adsabs/AstroCLIMB huggingface dataset:
Paper: A Testbed for Tidal Migration: The 3D Architecture of an Eccentric Hot Jupiter HD 118203 b Accompanied by a Possibly Aligned Outer Giant Planet
Authors: Jingwen Zhang, 婧雯 张, Daniel Huber, Lauren M. Weiss, Jerry W. Xuan, Jennifer A. Burt, Fei Dai, Nicholas Saunders, Erik A. Petigura, Ryan A. Rubenzahl, Joshua N. Winn, Sharon X. Wang, Judah Van Zandt, Max Brodheim, Zachary R. Claytor, Ian Crossfield, William Deich, Benjamin J. Fulton, Steven R. Gibson, Samuel Halverson, Grant M. Hill, Bradford Holden, Aaron Householder, Andrew W. Howard, Howard Isaacson, Stephen Kaye, Kyle Lanclos, Russ R. Laher, 嶺亞 良主, Jack Lubin, Joel Payne, Arpita Roy, Christian Schwab, Abby P. Shaum, Josh Walawender, Edward Wishnow, Sherry Yeh
Figure caption: Best-fit two-planet Keplerian orbital model for HD 118203. Panel (a): HD 118203 RVs with errors (black) and their best-fit model (blue) as a function of time. Panel (b): the residuals. Panels (c) and (d): RV data and models for each planet phase-folded at the best-fit orbital period with all other planets’ signals removed.
Paper: A Testbed for Tidal Migration: The 3D Architecture of an Eccentric Hot Jupiter HD 118203 b Accompanied by a Possibly Aligned Outer Giant Planet
Authors: Jingwen Zhang, 婧雯 张, Daniel Huber, Lauren M. Weiss, Jerry W. Xuan, Jennifer A. Burt, Fei Dai, Nicholas Saunders, Erik A. Petigura, Ryan A. Rubenzahl, Joshua N. Winn, Sharon X. Wang, Judah Van Zandt, Max Brodheim, Zachary R. Claytor, Ian Crossfield, William Deich, Benjamin J. Fulton, Steven R. Gibson, Samuel Halverson, Grant M. Hill, Bradford Holden, Aaron Householder, Andrew W. Howard, Howard Isaacson, Stephen Kaye, Kyle Lanclos, Russ R. Laher, 嶺亞 良主, Jack Lubin, Joel Payne, Arpita Roy, Christian Schwab, Abby P. Shaum, Josh Walawender, Edward Wishnow, Sherry Yeh
Figure caption: The Rossiter–McLaughlin (RM) model for HD 118203 b without GP for oscillation, integrating a global fitting of photometric data, nontransit radial velocity (RV) measurements, and RM data during transit. Panel (a): TESS SPOC light curves phase-folded to the best-fit orbital period of HD 118203 b. The pink points represent the TESS data binned every 15 minutes, and the red line shows the best-fit transit model. Panel (b): the out-of-transit RVs from ELODIE (green) and HIRES (orange) phase-folded to the best-fit orbital period of HD 118203 b. The red line depicts the best-fit RV model. Panel (c): the in-transit RVs from KPF (blue) and best-fit RM model (red). Panel (d): the residuals of the fitting. The residuals show periodic patterns that could come from the oscillation of the star.
