adsabs/AstroCLIMB huggingface dataset:
Paper: Down But Not Out: The Case of Long-period Comet C/2021 O3 (Panstarrs)
Authors: David Jewitt, Jing Li, Michael Jaeger, Yoonyoung Kim
Figure caption: Composite from STEREO-A computed from 173 COR2 images taken in the period UT 2022 April 27.6 to 30.6 (DOY 482 to 485). Arrows show the projected negative heliocentric velocity vector (−V) and the projected antisolar direction (−S), both for the midtime (UT 2022 April 29.1) of the observation sequence. The cardinal directions and a 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 diameter circle representing the apparent diameter of the Sun are also shown.
Paper: Down But Not Out: The Case of Long-period Comet C/2021 O3 (Panstarrs)
Authors: David Jewitt, Jing Li, Michael Jaeger, Yoonyoung Kim
Figure caption: Single COR2 image at rH = 0.37 au (DOY 483–484) showing the full 8﹩\mathop{.}\limits^{\unicode{x000b0}}﹩4 wide field of view, the central occulting spot, and coronal structures. C/2021 O3 is marked between the two arrows. The cardinal directions and a 1° scale bar are also shown.
Paper: Down But Not Out: The Case of Long-period Comet C/2021 O3 (Panstarrs)
Authors: David Jewitt, Jing Li, Michael Jaeger, Yoonyoung Kim
Figure caption: Preperihelion appearance of C/2021 O3 on UT 2021 September 3 (DOY 246) at rH = 3.865 au. This is a 60 s image through an r′ filter from the CFHT 3.6 m telescope, archived at CADC. A scale bar and cardinal directions are marked.
Paper: An Advanced Deep Learning Model for Identifying Blue Horizontal-branch Stars from LAMOST DR10
Authors: Yuhang Zhang, Yude Bu, Jiangchuan Zhang, Ke Wang, Huili Wu, Mengmeng Zhang, Shanshan Li, Jingzhen Sun, Xiaoming Kong, Zhenping Yi, Meng Liu
Figure caption: BHBNet overview. The collapsed normalized spectrum is input into the network, and the class serves as the network’s label. The RHAM extracts important spectral line features, consisting of three sequentially connected RHABs. The detailed structure of the RHAB is illustrated in panel (b). The CWDM module stacks three GRUs to model the dependencies between the corresponding fluxes at different wavelengths. The detailed structure of the GRU is illustrated in panel (c). The output module produces the final predicted results, consisting of two linear layers. Between the linear layers, a dropout layer is introduced to enhance the network’s generalization ability. During the forward propagation process the model computes the predicted results and evaluates the loss, whereas during the backward propagation process it optimizes the prediction performance by calculating gradients and updating parameters.
Paper: JVLA Measurement of Grain Size in the Compact Dust Ring Around Class I Protostar WL 17
Authors: Jun Hashimoto, Hauyu Baobab Liu, Ruobing Dong, Beibei Liu, Takayuki Muto
Figure caption: The 2–345 GHz spectral profile of WL 17. The top-left panel shows the flux densities obtained from all of our JVLA observations (Table 2) and the previous ALMA observations (H. C. Gulick et al. 2021) assuming nominal 10% (1σ) absolute flux uncertainty. The flux of ALMA observations taken from H. C. Gulick et al. (2021) are not from the data but from modeling (their Table 3), and the fluxes can be underestimated. The sizes of some symbols are larger than the error bars. Gray solid and dashed–dotted lines show the spectral indices of 2.0 and 4.0, respectively. Each of the other panels show the flux densities measured from a specific epoch of our JVLA observations and from the previous ALMA observations, which are overplotted with the dust and free–free emission models that best fit the observations presented in that panel.
