adsabs/AstroCLIMB huggingface dataset:
Paper: Minimizing Star-spot Contamination of Exoplanet Transit Spectroscopy Using Alternate Normalization
Authors: Drake Deming, Miles H. Currie, Victoria S. Meadows, Sarah Peacock
Figure caption: Example of our calculated CC functions for carbon dioxide, which is clearly detected in the transit spectrum of a temperate planet orbiting an M3V star 12 pc from Earth, using 100 transits. Two CCs are illustrated—the CC that models synthetic data including the planet transmission signal, and a CC from a pure noise source. For the latter CC, we generate noise at the same amplitude as in the simulated data. The negative peak on the CC indicates a detection of exoplanetary absorption, see Section 2.2 for an explanation of our sign convention. The S/N is 8 for this simulated detection.
Paper: Minimizing Star-spot Contamination of Exoplanet Transit Spectroscopy Using Alternate Normalization
Authors: Drake Deming, Miles H. Currie, Victoria S. Meadows, Sarah Peacock
Figure caption: Upper panel: Electrons detected by an ELT high-resolution spectrometer (R = 500,000) integrated over the transit of a temperate planet orbiting an M3V star at 12 pc distance (Table 1). Lower panel: Transmission spectrum of the planet (in parts-per-million, minus the minimum transmission value).
Paper: Minimizing Star-spot Contamination of Exoplanet Transit Spectroscopy Using Alternate Normalization
Authors: Drake Deming, Miles H. Currie, Victoria S. Meadows, Sarah Peacock
Figure caption: Ratio of the spotted spectrum of an M2V star to the same star without spots using PHOENIX models (T. O. Husser et al. 2013). (Only a small portion of the spectrum near a resonance line of neutral potassium is shown.) The spots have 5% filling factor and ΔT = −300 K. Colors indicate several atomic lines of different lower state excitation in electron volts (eV). The lowest excitation lines appear as extra absorption in the spectral ratio, whereas the higher excitation lines appear like emission (because they are weaker in the spot than in the quiet photosphere). The inset plot shows a CC detection of the line structure in this spectral ratio using realistic observational noise (noise is not plotted, see text). Wavelengths are in vacuum.
Paper: Multiple Generation Star Formation in Cepheus Flare
Authors: Fan Wang, Min Fang, Xiaoting Fu, Yang Su, Xuepeng Chen, Shiyu Zhang, Penghui Liu, Xiao-Long Wang, Haijun Tian, Wenyuan Cui, Zhongmu Li
Figure caption: Comparison the 5450 member candidates with the field stars in this region. The left subplot: the density map of the 5450 member candidates. The right subplot: the density map of the field stars in this region. The red-dashed line is the corrected-color isochrone from PARSEC model with an age of 50 Myr and solar metallicity ([M/H]=0).
Paper: Multiple Generation Star Formation in Cepheus Flare
Authors: Fan Wang, Min Fang, Xiaoting Fu, Yang Su, Xuepeng Chen, Shiyu Zhang, Penghui Liu, Xiao-Long Wang, Haijun Tian, Wenyuan Cui, Zhongmu Li
Figure caption: Distributions of 5450 member candidates (black dots), identified by the Friends-of-Friends (FoF) algorithm, in five-parameter space (Galactocentric coordinate (ℓ, b), parallax, tangential velocity (vℓ, vb)), and the CMD (MG vs. BP−RP).
Paper: Multiple Generation Star Formation in Cepheus Flare
Authors: Fan Wang, Min Fang, Xiaoting Fu, Yang Su, Xuepeng Chen, Shiyu Zhang, Penghui Liu, Xiao-Long Wang, Haijun Tian, Wenyuan Cui, Zhongmu Li
Figure caption: Comparison of tangential velocity distribution for Group 3 before and after noise elimination. Group 3 is divided into member candidates (red dots) and noise (black dots).
Paper: Multiple Generation Star Formation in Cepheus Flare
Authors: Fan Wang, Min Fang, Xiaoting Fu, Yang Su, Xuepeng Chen, Shiyu Zhang, Penghui Liu, Xiao-Long Wang, Haijun Tian, Wenyuan Cui, Zhongmu Li
Figure caption: Comparison the results before and after noise elimination in CMD. The black dots are the 4140 remaining member candidates, while the gray dots indicate the 1310 field stars that were removed.
