scattering (or Thomson-scattering; in orange) opacities being contributed by different atomic species (in Figure 11) in the stratified winds of the model atmosphere.
Paper: Detection of High-frequency Pulsation in WR 135: Investigation of Stellar Wind Dynamics
Authors: Subhajit Kar, Ramkrishna Das, Blesson Mathew, Tapas Baug, Avijit Mandal
Figure caption: Velocity stratification in the model atmosphere of WR135: isothermal sound speed (in blue) and wind velocity (in red). The mass outflow follows the wind velocity profile beyond the sonic point (R  s ).
Paper: Detection of High-frequency Pulsation in WR 135: Investigation of Stellar Wind Dynamics
Authors: Subhajit Kar, Ramkrishna Das, Blesson Mathew, Tapas Baug, Avijit Mandal
Figure caption: Relative ionic population of the most abundant atomic elements contributing to the opacities (in Figure 10) that are driving different layers of the model atmosphere.
Paper: Detection of High-frequency Pulsation in WR 135: Investigation of Stellar Wind Dynamics
Authors: Subhajit Kar, Ramkrishna Das, Blesson Mathew, Tapas Baug, Avijit Mandal
Figure caption: Ratio of the gas pressure (P gas) and radiation pressure (P rad) in the stellar model atmosphere. In the supersonic regime, the P gas becomes almost negligible compared to the P rad.
Paper: Detection of High-frequency Pulsation in WR 135: Investigation of Stellar Wind Dynamics
Authors: Subhajit Kar, Ramkrishna Das, Blesson Mathew, Tapas Baug, Avijit Mandal
Figure caption: Power spectra of WR 135 generated from the LSP fitted photometric lightcurves from TESS Sector-41, 54 and 55.
Paper: Detection of High-frequency Pulsation in WR 135: Investigation of Stellar Wind Dynamics
Authors: Subhajit Kar, Ramkrishna Das, Blesson Mathew, Tapas Baug, Avijit Mandal
Figure caption: Influence of acceleration exponent (β 2) on the unblended diagnostic emission lines (for f   VFF  = 0.29). The β 2-exponent affects the outer wind (τ ross > 0.1) density, which in turn affects the line strengths.
Paper: Detection of High-frequency Pulsation in WR 135: Investigation of Stellar Wind Dynamics
Authors: Subhajit Kar, Ramkrishna Das, Blesson Mathew, Tapas Baug, Avijit Mandal
Figure caption: Influence of VFF on the unblended diagnostic emission lines for a fixed outer-wind acceleration exponent (β 2 = 50). The observed spectrum is represented as a black-dashed curve. Models computed for different VFF values are also labeled.
Paper: Detection of High-frequency Pulsation in WR 135: Investigation of Stellar Wind Dynamics
Authors: Subhajit Kar, Ramkrishna Das, Blesson Mathew, Tapas Baug, Avijit Mandal
Figure caption: Comparison of the best-fitting spectroscopic model with the observed data of WR 135.
Paper: Detection of High-frequency Pulsation in WR 135: Investigation of Stellar Wind Dynamics
Authors: Subhajit Kar, Ramkrishna Das, Blesson Mathew, Tapas Baug, Avijit Mandal
Figure caption: Dual phase sinusoids (ν = 21 ± 1 day−1) fitted over the observed line strength time series.
Paper:  Gaspery: Optimized Scheduling of Radial Velocity Follow-up Observations for Active Host Stars
Authors: Christopher Lam, Megan Bedell, Lily L. Zhao, Arvind F. Gupta, Sarah A. Ballard
Figure caption: Sensitivity map showing the uncertainty on the RV semi-amplitude, σ  K , for different combinations of orbital period and observing cadence. We overplot analytic curves and labels corresponding to key frequencies that hinder our ability to measure K, which are described in Section 3.3.
Paper:  Gaspery: Optimized Scheduling of Radial Velocity Follow-up Observations for Active Host Stars
Authors: Christopher Lam, Megan Bedell, Lily L. Zhao, Arvind F. Gupta, Sarah A. Ballard
Figure caption: Sensitivity maps, identical to Figure 3, but here we vary each of the quasiperiodic GP kernel hyperparameters, which produces changes in key features from Figure 3. For each plot, only one free parameter is changed from our fiducial system’s values: {P rot = 4.84 days, τ = 100 days, σ corr = 43 m s−1, η = 0.4} (see Table 1). Drawn contours are left from Figure 3 for ease of comparison. The top left panel shows how the sensitivity map changes when P rot is increased from 4.84 to 28 days. The top-right panel shows how this picture changes for a much shorter spot lifetime, when τ is decreased from 100 to 3 days (specifically, shorter than P rot). The bottom left panel shows what happens when σ corr is decreased from 47 to 5 m s−1, which is more commensurate with the planet RV semi-amplitude. Finally, the text in the bottom right panel shows how increasing η from 0.4 to 0.9 lowers the complexity of the correlated noise from Figure 3.
Paper:  Gaspery: Optimized Scheduling of Radial Velocity Follow-up Observations for Active Host Stars
Authors: Christopher Lam, Megan Bedell, Lily L. Zhao, Arvind F. Gupta, Sarah A. Ballard
Figure caption: Phase-folded RV curves showing three different scenarios of observation cadence and planet orbital period combinations. Blue points indicate the sampled injected planet signal. Red filled-in points indicate the sum of the sampled stellar signal and the planet signal. Red open circles indicate the binned stellar plus planet signal, where bin width is one-tenth of the P orb, such that there are ten bins. Each panel is associated with a different location in Figure 3. Top: suboptimal case with P orb = P rot ((1) in Figure 3). Middle: an observation strategy on a beat frequency curve ((2) in Figure 3). Bottom: when the observing cadence is equal to P rot and P orb is not equal to P rot ((5) in Figure 3), making the sampled stellar noise effectively offset from the planet signal.
Paper:  Gaspery: Optimized Scheduling of Radial Velocity Follow-up Observations for Active Host Stars
Authors: Christopher Lam, Megan Bedell, Lily L. Zhao, Arvind F. Gupta, Sarah A. Ballard
Figure caption: Sensitivity maps showing how the uncertainty on the planet RV semi-amplitude, σ  K , changes for different combinations of a number of observations (x-axis) and observing cadence (y-axis). The color bar is log-scaled in order to highlight the structure in these plots. Left: in the white noise case, the uncertainty on K decreases gradually as the number of observations increases. Additionally, there is a band of high uncertainty for an observation cadence equal to half of the planet’s orbital period. Right: in the correlated noise regime, other observing cadences also give rise to high uncertainties at beat frequencies between the planet's orbital period and modes of the stellar rotation period.