Paper: JVLA Measurement of Grain Size in the Compact Dust Ring Around Class I Protostar WL 17
Authors: Jun Hashimoto, Hauyu Baobab Liu, Ruobing Dong, Beibei Liu, Takayuki Muto
Figure caption: The JVLA intraband images of WL 17. The observing frequency and epoch are labeled in each panel. The center of the image corresponds to the stellar position in FK5 J2000.0 at the observing epoch of 2024.1, calculated as (16﹩{}^{{\rm{h}}}2{7}^{{\rm{m}}}06\mathop{.}\limits^{s}﹩7639, ﹩-24^\circ 3{8}^{{\rm{m}}}15\mathop{.}\limits^{s}﹩53589) (see the text for details). The offset between the stellar position and the peak emission is approximately 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩1–0﹩\mathop{.}\limits^{^{\prime\prime} }﹩2. The synthesized beams are represented as white ellipses in the lower-left corner of each image. The beam shape and rms noise are summarized in Table 2.
Paper: JVLA Measurement of Grain Size in the Compact Dust Ring Around Class I Protostar WL 17
Authors: Jun Hashimoto, Hauyu Baobab Liu, Ruobing Dong, Beibei Liu, Takayuki Muto
Figure caption: Same as Figure 1, except different intraband frequency and epoch. The white circles highlight a radio burst from [GY92] 253 (see text in Section 2).
Paper: An Advanced Deep Learning Model for Identifying Blue Horizontal-branch Stars from LAMOST DR10
Authors: Yuhang Zhang, Yude Bu, Jiangchuan Zhang, Ke Wang, Huili Wu, Mengmeng Zhang, Shanshan Li, Jingzhen Sun, Xiaoming Kong, Zhenping Yi, Meng Liu
Figure caption: Predicted uncertainty distributions of BHBNet. The KDE curves in the left panel represent the epistemic uncertainty distributions for the six-class and binary classification models, while those in the right panel illustrate the aleatoric uncertainty distributions. The green and pink dashed lines mark the 90th percentiles of the predicted uncertainty for the six-class and binary classification models, respectively.
Paper: An Advanced Deep Learning Model for Identifying Blue Horizontal-branch Stars from LAMOST DR10
Authors: Yuhang Zhang, Yude Bu, Jiangchuan Zhang, Ke Wang, Huili Wu, Mengmeng Zhang, Shanshan Li, Jingzhen Sun, Xiaoming Kong, Zhenping Yi, Meng Liu
Figure caption: The P-R curve and confusion matrix of the binary classification model constructed through linear-layer transfer training.
Paper: An Advanced Deep Learning Model for Identifying Blue Horizontal-branch Stars from LAMOST DR10
Authors: Yuhang Zhang, Yude Bu, Jiangchuan Zhang, Ke Wang, Huili Wu, Mengmeng Zhang, Shanshan Li, Jingzhen Sun, Xiaoming Kong, Zhenping Yi, Meng Liu
Figure caption: The P-R curve and confusion matrix of the six-class classification model.
Paper: JVLA Measurement of Grain Size in the Compact Dust Ring Around Class I Protostar WL 17
Authors: Jun Hashimoto, Hauyu Baobab Liu, Ruobing Dong, Beibei Liu, Takayuki Muto
Figure caption: Same as Figure 1, except different intraband frequency and epoch.
Paper: The Chemical Clock of High-mass Star-forming Regions: N2H+/CCS
Authors: J. L. Chen, 家梁 陈, J. S. Zhang, 江水 张, J. X. Ge, 继兴 葛, Y. X. Wang, 友鑫 汪, H. Z. Yu, 鸿智 余, Y. P. Zou, 益鹏 邹, Y. T. Yan, 耀庭 闫, X. Y. Wang, 雪莹 王, D. Y. Wei, 丁元 韦
Figure caption: The modeled column density for N2H+ (a) and CCS (b), and their ratio (c) from our best-fit models were plotted as a function of the age for HMSC, HMPO and UC H II stages (solid lines with dashed lines for standard deviation). Those dotted lines show the average values of measured N(N2H+), N(CCS) and their ratio at different stages, with the area for the confidence levels.
