adsabs/AstroCLIMB huggingface dataset:
Paper: MOA-2020-BLG-208Lb: Cool Sub-Saturn-mass Planet within Predicted Desert
Authors: Greg Olmschenk, David P. Bennett, Ian A. Bond, Weicheng Zang, Youn Kil Jung, Jennifer C. Yee, Etienne Bachelet, Fumio Abe, Richard K. Barry, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Brandon Munford, Yasushi Muraki, Arisa Okamura, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Taiga Toda, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Michael D. Albrow, Sang-Mok Cha, Sun-Ju Chung, Andrew Gould, Cheongho Han, Kyu-Ha Hwang, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Grant Christie, Tony Cooper, John Drummond, Jonathan Green, Steve Hennerley, Jennie McCormick, L. A. G. Monard, Tim Natusch, Ian Porritt, Thiam-Guan Tan, Shude Mao, Dan Maoz, Matthew T. Penny, Wei Zhu, V. Bozza, Arnaud Cassan, Martin Dominik, Markus Hundertmark, R. Figuera Jaimes, K. Kruszyńska, K. A. Rybicki, R. A. Street, Y. Tsapras, Joachim Wambsganss, Ł. Wyrzykowski, P. Zieliński, Gioia Rau
Figure caption: Color–magnitude diagram of the stars in the OGLE-III catalog within 180″ of MOA-2020-BLG-208. The blue dot shows the source magnitude and color for the best-fit wide-orbit model (see Table 1).
Paper: MOA-2020-BLG-208Lb: Cool Sub-Saturn-mass Planet within Predicted Desert
Authors: Greg Olmschenk, David P. Bennett, Ian A. Bond, Weicheng Zang, Youn Kil Jung, Jennifer C. Yee, Etienne Bachelet, Fumio Abe, Richard K. Barry, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Brandon Munford, Yasushi Muraki, Arisa Okamura, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Taiga Toda, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Michael D. Albrow, Sang-Mok Cha, Sun-Ju Chung, Andrew Gould, Cheongho Han, Kyu-Ha Hwang, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Grant Christie, Tony Cooper, John Drummond, Jonathan Green, Steve Hennerley, Jennie McCormick, L. A. G. Monard, Tim Natusch, Ian Porritt, Thiam-Guan Tan, Shude Mao, Dan Maoz, Matthew T. Penny, Wei Zhu, V. Bozza, Arnaud Cassan, Martin Dominik, Markus Hundertmark, R. Figuera Jaimes, K. Kruszyńska, K. A. Rybicki, R. A. Street, Y. Tsapras, Joachim Wambsganss, Ł. Wyrzykowski, P. Zieliński, Gioia Rau
Figure caption: The source trajectory and magnification pattern of the wide-orbit best-fit solution. The magnification pattern shows the difference between the point-source-binary-lens (PSBL) and the point-source-point-lens (PSPL) models. White lines represent the caustic.
Paper: MOA-2020-BLG-208Lb: Cool Sub-Saturn-mass Planet within Predicted Desert
Authors: Greg Olmschenk, David P. Bennett, Ian A. Bond, Weicheng Zang, Youn Kil Jung, Jennifer C. Yee, Etienne Bachelet, Fumio Abe, Richard K. Barry, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Brandon Munford, Yasushi Muraki, Arisa Okamura, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Taiga Toda, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Michael D. Albrow, Sang-Mok Cha, Sun-Ju Chung, Andrew Gould, Cheongho Han, Kyu-Ha Hwang, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Grant Christie, Tony Cooper, John Drummond, Jonathan Green, Steve Hennerley, Jennie McCormick, L. A. G. Monard, Tim Natusch, Ian Porritt, Thiam-Guan Tan, Shude Mao, Dan Maoz, Matthew T. Penny, Wei Zhu, V. Bozza, Arnaud Cassan, Martin Dominik, Markus Hundertmark, R. Figuera Jaimes, K. Kruszyńska, K. A. Rybicki, R. A. Street, Y. Tsapras, Joachim Wambsganss, Ł. Wyrzykowski, P. Zieliński, Gioia Rau
Figure caption: The source trajectory and magnification pattern of the close-orbit best-fit solution. The magnification pattern shows the difference between the PSBL and the PSPL models. White lines represent the caustic.
