adsabs/AstroCLIMB huggingface dataset:
Paper: 3D Selection of 167 Substellar Companions to Nearby Stars
Authors: Fabo Feng, R. Paul Butler, Steven S. Vogt, Matthew S. Clement, C. G. Tinney, Kaiming Cui, Masataka Aizawa, Hugh R. A. Jones, J. Bailey, Jennifer Burt, B. D. Carter, Jeffrey D. Crane, Francesco Flammini Dotti, Bradford Holden, Bo Ma, Masahiro Ogihara, Rebecca Oppenheimer, S. J. O'Toole, Stephen A. Shectman, Robert A. Wittenmyer, Sharon X. Wang, D. J. Wright, Yifan Xuan
Figure caption: The Hertzsprung–Russell diagram for the stellar sample in this work. The x-axis is the BP–RP color, while the y-axis is the absolute G magnitude derived from the Gaia EDR3 catalog. The 869 stars showing long-period RV signals are shown in blue. Of these, 161 stars are found to host companions with masses ranging from 5 M Jup to 120 M Jup, and are shown in red.
Paper: 3D Selection of 167 Substellar Companions to Nearby Stars
Authors: Fabo Feng, R. Paul Butler, Steven S. Vogt, Matthew S. Clement, C. G. Tinney, Kaiming Cui, Masataka Aizawa, Hugh R. A. Jones, J. Bailey, Jennifer Burt, B. D. Carter, Jeffrey D. Crane, Francesco Flammini Dotti, Bradford Holden, Bo Ma, Masahiro Ogihara, Rebecca Oppenheimer, S. J. O'Toole, Stephen A. Shectman, Robert A. Wittenmyer, Sharon X. Wang, D. J. Wright, Yifan Xuan
Figure caption: Similar to Figure 4, but for other targets.
Paper: The Velocity Map Asymmetry of Ionized Gas in MaNGA. I. The Catalog and General Properties
Authors: Shuai Feng, 帅 冯, Shi-Yin Shen, 世银 沈, Fang-Ting Yuan, 方婷 袁, Y. Sophia Dai, 昱 戴, Karen L. Masters
Figure caption: Left: dependency of the ﹩\mathrm{log}{M}_{\star }﹩–﹩\mathrm{log}{\bar{v}}_{\mathrm{asym}}﹩ relation on redshift. The color-coded symbols represent the subsamples defined by redshifts. Right: dependency of the ﹩\mathrm{log}{M}_{\star }﹩–﹩\mathrm{log}{\bar{v}}_{\mathrm{asym}}﹩ relation on inclination angle. The red circles represent edge-on-like galaxies with P edge > 0.5 and P disk > 0.5; the blue squares represent face-on-like galaxies with P edge < 0.5 and P disk > 0.5.
Paper: The Velocity Map Asymmetry of Ionized Gas in MaNGA. I. The Catalog and General Properties
Authors: Shuai Feng, 帅 冯, Shi-Yin Shen, 世银 沈, Fang-Ting Yuan, 方婷 袁, Y. Sophia Dai, 昱 戴, Karen L. Masters
Figure caption: The case of dusty edge-on galaxy 9040−12701. The panels from left to right are the SDSS image, E(B − V) map, and Hα velocity map. The gray contours in the velocity map represent the E(B − V) distribution.
Paper: SWASTi-SW: Space Weather Adaptive Simulation Framework for Solar Wind and Its Relevance to the Aditya-L1 Mission
Authors: Prateek Mayank, Bhargav Vaidya, D. Chakrabarty
Figure caption: Variation of solar wind speed for the range of values of d and f  s  based on a different set of values of β and w while keeping V min and V max constant (240 and 725 km s−1). d varies from 0° to 12°, and the value of f  s  goes from 1 (green at top) to 99 (red at bottom) with increments of 1. The dotted vertical lines are placed corresponding to values of w. For β = 2, ﹩{V}_{{R}_{\mathrm{in}}}﹩ becomes independent of d at a much smaller value as compared to the β = 1 case.