Paper: The Spin–Orbit Alignment of Eight Warm Gas Giant Systems 
Authors: Juan I. Espinoza-Retamal, Andrés Jordán, Rafael Brahm, Cristobal Petrovich, Elyar Sedaghati, Guðmundur Stefánsson, Melissa J. Hobson, Marcelo Tala Pinto, Diego J. Muñoz, Gavin Boyle, Rodrigo Leiva, Vincent Suc
Figure caption: Lomb–Scargle periodogram of the K2 light curves of K2-139 (top) and K2-329 A (bottom), with transit data masked out. A false-alarm probability level of 1% is marked with a dashed red line. The highest-power peaks are marked with an arrow, indicating the most likely stellar rotation period. In both cases, an alias corresponding to half the period is also clearly visible.
Paper: The Spin–Orbit Alignment of Eight Warm Gas Giant Systems 
Authors: Juan I. Espinoza-Retamal, Andrés Jordán, Rafael Brahm, Cristobal Petrovich, Elyar Sedaghati, Guðmundur Stefánsson, Melissa J. Hobson, Marcelo Tala Pinto, Diego J. Muñoz, Gavin Boyle, Rodrigo Leiva, Vincent Suc
Figure caption: ESPRESSO observations of the RM effect produced by our different targets (purple—and also pink for K2-329 A b to show the second transit), along with the best model (red). Shaded red areas represent 1σ, 2σ, and 3σ models. All error bars include a white-noise jitter term applied in quadrature to the RV data points. The different data sets are available in Appendix A.
Paper: The Chemical Clock of High-mass Star-forming Regions: N2H+/CCS
Authors: J. L. Chen, 家梁 陈, J. S. Zhang, 江水 张, J. X. Ge, 继兴 葛, Y. X. Wang, 友鑫 汪, H. Z. Yu, 鸿智 余, Y. P. Zou, 益鹏 邹, Y. T. Yan, 耀庭 闫, X. Y. Wang, 雪莹 王, D. Y. Wei, 丁元 韦
Figure caption: Rotational diagrams of CCS for sources with CCS (JN = 87–76) and CCS (JN = 77–66) line detections.
Paper: The Chemical Clock of High-mass Star-forming Regions: N2H+/CCS
Authors: J. L. Chen, 家梁 陈, J. S. Zhang, 江水 张, J. X. Ge, 继兴 葛, Y. X. Wang, 友鑫 汪, H. Z. Yu, 鸿智 余, Y. P. Zou, 益鹏 邹, Y. T. Yan, 耀庭 闫, X. Y. Wang, 雪莹 王, D. Y. Wei, 丁元 韦
Figure caption: The comparison of the optical depth from the intensity ratio and HF fitting method. Sources with only N2H+ detection are in solid black circle, while sources with both N2H+ and CCS detections are in solid red circle. The black dashed line means that both optical depth have the same value.
Paper: The Chemical Clock of High-mass Star-forming Regions: N2H+/CCS
Authors: J. L. Chen, 家梁 陈, J. S. Zhang, 江水 张, J. X. Ge, 继兴 葛, Y. X. Wang, 友鑫 汪, H. Z. Yu, 鸿智 余, Y. P. Zou, 益鹏 邹, Y. T. Yan, 耀庭 闫, X. Y. Wang, 雪莹 王, D. Y. Wei, 丁元 韦
Figure caption: The N(N2H+)/N(CCS) ratio is plotted against the N(N2H+) and the histograms of the x-axis and y-axis on the top and right panel for the three groups (HMSC, HMPO, UC H II) are showed. Sources at three stages can be divided distinctly and a strong correlation between the ratio and the N(N2H+) can be found.