Paper: MOA-2020-BLG-208Lb: Cool Sub-Saturn-mass Planet within Predicted Desert
Authors: Greg Olmschenk, David P. Bennett, Ian A. Bond, Weicheng Zang, Youn Kil Jung, Jennifer C. Yee, Etienne Bachelet, Fumio Abe, Richard K. Barry, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Brandon Munford, Yasushi Muraki, Arisa Okamura, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Taiga Toda, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Michael D. Albrow, Sang-Mok Cha, Sun-Ju Chung, Andrew Gould, Cheongho Han, Kyu-Ha Hwang, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Grant Christie, Tony Cooper, John Drummond, Jonathan Green, Steve Hennerley, Jennie McCormick, L. A. G. Monard, Tim Natusch, Ian Porritt, Thiam-Guan Tan, Shude Mao, Dan Maoz, Matthew T. Penny, Wei Zhu, V. Bozza, Arnaud Cassan, Martin Dominik, Markus Hundertmark, R. Figuera Jaimes, K. Kruszyńska, K. A. Rybicki, R. A. Street, Y. Tsapras, Joachim Wambsganss, Ł. Wyrzykowski, P. Zieliński, Gioia Rau
Figure caption: Galactic-model posterior distributions with a mass prior that assumes all stars have an equal probability of hosting planets.
Paper: MOA-2020-BLG-208Lb: Cool Sub-Saturn-mass Planet within Predicted Desert
Authors: Greg Olmschenk, David P. Bennett, Ian A. Bond, Weicheng Zang, Youn Kil Jung, Jennifer C. Yee, Etienne Bachelet, Fumio Abe, Richard K. Barry, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Brandon Munford, Yasushi Muraki, Arisa Okamura, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Taiga Toda, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Michael D. Albrow, Sang-Mok Cha, Sun-Ju Chung, Andrew Gould, Cheongho Han, Kyu-Ha Hwang, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Grant Christie, Tony Cooper, John Drummond, Jonathan Green, Steve Hennerley, Jennie McCormick, L. A. G. Monard, Tim Natusch, Ian Porritt, Thiam-Guan Tan, Shude Mao, Dan Maoz, Matthew T. Penny, Wei Zhu, V. Bozza, Arnaud Cassan, Martin Dominik, Markus Hundertmark, R. Figuera Jaimes, K. Kruszyńska, K. A. Rybicki, R. A. Street, Y. Tsapras, Joachim Wambsganss, Ł. Wyrzykowski, P. Zieliński, Gioia Rau
Figure caption: Galactic-model posterior distributions with a mass prior that assumes greater star mass corresponds to a higher probability of hosting planets.
Paper: MOA-2020-BLG-208Lb: Cool Sub-Saturn-mass Planet within Predicted Desert
Authors: Greg Olmschenk, David P. Bennett, Ian A. Bond, Weicheng Zang, Youn Kil Jung, Jennifer C. Yee, Etienne Bachelet, Fumio Abe, Richard K. Barry, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Brandon Munford, Yasushi Muraki, Arisa Okamura, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Taiga Toda, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Michael D. Albrow, Sang-Mok Cha, Sun-Ju Chung, Andrew Gould, Cheongho Han, Kyu-Ha Hwang, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Grant Christie, Tony Cooper, John Drummond, Jonathan Green, Steve Hennerley, Jennie McCormick, L. A. G. Monard, Tim Natusch, Ian Porritt, Thiam-Guan Tan, Shude Mao, Dan Maoz, Matthew T. Penny, Wei Zhu, V. Bozza, Arnaud Cassan, Martin Dominik, Markus Hundertmark, R. Figuera Jaimes, K. Kruszyńska, K. A. Rybicki, R. A. Street, Y. Tsapras, Joachim Wambsganss, Ł. Wyrzykowski, P. Zieliński, Gioia Rau
Figure caption: Our best-fit binary-source-model light curve for the MOA-2020-BLG-208 event. The extreme blueness of the second source makes this solution unlikely.
Paper: Measurement of the Angular Momenta of Pre-main-sequence Stars: Early Evolution of Slow and Fast Rotators and Empirical Constraints on Spin-down Torque Mechanisms
Authors: Marina Kounkel, Keivan G. Stassun, Lynne A. Hillenbrand, Jesús Hernández, Javier Serna, Jason Lee Curtis
Figure caption: Distribution of rotational periods in the sample as a function of T eff. Left panel: all sources in the Orion Complex from Paper I using the T eff estimate from TIC (Stassun et al. 2019). Right: subset of sources observed by APOGEE with spectroscopically determined T eff.