Paper: A Testbed for Tidal Migration: The 3D Architecture of an Eccentric Hot Jupiter HD 118203 b Accompanied by a Possibly Aligned Outer Giant Planet
Authors: Jingwen Zhang, 婧雯 张, Daniel Huber, Lauren M. Weiss, Jerry W. Xuan, Jennifer A. Burt, Fei Dai, Nicholas Saunders, Erik A. Petigura, Ryan A. Rubenzahl, Joshua N. Winn, Sharon X. Wang, Judah Van Zandt, Max Brodheim, Zachary R. Claytor, Ian Crossfield, William Deich, Benjamin J. Fulton, Steven R. Gibson, Samuel Halverson, Grant M. Hill, Bradford Holden, Aaron Householder, Andrew W. Howard, Howard Isaacson, Stephen Kaye, Kyle Lanclos, Russ R. Laher, 嶺亞 良主, Jack Lubin, Joel Payne, Arpita Roy, Christian Schwab, Abby P. Shaum, Josh Walawender, Edward Wishnow, Sherry Yeh
Figure caption: Panel (a): the periodogram of RV residuals computed using RVsearch. The signal from the hot Jupiter HD 118203 b has been subtracted. The blue line corresponds to the periodogram using all RVs. The black line corresponds to the periodogram using only HIRES RVs. Panel (b): the periodogram of HIRES S HK index.
Paper: A Testbed for Tidal Migration: The 3D Architecture of an Eccentric Hot Jupiter HD 118203 b Accompanied by a Possibly Aligned Outer Giant Planet
Authors: Jingwen Zhang, 婧雯 张, Daniel Huber, Lauren M. Weiss, Jerry W. Xuan, Jennifer A. Burt, Fei Dai, Nicholas Saunders, Erik A. Petigura, Ryan A. Rubenzahl, Joshua N. Winn, Sharon X. Wang, Judah Van Zandt, Max Brodheim, Zachary R. Claytor, Ian Crossfield, William Deich, Benjamin J. Fulton, Steven R. Gibson, Samuel Halverson, Grant M. Hill, Bradford Holden, Aaron Householder, Andrew W. Howard, Howard Isaacson, Stephen Kaye, Kyle Lanclos, Russ R. Laher, 嶺亞 良主, Jack Lubin, Joel Payne, Arpita Roy, Christian Schwab, Abby P. Shaum, Josh Walawender, Edward Wishnow, Sherry Yeh
Figure caption: Eccentricity vs. spin–orbit angle of HD 118203 b in comparison to other hot Jupiters (P < 10 days) from M. Rice et al. (2022). HD 118203 b is one of few systems where the mutual inclinations between the hot Jupiters and outer planets have been directly measured. The colors denote the effective temperature of the host star.
Paper: A Testbed for Tidal Migration: The 3D Architecture of an Eccentric Hot Jupiter HD 118203 b Accompanied by a Possibly Aligned Outer Giant Planet
Authors: Jingwen Zhang, 婧雯 张, Daniel Huber, Lauren M. Weiss, Jerry W. Xuan, Jennifer A. Burt, Fei Dai, Nicholas Saunders, Erik A. Petigura, Ryan A. Rubenzahl, Joshua N. Winn, Sharon X. Wang, Judah Van Zandt, Max Brodheim, Zachary R. Claytor, Ian Crossfield, William Deich, Benjamin J. Fulton, Steven R. Gibson, Samuel Halverson, Grant M. Hill, Bradford Holden, Aaron Householder, Andrew W. Howard, Howard Isaacson, Stephen Kaye, Kyle Lanclos, Russ R. Laher, 嶺亞 良主, Jack Lubin, Joel Payne, Arpita Roy, Christian Schwab, Abby P. Shaum, Josh Walawender, Edward Wishnow, Sherry Yeh
Figure caption: The joint posterior distributions for orbital inclination I  c , mass m  c , and semimajor axis a  c  of HD 118203 c from combined fitting of RV and Hipparcos-Gaia astrometric acceleration. Moving outward, the dashed lines on the corner plots correspond to 1σ, 2σ, and 3σ contours. The orange dashed lines in the 1D distribution denote mean values with 1σ interval.