Paper: Multiple Generation Star Formation in Cepheus Flare
Authors: Fan Wang, Min Fang, Xiaoting Fu, Yang Su, Xuepeng Chen, Shiyu Zhang, Penghui Liu, Xiao-Long Wang, Haijun Tian, Wenyuan Cui, Zhongmu Li
Figure caption: Dust extinction map from G. Edenhofer et al. (2024), displayed in Galactic coordinates. The black-dashed circle marks the Cepheus Flare Shell, provided by M. Kun et al. (2009), and the black-solid circle indicates Loop III, provided by M. Kun (2007). The black-dashed rectangle outlines the nearby star-forming region Polaris. The lime-dashed line marks cavity, and cyan points represent YSOs from M. Szilágyi et al. (2021), with black-dashed lines enclosing YSOs associated with seven different molecular clouds. Stellar groups are marked in different colors (as shown in Figures 5 and 6). The distribution trend of Group 4 is outlined with yellow color and thick white solid lines. Black arrow shows the direction of median proper motion of group members, with the length indicating its value.
Paper: Multiple Generation Star Formation in Cepheus Flare
Authors: Fan Wang, Min Fang, Xiaoting Fu, Yang Su, Xuepeng Chen, Shiyu Zhang, Penghui Liu, Xiao-Long Wang, Haijun Tian, Wenyuan Cui, Zhongmu Li
Figure caption: Distribution of Groups 1−5 in the Galactocentric coordinate (ℓ, b), parallax, tangential velocity (vℓ, vb). In all of the panels, green dots, hotpink dots, red dots, orange dots, and blue dots represent the candidate members of Group 1, Group 2, Group 3, Group 4, and Group 5, respectively.
Paper: Multiple Generation Star Formation in Cepheus Flare
Authors: Fan Wang, Min Fang, Xiaoting Fu, Yang Su, Xuepeng Chen, Shiyu Zhang, Penghui Liu, Xiao-Long Wang, Haijun Tian, Wenyuan Cui, Zhongmu Li
Figure caption: Position–velocity diagrams along the cavity (from upper-right to lower left). Left panel: the lime solid line represents the velocity trend of CO along ℓ direction. Right panel: the lime solid line is the velocity trend of H I along the same direction.
Paper: Multiple Generation Star Formation in Cepheus Flare
Authors: Fan Wang, Min Fang, Xiaoting Fu, Yang Su, Xuepeng Chen, Shiyu Zhang, Penghui Liu, Xiao-Long Wang, Haijun Tian, Wenyuan Cui, Zhongmu Li
Figure caption: CMDs for Groups 1−5 (same color coding as in Figure 5). The black-solid, dotted-dashed, and dashed curves in each panel represent the best-fit, 50 Myr, and 1 Myr PARSEC isochrones with empirical color correction, respectively.
Paper: Multiple Generation Star Formation in Cepheus Flare
Authors: Fan Wang, Min Fang, Xiaoting Fu, Yang Su, Xuepeng Chen, Shiyu Zhang, Penghui Liu, Xiao-Long Wang, Haijun Tian, Wenyuan Cui, Zhongmu Li
Figure caption: 2D trajectory plot (X, Y) of the backwards orbit integrations of Groups 1−5, tracing their motion from the past (32 Myr ago) to the present in Heliocentric Cartesian coordinates (X, Y, Z). The open circle with a dotted outline represents that the group had not yet formed, while the star denotes that the group had formed. These symbols are placed at specific times: 32, 20, and 15 Myr ago, and at present. The errorbar represent the positional dispersion in (X, Y), and the arrows indicate the median motion direction of each group.
Paper: Multiple Generation Star Formation in Cepheus Flare
Authors: Fan Wang, Min Fang, Xiaoting Fu, Yang Su, Xuepeng Chen, Shiyu Zhang, Penghui Liu, Xiao-Long Wang, Haijun Tian, Wenyuan Cui, Zhongmu Li
Figure caption: Left panel: CO integrated intensity map (lime contour) from T. M. Dame et al. (2001), and H I integrated intensity map (gray background) from HI4PI Collaboration et al. (2016). The light-yellow line with the direction from upper-right to lower left shows the routing of the position–velocity diagram of the cavity.
Paper: Multiple Generation Star Formation in Cepheus Flare
Authors: Fan Wang, Min Fang, Xiaoting Fu, Yang Su, Xuepeng Chen, Shiyu Zhang, Penghui Liu, Xiao-Long Wang, Haijun Tian, Wenyuan Cui, Zhongmu Li
Figure caption: CMDs for 319 nearby young stellar objects (YSOs, gray and cyan dots), including 149 YSOs (cyan dots) that are part of Group 4. The black-solid, dotted-dashed, and dashed curves in each panel represent the best-fit, 50 Myr and 1 Myr PARSEC isochrones with empirical color correction, respectively.