Paper: The Chemical Clock of High-mass Star-forming Regions: N2H+/CCS
Authors: J. L. Chen, 家梁 陈, J. S. Zhang, 江水 张, J. X. Ge, 继兴 葛, Y. X. Wang, 友鑫 汪, H. Z. Yu, 鸿智 余, Y. P. Zou, 益鹏 邹, Y. T. Yan, 耀庭 闫, X. Y. Wang, 雪莹 王, D. Y. Wei, 丁元 韦
Figure caption: N(N2H+)/N(CCS) against the heliocentric distance; no significant variation can be found between them.
Paper: The Chemical Clock of High-mass Star-forming Regions: N2H+/CCS
Authors: J. L. Chen, 家梁 陈, J. S. Zhang, 江水 张, J. X. Ge, 继兴 葛, Y. X. Wang, 友鑫 汪, H. Z. Yu, 鸿智 余, Y. P. Zou, 益鹏 邹, Y. T. Yan, 耀庭 闫, X. Y. Wang, 雪莹 王, D. Y. Wei, 丁元 韦
Figure caption: The cumulative distributions for N(N2H+)/N(CCS) (a), N(N2H+) (b) and N(CCS) (c) for HMSCs, HMPOs, and UC H IIs.
Paper: The Spin–Orbit Alignment of Eight Warm Gas Giant Systems 
Authors: Juan I. Espinoza-Retamal, Andrés Jordán, Rafael Brahm, Cristobal Petrovich, Elyar Sedaghati, Guðmundur Stefánsson, Melissa J. Hobson, Marcelo Tala Pinto, Diego J. Muñoz, Gavin Boyle, Rodrigo Leiva, Vincent Suc
Figure caption: Sky-projected obliquity λ (top panels) and true 3D obliquity ψ (bottom panels) measurements as a function of stellar effective temperature for the sample of planets around single-star (left panels) and known binary/triple systems (right panels). The dashed blue line demarks the Kraft break at Teff ≈ 6100 K. Hot Jupiters (0.4 < Mp/MJ < 13 and a/R⋆ < 11) are shown in red, warm Jupiters (0.4 < Mp/MJ < 13 and a/R⋆ > 11) in orange, and Saturns (0.2 < Mp/MJ < 0.4) in green. Measurements reported in this work are shown as stars, while circles are the data from TEPCat, X.-Y. Wang et al. (2024), and E. Knudstrup et al. (2024).
Paper: The Spin–Orbit Alignment of Eight Warm Gas Giant Systems 
Authors: Juan I. Espinoza-Retamal, Andrés Jordán, Rafael Brahm, Cristobal Petrovich, Elyar Sedaghati, Guðmundur Stefánsson, Melissa J. Hobson, Marcelo Tala Pinto, Diego J. Muñoz, Gavin Boyle, Rodrigo Leiva, Vincent Suc
Figure caption: Inferred stellar obliquity distribution of hot Jupiters (red), warm Jupiters (orange), and Saturns (green). This inference was done from the sky-projected obliquity measurements following the methodology from J. Dong & D. Foreman-Mackey (2023), without including information about the stellar inclination. Shaded regions show 1σ models. (a) Sample of Jovian planets around single stars. (b) Sample of warm planets around single stars. (c) Sample of Jovian planets around binaries/triples.
