adsabs/AstroCLIMB huggingface dataset:
Paper: Deconvolving X-Ray Galaxy Cluster Spectra Using a Recurrent Inference Machine
Authors: Carter Lee Rhea, Julie Hlavacek-Larrondo, Alexandre Adam, Ralph Kraft, Ákos Bogdán, Laurence Perreault-Levasseur, Marine Prunier
Figure caption: Schematic view of the RIM where the teal box represents the RIM itself. As an input, the RIM takes the solution at the previous time step (Equation (4); at time 0 this is the initial solution), xt, and the gradient of the log likelihood (Equation (8)), ﹩{\rm{\nabla }}{\mathfrak{L}}﹩. The RIM returns the update of the solution, Δx(t). This update is fed into Equation (4) to calculate the new solution. This new solution is used to calculate a new gradient of the log likelihood. If t is less than the prescribed maximum value, these new values will be passed back into the RIM to calculate a new update to the solution. Note that we separate the hidden layers, ht, before applying the RIM and combine them after applying the RIM, ht+1. This diagram demonstrates graphically the inputs and outputs of the RIM.
Paper: Deconvolving X-Ray Galaxy Cluster Spectra Using a Recurrent Inference Machine
Authors: Carter Lee Rhea, Julie Hlavacek-Larrondo, Alexandre Adam, Ralph Kraft, Ákos Bogdán, Laurence Perreault-Levasseur, Marine Prunier
Figure caption: Results of the RIM on the galaxy group NGC 1550. In the left panels, we show the RIM solution (i.e., the result of the deconvolution process) for ObsID 3186 and 3187, top and bottom, respectively (red). The middle panel shows the observed spectrum after background subtraction (black) and the RIM reconstruction (blue). The RIM reconstruction results from passing the RIM solution through the forward model developed in Equation (2). The right panel shows the residual between the observed spectrum and the RIM reconstruction normalized to the noise level of the observation. These figures demonstrate that the RIM performs well, below the 1σ limit, over the spectral range of the observations.
Paper: Deconvolving X-Ray Galaxy Cluster Spectra Using a Recurrent Inference Machine
Authors: Carter Lee Rhea, Julie Hlavacek-Larrondo, Alexandre Adam, Ralph Kraft, Ákos Bogdán, Laurence Perreault-Levasseur, Marine Prunier
Figure caption: Schematic of the convolution applied by the ACIS instrument on Chandra. This graphic demonstrates the response matrix’s profound effect on the observed spectrum; the response matrix is responsible for the lack of strong emission lines in the convolved observation. The true intrinsic spectrum, the ground truth spectrum, is a typical emission spectrum from the ICM modeled using the apec model with a temperature of 2.0 keV and a metallicity of 0.3 Z⊙. The response matrix was taken from a randomly chosen ObsID (2707); the matrix displayed is the log of the response matrix. The convolved observed spectrum was created following the methodology outlined in Section 2.2.
Paper: Deconvolving X-Ray Galaxy Cluster Spectra Using a Recurrent Inference Machine
Authors: Carter Lee Rhea, Julie Hlavacek-Larrondo, Alexandre Adam, Ralph Kraft, Ákos Bogdán, Laurence Perreault-Levasseur, Marine Prunier
Figure caption: Results of the RIM on the massive galaxy cluster A1795. In the left panels, we show the RIM solution (i.e., the result of the deconvolution process) for ObsID 5289 (red). The middle panel shows the observed spectrum after background subtraction (black) and the RIM reconstruction (blue). The RIM reconstruction results from passing the RIM solution through the forward model developed in Equation (2). The right panel shows the residual between the observed spectrum and the RIM reconstruction normalized to the noise level of the observation. This figure similarly demonstrates how the RIM reconstruction matches the observed spectrum.
Paper: Deconvolving X-Ray Galaxy Cluster Spectra Using a Recurrent Inference Machine
Authors: Carter Lee Rhea, Julie Hlavacek-Larrondo, Alexandre Adam, Ralph Kraft, Ákos Bogdán, Laurence Perreault-Levasseur, Marine Prunier
Figure caption: Montage of 16 randomly selected mock observed spectra (black) and the RIM reconstructions (blue) for a variety of temperatures and metalicities. Included in each subfigure is the reduced chi-squared value. The temperature increases from top to bottom, and the metalicity increases from left to right. This figure demonstrates the ability of the RIM to consistently return reconstructions similar to the observed spectra over a wide range of temperatures and abundances.