Paper: Multiple Generation Star Formation in Cepheus Flare
Authors: Fan Wang, Min Fang, Xiaoting Fu, Yang Su, Xuepeng Chen, Shiyu Zhang, Penghui Liu, Xiao-Long Wang, Haijun Tian, Wenyuan Cui, Zhongmu Li
Figure caption: Distributions of 3971 member candidates (purple dots) from this work and 2124 member candidates (lime dots) from KC19 in five-parameter space (Galactocentric coordinate (ℓ, b), parallax, tangential velocity (vℓ, vb)) and the CMD (MG vs. BP − RP).
Paper: Observation and Simulation of Mutual Approximations between Five Main Uranian Satellites
Authors: Jian Chen, 健 陈, Hao-Ran Song, 浩冉 宋, Ye Yuan, 烨 袁, Fan Li, 凡 李, Yan-Ning Fu, 燕宁 傅, Tian-Rui Sun, 天瑞 孙, Yu-Xi Jiang, 雨汐 蒋
Figure caption: Geometry of observed events. The Uranus is located at the origin. The curves in different colors represent satellites' orbits around Uranus in the middle of 2022. Two points linked by a line correspond to a mutual approximation event. The black line denotes events with d0/Δa < 1.1, and the red line denotes d0/Δa > 1.1.
Paper: Observation and Simulation of Mutual Approximations between Five Main Uranian Satellites
Authors: Jian Chen, 健 陈, Hao-Ran Song, 浩冉 宋, Ye Yuan, 烨 袁, Fan Li, 凡 李, Yan-Ning Fu, 燕宁 傅, Tian-Rui Sun, 天瑞 孙, Yu-Xi Jiang, 雨汐 蒋
Figure caption: Relation between the ﹩{\mathop{\sigma }\limits^{\unicode{x00304}}}_{{\rm{eq}}}﹩ and ∣v0∣/Δv. ﹩{\mathop{\sigma }\limits^{\unicode{x00304}}}_{{\rm{eq}}}﹩ represents the enhancement of precision by mutual approximation; ∣v0∣/Δv represents the ephemeris relative velocity at the central instant divided by the difference of two satellites’ apparent average orbital velocity. Values of ﹩{\mathop{\sigma }\limits^{\unicode{x00304}}}_{{\rm{eq}}}﹩ and ∣v0∣/Δv are from Table 3.
Paper: Observation and Simulation of Mutual Approximations between Five Main Uranian Satellites
Authors: Jian Chen, 健 陈, Hao-Ran Song, 浩冉 宋, Ye Yuan, 烨 袁, Fan Li, 凡 李, Yan-Ning Fu, 燕宁 傅, Tian-Rui Sun, 天瑞 孙, Yu-Xi Jiang, 雨汐 蒋
Figure caption: The distance curve of a valid mutual approximation event. In the upper frame, the blue curve is the observed distance between U4 and U5, the green curve is the fitted one, and the red curve is obtained from the JPL ephemeris (DE440+URA111). The green and red vertical lines are the central instant of the fitted curve and the ephemeris curve. The black horizontal line at the top of the green vertical line denote the ﹩{\sigma }_{{t}_{0}}﹩ mentioned in Table 3. In the lower frame, the scatters marked with “+” are the residuals of the observed data and the fitted curve.
Paper: Observation and Simulation of Mutual Approximations between Five Main Uranian Satellites
Authors: Jian Chen, 健 陈, Hao-Ran Song, 浩冉 宋, Ye Yuan, 烨 袁, Fan Li, 凡 李, Yan-Ning Fu, 燕宁 傅, Tian-Rui Sun, 天瑞 孙, Yu-Xi Jiang, 雨汐 蒋
Figure caption: Relation between the ﹩{\mathop{\sigma }\limits^{\unicode{x00304}}}_{{\rm{eq}}}﹩ and d0/Δa. ﹩{\mathop{\sigma }\limits^{\unicode{x00304}}}_{{\rm{eq}}}﹩ represents the enhancement of precision by mutual approximation; d0/Δa represents the impact parameter divided by the difference of two satellites’ semimajor axes. Values of ﹩{\mathop{\sigma }\limits^{\unicode{x00304}}}_{{\rm{eq}}}﹩ and d0/Δa are from Table 3.