Paper: A Testbed for Tidal Migration: The 3D Architecture of an Eccentric Hot Jupiter HD 118203 b Accompanied by a Possibly Aligned Outer Giant Planet
Authors: Jingwen Zhang, 婧雯 张, Daniel Huber, Lauren M. Weiss, Jerry W. Xuan, Jennifer A. Burt, Fei Dai, Nicholas Saunders, Erik A. Petigura, Ryan A. Rubenzahl, Joshua N. Winn, Sharon X. Wang, Judah Van Zandt, Max Brodheim, Zachary R. Claytor, Ian Crossfield, William Deich, Benjamin J. Fulton, Steven R. Gibson, Samuel Halverson, Grant M. Hill, Bradford Holden, Aaron Householder, Andrew W. Howard, Howard Isaacson, Stephen Kaye, Kyle Lanclos, Russ R. Laher, 嶺亞 良主, Jack Lubin, Joel Payne, Arpita Roy, Christian Schwab, Abby P. Shaum, Josh Walawender, Edward Wishnow, Sherry Yeh
Figure caption: Three-dimensional orbit characterization of the outer giant planet around HD 118203 using RVs and Hipparcos-Gaia astrometric acceleration. Panels (a) and (b): observed and fitted Hipparcos and Gaia proper motion of HD 118203 in R.A. and decl. Panel (c): astrometric orbits of HD 118203 c projected on the sky plane from our model. In all of the above panels, the thicker black lines represent the best-fit orbit in the MCMC chain while the other 100 blue lines represent random draws from the chain.
Paper: A Testbed for Tidal Migration: The 3D Architecture of an Eccentric Hot Jupiter HD 118203 b Accompanied by a Possibly Aligned Outer Giant Planet
Authors: Jingwen Zhang, 婧雯 张, Daniel Huber, Lauren M. Weiss, Jerry W. Xuan, Jennifer A. Burt, Fei Dai, Nicholas Saunders, Erik A. Petigura, Ryan A. Rubenzahl, Joshua N. Winn, Sharon X. Wang, Judah Van Zandt, Max Brodheim, Zachary R. Claytor, Ian Crossfield, William Deich, Benjamin J. Fulton, Steven R. Gibson, Samuel Halverson, Grant M. Hill, Bradford Holden, Aaron Householder, Andrew W. Howard, Howard Isaacson, Stephen Kaye, Kyle Lanclos, Russ R. Laher, 嶺亞 良主, Jack Lubin, Joel Payne, Arpita Roy, Christian Schwab, Abby P. Shaum, Josh Walawender, Edward Wishnow, Sherry Yeh
Figure caption: Left panel: the stellar evolution models fit to HD 118203, and traces back to their zero-age main-sequence location. Right panel: the mass fraction of hydrogen, helium, and carbon in the core of the star from the evolution models. At the estimated stellar age, the hydrogen has just been used up and the star evolved to subgiant.
Paper: A Testbed for Tidal Migration: The 3D Architecture of an Eccentric Hot Jupiter HD 118203 b Accompanied by a Possibly Aligned Outer Giant Planet
Authors: Jingwen Zhang, 婧雯 张, Daniel Huber, Lauren M. Weiss, Jerry W. Xuan, Jennifer A. Burt, Fei Dai, Nicholas Saunders, Erik A. Petigura, Ryan A. Rubenzahl, Joshua N. Winn, Sharon X. Wang, Judah Van Zandt, Max Brodheim, Zachary R. Claytor, Ian Crossfield, William Deich, Benjamin J. Fulton, Steven R. Gibson, Samuel Halverson, Grant M. Hill, Bradford Holden, Aaron Householder, Andrew W. Howard, Howard Isaacson, Stephen Kaye, Kyle Lanclos, Russ R. Laher, 嶺亞 良主, Jack Lubin, Joel Payne, Arpita Roy, Christian Schwab, Abby P. Shaum, Josh Walawender, Edward Wishnow, Sherry Yeh
Figure caption: Joint posterior distributions for 27 parameters used in the nested sampling fitting of the RM effect with SHO GP to account for stellar oscillation. The values and histogram distributions of all parameters are shown, along with 1σ uncertainties.
