adsabs/AstroCLIMB huggingface dataset:
Paper: Ultradeep Imaging of Nearby Dwarf Irregular Galaxies: Young Objects in the Far Outer Disk
Authors: Deidre A. Hunter, Hong-Xin Zhang, Bruce G. Elmegreen, Ella R. Castelloe, Hannah Michaye Ledford, Ishara Nisley, Ryuga Hatano
Figure caption: DDO 187’s objects with FUV emission in the far outer disk are circled in black/white on the V (top) and FUV (bottom) images. The red ellipses and blue circles are as in Figure 4.
Paper: Ultradeep Imaging of Nearby Dwarf Irregular Galaxies: Young Objects in the Far Outer Disk
Authors: Deidre A. Hunter, Hong-Xin Zhang, Bruce G. Elmegreen, Ella R. Castelloe, Hannah Michaye Ledford, Ishara Nisley, Ryuga Hatano
Figure caption: DDO 69’s objects with FUV emission in the far outer disk are circled in black/white on the V (top) and FUV (bottom) images. The red ellipses and blue circles are as in Figure 4.
Paper: Ultradeep Imaging of Nearby Dwarf Irregular Galaxies: Young Objects in the Far Outer Disk
Authors: Deidre A. Hunter, Hong-Xin Zhang, Bruce G. Elmegreen, Ella R. Castelloe, Hannah Michaye Ledford, Ishara Nisley, Ryuga Hatano
Figure caption: DDO 47’s objects with FUV emission in the far outer disk are circled in black on the V (top) and FUV (bottom) images. The red ellipses and blue circles are as in Figure 4.
Paper: Ultradeep Imaging of Nearby Dwarf Irregular Galaxies: Young Objects in the Far Outer Disk
Authors: Deidre A. Hunter, Hong-Xin Zhang, Bruce G. Elmegreen, Ella R. Castelloe, Hannah Michaye Ledford, Ishara Nisley, Ryuga Hatano
Figure caption: CMDs and CCDs for far disk objects in DDO 47 with FUV emission. Quantities are corrected for foreground extinction. Dashed lines are single-age stellar population Z = 0.004 metallicity models from G. Bruzual & S. Charlot (2003), one scaled to a cluster of 15,000 M⊙ and the other to 2500 M⊙. The red ×'s mark the age of the model cluster in gigayears, so the first three from the left are 3, 10, and 30 Myr.
Paper: Ultradeep Imaging of Nearby Dwarf Irregular Galaxies: Young Objects in the Far Outer Disk
Authors: Deidre A. Hunter, Hong-Xin Zhang, Bruce G. Elmegreen, Ella R. Castelloe, Hannah Michaye Ledford, Ishara Nisley, Ryuga Hatano
Figure caption: CMDs and CCDs for far disk objects in DDO 46 with FUV emission. Quantities are corrected for foreground extinction. Dashed lines are single-age stellar population Z = 0.004 metallicity models from G. Bruzual & S. Charlot (2003), one scaled to a cluster of 3000 M⊙ and the other to 100 M⊙. The red ×'s mark the age of the model cluster in gigayears, so the first three from the left are 3, 10, and 30 Myr.
Paper: Ultradeep Imaging of Nearby Dwarf Irregular Galaxies: Young Objects in the Far Outer Disk
Authors: Deidre A. Hunter, Hong-Xin Zhang, Bruce G. Elmegreen, Ella R. Castelloe, Hannah Michaye Ledford, Ishara Nisley, Ryuga Hatano
Figure caption: CMDs and CCDs for far disk objects in DDO 187 with FUV emission. Dashed lines are single-age stellar population Z = 0.004 metallicity models from G. Bruzual & S. Charlot (2003), one scaled to a cluster of 15,000 M⊙ and the other to 2500 M⊙. The red ×'s mark the age of the model cluster in gigayears, so the first three from the left are 3, 10, and 30 Myr.
Paper: Ultradeep Imaging of Nearby Dwarf Irregular Galaxies: Young Objects in the Far Outer Disk
Authors: Deidre A. Hunter, Hong-Xin Zhang, Bruce G. Elmegreen, Ella R. Castelloe, Hannah Michaye Ledford, Ishara Nisley, Ryuga Hatano
Figure caption: CMDs and CCDs for far disk objects in DDO 69 with FUV emission. The dashed line is a single-age stellar population Z = 0.0004 metallicity model from G. Bruzual & S. Charlot (2003) scaled to a cluster mass of 30,000 M⊙. The red ×'s mark the age of the model cluster in gigayears, so the first three from the left are 3, 10, and 30 Myr.