Paper: Observation and Simulation of Mutual Approximations between Five Main Uranian Satellites
Authors: Jian Chen, 健 陈, Hao-Ran Song, 浩冉 宋, Ye Yuan, 烨 袁, Fan Li, 凡 李, Yan-Ning Fu, 燕宁 傅, Tian-Rui Sun, 天瑞 孙, Yu-Xi Jiang, 雨汐 蒋
Figure caption: Relation between the ﹩{\mathop{\sigma }\limits^{\unicode{x00304}}}_{{\rm{eq}}}﹩ and d0/Δa for simulated mutual approximations of set B. The condition of set B is shown in Table 5. The Pearson coefficient is 0.81 with the p-value of 0.
Paper: Observation and Simulation of Mutual Approximations between Five Main Uranian Satellites
Authors: Jian Chen, 健 陈, Hao-Ran Song, 浩冉 宋, Ye Yuan, 烨 袁, Fan Li, 凡 李, Yan-Ning Fu, 燕宁 傅, Tian-Rui Sun, 天瑞 孙, Yu-Xi Jiang, 雨汐 蒋
Figure caption: Relation between the ﹩{\mathop{\sigma }\limits^{\unicode{x00304}}}_{{\rm{eq}}}﹩ and d0/Δa for simulated mutual approximations of set A. The condition of set A is shown in Table 5. The Pearson coefficient is 0.79 with the p-value of 0.
Paper: Observation and Simulation of Mutual Approximations between Five Main Uranian Satellites
Authors: Jian Chen, 健 陈, Hao-Ran Song, 浩冉 宋, Ye Yuan, 烨 袁, Fan Li, 凡 李, Yan-Ning Fu, 燕宁 傅, Tian-Rui Sun, 天瑞 孙, Yu-Xi Jiang, 雨汐 蒋
Figure caption: The distance curve of an invalid mutual approximation event. The symbols share the same meaning with Figure 1.
Paper: Multiband, Multiepoch Photometry of the Spot-crossing System TOI-3884: Refined System Geometry and Spot Properties
Authors: Mayuko Mori, Akihiko Fukui, Teruyuki Hirano, Norio Narita, John H. Livingston, Khalid Barkaoui, Karen A. Collins, Jerome P. de Leon, Kai Ikuta, Yugo Kawai, Richard P. Schwarz, Avi Shporer, Gregor Srdoc
Figure caption: Left: GLS periodogram of the monitoring light curve observed in Sinistro r band. A strong peak is detected at 11.03 ± 0.03 days. The dashed horizontal lines indicate the FAP corresponding to the peak height. Right: GP models (blue lines), generated using 100 randomly selected parameter sets from the converged emcee samples, overlaid on the observed light curve (black points). The error bars are scaled by the best-fit α factor.
Paper: Multiband, Multiepoch Photometry of the Spot-crossing System TOI-3884: Refined System Geometry and Spot Properties
Authors: Mayuko Mori, Akihiko Fukui, Teruyuki Hirano, Norio Narita, John H. Livingston, Khalid Barkaoui, Karen A. Collins, Jerome P. de Leon, Kai Ikuta, Yugo Kawai, Richard P. Schwarz, Avi Shporer, Gregor Srdoc
Figure caption: Observed transit light curves of TOI-3884 b (top to bottom: three transits observed with MuSCAT3 or MuSCAT4; left to right: g, r, i, and z band) and the corresponding best-fit models (black lines). The error bars in the data points are scaled to make reduced χ2 values equal to 1. To the right of each light curve, the spot distribution on the stellar surface at the corresponding epoch is shown, as modeled with fleck. The “×” mark in the figure shows the location of the stellar south pole, the dotted lines show the stellar equator, and the regions inside dashed lines indicate the transit chord.
Paper: Multiband, Multiepoch Photometry of the Spot-crossing System TOI-3884: Refined System Geometry and Spot Properties
Authors: Mayuko Mori, Akihiko Fukui, Teruyuki Hirano, Norio Narita, John H. Livingston, Khalid Barkaoui, Karen A. Collins, Jerome P. de Leon, Kai Ikuta, Yugo Kawai, Richard P. Schwarz, Avi Shporer, Gregor Srdoc
Figure caption: Monitoring light curve of TOI-3884 obtained with Sinistro. The horizontal axis indicates the MJD. Gray points represent the r-band photometric measurements, green points show the binned light curve in 0.5 day intervals, and red crosses mark the data points that were removed as outliers. The yellow points indicate the i-band measurements.