Paper: Measurement of the Angular Momenta of Pre-main-sequence Stars: Early Evolution of Slow and Fast Rotators and Empirical Constraints on Spin-down Torque Mechanisms
Authors: Marina Kounkel, Keivan G. Stassun, Lynne A. Hillenbrand, Jesús Hernández, Javier Serna, Jason Lee Curtis
Figure caption: Fraction of rapid rotators among CTTSs and WTTSs with T eff < 6700 K as a function of age. The top panel shows all rapid rotators with periods <2 days, and the bottom panel is restricted to the subset with periods <1 day.
Paper: Measurement of the Angular Momenta of Pre-main-sequence Stars: Early Evolution of Slow and Fast Rotators and Empirical Constraints on Spin-down Torque Mechanisms
Authors: Marina Kounkel, Keivan G. Stassun, Lynne A. Hillenbrand, Jesús Hernández, Javier Serna, Jason Lee Curtis
Figure caption: Dependence of radius, rotational period, angular momentum, and specific angular momentum on the temperature and age of stars in Orion with P > 2 days. The typical uncertainties in the data are 30 K in T eff, 0.1 R ⊙ in radius, 0.01 day in period, 0.05 dex in L, and 0.04 dex in H. In young disk-bearing stars, the typical uncertainties in radius are larger due to the infrared excess affecting the quality of the SED fitting.
Paper: Measurement of the Angular Momenta of Pre-main-sequence Stars: Early Evolution of Slow and Fast Rotators and Empirical Constraints on Spin-down Torque Mechanisms
Authors: Marina Kounkel, Keivan G. Stassun, Lynne A. Hillenbrand, Jesús Hernández, Javier Serna, Jason Lee Curtis
Figure caption: Period distribution between CTTSs and WTTSs.
Paper: Measurement of the Angular Momenta of Pre-main-sequence Stars: Early Evolution of Slow and Fast Rotators and Empirical Constraints on Spin-down Torque Mechanisms
Authors: Marina Kounkel, Keivan G. Stassun, Lynne A. Hillenbrand, Jesús Hernández, Javier Serna, Jason Lee Curtis
Figure caption: Left: distribution of the adopted ages for the stars in the Orion Complex. Right: typical uncertainties in the sample.
Paper: Searching for Compact Object Candidates from LAMOST Time-domain Survey of Four K2 Plates
Authors: Senyu Qi, Wei-Min Gu, Tuan Yi, Zhi-Xiang Zhang, Song Wang, Jifeng Liu
Figure caption: Phase-folded radial velocity data (dots) and the best-fitted radial velocity curves (lines) of the selected sources. The error bars for most data points are too small to be seen.
Paper: Planetary Orbit Eccentricity Trends (POET). I. The Eccentricity–Metallicity Trend for Small Planets Revealed by the LAMOST–Gaia–Kepler Sample
Authors: Dong-Sheng An, 东升 安, Ji-Wei Xie, 基伟 谢, Yuan-Zhe Dai, 远哲 戴, Ji-Lin Zhou, 济林 周
Figure caption: Stellar properties in our sample. The left panel shows stellar effective temperature vs. stellar radius, and the right panel shows stellar mass vs. metallicity, i.e., [Fe/H].
Paper: Planetary Orbit Eccentricity Trends (POET). I. The Eccentricity–Metallicity Trend for Small Planets Revealed by the LAMOST–Gaia–Kepler Sample
Authors: Dong-Sheng An, 东升 安, Ji-Wei Xie, 基伟 谢, Yuan-Zhe Dai, 远哲 戴, Ji-Lin Zhou, 济林 周
Figure caption: Metallicity ([Fe/H])–TDR diagram for single (left panel) and multiple (right panel) transit systems.
Paper: Planetary Orbit Eccentricity Trends (POET). I. The Eccentricity–Metallicity Trend for Small Planets Revealed by the LAMOST–Gaia–Kepler Sample
Authors: Dong-Sheng An, 东升 安, Ji-Wei Xie, 基伟 谢, Yuan-Zhe Dai, 远哲 戴, Ji-Lin Zhou, 济林 周
Figure caption: Orbital period vs. planet radius in our sample.