Paper: A Testbed for Tidal Migration: The 3D Architecture of an Eccentric Hot Jupiter HD 118203 b Accompanied by a Possibly Aligned Outer Giant Planet
Authors: Jingwen Zhang, 婧雯 张, Daniel Huber, Lauren M. Weiss, Jerry W. Xuan, Jennifer A. Burt, Fei Dai, Nicholas Saunders, Erik A. Petigura, Ryan A. Rubenzahl, Joshua N. Winn, Sharon X. Wang, Judah Van Zandt, Max Brodheim, Zachary R. Claytor, Ian Crossfield, William Deich, Benjamin J. Fulton, Steven R. Gibson, Samuel Halverson, Grant M. Hill, Bradford Holden, Aaron Householder, Andrew W. Howard, Howard Isaacson, Stephen Kaye, Kyle Lanclos, Russ R. Laher, 嶺亞 良主, Jack Lubin, Joel Payne, Arpita Roy, Christian Schwab, Abby P. Shaum, Josh Walawender, Edward Wishnow, Sherry Yeh
Figure caption: Joint posterior distributions for 24 parameters used in the nested sampling fitting of the RM effect without oscillation. The values and histogram distributions of all parameters are shown, along with 1σ uncertainties.
Paper: A Testbed for Tidal Migration: The 3D Architecture of an Eccentric Hot Jupiter HD 118203 b Accompanied by a Possibly Aligned Outer Giant Planet
Authors: Jingwen Zhang, 婧雯 张, Daniel Huber, Lauren M. Weiss, Jerry W. Xuan, Jennifer A. Burt, Fei Dai, Nicholas Saunders, Erik A. Petigura, Ryan A. Rubenzahl, Joshua N. Winn, Sharon X. Wang, Judah Van Zandt, Max Brodheim, Zachary R. Claytor, Ian Crossfield, William Deich, Benjamin J. Fulton, Steven R. Gibson, Samuel Halverson, Grant M. Hill, Bradford Holden, Aaron Householder, Andrew W. Howard, Howard Isaacson, Stephen Kaye, Kyle Lanclos, Russ R. Laher, 嶺亞 良主, Jack Lubin, Joel Payne, Arpita Roy, Christian Schwab, Abby P. Shaum, Josh Walawender, Edward Wishnow, Sherry Yeh
Figure caption: Joint posterior distributions for 18 parameters used in the MCMC fitting for the 3D orbits of the outer planet HD 118203 c. The values and histogram distributions of all parameters are shown, along with 1σ uncertainties.
Paper: Search for Classical Cepheids in Galactic Open Clusters and Calibration of the Period–Wesenheit–Metallicity Relation in the Gaia Bands
Authors: Huajian Wang, Ye Xu, Zehao Lin, Chaojie Hao, Dejian Liu, Yingjie Li
Figure caption: Examples of the OCs (blue dots) harboring one or more DCEPs (red stars). The upper left, lower left, and middle images of each panels show their coordinates (α and δ), proper motion (﹩{\mu }_{{\alpha }^{* }}﹩ and μ  δ ) distribution, and the CMD, respectively. The blue histogram on the right shows the parallax distribution of the member stars, where the black solid line represents the mean parallax of the OC and the red dotted line represents the parallax of the DCEP. (a) An example of OC–DCEPs. (b) An example of rejected associations.
Paper: Search for Classical Cepheids in Galactic Open Clusters and Calibration of the Period–Wesenheit–Metallicity Relation in the Gaia Bands
Authors: Huajian Wang, Ye Xu, Zehao Lin, Chaojie Hao, Dejian Liu, Yingjie Li
Figure caption: Normalized histogram of parallax offset (Δϖ) estimated using our F+1O-mode PWZR. The orange curve represents the Gaussian kernel density estimation for this distribution. The red dashed line represents the highest probability density of Δϖ.