Paper: Multiband, Multiepoch Photometry of the Spot-crossing System TOI-3884: Refined System Geometry and Spot Properties
Authors: Mayuko Mori, Akihiko Fukui, Teruyuki Hirano, Norio Narita, John H. Livingston, Khalid Barkaoui, Karen A. Collins, Jerome P. de Leon, Kai Ikuta, Yugo Kawai, Richard P. Schwarz, Avi Shporer, Gregor Srdoc
Figure caption: The rotational modulation light curve of TOI-3884 observed with Sinistro, overlaid with the model light curve generated using the best-fit parameters from the spot-crossing analyses. The blue dashed line shows the forward model without any adjustment, while the red solid line represents the model after applying a temporal offset optimized to best match the observed modulation.
Paper: Multiband, Multiepoch Photometry of the Spot-crossing System TOI-3884: Refined System Geometry and Spot Properties
Authors: Mayuko Mori, Akihiko Fukui, Teruyuki Hirano, Norio Narita, John H. Livingston, Khalid Barkaoui, Karen A. Collins, Jerome P. de Leon, Kai Ikuta, Yugo Kawai, Richard P. Schwarz, Avi Shporer, Gregor Srdoc
Figure caption: Tphot–ΔT relation for dwarf stars with Tphot ranging from 3000 to 4500 K. The empirical relation and its uncertainties from Equation (4) in K. Herbst et al. (2021; originally derived by S. V. Berdyugina 2005) are shown as the blue line and shaded region, respectively. Error bars for Tphot are omitted for all stars except TOI-3884. For data points without error bars in ΔT, uncertainties were not reported.
Paper: Multiband, Multiepoch Photometry of the Spot-crossing System TOI-3884: Refined System Geometry and Spot Properties
Authors: Mayuko Mori, Akihiko Fukui, Teruyuki Hirano, Norio Narita, John H. Livingston, Khalid Barkaoui, Karen A. Collins, Jerome P. de Leon, Kai Ikuta, Yugo Kawai, Richard P. Schwarz, Avi Shporer, Gregor Srdoc
Figure caption: SAP light curves of TOI-3884 from TESS Sectors 46 and 49, overlaid with the forward model (orange lines) of the rotational modulation generated using the best-fit parameters from the transit fitting with MuSCAT3/MuSCAT3 data. The discrepancy between the model and the TESS light curves suggests that the spot configuration may have been different during the TESS observations compared to the MuSCAT3/MuSCAT4 observations.
Paper: Multiband, Multiepoch Photometry of the Spot-crossing System TOI-3884: Refined System Geometry and Spot Properties
Authors: Mayuko Mori, Akihiko Fukui, Teruyuki Hirano, Norio Narita, John H. Livingston, Khalid Barkaoui, Karen A. Collins, Jerome P. de Leon, Kai Ikuta, Yugo Kawai, Richard P. Schwarz, Avi Shporer, Gregor Srdoc
Figure caption: Derived transit depth of TOI-3884 in each band (g, r, i, and z band from left to right). The dashed line indicates the expected chromatic variation in transit depth due to the TLS effect, assuming a true transit depth of 3.4% and a spot covering fraction of 20%.
Paper: Multiband, Multiepoch Photometry of the Spot-crossing System TOI-3884: Refined System Geometry and Spot Properties
Authors: Mayuko Mori, Akihiko Fukui, Teruyuki Hirano, Norio Narita, John H. Livingston, Khalid Barkaoui, Karen A. Collins, Jerome P. de Leon, Kai Ikuta, Yugo Kawai, Richard P. Schwarz, Avi Shporer, Gregor Srdoc
Figure caption: Comparison of the two best-fit models from group 1 (blue) and group 2 (orange). (a) Model light curves for each group, overlaid on the same observed data as shown in Figure 3, are plotted in gray here for clarity. The two models are nearly indistinguishable. The right panels show the corresponding spot configurations at the time of each transit. (b) Distribution of log-probability values from the transit fits. (c) Predicted rotational modulation as a function of stellar rotation phase.
Paper: Multiband, Multiepoch Photometry of the Spot-crossing System TOI-3884: Refined System Geometry and Spot Properties
Authors: Mayuko Mori, Akihiko Fukui, Teruyuki Hirano, Norio Narita, John H. Livingston, Khalid Barkaoui, Karen A. Collins, Jerome P. de Leon, Kai Ikuta, Yugo Kawai, Richard P. Schwarz, Avi Shporer, Gregor Srdoc
Figure caption: Corner plot showing the posterior distributions of the fitted parameters from the transit analysis. The plot includes a subset of the posteriors, omitting the 12 additional parameters (k, q1, and q2 for each band) that were also sampled. Blue and orange contours represent posterior samples from group 1 (spot latitude θspot ≤ −78°) and group 2 (>−78°), respectively. The apparent overlap in the θspot contours is due to smoothing in the visualization and does not indicate actual mixing. The blue and orange lines indicate the best-fit parameter values for each group, respectively. The green solid line in each histogram marks the best-fit value from the full posterior.