Paper: Planetary Orbit Eccentricity Trends (POET). I. The Eccentricity–Metallicity Trend for Small Planets Revealed by the LAMOST–Gaia–Kepler Sample
Authors: Dong-Sheng An, 东升 安, Ji-Wei Xie, 基伟 谢, Yuan-Zhe Dai, 远哲 戴, Ji-Lin Zhou, 济林 周
Figure caption: Cumulative distributions for T eff, M *, P, and R  p  in the different subsamples before (top four panels) and after (bottom four panels) parameter control, where bin1 (dotted line), bin2 (dashed line), and bin3 (solid line) represent the lowest, the intermediate, and the highest metallicity bin, respectively. The p-values of the KS test between the different bins are provided, where p-value13 and p-value23 represent the p-value of bin1 vs. bin3 and bin2 vs. bin3, respectively.
Paper: Planetary Orbit Eccentricity Trends (POET). I. The Eccentricity–Metallicity Trend for Small Planets Revealed by the LAMOST–Gaia–Kepler Sample
Authors: Dong-Sheng An, 东升 安, Ji-Wei Xie, 基伟 谢, Yuan-Zhe Dai, 远哲 戴, Ji-Lin Zhou, 济林 周
Figure caption: Similar to Figure 7, but showing the mean eccentricities of singles vs. multiples under different metallicities. The solid error bars represent ﹩\bar{e}﹩ constrained via TDR (Sections 4.1 and 4.2.1), while the dashed error bars represent ﹩\bar{e}﹩ calculated by assuming ﹩\bar{e}=\bar{i}﹩ (see Section 5.2) and ﹩\bar{i}﹩ is constrained by the distribution of the mutual TDR, i.e., ξ (Section 4.2.2). In addition, the dashed error bar of the medium metallicity has been artificially moved to the right by 0.02 dex to avoid overlapping symbols.
Paper: Planetary Orbit Eccentricity Trends (POET). I. The Eccentricity–Metallicity Trend for Small Planets Revealed by the LAMOST–Gaia–Kepler Sample
Authors: Dong-Sheng An, 东升 安, Ji-Wei Xie, 基伟 谢, Yuan-Zhe Dai, 远哲 戴, Ji-Lin Zhou, 济林 周
Figure caption: The mutual TDR (ξ) fitting for multiple transiting systems. Left panels: the observed ξ distribution (red) and the best fit (turquoise). Right panels: the relative likelihood of fitting the observed ξ distribution as a function of the ﹩\bar{i}﹩ and ﹩\bar{e}﹩ assumed in modeling the ξ distributions, which gives the 1σ confidence intervals of ﹩\bar{i}﹩ and ﹩\bar{e}﹩. The metallicity increases from the top to the bottom panels, i.e., [Fe/H] < −0.02, −0.02 ≤ [Fe/H] < 0.16, and [Fe/H] ≥ 0.16, respectively.
Paper: Planetary Orbit Eccentricity Trends (POET). I. The Eccentricity–Metallicity Trend for Small Planets Revealed by the LAMOST–Gaia–Kepler Sample
Authors: Dong-Sheng An, 东升 安, Ji-Wei Xie, 基伟 谢, Yuan-Zhe Dai, 远哲 戴, Ji-Lin Zhou, 济林 周
Figure caption: Mean eccentricities (median ﹩\bar{e}﹩ from Sections 4.1.1 and 4.1.2) vs. [Fe/H] (median [Fe/H] of each subsample), where the error bars represent the 1σ uncertainties of the mean eccentricity. The gray dashed lines are the boundaries of each subsample. The boundaries between each subsample change by less than 0.01 after the parameter control, so we do not update the boundaries here. In addition, the result of the highest metallicity subsample before the parameter control has been artificially moved to the left by 0.02 dex to avoid overlapping symbols.
Paper: Planetary Orbit Eccentricity Trends (POET). I. The Eccentricity–Metallicity Trend for Small Planets Revealed by the LAMOST–Gaia–Kepler Sample
Authors: Dong-Sheng An, 东升 安, Ji-Wei Xie, 基伟 谢, Yuan-Zhe Dai, 远哲 戴, Ji-Lin Zhou, 济林 周
Figure caption: Transit duration fitting for multiple transiting systems. Left panels: the cumulative distributions for the modeled and observed (red) TDRs. For comparison, simulations of ﹩\bar{e}=0\mbox{--}0.4﹩ and ﹩\bar{i}=10^\circ ﹩ are shown in gray and simulations of ﹩\bar{e}=0﹩ and ﹩\bar{i}=0^\circ \mbox{--}10^\circ ﹩ are shown in yellow to blue. Right panel: contours of the relative likelihood in the ﹩\bar{e}﹩–﹩\bar{i}﹩ plane. The best fit of ﹩\bar{e}﹩ and ﹩\bar{i}﹩ (also shown as black stars) and the corresponding confidence intervals (1σ, 2σ, and 3σ) are also printed.