Paper: The Spin–Orbit Alignment of Eight Warm Gas Giant Systems 
Authors: Juan I. Espinoza-Retamal, Andrés Jordán, Rafael Brahm, Cristobal Petrovich, Elyar Sedaghati, Guðmundur Stefánsson, Melissa J. Hobson, Marcelo Tala Pinto, Diego J. Muñoz, Gavin Boyle, Rodrigo Leiva, Vincent Suc
Figure caption: Observations of K2-139 along with the best model. All error bars include a white-noise jitter term applied in quadrature to the RV and photometric data points. (a) ESPRESSO observations of the RM effect. We show the best model as the red line and the 1σ, 2σ, and 3σ models as the shaded areas. (b) Phase-folded out-of-transit RVs along with the best, 1σ, 2σ, and 3σ models. (c) RV residuals as a function of time. (d–f) Different light curves along with the best model. Data used to create this figure are available as the data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The Spin–Orbit Alignment of Eight Warm Gas Giant Systems 
Authors: Juan I. Espinoza-Retamal, Andrés Jordán, Rafael Brahm, Cristobal Petrovich, Elyar Sedaghati, Guðmundur Stefánsson, Melissa J. Hobson, Marcelo Tala Pinto, Diego J. Muñoz, Gavin Boyle, Rodrigo Leiva, Vincent Suc
Figure caption: Simulated RM effect for a system with the same configuration as TOI-5027 b but assuming an impact parameter of (a) b = 0.25 and (b) b = 0.91. Different colors represent different sky-projected obliquities to show that for high impact parameter values, although the amplitude of the RM effect is lower, the effect becomes highly sensitive to small changes in λ. In particular, the shape becomes asymmetric faster than for the smaller impact parameter case. Thanks to the ESPRESSO capability of detecting such low-amplitude signals, we were able to measure the sky-projected obliquity for TOI-558 b and TOI-5027 b with a relatively good precision.
Paper: The Spin–Orbit Alignment of Eight Warm Gas Giant Systems 
Authors: Juan I. Espinoza-Retamal, Andrés Jordán, Rafael Brahm, Cristobal Petrovich, Elyar Sedaghati, Guðmundur Stefánsson, Melissa J. Hobson, Marcelo Tala Pinto, Diego J. Muñoz, Gavin Boyle, Rodrigo Leiva, Vincent Suc
Figure caption: Sky-projected obliquity as a function of eccentricity for all giant planets (Mp > 0.2MJ) colored by their final scaled semimajor axis ﹩{(a/{R}_{\star })}_{{\rm{final}}}=(a/{R}_{\star })(1-{e}^{2})﹩ to show which gas giants are or will become hot planets with enough time. The left panel shows single stars, while the right panel shows known binary/triple systems. Measurements reported in this work are shown as stars, while circles are the data from TEPCat, X.-Y. Wang et al. (2024), and E. Knudstrup et al. (2024).
Paper: The Spin–Orbit Alignment of Eight Warm Gas Giant Systems 
Authors: Juan I. Espinoza-Retamal, Andrés Jordán, Rafael Brahm, Cristobal Petrovich, Elyar Sedaghati, Guðmundur Stefánsson, Melissa J. Hobson, Marcelo Tala Pinto, Diego J. Muñoz, Gavin Boyle, Rodrigo Leiva, Vincent Suc
Figure caption: Inferred stellar obliquity distribution of hot Jupiters (red) and warm Jupiters (orange) around cool stars below the Kraft break. This inference was done from the sky-projected obliquity measurements following the methodology from J. Dong & D. Foreman-Mackey (2023), without including information about the stellar inclination. Shaded regions show 1σ models.