Paper: Multiband, Multiepoch Photometry of the Spot-crossing System TOI-3884: Refined System Geometry and Spot Properties
Authors: Mayuko Mori, Akihiko Fukui, Teruyuki Hirano, Norio Narita, John H. Livingston, Khalid Barkaoui, Karen A. Collins, Jerome P. de Leon, Kai Ikuta, Yugo Kawai, Richard P. Schwarz, Avi Shporer, Gregor Srdoc
Figure caption: GLS periodograms of TOI-3884’s ZTF light curves for each band and each year. The upper panels (blue) correspond to the g band, while the lower panels (green) correspond to the r band. The black horizontal dashed lines indicate the FAP = 1% threshold. The red vertical dashed lines mark the period of 11.04 days, and red dots indicate cases where peaks are detected near this period with FAP < 1%.
Paper: Multiband, Multiepoch Photometry of the Spot-crossing System TOI-3884: Refined System Geometry and Spot Properties
Authors: Mayuko Mori, Akihiko Fukui, Teruyuki Hirano, Norio Narita, John H. Livingston, Khalid Barkaoui, Karen A. Collins, Jerome P. de Leon, Kai Ikuta, Yugo Kawai, Richard P. Schwarz, Avi Shporer, Gregor Srdoc
Figure caption: Light curves of TOI-3884 observed with ZTF in the g band (blue, upper figure) and r band (green, lower figure). The gray dashed lines indicate the boundaries between different observing seasons (Year 0 to Year 6). The orange-shaded regions mark the periods of TESS observations in Sectors 46 and 49, from left to right. The red lines indicate the timings of the three transit observations conducted with MuSCAT3 and MuSCAT4.
Paper: Multiband, Multiepoch Photometry of the Spot-crossing System TOI-3884: Refined System Geometry and Spot Properties
Authors: Mayuko Mori, Akihiko Fukui, Teruyuki Hirano, Norio Narita, John H. Livingston, Khalid Barkaoui, Karen A. Collins, Jerome P. de Leon, Kai Ikuta, Yugo Kawai, Richard P. Schwarz, Avi Shporer, Gregor Srdoc
Figure caption: Distribution of measured stellar obliquities as a function of stellar effective temperature Teff. Data for systems other than TOI-3884 b are taken from TEPCat (J. Southworth 2011). TOI-3884 b is highlighted in red. Systems with a similar Teff and obliquity to TOI-3884 b, namely GJ 436 b and GJ 3470 b, are also highlighted.
Paper: Multiband, Multiepoch Photometry of the Spot-crossing System TOI-3884: Refined System Geometry and Spot Properties
Authors: Mayuko Mori, Akihiko Fukui, Teruyuki Hirano, Norio Narita, John H. Livingston, Khalid Barkaoui, Karen A. Collins, Jerome P. de Leon, Kai Ikuta, Yugo Kawai, Richard P. Schwarz, Avi Shporer, Gregor Srdoc
Figure caption: Light curves of the eight transits observed by TESS, overlaid with the best-fit transit models. The right panel shows the corresponding spot configuration on the stellar surface at the time of the TESS observations, as derived from the best-fit parameters. Since the spot latitude is close to the pole, the spot appears in almost the same position in all transits.
Paper: Multiband, Multiepoch Photometry of the Spot-crossing System TOI-3884: Refined System Geometry and Spot Properties
Authors: Mayuko Mori, Akihiko Fukui, Teruyuki Hirano, Norio Narita, John H. Livingston, Khalid Barkaoui, Karen A. Collins, Jerome P. de Leon, Kai Ikuta, Yugo Kawai, Richard P. Schwarz, Avi Shporer, Gregor Srdoc
Figure caption: Phase-folded ZTF light curves of TOI-3884 with a period of 11.04 days, for each band and each year. The panel arrangement follows the same order as in Figure 12.
Paper: Predicting Exoplanet Occurrence Using Association Analysis
Authors: Vasundhara Gatne, Michael L. Wong, Anirudh Prabhu
Figure caption: Histogram of planets by primary planetary subtype.