Paper: Survey of Oxygen-rich AGB Stars Using the KVN 4 Receiving Bands—SMASTES. I.
Authors: Hyeon Baek, Se-Hyung Cho, Jaeheon Kim, Seung-Min Son, Dong-Hwan Yoon, Kyung-Won Suh
Figure caption: Measured expansion velocities of simultaneously observed molecular lines according to radial distances from the central star for 11 HCN detected sources. The distances of the dominant line formation region in units of stellar radius from the central star are as follows. SiO maser adopted 3 R* as the median value between 2 and 4 R* (P. Diamond et al. 1994; D. A. Boboltz & M. Wittkowski 2005), H2O maser adopted 36 R* (A. Richards et al. 2012) and 120 R* for HCN, 210 R* for the SiS, 440 R* for the SiO thermal lines, and 1300 R* for CO based on the median values measured by S. Wallström et al. (2024). These values are indicated at the top of the graph. The vertical dashed line indicates dust condensation radius, Rdust at ∼6 R* derived by C. A. Gottlieb et al. (2022).
Paper: Survey of Oxygen-rich AGB Stars Using the KVN 4 Receiving Bands—SMASTES. I.
Authors: Hyeon Baek, Se-Hyung Cho, Jaeheon Kim, Seung-Min Son, Dong-Hwan Yoon, Kyung-Won Suh
Figure caption: Distributions of the peak and integrated flux (P.F and I.F) ratios of SiO21 to SiO11 for SiO31 detected sources. (a) P.F of Mira, (b) I.F of Mira, (c) P.F of OH/IR, and (d) I.F of OH/IR. The solid line represents the average value of the flux ratios.
Paper: Survey of Oxygen-rich AGB Stars Using the KVN 4 Receiving Bands—SMASTES. I.
Authors: Hyeon Baek, Se-Hyung Cho, Jaeheon Kim, Seung-Min Son, Dong-Hwan Yoon, Kyung-Won Suh
Figure caption: IRAS two-color diagram of observational results for the H2O and SiO masers according to SRs, Miras, and OH/IR stars. The curved dashed line is the evolutionary track defined by W. van der Veen & H. Habing (1988). The blue dashed line indicates the two groups of post-AGB stars, LI (left of IRAS, blue group) and RI (Right of IRAS, red group; M. N. Sevenster 2002). Undetected sources are marked with the yellow inverted filled triangles, the green filled triangles represent sources with H2O maser only detected sources, the blue triangles, circles, and squares indicate sources with SiO maser only detected sources, and the pink triangles, circles, and squares indicate sources with both H2O and SiO maser detected sources. Triangles represent SRs, squares represent Miras, and circles represent OH/IR stars. The numbers indicate identification numbers in Table 1. The numbers indicated on the graph correspond to sources where SiO22 has been detected (#17, #21, #22, and #99), three famous sources for each type of SRs, Miras, and OH/IR stars (in total, nine stars) mentioned in Section 3 (#3, #13, #22, #50, #62, #83, #99, #106, and #117) and mentioned in Section 4.4 (#21, #26, #27, #46, #49, #79 and #99).
Paper: Survey of Oxygen-rich AGB Stars Using the KVN 4 Receiving Bands—SMASTES. I.
Authors: Hyeon Baek, Se-Hyung Cho, Jaeheon Kim, Seung-Min Son, Dong-Hwan Yoon, Kyung-Won Suh
Figure caption: IRAS two-color diagram of observational results for the P.F values of SiO21 and SiO11 masers according to the SRs, Miras, and OH/IR stars. Sources with a higher P.F value for SiO11 than SiO21 are marked in green, while those with a higher P.F value for SiO21 are marked in red. SiO21-only sources are identified in black with numbers (V Leo (#47) and OH43.8+0.5 (#112)). The curved and blue dashed lines represent the same as in Figure 8.
Paper: Survey of Oxygen-rich AGB Stars Using the KVN 4 Receiving Bands—SMASTES. I.
Authors: Hyeon Baek, Se-Hyung Cho, Jaeheon Kim, Seung-Min Son, Dong-Hwan Yoon, Kyung-Won Suh
Figure caption: IRAS two-color diagram of observational results for the SiO12 and SiO13 masers according to the SRs, Miras, and OH/IR stars. The curved and blue dashed lines represent the same as in Figure 8. The sources where SiO11 and SiO12 are detected are shown in blue, while those where SiO11, SiO12, and SiO13 are all detected are shown in pink.