Paper: Planetary Orbit Eccentricity Trends (POET). I. The Eccentricity–Metallicity Trend for Small Planets Revealed by the LAMOST–Gaia–Kepler Sample
Authors: Dong-Sheng An, 东升 安, Ji-Wei Xie, 基伟 谢, Yuan-Zhe Dai, 远哲 戴, Ji-Lin Zhou, 济林 周
Figure caption: Transit duration fitting for single transiting systems. Left panels: the cumulative distributions for modeled (gray) and observed (red) TDRs. The range of metallicity and the number of planets for each subsample are also printed. Right panels: the relative likelihood of fitting the observed TDR distribution vs. the ﹩\bar{e}﹩ assumed in the modeled TDR distributions, which gives the 1σ, 2σ, and 3σ confidence intervals of ﹩\bar{e}﹩.
Paper: Planetary Orbit Eccentricity Trends (POET). I. The Eccentricity–Metallicity Trend for Small Planets Revealed by the LAMOST–Gaia–Kepler Sample
Authors: Dong-Sheng An, 东升 安, Ji-Wei Xie, 基伟 谢, Yuan-Zhe Dai, 远哲 戴, Ji-Lin Zhou, 济林 周
Figure caption: Same as Figure 4, but the results after applying parameter control to T eff, M *, P, and R  p .
Paper: Planetary Orbit Eccentricity Trends (POET). I. The Eccentricity–Metallicity Trend for Small Planets Revealed by the LAMOST–Gaia–Kepler Sample
Authors: Dong-Sheng An, 东升 安, Ji-Wei Xie, 基伟 谢, Yuan-Zhe Dai, 远哲 戴, Ji-Lin Zhou, 济林 周
Figure caption: Same as Figure 4, but results for the four subsamples after the parameter control on T eff, M *, P, and R  p .
Paper: Planetary Orbit Eccentricity Trends (POET). I. The Eccentricity–Metallicity Trend for Small Planets Revealed by the LAMOST–Gaia–Kepler Sample
Authors: Dong-Sheng An, 东升 安, Ji-Wei Xie, 基伟 谢, Yuan-Zhe Dai, 远哲 戴, Ji-Lin Zhou, 济林 周
Figure caption: Left panel: the fits for the three subsamples, where the turquoise dashed line represents the exponential best fit. ΔAIC is the AIC difference between the constant and exponential best fits. The light turquoise band is the 1σ confidence interval for the exponential best fit. Right panel: same as the left panel, but shows the fits for the four subsamples.
Paper: Planetary Orbit Eccentricity Trends (POET). I. The Eccentricity–Metallicity Trend for Small Planets Revealed by the LAMOST–Gaia–Kepler Sample
Authors: Dong-Sheng An, 东升 安, Ji-Wei Xie, 基伟 谢, Yuan-Zhe Dai, 远哲 戴, Ji-Lin Zhou, 济林 周
Figure caption: Mean mutual inclination ﹩\bar{i}﹩ of multiple transiting systems constrained by their ξ distributions (Section 4.2.2) as a function of [Fe/H]. Each point (squares) represents the median of [Fe/H] and ﹩\bar{i}﹩ in each subsample.
Paper: Planetary Orbit Eccentricity Trends (POET). I. The Eccentricity–Metallicity Trend for Small Planets Revealed by the LAMOST–Gaia–Kepler Sample
Authors: Dong-Sheng An, 东升 安, Ji-Wei Xie, 基伟 谢, Yuan-Zhe Dai, 远哲 戴, Ji-Lin Zhou, 济林 周
Figure caption: Planet eccentricity (e) as a function of the stellar metallicity ([Fe/H]) for single (left panel) and multiple (right panel) systems in the RV sample. For the RV singles, the data prefer an exponential model and the best fit is denoted by the gray dashed lines. For comparison, we also plot the best fit for Kepler singles (Section 4.1.4, the turquoise dashed lines). The colored bands represent the 1σ confidence interval of the exponential best fit. For the RV multiples, the data prefer a flat model, e = 0.12 (gray dashed line). For comparison, we also plot the best fit of Kepler multiples (﹩\bar{e}=0.03﹩, the yellow dashed line).