Paper: Search for Classical Cepheids in Galactic Open Clusters and Calibration of the Period–Wesenheit–Metallicity Relation in the Gaia Bands
Authors: Huajian Wang, Ye Xu, Zehao Lin, Chaojie Hao, Dejian Liu, Yingjie Li
Figure caption: Blue dots are the field DCEPs in Trentin et al. (2024). Red dots are our 42 F+1O-mode OC–DCEPs. The black line is the fitting result of our F+1O-mode PWR.
Paper: Search for Classical Cepheids in Galactic Open Clusters and Calibration of the Period–Wesenheit–Metallicity Relation in the Gaia Bands
Authors: Huajian Wang, Ye Xu, Zehao Lin, Chaojie Hao, Dejian Liu, Yingjie Li
Figure caption: Literature estimates of the zp in field DCEPs.
Paper: Search for Classical Cepheids in Galactic Open Clusters and Calibration of the Period–Wesenheit–Metallicity Relation in the Gaia Bands
Authors: Huajian Wang, Ye Xu, Zehao Lin, Chaojie Hao, Dejian Liu, Yingjie Li
Figure caption: The upper and lower corner plots represent the marginalized posterior distributions of the free parameters in PWR and PWZR, respectively. The vertical blue lines represent the median values, and the black dashed lines represent the 16th and 84th percentiles.
Paper: Search for Classical Cepheids in Galactic Open Clusters and Calibration of the Period–Wesenheit–Metallicity Relation in the Gaia Bands
Authors: Huajian Wang, Ye Xu, Zehao Lin, Chaojie Hao, Dejian Liu, Yingjie Li
Figure caption: PWR and PWZR fitting results from our OC–DCEPs. The color represents the value of metal abundance. The black dots in the two panels on the left are OC–DCEPs without literature metal abundances.
Paper: Scalable, Advanced Machine Learning Based Approaches for Stellar Flare Identification: Application to TESS Short-cadence Data and Analysis of a New Flare Catalog
Authors: Chia-Lung Lin, Dániel Apai, Mark S. Giampapa, Wing-Huen Ip
Figure caption: The illustration of the four classification characteristics in the flare light-curve profile. The blue horizontal dashed lines at the top and the bottom mark the peak amplitude (A  f ) and the ﹩\sigma ({F}_{{\mathrm{LC}}_{1}})﹩. The red horizontal dashed line represents the median flux of the light curve. The purple horizontal dashed line represents half of the peak amplitude. The highlighted areas separated by the purple line represent the regions under the curve used to calculate ED1 and ED2. The green vertical dashed lines from left to right mark the time positions of the flare start, peak, and end, with the impulsive rise and decay time intervals indicated by δ t 1 and δ t 2, respectively.
Paper: Scalable, Advanced Machine Learning Based Approaches for Stellar Flare Identification: Application to TESS Short-cadence Data and Analysis of a New Flare Catalog
Authors: Chia-Lung Lin, Dániel Apai, Mark S. Giampapa, Wing-Huen Ip
Figure caption: The ﹩{A}_{f}/\sigma ({F}_{{\mathrm{LC}}_{1}})﹩ distributions of the true (purple bars with blue edges) and false flares (orange bars) in our preclassified data set. The ﹩{A}_{f}/\sigma ({F}_{{\mathrm{LC}}_{1}})﹩ of true flares are generally greater than those of false flares and cover a broader range. The number or frequency of flares gradually declines as ﹩{A}_{f}/\sigma ({F}_{{\mathrm{LC}}_{1}})﹩ increases.
Paper: Scalable, Advanced Machine Learning Based Approaches for Stellar Flare Identification: Application to TESS Short-cadence Data and Analysis of a New Flare Catalog
Authors: Chia-Lung Lin, Dániel Apai, Mark S. Giampapa, Wing-Huen Ip
Figure caption: Example profiles of true (upper three panels) and false (lower three panels) flares. The estimated values of their four classification characteristics are displayed in Table 2. The dashed lines and highlighted areas in these panels represent the same properties described in Figure 1.