Paper: Survey of Oxygen-rich AGB Stars Using the KVN 4 Receiving Bands—SMASTES. I.
Authors: Hyeon Baek, Se-Hyung Cho, Jaeheon Kim, Seung-Min Son, Dong-Hwan Yoon, Kyung-Won Suh
Figure caption: Distributions of the P.F and I.F ratios of SiO13 to SiO11. (a) P.F of SR, (b) I.F of SR, (c) P.F of Mira, (d) I.F of Mira, (e) P.F of OH/IR, and (f) I.F of OH/IR. The solid line represents the average value of the flux ratios.
Paper: Two Ultralow-mass-ratio Binary Systems at Critical Evolutionary Stages
Authors: Di-Fu Guo, Kai Li, Fen Liu, Li-heng Wang, Huai-Zhen Li, Xu Chen, Xiang Gao
Figure caption: The left panel shows the O − C diagram of J053525, while the right panel displays the O − C diagram J175200. Different symbols refer to different observations.
Paper: Two Ultralow-mass-ratio Binary Systems at Critical Evolutionary Stages
Authors: Di-Fu Guo, Kai Li, Fen Liu, Li-heng Wang, Huai-Zhen Li, Xu Chen, Xiang Gao
Figure caption: The left panel shows the RcIc light curves of J053525 obtained by the 50 cm telescope at Weideng station of Weihai Observatory. The right panel shows the VRcIc light curves of J175200 derived from the 100 cm telescope at Weihai Observatory.
Paper: Two Ultralow-mass-ratio Binary Systems at Critical Evolutionary Stages
Authors: Di-Fu Guo, Kai Li, Fen Liu, Li-heng Wang, Huai-Zhen Li, Xu Chen, Xiang Gao
Figure caption: The normalized TESS light curves of J053525 observed across different sectors. For comparison, all the light curves are overlaid in the last panel.
Paper: Two Ultralow-mass-ratio Binary Systems at Critical Evolutionary Stages
Authors: Di-Fu Guo, Kai Li, Fen Liu, Li-heng Wang, Huai-Zhen Li, Xu Chen, Xiang Gao
Figure caption: Similar to Figure 2, but showing the light curves for J175200.
Paper: The Transit Signal of KOI-1755 Originates from a Background Eclipsing Binary Star—Extracting the Light Curve of a Faint Background Star from Kepler Target Pixel File Data
Authors: Haozhi Wang, Ali Esamdin, Chenglong Lv, Lixian Shen, Jin-zhong Liu, Abdusamatjan Iskandar, Umut Mahmut, Rivkat Karimov, Shuhrat A. Ehgamberdiev
Figure caption: Top panel: contamination-corrected TSS starlight curve for all quarters. Middle panel: final light curve for the TSS Star. Bottom panel: local final light curve for the TSS star.
Paper: The Transit Signal of KOI-1755 Originates from a Background Eclipsing Binary Star—Extracting the Light Curve of a Faint Background Star from Kepler Target Pixel File Data
Authors: Haozhi Wang, Ali Esamdin, Chenglong Lv, Lixian Shen, Jin-zhong Liu, Abdusamatjan Iskandar, Umut Mahmut, Rivkat Karimov, Shuhrat A. Ehgamberdiev
Figure caption: Top panel: the phase-folded light curve was obtained using the eclipse frequency fecl listed in Table 5. The white line represents the smoothed curve derived by averaging the data within phase bins. Bottom panel: a zoomed-in view around the primary eclipse phase (0.55–0.65).
Paper: The Transit Signal of KOI-1755 Originates from a Background Eclipsing Binary Star—Extracting the Light Curve of a Faint Background Star from Kepler Target Pixel File Data
Authors: Haozhi Wang, Ali Esamdin, Chenglong Lv, Lixian Shen, Jin-zhong Liu, Abdusamatjan Iskandar, Umut Mahmut, Rivkat Karimov, Shuhrat A. Ehgamberdiev
Figure caption: Top panel: amplitude spectrum of the TSS star’s light curve. Bottom panel: local amplitude spectrum of the low-frequency region.
Paper: The Transit Signal of KOI-1755 Originates from a Background Eclipsing Binary Star—Extracting the Light Curve of a Faint Background Star from Kepler Target Pixel File Data
Authors: Haozhi Wang, Ali Esamdin, Chenglong Lv, Lixian Shen, Jin-zhong Liu, Abdusamatjan Iskandar, Umut Mahmut, Rivkat Karimov, Shuhrat A. Ehgamberdiev
Figure caption: The magnitude-based light curve of the TSS star.