Paper: SWASTi-SW: Space Weather Adaptive Simulation Framework for Solar Wind and Its Relevance to the Aditya-L1 Mission
Authors: Prateek Mayank, Bhargav Vaidya, D. Chakrabarty
Figure caption: Graphical depiction of solar wind speed variation with different values of β at 0.1 au for CR2081. Speed profiles are of those field lines that reach sub-Earth points (location of Earth in Carrington heliographic coordinates). Here, ﹩{V}_{\min }=240\,\mathrm{km}\,{{\rm{s}}}^{-1}﹩, ﹩{V}_{\max }=725\,\mathrm{km}\,{{\rm{s}}}^{-1}﹩, and w = 0.54 (median of d  E ). For each field line, values of d  E  and ﹩{f}_{{s}_{E}}﹩ are calculated from the coronal model, and the vertical dotted line represents the value of w. ﹩{f}_{{s}_{E}}﹩ has been distributed in three equal bins (green, blue, and red), with green showing the lowest (from top) and red showing the largest values (at bottom).
Paper: SWASTi-SW: Space Weather Adaptive Simulation Framework for Solar Wind and Its Relevance to the Aditya-L1 Mission
Authors: Prateek Mayank, Bhargav Vaidya, D. Chakrabarty
Figure caption: Plots showing the statistical results for variation of β from 0.75 to 1.75 in 20 equal steps, for five selected CRs. On the basis of the minimum score value, the optimum β value has been deduced. The chosen optimum for each CR has been marked with a cross, whose values have been mentioned in Table 1. All panels have a common plot legend, shown in panel (a).
Paper: SWASTi-SW: Space Weather Adaptive Simulation Framework for Solar Wind and Its Relevance to the Aditya-L1 Mission
Authors: Prateek Mayank, Bhargav Vaidya, D. Chakrabarty
Figure caption: PFSS model results for CR2081. Panel (a) is the computed radial magnetic field (Gauss) at 1 R ⊙, panel (b) is the radial magnetic field (Gauss) output at 2.5 R ⊙, and panel (c) is the tracing of field lines from solar to source surface that will reach sub-Earth points. Here cyan/orange and light/dark gray shows the open and closed field lines of opposite polarity. The green area is the coronal hole, and red circles are the footpoints of open field lines. The horizontal black line is the location of Earth in heliographic coordinates for CR2081.
Paper: SWASTi-SW: Space Weather Adaptive Simulation Framework for Solar Wind and Its Relevance to the Aditya-L1 Mission
Authors: Prateek Mayank, Bhargav Vaidya, D. Chakrabarty
Figure caption: Process flow diagram of the proposed solar wind model showing the range of numerical models involved in the subdomains.
Paper: A Dynamic Deep-learning Model for Generating a Magnetogram Sequence from an SDO/AIA EUV Image Sequence
Authors: Wenqing Sun, Long Xu, Suli Ma, Yihua Yan, Tie Liu, Weiqiang Zhang
Figure caption: Subjective comparison among the ground truth, our model, multichannel pix2pix, and pix2pix baseline. (Magnetogram difference describes the difference between two consecutive frames of an AR sequence. It is illustrated by a color map. To better characterize the morphological similarity between the color maps of real observed data and generated ones from different models, pixel-to-pixel correlation coefficient (cc) between two compared color maps is computed and labeled accordingly.)
Paper: Mining S-PLUS for Metal-poor Stars in the Milky Way
Authors: Vinicius M. Placco, Felipe Almeida-Fernandes, Anke Arentsen, Young Sun Lee, William Schoenell, Tiago Ribeiro, Antonio Kanaan
Figure caption: Left panel: stellar density for the selected S-PLUS DR3 sample in a color–color diagram. The red box outlines the color window for the spectroscopic follow-up (see the text for details). The inset (bottom right panel) shows the crossmatch with the SDSS/SEGUE spectroscopic database, color-coded by the average metallicity in each bin. The number of stars in each bin is also shown. Top right panel: S-PLUS transmission curves for the six narrowband and broadband filters used in this selection.
Paper: Mining S-PLUS for Metal-poor Stars in the Milky Way
Authors: Vinicius M. Placco, Felipe Almeida-Fernandes, Anke Arentsen, Young Sun Lee, William Schoenell, Tiago Ribeiro, Antonio Kanaan
Figure caption: Color–color diagram for three different [Fe/H] regimes. The bins in each panel are color-coded by the fraction of stars with an average metallicity in a given range. The number of stars in each bin is also shown.
Paper: Mining S-PLUS for Metal-poor Stars in the Milky Way
Authors: Vinicius M. Placco, Felipe Almeida-Fernandes, Anke Arentsen, Young Sun Lee, William Schoenell, Tiago Ribeiro, Antonio Kanaan
Figure caption: Absolute carbon, (A(C), corrected as described in the text; left panel), and α-element abundance ratios, [α/Fe] (right panel), as a function of the metallicity calculated by the n-SSPP. The side and bottom panels show the marginal distributions. The solid line in the bottom left panel shows the cumulative CEMP fractions for the stars with −3.5 ≤ [Fe/H] ≤ −1.0 and the numbers on the top part of the panel are the differential fractions for 0.5 dex [Fe/H] bins. Point sizes are proportional to T eff.