Paper: The Spin–Orbit Alignment of Eight Warm Gas Giant Systems 
Authors: Juan I. Espinoza-Retamal, Andrés Jordán, Rafael Brahm, Cristobal Petrovich, Elyar Sedaghati, Guðmundur Stefánsson, Melissa J. Hobson, Marcelo Tala Pinto, Diego J. Muñoz, Gavin Boyle, Rodrigo Leiva, Vincent Suc
Figure caption: Same as Figure A1, but for WASP-106. The simultaneous MOANA/ES light curve is shown in green. Data used to create this figure are available as the data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The Spin–Orbit Alignment of Eight Warm Gas Giant Systems 
Authors: Juan I. Espinoza-Retamal, Andrés Jordán, Rafael Brahm, Cristobal Petrovich, Elyar Sedaghati, Guðmundur Stefánsson, Melissa J. Hobson, Marcelo Tala Pinto, Diego J. Muñoz, Gavin Boyle, Rodrigo Leiva, Vincent Suc
Figure caption: Same as Figure A1, but for WASP-130. The simultaneous MOANA/ES light curve is shown in green. Data used to create this figure are available as the data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The Spin–Orbit Alignment of Eight Warm Gas Giant Systems 
Authors: Juan I. Espinoza-Retamal, Andrés Jordán, Rafael Brahm, Cristobal Petrovich, Elyar Sedaghati, Guðmundur Stefánsson, Melissa J. Hobson, Marcelo Tala Pinto, Diego J. Muñoz, Gavin Boyle, Rodrigo Leiva, Vincent Suc
Figure caption: Same as Figure A1, but for K2-329 A. Data used to create this figure are available as the data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The Chemical Clock of High-mass Star-forming Regions: N2H+/CCS
Authors: J. L. Chen, 家梁 陈, J. S. Zhang, 江水 张, J. X. Ge, 继兴 葛, Y. X. Wang, 友鑫 汪, H. Z. Yu, 鸿智 余, Y. P. Zou, 益鹏 邹, Y. T. Yan, 耀庭 闫, X. Y. Wang, 雪莹 王, D. Y. Wei, 丁元 韦
Figure caption: The spectra of N2H+ J = 1−0 (top panels), CCS JN = 87–76 (middle panels) and CCS JN = 77–66 (bottom panels) of our UC H II sample observed by the IRAM 30 m telescope. For those detections, Green Gaussian fit lines were presented. For those six sources that were not observed in CCS JN = 77–66 line, the corresponding panels are blank.
Paper: The Chemical Clock of High-mass Star-forming Regions: N2H+/CCS
Authors: J. L. Chen, 家梁 陈, J. S. Zhang, 江水 张, J. X. Ge, 继兴 葛, Y. X. Wang, 友鑫 汪, H. Z. Yu, 鸿智 余, Y. P. Zou, 益鹏 邹, Y. T. Yan, 耀庭 闫, X. Y. Wang, 雪莹 王, D. Y. Wei, 丁元 韦
Figure caption: The two panels show the comparison of the line width between CCS JN = 87–76 and 77–66 and N2H+ J = 1−0. The black dashed line means that both lines have the same line width.
Paper: The Chemical Clock of High-mass Star-forming Regions: N2H+/CCS
Authors: J. L. Chen, 家梁 陈, J. S. Zhang, 江水 张, J. X. Ge, 继兴 葛, Y. X. Wang, 友鑫 汪, H. Z. Yu, 鸿智 余, Y. P. Zou, 益鹏 邹, Y. T. Yan, 耀庭 闫, X. Y. Wang, 雪莹 王, D. Y. Wei, 丁元 韦
Figure caption: Synthetic N2H+ J = 1−0 spectra for an intrinsic velocity dispersion of 0.6 km s−1 and a Gaussian line shape.