Paper: Scalable, Advanced Machine Learning Based Approaches for Stellar Flare Identification: Application to TESS Short-cadence Data and Analysis of a New Flare Catalog
Authors: Chia-Lung Lin, Dániel Apai, Mark S. Giampapa, Wing-Huen Ip
Figure caption: This illustration outlines our approach to estimating the rotation period of the stars. Panel (a) shows a short-cadence light curve of TIC 126803030 observed in TESS Sector 1. Panel (b) shows the phase curve (black) created by folding the light curve with a period of 0.42 days. The binned phase curve (yellow) is produced by averaging the normalized flux and the corresponding one standard deviation within the bins with a bin width of 0.005 phase. We fit the binned phase curve with a fifth-order Fourier series function (red curve) and calculate the the R-square of the fit model to evaluate the validity of the period. In this case, the R-square of the fit is 0.98. This period is estimated from the LS periodogram, shown in panel (c). The horizontal black dashed line represents the false alarm probability (FAP) threshold of 1%. The peaks with a FAP smaller than the threshold are marked with red crosses. The vertical red dashed line pinpoints the highest peak in the periodogram, which corresponds to a period of 0.42 days. Panel (d) is the ACF of the light curve. The vertical blue dashed line represents the best period of 0.41 days from the ACF, which is consistent with the result derived from the LS method with a <5% divergence. Given the high R-square value and the agreement between the LS and ACF methods, this period is considered a valid measurement.
Paper: Scalable, Advanced Machine Learning Based Approaches for Stellar Flare Identification: Application to TESS Short-cadence Data and Analysis of a New Flare Catalog
Authors: Chia-Lung Lin, Dániel Apai, Mark S. Giampapa, Wing-Huen Ip
Figure caption: The ﹩{A}_{f}/\sigma ({F}_{{\mathrm{LC}}_{1}})﹩ relationships with δ t (left panel), δ t 1/δ t 2 (middle panel), and ED1/ED2 (right panel) in our preclassified sample data set. The distributions of true and false events in the two-dimensional spaces are also shown. The second row zooms in on the area of ﹩{A}_{f}/\sigma ({F}_{{\mathrm{LC}}_{1}})=﹩ 1–10. For the true flares, their ﹩{A}_{f}/\sigma ({F}_{{\mathrm{LC}}_{1}})﹩ increase with increasing δ t but decline as δ t 1/δ t 2 grows greater. The flares with ﹩{A}_{f}/\sigma ({F}_{{\mathrm{LC}}_{1}})\gt 20﹩ exhibit no apparent trend in ED1/ED2, whereas smaller flares could have a larger ED1/ED2, yet this ratio does not surpass 1. The distributions of all three parameters become less scattering as ﹩{A}_{f}/\sigma ({F}_{{\mathrm{LC}}_{1}})﹩ grows. For the false events, the distributions of all three parameters are way more dispersed than those of the true flares.
Paper: Scalable, Advanced Machine Learning Based Approaches for Stellar Flare Identification: Application to TESS Short-cadence Data and Analysis of a New Flare Catalog
Authors: Chia-Lung Lin, Dániel Apai, Mark S. Giampapa, Wing-Huen Ip
Figure caption: The normalized confusion matrix of the predictions our machine learning models made for the testing set: (a) DNN, (b) RF, (c) XGBoost, and (d) flares voted by all models or the multialgorithm approach. The horizontal label is the predicted class label, and the vertical is the reality class label. The matrix contains the TP, TN, FP, and FN of the model’s predictions.
Paper: Scalable, Advanced Machine Learning Based Approaches for Stellar Flare Identification: Application to TESS Short-cadence Data and Analysis of a New Flare Catalog
Authors: Chia-Lung Lin, Dániel Apai, Mark S. Giampapa, Wing-Huen Ip
Figure caption: (a) A Venn diagram illustrates the flares detected from the same TESS data set by M. N. Günther et al. (2020, red) and our models (yellow) and the detection overlap. (b) The ﹩{A}_{f}/\sigma ({F}_{{\mathrm{LC}}_{1}})﹩ distributions of all voted flares (the flares recognized by at least two different machine learning models) and those also reported by M. N. Günther et al. (2020).