Paper: Deconvolving X-Ray Galaxy Cluster Spectra Using a Recurrent Inference Machine
Authors: Carter Lee Rhea, Julie Hlavacek-Larrondo, Alexandre Adam, Ralph Kraft, Ákos Bogdán, Laurence Perreault-Levasseur, Marine Prunier
Figure caption: In this figure we compare the RIM solution for both ObIDs (ObsID 3186 and ObsID 3187 in red) and the model taken from literature values (green) for NGC 1550. The latter was obtained by estimating the thermodynamic properties of the cluster from the convolved observed spectrum in K20 and then creating a mock spectrum using SOXS. Despite the difference between the K2020 model and the RIM solutions, the RIM solutions are consistent across observations with different responses.
Paper: Deconvolving X-Ray Galaxy Cluster Spectra Using a Recurrent Inference Machine
Authors: Carter Lee Rhea, Julie Hlavacek-Larrondo, Alexandre Adam, Ralph Kraft, Ákos Bogdán, Laurence Perreault-Levasseur, Marine Prunier
Figure caption: Same as in Figure 7 but for A1795. In this figure we compare the RIM solution for ObsID 5289 (red) and the model taken from literature values (green) taken from W14. The figure shows how the RIM solution follows the same power-law shape as the model W14.
Paper: Early r-process Enrichment and Hierarchical Assembly Across the Sagittarius Dwarf Galaxy 
Authors: Xiaowei Ou, 筱葳 欧, Alexander Yelland, Anirudh Chiti, Anna Frebel, Guilherme Limberg, Mohammad K. Mardini
Figure caption: Light element abundances for the full Sgr sample. Stars in the Sgr streams are marked with open-face circles (∘), whereas stars in the Sgr core are marked with black-filled circles (•). Literature values from C. J. Hansen et al. (2018) and APOGEE (S. Hasselquist et al. 2017) are shown as transparent blue diamonds. Sgr stars from F. Sestito et al. (2024a) are shown as green diamonds (PIGS IX). Halo stars compiled from JINAbase (A. Abohalima & A. Frebel 2018) are shown as gray dots. Example error bars reflecting the typical uncertainties in the abundances are shown at the bottom left of each panel.
Paper: Early r-process Enrichment and Hierarchical Assembly Across the Sagittarius Dwarf Galaxy 
Authors: Xiaowei Ou, 筱葳 欧, Alexander Yelland, Anirudh Chiti, Anna Frebel, Guilherme Limberg, Mohammad K. Mardini
Figure caption: Average [α/Fe] vs. [Fe/H] (left), [Sr/Ba] vs. [Ba/Fe] (middle), and [Ba/Eu] vs. [Ba/H] (right) abundances for our Sgr stars. Legends are the same as Figure 3. The left panel showcases the one star, Sgr438 with low [α/Fe] abundances, whose origin we discuss in detail in Section 4.1. The middle panel shows one potential UFD star, Sgr471, discussed in Section 4.4 with the rest of the sample distributed above the empirical cut. The right panel shows the confirmed r-process stars (Section 4.5) covering a range of −0.7 < [Ba/Eu] < −0.3, consistent with being enriched primarily by r-process enrichment events.
Paper: Early r-process Enrichment and Hierarchical Assembly Across the Sagittarius Dwarf Galaxy 
Authors: Xiaowei Ou, 筱葳 欧, Alexander Yelland, Anirudh Chiti, Anna Frebel, Guilherme Limberg, Mohammad K. Mardini
Figure caption: Neutron-capture elements abundances for the full Sgr sample. Stars in the Sgr streams are marked with open-face circles (∘), whereas stars in the Sgr core are marked with black-filled circles (•). Literature values from C. J. Hansen et al. (2018) and APOGEE (S. Hasselquist et al. 2017) are shown as transparent blue diamonds. Sgr stars from F. Sestito et al. (2024a) are shown as green diamonds (PIGS IX). Halo stars compiled from JINAbase (A. Abohalima & A. Frebel 2018) are shown as gray dots.
Paper: Early r-process Enrichment and Hierarchical Assembly Across the Sagittarius Dwarf Galaxy 
Authors: Xiaowei Ou, 筱葳 欧, Alexander Yelland, Anirudh Chiti, Anna Frebel, Guilherme Limberg, Mohammad K. Mardini
Figure caption: Phase space distribution of the Sgr core and stream stars from this study (yellow dots) and the stream members from G. Limberg et al. (2023), compared with the N-body model from E. Vasiliev et al. (2021). From top to bottom, the first panel shows the distribution of the stars in the heliocentric Sgr coordinate system. The measured radial velocities and adopted proper motions from Gaia as a function of Λ are shown in the second to last panels. The phase space target selection was performed in coordinates and proper motion space, and later confirmed with radial velocities from the observed spectra (see Section 2).