Paper: Meteoroid Stream Identification with HDBSCAN Unsupervised Clustering Algorithm
Authors: Eloy Peña-Asensio, Fabio Ferrari
Figure caption: The top row displays the geocentric radiant distribution in a Mollweide projection, where R.A. is mapped along the horizontal axis and decl. along the vertical axis, with the ecliptic plane shown as a solid yellow line. The bottom row presents the principal component analysis results for meteor showers using the ORBIT (left), GEO (center), and LUTAB (right) vectors. Arrows indicate the loadings of the original vector components (v) of ORBIT, GEO, and LUTAB, illustrating their influence on the first two principal components. In both rows, meteors are colored according to their CAMS meteor shower classification, while sporadic events are represented by smaller black points. GEO is represented here with Z-score normalization as well.
Paper: Meteoroid Stream Identification with HDBSCAN Unsupervised Clustering Algorithm
Authors: Eloy Peña-Asensio, Fabio Ferrari
Figure caption: Sporadic percentage (blue lines) and the number of clusters (red lines) obtained from the HDBSCAN clustering algorithm as a function of the minimum cluster size for the (top) eom and (bottom) leaf selection methods. Solid lines represent the ORBIT vector, dashed lines correspond to GEO, and dashed–dotted lines indicate LUTAB. For reference, CAMS values are shown as dots with horizontal dotted lines for the minimum cluster size of 100.
Paper: Collision Probability Evaluation of LAMOST Robotic Fiber Positioners in the Design Phase
Authors: Baolong Chen, Jianping Wang, Jiahao Zhou, Zhigang Liu, Hongzhuan Hu, Zengxiang Zhou, Feifan Zhang
Figure caption: Results of different methods. (a) The Monte Carlo method. (b) Residuals between the Monte Carlo and mathematical methods (results are normalized). In each plot, the color depth represents the normalized collision probability, with darker colors indicating higher collision probabilities.
Paper: Collision Probability Evaluation of LAMOST Robotic Fiber Positioners in the Design Phase
Authors: Baolong Chen, Jianping Wang, Jiahao Zhou, Zhigang Liu, Hongzhuan Hu, Zengxiang Zhou, Feifan Zhang
Figure caption: The diagram illustrating the calculation of collision probability. The green, blue, and yellow areas represent the patrol area of one positioner, the potential collision zones of the eccentric arm, and the conflict area, respectively. The red areas represent the actual inner and outer diameters, considering obstacle avoidance.
Paper: Collision Probability Evaluation of LAMOST Robotic Fiber Positioners in the Design Phase
Authors: Baolong Chen, Jianping Wang, Jiahao Zhou, Zhigang Liu, Hongzhuan Hu, Zengxiang Zhou, Feifan Zhang
Figure caption: This distribution map shows seven RFP. The larger circles represent the actual movement areas, while the smaller circles denote the theoretical movement areas of the RFP. The light blue area indicates the theoretical conflict zone, excluding the fiber heads’ physical volume. The gray area accounts for the additional physical volume needed to avoid collisions with the fiber positioner’s eccentric arm. The pitch is 25.6 mm, leaving little remaining safety area.
Paper: Collision Probability Evaluation of LAMOST Robotic Fiber Positioners in the Design Phase
Authors: Baolong Chen, Jianping Wang, Jiahao Zhou, Zhigang Liu, Hongzhuan Hu, Zengxiang Zhou, Feifan Zhang
Figure caption: Comparison of three different collision cases. (a) Type 1: two RFP do not collide with each other. (b) Type 2: the RFP experiences collisions limited to its neighboring ring of positioners. (c) Type 3: this collision involves the RFP’s collision with RFP more than its neighbor positioners. In the images, the green region represents the area covered by a single RFP, the yellow region is covered by two RFPs, and the red region is covered by three RFPs.
Paper: Collision Probability Evaluation of LAMOST Robotic Fiber Positioners in the Design Phase
Authors: Baolong Chen, Jianping Wang, Jiahao Zhou, Zhigang Liu, Hongzhuan Hu, Zengxiang Zhou, Feifan Zhang
Figure caption: This distribution map shows the best results when changing arm length ratio and pitch.