Paper: Scalable, Advanced Machine Learning Based Approaches for Stellar Flare Identification: Application to TESS Short-cadence Data and Analysis of a New Flare Catalog
Authors: Chia-Lung Lin, Dániel Apai, Mark S. Giampapa, Wing-Huen Ip
Figure caption: A partial 2 minute light curve of TIC 140045538, an extremely flare-active star reported by M. N. Günther et al. (2020). The light-curve profiles in red and purple are the flares detected only by the RF model and the voted flares, respectively. The blue horizontal dashed line represents the 1σ level of noise of the flattened light curve, i.e., ﹩\sigma ({F}_{{\mathrm{LC}}_{1}})﹩. RF-only flares are generally smaller than voted flares. The inset panel in the figure shows a detailed view of the pattern enclosed within a black box between BTJD = 1326.05 and 1326.35. This highlights the profile of RF-only flares and offers a detailed comparison with small voted flares.
Paper: Scalable, Advanced Machine Learning Based Approaches for Stellar Flare Identification: Application to TESS Short-cadence Data and Analysis of a New Flare Catalog
Authors: Chia-Lung Lin, Dániel Apai, Mark S. Giampapa, Wing-Huen Ip
Figure caption: The 2 minute TESS light curve of TIC 140045538 observed in Sector 1 (top panel). The blue horizontal dashed line represents the 1σ level of noise of the flattened light curve, i.e., ﹩\sigma ({F}_{{\mathrm{LC}}_{1}})﹩. In total, the purple profiles present 158 voted flares detected by our machine learning models. The red vertical dashed lines mark the time positions of the 56 flares reported by M. N. Günther et al. (2020). The middle and bottom panels display zoomed-in views of the time spans in box (a) and box (b) from the all Sector 1 time span, respectively.
Paper: Scalable, Advanced Machine Learning Based Approaches for Stellar Flare Identification: Application to TESS Short-cadence Data and Analysis of a New Flare Catalog
Authors: Chia-Lung Lin, Dániel Apai, Mark S. Giampapa, Wing-Huen Ip
Figure caption: The loss (left) and the accuracy (right) of the training set and validation set across the training epochs. The black vertical dashed line marks the best-fitting epoch of 164 for our DNN model.
Paper: Scalable, Advanced Machine Learning Based Approaches for Stellar Flare Identification: Application to TESS Short-cadence Data and Analysis of a New Flare Catalog
Authors: Chia-Lung Lin, Dániel Apai, Mark S. Giampapa, Wing-Huen Ip
Figure caption: The 2 minute TESS light curve of TIC 434103039 observed in Sector 2 (top panel). The horizontal dashed line in blue represents the 1σ noise level of the flattened light curve. The light-curve profiles in purple are the 40 voted flares detected by our machine learning models. The red vertical dashed lines represent the time positions of the flares from M. N. Günther et al. (2020). The zoomed-in time spans in box (a) and box (b) from the top panel are shown in the middle and bottom panels, respectively.
Paper: Scalable, Advanced Machine Learning Based Approaches for Stellar Flare Identification: Application to TESS Short-cadence Data and Analysis of a New Flare Catalog
Authors: Chia-Lung Lin, Dániel Apai, Mark S. Giampapa, Wing-Huen Ip
Figure caption: A series of comparisons of ﹩{A}_{f}/\sigma ({F}_{{\mathrm{LC}}_{1}})﹩ distributions between the RF (top), DNN (middle), XGBoost (bottom), and voted flares. The RF model reported significantly more small flares with ﹩{A}_{f}/\sigma ({F}_{{\mathrm{LC}}_{1}})﹩ between 2 and 3 than the others.