Paper: Early r-process Enrichment and Hierarchical Assembly Across the Sagittarius Dwarf Galaxy 
Authors: Xiaowei Ou, 筱葳 欧, Alexander Yelland, Anirudh Chiti, Anna Frebel, Guilherme Limberg, Mohammad K. Mardini
Figure caption: Fe-peak elements abundances for the full Sgr sample. Stars in the Sgr streams are marked with open-face circles (∘), whereas stars in the Sgr core are marked with black-filled circles (•). Literature values from C. J. Hansen et al. (2018) and APOGEE (S. Hasselquist et al. 2017) are shown as transparent blue diamonds. Sgr stars from F. Sestito et al. (2024a) are shown as green diamonds (PIGS IX). Halo stars compiled from JINAbase (A. Abohalima & A. Frebel 2018) are shown as gray dots.
Paper: Early r-process Enrichment and Hierarchical Assembly Across the Sagittarius Dwarf Galaxy 
Authors: Xiaowei Ou, 筱葳 欧, Alexander Yelland, Anirudh Chiti, Anna Frebel, Guilherme Limberg, Mohammad K. Mardini
Figure caption: Kiel diagram for the sample with all stars shown in dots. The Dartmouth isochrones are shown in solid lines. The dashed line represents the extrapolated isochrone. Both the stars and isochrones are color-coded by metallicity.
Paper: Early r-process Enrichment and Hierarchical Assembly Across the Sagittarius Dwarf Galaxy 
Authors: Xiaowei Ou, 筱葳 欧, Alexander Yelland, Anirudh Chiti, Anna Frebel, Guilherme Limberg, Mohammad K. Mardini
Figure caption: Comparison of means and spreads of various element abundances of all the stars located in the Sgr core and the stream.
Paper: Early r-process Enrichment and Hierarchical Assembly Across the Sagittarius Dwarf Galaxy 
Authors: Xiaowei Ou, 筱葳 欧, Alexander Yelland, Anirudh Chiti, Anna Frebel, Guilherme Limberg, Mohammad K. Mardini
Figure caption: Heavy element abundance patterns of six r-I stars (Sgr9, Sgr428, Sgr462, Sgr431, Sgr422, Sgr468) and one r-II star (Sgr421), compared to the scaled (normalized to the stellar europium, Eu, abundance) solar r-process abundance pattern (black line).
Paper: Tidally Heated Sub-Neptunes, Refined Planetary Compositions, and Confirmation of a Third Planet in the TOI-1266 System
Authors: Michael Greklek-McKeon, Shreyas Vissapragada, Heather A. Knutson, Akihiko Fukui, Morgan Saidel, Jonathan Gomez Barrientos, W. Garrett Levine, Aida Behmard, Konstantin Batygin, Yayaati Chachan, Gautam Vasisht, Renyu Hu, Ryan Cloutier, David Latham, Mercedes López-Morales, Andrew Vanderburg, Carolyn Heffner, Paul Nied, Jennifer Milburn, Isaac Wilson, Diana Roderick, Kathleen Koviak, Tom Barlow, John F. Stone, Rocio Kiman, Judith Korth, Jerome P. de Leon, Izuru Fukuda, Yuya Hayashi, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Yugo Kawai, Kiyoe Kawauchi, Nobuhiko Kusakabe, John H. Livingston, Mayuko Mori, Norio Narita, Motohide Tamura, Noriharu Watanabe, Gareb Fernández-Rodríguez
Figure caption: TTVs from TESS (blue circles), WIRC (red squares), and MuSCATs + Sinistro (yellow triangles) for TOI-1266 b (panels (1) and (3)) and TOI-1266 c (panels (2) and (4)) with 100 random posterior draws from our TTV model. Panels (1) and (2) show our two-planet models with posterior draws from the samples with low Mc and higher eccentricities shown in light blue, while those with higher Mc and lower eccentricities are shown in light gray. Panels (3) and (4) show 100 random posterior draws from our three-planet TTV model in dark gray. One TESS and one WIRC transit time each for TOI-1266 c are included in TTV fitting but omitted from these plots for clarity, as they have timing uncertainties  >15 minutes.