Paper: Collision Probability Evaluation of LAMOST Robotic Fiber Positioners in the Design Phase
Authors: Baolong Chen, Jianping Wang, Jiahao Zhou, Zhigang Liu, Hongzhuan Hu, Zengxiang Zhou, Feifan Zhang
Figure caption: Distance computation between RFPs. The thick black line represents the simplified segment of the RFP. The blue arrowed line segment represents the distance between RFPs.
Paper: Collision Probability Evaluation of LAMOST Robotic Fiber Positioners in the Design Phase
Authors: Baolong Chen, Jianping Wang, Jiahao Zhou, Zhigang Liu, Hongzhuan Hu, Zengxiang Zhou, Feifan Zhang
Figure caption: Collision probability calculation flowchart.
Paper: Regression for Astronomical Data with Realistic Distributions, Errors, and Nonlinearity
Authors: Tao Jing, Cheng Li
Figure caption: The residual distribution of k and b for OLS, WLS, ODR, wODR, and mODR. The black histogram represents the distribution of all data sets in Sample 1, while the red and blue histograms represent the distribution of the data sets with intrinsic value higher and lower than zero, respectively. The vertical dashed lines show the median value of the distribution with the same color. The median of the residuals for the entire data set (μr), half of the difference between the 84% and 16% quantiles (σr), the extreme error fraction (η), the median of the residuals for the subsample with true values greater than zero (μr,>0), and the median for the subsample with true values less than zero (μr,<0) are presented in each panel.
Paper: Regression for Astronomical Data with Realistic Distributions, Errors, and Nonlinearity
Authors: Tao Jing, Cheng Li
Figure caption: Same as Figure 1, but for LINMIX, LtsFit, Leopy, the ML-based method, and the KS-test-based method. The bottom row is added to show the residual distribution of σ. Only the distribution of all data sets is shown in the bottom row because of the nonnegative nature of σ.
Paper: Stellar Obliquity of the Ultra-short-period Planet System HD 93963
Authors: Huan-Yu Teng, 环宇 滕, Fei Dai, 飞 戴, Andrew W. Howard, Samuel Halverson, Howard Isaacson, Eiichiro Kokubo, 英一郎 小久保, Ryan A. Rubenzahl, Benjamin Fulton, Aaron Householder, Jack Lubin, Steven Giacalone, Luke Handley, Judah Van Zandt, Erik A. Petigura, J. M. Joel Ong, 加冕 王, Pranav Premnath, Haochuan Yu, 皓川 于, Steven R. Gibson, Kodi Rider, Arpita Roy, Ashley Baker, Jerry Edelstein, Chris Smith, Josh Walawender, Byeong-Cheol Lee, Yu-Juan Liu, 玉娟 刘, Joshua N. Winn
Figure caption: Top: normalized spectra of the Hα line during a transit event of planet c with the color indicating the observation number (epoch). The dashed line marks the line center at 6564.7 Å, and the dotted lines indicate 1 Å from the line center. Left: excess absorption of Hα variation with time, with the absorption referenced by a spectrum averaged from preingress and postegress spectra, and calculated in a bandpass of 2 Å centered at 6564.7 Å. The color scale is the same for the top subplot. The dashed line and dotted line indicate midtransit and ingress/egress, respectively. Bottom right (main plot): the measured Hα line profile residuals as a function of time and wavelength. The dashed line and vertical dotted line correspond to the top subplot, while the horizontal dotted line indicates the egress as in the left subplot. The predicted planetary velocity is marked by a green solid line. Neither excess absorption nor color shift occurred during the transit event.
Paper: Stellar Obliquity of the Ultra-short-period Planet System HD 93963
Authors: Huan-Yu Teng, 环宇 滕, Fei Dai, 飞 戴, Andrew W. Howard, Samuel Halverson, Howard Isaacson, Eiichiro Kokubo, 英一郎 小久保, Ryan A. Rubenzahl, Benjamin Fulton, Aaron Householder, Jack Lubin, Steven Giacalone, Luke Handley, Judah Van Zandt, Erik A. Petigura, J. M. Joel Ong, 加冕 王, Pranav Premnath, Haochuan Yu, 皓川 于, Steven R. Gibson, Kodi Rider, Arpita Roy, Ashley Baker, Jerry Edelstein, Chris Smith, Josh Walawender, Byeong-Cheol Lee, Yu-Juan Liu, 玉娟 刘, Joshua N. Winn
Figure caption: Top two panels: TESS 2 minute cadence light curves of HD 93963 A, with the upper plot showing Sector 22 and lower plot showing Sector 48. Smoothed light curves are also plotted, to give a clearer view of the stellar variation. Transits of planets b and c are marked in blue and orange, respectively. Bottom three panels: period analysis of the TESS light curves. The top and middle panels show Lomb–Scargle periodograms of the light curves from Sectors 22 and 48, respectively. The bottom panel shows the autocorrelation function (ACF) of the light curves from Sectors 22 and 48, with rotational periods and harmonics marked.