Paper: Planetary Orbit Eccentricity Trends (POET). I. The Eccentricity–Metallicity Trend for Small Planets Revealed by the LAMOST–Gaia–Kepler Sample
Authors: Dong-Sheng An, 东升 安, Ji-Wei Xie, 基伟 谢, Yuan-Zhe Dai, 远哲 戴, Ji-Lin Zhou, 济林 周
Figure caption: Same as Figure 6, but results for the consideration of an asymmetric density distribution.
Paper: Measuring the Obliquities of the TRAPPIST-1 Planets with MAROON-X
Authors: Madison Brady, Jacob L. Bean, Andreas Seifahrt, David Kasper, Rafael Luque, Ansgar Reiners, Björn Benneke, Gudmundur Stefánsson, Julian Stürmer
Figure caption: The observed RVs for the TRAPPIST-1 planets, with the best-fit RM effect model overplotted in red. Each individual transit is plotted separately. The x-axis is expressed in time since mid-transit, with the mid-transit time defined as that corresponding to the fit values from Section 3.2.
Paper: Measuring the Obliquities of the TRAPPIST-1 Planets with MAROON-X
Authors: Madison Brady, Jacob L. Bean, Andreas Seifahrt, David Kasper, Rafael Luque, Ansgar Reiners, Björn Benneke, Gudmundur Stefánsson, Julian Stürmer
Figure caption: The peak S/N of the each template spectral order vs. wavelength, in Å. The template including only out-of-transit data is shown in black, while the template including all TRAPPIST-1 data is shown in red. Only data from the redder channel of MAROON-X are included, as the blue channel data have very low signals.
Paper: Measuring the Obliquities of the TRAPPIST-1 Planets with MAROON-X
Authors: Madison Brady, Jacob L. Bean, Andreas Seifahrt, David Kasper, Rafael Luque, Ansgar Reiners, Björn Benneke, Gudmundur Stefánsson, Julian Stürmer
Figure caption: The Doppler tomography signals of the nine observed transits, in order of observation date (c, g, b, e, e, d, c, d, and f). The leftmost column shows the data residuals without accounting for Doppler shadow. The center column shows the expected tomographic signal for a Doppler tomography model, plotted on the same color axis as the data. The model has a ﹩v\,\sin \,i﹩ = 2.1 km s−1 and λ = 0°, in accordance with what was found in Section 3.2, and a FWHM = 3.2 km s−1, which is a rough estimate of the FWHM taken directly from the shape of the out-of-transit CCF profile. The right column shows the data residuals with the model subtracted. The gray dashed lines show the beginning and end times of each transit. The data in-transit appear noisier than the data out-of-transit primarily due to the shorter exposure times. The velocities are binned in increments of 2 km s−1, which is slightly smaller than the binning of 3.5 km s−1 used in our analysis. This is primarily for the purposes of demonstrating the theoretical shape of the modeled signal, which is difficult to display with a coarser binning.
Paper: Multibeam Blind Search of Targeted SETI Observations toward 33 Exoplanet Systems with FAST
Authors: Xiao-Hang Luan, Zhen-Zhao Tao, Hai-Chen Zhao, Bo-Lun Huang, Shi-Yu Li, Cong Liu, Hong-Feng Wang, Wen-Fei Liu, Tong-Jie Zhang, Vishal Gajjar, Dan Werthimer
Figure caption: The distributions of frequency, drift rate, and S/N in XX polarization. The frequency bands of the cataloged interference sources are displayed on the frequency panel. The dark blue bars show the distributions of the hits detected by all 19 beams. The light blue bars show the distributions of the events removed the zero drift rate signals and detected by the MBCM blind search mode. The yellow bars show the events passed by manual visual inspection.
Paper: Measuring the Obliquities of the TRAPPIST-1 Planets with MAROON-X
Authors: Madison Brady, Jacob L. Bean, Andreas Seifahrt, David Kasper, Rafael Luque, Ansgar Reiners, Björn Benneke, Gudmundur Stefánsson, Julian Stürmer
Figure caption: The CCF FWHM as a function of the ﹩v\,\sin \,i﹩ used to broaden the template spectrum. Each line represents a different order, where the colors are determined by the central wavelength of the order (redder orders are redder, bluer orders are bluer). The dashed gray lines represent orders that were not used in our final analysis.