Paper: Tidally Heated Sub-Neptunes, Refined Planetary Compositions, and Confirmation of a Third Planet in the TOI-1266 System
Authors: Michael Greklek-McKeon, Shreyas Vissapragada, Heather A. Knutson, Akihiko Fukui, Morgan Saidel, Jonathan Gomez Barrientos, W. Garrett Levine, Aida Behmard, Konstantin Batygin, Yayaati Chachan, Gautam Vasisht, Renyu Hu, Ryan Cloutier, David Latham, Mercedes López-Morales, Andrew Vanderburg, Carolyn Heffner, Paul Nied, Jennifer Milburn, Isaac Wilson, Diana Roderick, Kathleen Koviak, Tom Barlow, John F. Stone, Rocio Kiman, Judith Korth, Jerome P. de Leon, Izuru Fukuda, Yuya Hayashi, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Yugo Kawai, Kiyoe Kawauchi, Nobuhiko Kusakabe, John H. Livingston, Mayuko Mori, Norio Narita, Motohide Tamura, Noriharu Watanabe, Gareb Fernández-Rodríguez
Figure caption: Geometric transit probability for TOI-1266 d when projecting out the orbital inclination distribution of TOI-1266 c, for both grazing configurations where b < 1 + Rp/R* and nongrazing configurations where b < 1 − Rp/R*.
Paper: Tidally Heated Sub-Neptunes, Refined Planetary Compositions, and Confirmation of a Third Planet in the TOI-1266 System
Authors: Michael Greklek-McKeon, Shreyas Vissapragada, Heather A. Knutson, Akihiko Fukui, Morgan Saidel, Jonathan Gomez Barrientos, W. Garrett Levine, Aida Behmard, Konstantin Batygin, Yayaati Chachan, Gautam Vasisht, Renyu Hu, Ryan Cloutier, David Latham, Mercedes López-Morales, Andrew Vanderburg, Carolyn Heffner, Paul Nied, Jennifer Milburn, Isaac Wilson, Diana Roderick, Kathleen Koviak, Tom Barlow, John F. Stone, Rocio Kiman, Judith Korth, Jerome P. de Leon, Izuru Fukuda, Yuya Hayashi, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Yugo Kawai, Kiyoe Kawauchi, Nobuhiko Kusakabe, John H. Livingston, Mayuko Mori, Norio Narita, Motohide Tamura, Noriharu Watanabe, Gareb Fernández-Rodríguez
Figure caption: Predicted TTVs for TOI-1266 d from our best-fit TTV+RV joint model (black points) spanning the same time range as in the previous TTV plots, with 100 random draws from the posterior distribution (gray). The TTV spread of  ∼30 minutes could prohibit the detection of shallow transits in a grazing configuration.
Paper: Tidally Heated Sub-Neptunes, Refined Planetary Compositions, and Confirmation of a Third Planet in the TOI-1266 System
Authors: Michael Greklek-McKeon, Shreyas Vissapragada, Heather A. Knutson, Akihiko Fukui, Morgan Saidel, Jonathan Gomez Barrientos, W. Garrett Levine, Aida Behmard, Konstantin Batygin, Yayaati Chachan, Gautam Vasisht, Renyu Hu, Ryan Cloutier, David Latham, Mercedes López-Morales, Andrew Vanderburg, Carolyn Heffner, Paul Nied, Jennifer Milburn, Isaac Wilson, Diana Roderick, Kathleen Koviak, Tom Barlow, John F. Stone, Rocio Kiman, Judith Korth, Jerome P. de Leon, Izuru Fukuda, Yuya Hayashi, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Yugo Kawai, Kiyoe Kawauchi, Nobuhiko Kusakabe, John H. Livingston, Mayuko Mori, Norio Narita, Motohide Tamura, Noriharu Watanabe, Gareb Fernández-Rodríguez
Figure caption: Detrended MuSCAT, MuSCAT3 and Sinistro light curves for TOI-1266 c. Colored lines are transit light-curve models generated using 100 random draws from the posterior distribution for each bandpass.