Paper: Stellar Obliquity of the Ultra-short-period Planet System HD 93963
Authors: Huan-Yu Teng, 环宇 滕, Fei Dai, 飞 戴, Andrew W. Howard, Samuel Halverson, Howard Isaacson, Eiichiro Kokubo, 英一郎 小久保, Ryan A. Rubenzahl, Benjamin Fulton, Aaron Householder, Jack Lubin, Steven Giacalone, Luke Handley, Judah Van Zandt, Erik A. Petigura, J. M. Joel Ong, 加冕 王, Pranav Premnath, Haochuan Yu, 皓川 于, Steven R. Gibson, Kodi Rider, Arpita Roy, Ashley Baker, Jerry Edelstein, Chris Smith, Josh Walawender, Byeong-Cheol Lee, Yu-Juan Liu, 玉娟 刘, Joshua N. Winn
Figure caption: 3D illustrations of transit shadow bands on the celestial sphere. Upper: a single transit toy model. The figure is modified from Figure 3 in J. N. Winn (2010), illustrating the geometry of a single transiting planet case. Lower: cases that both planets can transit, with the left one illustrating a simulated HD 93963 Ab and Ac, and right one illustrating HD 3167 b and c. The blue band and orange band respectively show two transit shadow bands of two transiting planets. The pink region shows the overlapping region, indicating the region where transits of both planets can be observed. The area of the pink region of the HD 3167 literature configuration is 0.0045.
Paper: Stellar Obliquity of the Ultra-short-period Planet System HD 93963
Authors: Huan-Yu Teng, 环宇 滕, Fei Dai, 飞 戴, Andrew W. Howard, Samuel Halverson, Howard Isaacson, Eiichiro Kokubo, 英一郎 小久保, Ryan A. Rubenzahl, Benjamin Fulton, Aaron Householder, Jack Lubin, Steven Giacalone, Luke Handley, Judah Van Zandt, Erik A. Petigura, J. M. Joel Ong, 加冕 王, Pranav Premnath, Haochuan Yu, 皓川 于, Steven R. Gibson, Kodi Rider, Arpita Roy, Ashley Baker, Jerry Edelstein, Chris Smith, Josh Walawender, Byeong-Cheol Lee, Yu-Juan Liu, 玉娟 刘, Joshua N. Winn
Figure caption: The dominant precession pattern of the planet b (USP) changes as the J2 value changes. The left panel shows the star having J2 = 1.0 × 10−4, where planets b and c precess follow different eigenmodes, while the right panels shows the stars having J2 = 1.0 × 10−5 where planets b and c mainly precess at the same eigenmode. A comparison providing various J2 values is in Figure 13 in the Appendix.
Paper: Stellar Obliquity of the Ultra-short-period Planet System HD 93963
Authors: Huan-Yu Teng, 环宇 滕, Fei Dai, 飞 戴, Andrew W. Howard, Samuel Halverson, Howard Isaacson, Eiichiro Kokubo, 英一郎 小久保, Ryan A. Rubenzahl, Benjamin Fulton, Aaron Householder, Jack Lubin, Steven Giacalone, Luke Handley, Judah Van Zandt, Erik A. Petigura, J. M. Joel Ong, 加冕 王, Pranav Premnath, Haochuan Yu, 皓川 于, Steven R. Gibson, Kodi Rider, Arpita Roy, Ashley Baker, Jerry Edelstein, Chris Smith, Josh Walawender, Byeong-Cheol Lee, Yu-Juan Liu, 玉娟 刘, Joshua N. Winn
Figure caption: Planetary systems containing USP planets and having measured obliquities. Host stars are represented by filled circles, with their effective temperatures indicated by color. The stellar spin orientation and orbital planes are marked by dotted arrows and solid lines, respectively. Planets are depicted as circles on the right part of the figure, where larger circles correspond to more massive planets. The color of each circle reflects the true stellar obliquity from observations, while gray circles represent transiting planets without obliquity measurements, and white circles represent nontransiting planets. Notably, the outer cold giant planet of HD 93963 system has not been confirmed.