Paper: Mining S-PLUS for Metal-poor Stars in the Milky Way
Authors: Vinicius M. Placco, Felipe Almeida-Fernandes, Anke Arentsen, Young Sun Lee, William Schoenell, Tiago Ribeiro, Antonio Kanaan
Figure caption: Surface gravity vs. T eff diagram for the program stars, using the parameters calculated by the n-SSPP, listed in Table 3. Typical uncertainties are shown for reference. The point size is inversely proportional to the metallicity. Also shown are the YY Isochrones (12 Gyr, 0.8 M ⊙, [α/Fe] = +0.4; Demarque et al. 2004) for [Fe/H] = −1.0, −2.0, and −3.0, and horizontal-branch tracks from Dotter et al. (2008).
Paper: Mining S-PLUS for Metal-poor Stars in the Milky Way
Authors: Vinicius M. Placco, Felipe Almeida-Fernandes, Anke Arentsen, Young Sun Lee, William Schoenell, Tiago Ribeiro, Antonio Kanaan
Figure caption: Spectral energy distribution (SED) for 20 selected program stars from Blanco and Gemini. Magnitudes were scaled to zSDSS = 14.9 (top) and 16.4 (bottom). The temperature range for each set is displayed right below the SEDs. The insets show the observed spectra around the Hβ and Ca II HK absorption features, sorted by their J0395 scaled magnitude. Also shown are the T eff and [Fe/H] for each star and the S-PLUS transmission curves. See the text for further details.
Paper: Mining S-PLUS for Metal-poor Stars in the Milky Way
Authors: Vinicius M. Placco, Felipe Almeida-Fernandes, Anke Arentsen, Young Sun Lee, William Schoenell, Tiago Ribeiro, Antonio Kanaan
Figure caption: Metallicity histogram for the program stars (top panel), compared with the distributions from Placco et al. (2018, 2019) and Limberg et al. (2021b) (middle panels). Each panel shows the total number of stars and the fractions for different metallicity regimes. The bottom panel shows the cumulative distribution functions (CDFs) for the three samples, marking the [Fe/H] value for which they reach 80%.
Paper: Mining S-PLUS for Metal-poor Stars in the Milky Way
Authors: Vinicius M. Placco, Felipe Almeida-Fernandes, Anke Arentsen, Young Sun Lee, William Schoenell, Tiago Ribeiro, Antonio Kanaan
Figure caption: Top: Galactic coordinates for the stars observed in this work, color coded by telescope. The point size is proportional to the g magnitude. The gray line traces the celestial equator. The dust map uses reddening values from Schlegel et al. (1998). Bottom: magnitude distribution of the observed stars in the 12-filter system of S-PLUS. Each panel also shows the name, transmission curve, and central wavelength (in angstroms) for the filters.
Paper: Mining S-PLUS for Metal-poor Stars in the Milky Way
Authors: Vinicius M. Placco, Felipe Almeida-Fernandes, Anke Arentsen, Young Sun Lee, William Schoenell, Tiago Ribeiro, Antonio Kanaan
Figure caption: S-PLUS color–color diagram for S-PLUS DR3 (light blue filled squares), SDSS/SEGUE crossmatch (divided in four metallicity intervals), and the stars observed in this work (dark blue filled squares, with point sizes inversely proportional to the metallicity). The gray rectangle outlines the selection window for the spectroscopic follow-up, described in the text. Also shown is SPLUS J2104−0049, an ultra metal-poor star identified in S-PLUS by Placco et al. (2021).
Paper: Mining S-PLUS for Metal-poor Stars in the Milky Way
Authors: Vinicius M. Placco, Felipe Almeida-Fernandes, Anke Arentsen, Young Sun Lee, William Schoenell, Tiago Ribeiro, Antonio Kanaan
Figure caption: Example spectra for 100 program stars observed with Blanco (left panel) and Gemini South (right panel), sorted by decreasing metallicity. The shaded areas highlight absorption features of interest for the determination of the stellar parameters and chemical abundances (see the text for details). Also shown are the values calculated by the n-SSPP, as well as the S-PLUS filters that probe such features, with the exception of Hγ and Hβ.