Paper: The Spin–Orbit Alignment of Eight Warm Gas Giant Systems 
Authors: Juan I. Espinoza-Retamal, Andrés Jordán, Rafael Brahm, Cristobal Petrovich, Elyar Sedaghati, Guðmundur Stefánsson, Melissa J. Hobson, Marcelo Tala Pinto, Diego J. Muñoz, Gavin Boyle, Rodrigo Leiva, Vincent Suc
Figure caption: Same as Figure A1, but for TOI-2179. Panel (c) here also shows the RVs as a function of time to show the quadratic RV trend detected at ∼4σ. The simultaneous MOANA/ES light curve is shown in green, with binned data in black. Data used to create this figure are available as the data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The Spin–Orbit Alignment of Eight Warm Gas Giant Systems 
Authors: Juan I. Espinoza-Retamal, Andrés Jordán, Rafael Brahm, Cristobal Petrovich, Elyar Sedaghati, Guðmundur Stefánsson, Melissa J. Hobson, Marcelo Tala Pinto, Diego J. Muñoz, Gavin Boyle, Rodrigo Leiva, Vincent Suc
Figure caption: Same as Figure A1, but for TOI-5027. Panel (c) here also shows the RVs as a function of time to show the linear RV trend detected at ∼3σ. The simultaneous MOANA/ES light curve is shown in green, with binned data in black. Data used to create this figure are available as the data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The Spin–Orbit Alignment of Eight Warm Gas Giant Systems 
Authors: Juan I. Espinoza-Retamal, Andrés Jordán, Rafael Brahm, Cristobal Petrovich, Elyar Sedaghati, Guðmundur Stefánsson, Melissa J. Hobson, Marcelo Tala Pinto, Diego J. Muñoz, Gavin Boyle, Rodrigo Leiva, Vincent Suc
Figure caption: Same as Figure A1, but for TOI-558. The simultaneous MOANA/ES light curve is shown in green. Data used to create this figure are available as the data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The Spin–Orbit Alignment of Eight Warm Gas Giant Systems 
Authors: Juan I. Espinoza-Retamal, Andrés Jordán, Rafael Brahm, Cristobal Petrovich, Elyar Sedaghati, Guðmundur Stefánsson, Melissa J. Hobson, Marcelo Tala Pinto, Diego J. Muñoz, Gavin Boyle, Rodrigo Leiva, Vincent Suc
Figure caption: Same as Figure A1, but for TOI-4515. Data used to create this figure are available as the data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The Epoch of Giant Planet Migration Planet Search Program. III. The Occurrence Rate of Young Giant Planets inside the Water Ice Line 
Authors: Quang H. Tran, Brendan P. Bowler, William D. Cochran, Chad F. Bender, Samuel Halverson, Suvrath Mahadevan, Joe P. Ninan, Paul Robertson, Arpita Roy, Guðmundur Stefánsson, Ryan C. Terrien
Figure caption: The inferred occurrence rates of giant planets orbiting interior to the water ice line of Sun-like stars as a function of age. Schematic decreasing, consistent, and increasing giant planet frequency over time trends, resulting from different migration pathways, are also plotted as gray dashed, solid, and dotted lines, respectively. Our young measurement of ﹩1.9{ \% }_{-1.4 \% }^{+2.6 \% }﹩ and the field-age measurement of 6.5%  ±  0.7% from J. A. Johnson et al. (2010) are displayed in the blue and orange distributions, respectively. The shaded regions under each distribution show the 1σ, 2σ, and 3σ confidence intervals. If the occurrence rate of giant planets increases over time, then dynamical processes are the dominant migration pathway of giant planets. If the giant planet frequency is consistent between young and old systems, then giant planets likely arrived at their present-day locations through disk migration. A decreasing trend suggests that giant planets are efficiently engulfed by their host stars at early ages.
Paper: The Epoch of Giant Planet Migration Planet Search Program. III. The Occurrence Rate of Young Giant Planets inside the Water Ice Line 
Authors: Quang H. Tran, Brendan P. Bowler, William D. Cochran, Chad F. Bender, Samuel Halverson, Suvrath Mahadevan, Joe P. Ninan, Paul Robertson, Arpita Roy, Guðmundur Stefánsson, Ryan C. Terrien
Figure caption: Left: constraints on the giant planet frequency inside the water ice line of Sun-like stars over time, assuming that this evolution follows a power-law functional form. Overplotted is the inferred occurrence rate of giant planets at young (blue circle) and old (orange square) ages. The spread of power-law trends represents the possible evolutionary pathways that the occurrence rate of giant planets may undergo. Right: the distribution of the power-law coefficient, α, generated from the young sample in this work compared with the field-age sample from J. A. Johnson et al. (2010). A positive α corresponds to an increase in the frequency of giant planets over time. A negative α means that the giant planet occurrence rate decays over Gyr timescales. If α is 0, then the frequency remains constant.