Paper: SWASTi-SW: Space Weather Adaptive Simulation Framework for Solar Wind and Its Relevance to the Aditya-L1 Mission
Authors: Prateek Mayank, Bhargav Vaidya, D. Chakrabarty
Figure caption: Plots showing the features of plasma properties at L1 corresponding to SIR for CR2081. Panel (a) represents the computed plasma properties at the L1 location, whereas panel (b) represents the mass-averaged properties at L1. The shaded region (S’ and F) shows the SIR where in the S’ region (between red and green dotted vertical lines) solar wind is getting accelerated and in the F region (between green and red dotted vertical lines) plasma is getting decelerated. V  r  and V  ϕ  are plasma velocity in radial and azimuthal direction in km s−1. ∣B∣ and ρ are IMF magnitude (nT) and proton density (N  p  cc−1). Panel (a5) shows the variation of flow angle in degree. ﹩{({V}_{r})}_{\mathrm{avg}}﹩ and ﹩{({V}_{\phi })}_{\mathrm{avg}}﹩ are averaged values of V  r  and V  ϕ  (km s−1). ﹩{(\rho {V}_{r})}_{\mathrm{avg}}﹩, ﹩{(\rho {V}_{\theta })}_{\mathrm{avg}}﹩, and ﹩{(\rho {V}_{\phi })}_{\mathrm{avg}}﹩ are averaged proton flux (N  p  cm−3 s−1) in radial, meridional, and azimuthal directions. The x-axis, longitude, is flipped Carrington longitude, as in Figures 9 and 10.
Paper: SWASTi-SW: Space Weather Adaptive Simulation Framework for Solar Wind and Its Relevance to the Aditya-L1 Mission
Authors: Prateek Mayank, Bhargav Vaidya, D. Chakrabarty
Figure caption: Schematic diagrams of RAE of (a) THA-1, (b) THA-2 of SWIS-ASPEX, and (c) the computational surfaces (A, B, and C) covering the openings of detectors. Computational surfaces A and B cover the THA-1, and C covers the THA-2. In panel (c), the solid eclipse represents the equatorial plane in the Sun-centered frame, and the dotted eclipse is the ecliptic plane. The directions of unit vectors in the ecliptic plane have been shown, and dr, d θ, and d ϕ are widths of computational surfaces along those directions.
Paper: SWASTi-SW: Space Weather Adaptive Simulation Framework for Solar Wind and Its Relevance to the Aditya-L1 Mission
Authors: Prateek Mayank, Bhargav Vaidya, D. Chakrabarty
Figure caption: Plots showing the comparison of plasma properties with the OMNI data at L1 for different values of specific heat ratio, γ. The results shown here are for CR2081, and the value used in this work is shown in blue (γ = 5/3). The Pearson cc and rmse are shown for MHDGONG with γ = 5/3.
Paper: SWASTi-SW: Space Weather Adaptive Simulation Framework for Solar Wind and Its Relevance to the Aditya-L1 Mission
Authors: Prateek Mayank, Bhargav Vaidya, D. Chakrabarty
Figure caption: Plasma speed profile at L1 for mentioned CRs. For CR2053, CR2077, CR2081, and CR2022 MHD (using GONG magnetogram) and HUX results are plotted along with the per-hour averaged OMNI data. For CR2104, additionally MHDHMI (using HMI magnetogram) have been plotted along with MHD (using GONG), HUX, and OMNI data. The Pearson cc and rmse have been shown for MHDGONG results, which are in blue.
Paper: SWASTi-SW: Space Weather Adaptive Simulation Framework for Solar Wind and Its Relevance to the Aditya-L1 Mission
Authors: Prateek Mayank, Bhargav Vaidya, D. Chakrabarty
Figure caption: Plots for CR2081: (a) d parameter in degrees; (b) ﹩{\mathrm{log}}_{10}({f}_{s})﹩; (c) radial magnetic field (nT) at R in, derived from Equation (10); and (d) solar wind speed (km s−1) profile as input for the MHD domain.
Paper: SWASTi-SW: Space Weather Adaptive Simulation Framework for Solar Wind and Its Relevance to the Aditya-L1 Mission
Authors: Prateek Mayank, Bhargav Vaidya, D. Chakrabarty
Figure caption: Effect of value of β on speed profile at 1 au. The difference in speed is greater at peaks and lesser at the base. The speed profile has smoother peaks for low values of β.
Paper: Integrated Geostationary Solar Energetic Particle Events Catalog: GSEP
Authors: Sumanth Rotti, Berkay Aydin, Manolis K. Georgoulis, Petrus C. Martens
Figure caption: Histograms of rise times (i.e., times elapsed between onset and peak flux) for the GSEP events. Shown are numbers of SEP events vs. their rise times, classified in bins of 0–3, 3–6, 6–12, 12–24, 24–48, 48–72, and >72 hr. Weak enhancements (<10 pfu for protons >10 MeV) and events above the NOAA S1 scale are included in (a)–(c) for SCs 22, 23, and 24, respectively.
Paper: Integrated Geostationary Solar Energetic Particle Events Catalog: GSEP
Authors: Sumanth Rotti, Berkay Aydin, Manolis K. Georgoulis, Petrus C. Martens
Figure caption: Time-series profiles of GSEP event 182 in (a) and event 183 in (b). The first SEP event was due to an X1.1 flare and a CME (2001 April 2 10:58:00), while the second event was triggered due to an X20 flare (2001 April 2 21:32:00) and a CME erupted after 6 minutes. Both events originated from NOAA AR 9393.
Paper: Integrated Geostationary Solar Energetic Particle Events Catalog: GSEP
Authors: Sumanth Rotti, Berkay Aydin, Manolis K. Georgoulis, Petrus C. Martens
Figure caption: Distribution of the absolute percentage differences classified in bins of 0–25, 25–50, and >50% in the peak proton fluxes between GSEP and (a) PSEP, (b) CDAW-SEP, and (c) NOAA-SEP.
Paper: A Bayesian Analysis of Physical Parameters for 783 Kepler Close Binaries: Extreme-mass-ratio Systems and a New Mass Ratio versus Period Lower Limit
Authors: Henry A. Kobulnicky, Lawrence A. Molnar, Evan M. Cook, Lauren E. Henderson
Figure caption: Grid of model light curves for four selected values of i (rows from top to bottom), f (columns from left to right), and q (colors) as indicated by labels within the panels. In all cases, the third-light fraction l3 = 0 and T 1 = T 2.
Paper: A Bayesian Analysis of Physical Parameters for 783 Kepler Close Binaries: Extreme-mass-ratio Systems and a New Mass Ratio versus Period Lower Limit
Authors: Henry A. Kobulnicky, Lawrence A. Molnar, Evan M. Cook, Lauren E. Henderson
Figure caption: Broadening function of KIC04853067 (black dots) showing a single peak with a small velocity difference between the two epochs. Red curves depict two Gaussian components fit to the data, while the blue curve is the sum of those components. Green x’s show the theoretical line profile generated by PHOEBE for the best-fitting contact binary system parameters as convolved with the instrumental spectral profile. The normalization of both curves is arbitrary. The stellar components are viewed at low i and are unresolved. The BF may be dominated by a third component that is not represented in the model line profile function. This system may also be a detached configuration.
Paper: A Bayesian Analysis of Physical Parameters for 783 Kepler Close Binaries: Extreme-mass-ratio Systems and a New Mass Ratio versus Period Lower Limit
Authors: Henry A. Kobulnicky, Lawrence A. Molnar, Evan M. Cook, Lauren E. Henderson
Figure caption:  O − C eclipse timing residuals of KIC04853067. The red curve is the best parabolic (constant period derivative) fit to the data, while the green dashed curve is the best sine function (periodic) fit.
Paper: A Bayesian Analysis of Physical Parameters for 783 Kepler Close Binaries: Extreme-mass-ratio Systems and a New Mass Ratio versus Period Lower Limit
Authors: Henry A. Kobulnicky, Lawrence A. Molnar, Evan M. Cook, Lauren E. Henderson
Figure caption: Distribution of orbital period, effective temperature, light-curve shape morphology parameter, and primary eclipse depth for binary stars in the Kepler field (Kirk et al. 2016; black points) and our ten targets (red stars).
Paper: A Bayesian Analysis of Physical Parameters for 783 Kepler Close Binaries: Extreme-mass-ratio Systems and a New Mass Ratio versus Period Lower Limit
Authors: Henry A. Kobulnicky, Lawrence A. Molnar, Evan M. Cook, Lauren E. Henderson
Figure caption: PHOEBE model light curves for contact binaries with f = 0.5, i = 60°, two different mass ratios (indicated by line style), and three different third-light fractions (indicated by color). Modest mass ratios with substantial third light closely resemble more extreme mass ratios with minimal third light.
Paper: A Bayesian Analysis of Physical Parameters for 783 Kepler Close Binaries: Extreme-mass-ratio Systems and a New Mass Ratio versus Period Lower Limit
Authors: Henry A. Kobulnicky, Lawrence A. Molnar, Evan M. Cook, Lauren E. Henderson
Figure caption: Folded Kepler light curve of KIC04853067 and mean light-curve shape (red curve) generated from the sum of low-order Fourier coefficients, as labeled. Only a fraction of the Kepler data are plotted, here and subsequently, to reduce figure file size and improve clarity.
Paper: A Bayesian Analysis of Physical Parameters for 783 Kepler Close Binaries: Extreme-mass-ratio Systems and a New Mass Ratio versus Period Lower Limit
Authors: Henry A. Kobulnicky, Lawrence A. Molnar, Evan M. Cook, Lauren E. Henderson
Figure caption: Depiction of the Roche surfaces for four q = 0.25 systems having fillout factors f = [0.05, 0.35, 0.65, 0.99].
Paper: A Bayesian Analysis of Physical Parameters for 783 Kepler Close Binaries: Extreme-mass-ratio Systems and a New Mass Ratio versus Period Lower Limit
Authors: Henry A. Kobulnicky, Lawrence A. Molnar, Evan M. Cook, Lauren E. Henderson
Figure caption: Light curve and velocity curve of KIC09164694 along with three competing model light curves and velocity curves. Both the T 2/T 1 = 1 model and the spotted model reproduce the observed component velocities, while the best-fitting variable-temperature-ratio model yields a mass ratios that is inconsistent with the kinematic data.
Paper: A Bayesian Analysis of Physical Parameters for 783 Kepler Close Binaries: Extreme-mass-ratio Systems and a New Mass Ratio versus Period Lower Limit
Authors: Henry A. Kobulnicky, Lawrence A. Molnar, Evan M. Cook, Lauren E. Henderson
Figure caption: Three competing contact binary models for KIC09345838 in comparison to the data. As in KIC09164694, the variable-temperature-ratio model yields an incorrect mass ratio, while the fixed-temperature-ratio models yield q ≈ 0.24, in agreement with the kinematic data.
Paper: A Bayesian Analysis of Physical Parameters for 783 Kepler Close Binaries: Extreme-mass-ratio Systems and a New Mass Ratio versus Period Lower Limit
Authors: Henry A. Kobulnicky, Lawrence A. Molnar, Evan M. Cook, Lauren E. Henderson
Figure caption: Posterior probability distributions for combinations of four free parameters in the KIC09345838 system. The most probable q of 0.14 provides a good match to the kinematic data. Like KIC09164694 there is some degeneracy between q and l3.
Paper: A Bayesian Analysis of Physical Parameters for 783 Kepler Close Binaries: Extreme-mass-ratio Systems and a New Mass Ratio versus Period Lower Limit
Authors: Henry A. Kobulnicky, Lawrence A. Molnar, Evan M. Cook, Lauren E. Henderson
Figure caption: Broadening function and model line profile function of KIC09345838.
Paper: A Bayesian Analysis of Physical Parameters for 783 Kepler Close Binaries: Extreme-mass-ratio Systems and a New Mass Ratio versus Period Lower Limit
Authors: Henry A. Kobulnicky, Lawrence A. Molnar, Evan M. Cook, Lauren E. Henderson
Figure caption: Probability distribution for combinations of eight free system parameters for the KIC09164694 system. Even with the additional free parameters entailed by a spot and T 2 < T 1, the Monte Carlo simulations provide a well-constrained measure of the q that is consistent with the spectroscopic data.
Paper: A Bayesian Analysis of Physical Parameters for 783 Kepler Close Binaries: Extreme-mass-ratio Systems and a New Mass Ratio versus Period Lower Limit
Authors: Henry A. Kobulnicky, Lawrence A. Molnar, Evan M. Cook, Lauren E. Henderson
Figure caption:  O − C eclipse timing residuals of KIC09164694. The red solid and green dashed curves depict a parabolic and a sine fit to the data, respectively, either of which provide an approximate match.
Paper: A Bayesian Analysis of Physical Parameters for 783 Kepler Close Binaries: Extreme-mass-ratio Systems and a New Mass Ratio versus Period Lower Limit
Authors: Henry A. Kobulnicky, Lawrence A. Molnar, Evan M. Cook, Lauren E. Henderson
Figure caption: Probability distribution for combinations of four free system parameters for the KIC09164694 system. Despite the asymmetric light curve modeled here as a spot with three free parameters, the constraints on mass ratio and inclination are strong.