Paper: Tidally Heated Sub-Neptunes, Refined Planetary Compositions, and Confirmation of a Third Planet in the TOI-1266 System
Authors: Michael Greklek-McKeon, Shreyas Vissapragada, Heather A. Knutson, Akihiko Fukui, Morgan Saidel, Jonathan Gomez Barrientos, W. Garrett Levine, Aida Behmard, Konstantin Batygin, Yayaati Chachan, Gautam Vasisht, Renyu Hu, Ryan Cloutier, David Latham, Mercedes López-Morales, Andrew Vanderburg, Carolyn Heffner, Paul Nied, Jennifer Milburn, Isaac Wilson, Diana Roderick, Kathleen Koviak, Tom Barlow, John F. Stone, Rocio Kiman, Judith Korth, Jerome P. de Leon, Izuru Fukuda, Yuya Hayashi, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Yugo Kawai, Kiyoe Kawauchi, Nobuhiko Kusakabe, John H. Livingston, Mayuko Mori, Norio Narita, Motohide Tamura, Noriharu Watanabe, Gareb Fernández-Rodríguez
Figure caption: Detrended MuSCAT and MuSCAT3 light curves for TOI-1266 b. Colored lines are transit light-curve models generated using 100 random draws from the posterior distribution for each bandpass.
Paper: Tidally Heated Sub-Neptunes, Refined Planetary Compositions, and Confirmation of a Third Planet in the TOI-1266 System
Authors: Michael Greklek-McKeon, Shreyas Vissapragada, Heather A. Knutson, Akihiko Fukui, Morgan Saidel, Jonathan Gomez Barrientos, W. Garrett Levine, Aida Behmard, Konstantin Batygin, Yayaati Chachan, Gautam Vasisht, Renyu Hu, Ryan Cloutier, David Latham, Mercedes López-Morales, Andrew Vanderburg, Carolyn Heffner, Paul Nied, Jennifer Milburn, Isaac Wilson, Diana Roderick, Kathleen Koviak, Tom Barlow, John F. Stone, Rocio Kiman, Judith Korth, Jerome P. de Leon, Izuru Fukuda, Yuya Hayashi, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Yugo Kawai, Kiyoe Kawauchi, Nobuhiko Kusakabe, John H. Livingston, Mayuko Mori, Norio Narita, Motohide Tamura, Noriharu Watanabe, Gareb Fernández-Rodríguez
Figure caption: Observed transit depths of TOI-1266 b (blue) and c (red), including TESS PM, EM, and SEM data (circles), WIRC data (squares), and MuSCATs + Sinistro data (triangles). The error-weighted average transit depths are shown with dashed lines along with their associated 1σ uncertainties (shaded region).
Paper: Tidally Heated Sub-Neptunes, Refined Planetary Compositions, and Confirmation of a Third Planet in the TOI-1266 System
Authors: Michael Greklek-McKeon, Shreyas Vissapragada, Heather A. Knutson, Akihiko Fukui, Morgan Saidel, Jonathan Gomez Barrientos, W. Garrett Levine, Aida Behmard, Konstantin Batygin, Yayaati Chachan, Gautam Vasisht, Renyu Hu, Ryan Cloutier, David Latham, Mercedes López-Morales, Andrew Vanderburg, Carolyn Heffner, Paul Nied, Jennifer Milburn, Isaac Wilson, Diana Roderick, Kathleen Koviak, Tom Barlow, John F. Stone, Rocio Kiman, Judith Korth, Jerome P. de Leon, Izuru Fukuda, Yuya Hayashi, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Yugo Kawai, Kiyoe Kawauchi, Nobuhiko Kusakabe, John H. Livingston, Mayuko Mori, Norio Narita, Motohide Tamura, Noriharu Watanabe, Gareb Fernández-Rodríguez
Figure caption: The same as Figure 6, with 100 random posterior draws from our three-planet joint TTV+RV model (gray curves).
Paper: Tidally Heated Sub-Neptunes, Refined Planetary Compositions, and Confirmation of a Third Planet in the TOI-1266 System
Authors: Michael Greklek-McKeon, Shreyas Vissapragada, Heather A. Knutson, Akihiko Fukui, Morgan Saidel, Jonathan Gomez Barrientos, W. Garrett Levine, Aida Behmard, Konstantin Batygin, Yayaati Chachan, Gautam Vasisht, Renyu Hu, Ryan Cloutier, David Latham, Mercedes López-Morales, Andrew Vanderburg, Carolyn Heffner, Paul Nied, Jennifer Milburn, Isaac Wilson, Diana Roderick, Kathleen Koviak, Tom Barlow, John F. Stone, Rocio Kiman, Judith Korth, Jerome P. de Leon, Izuru Fukuda, Yuya Hayashi, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Yugo Kawai, Kiyoe Kawauchi, Nobuhiko Kusakabe, John H. Livingston, Mayuko Mori, Norio Narita, Motohide Tamura, Noriharu Watanabe, Gareb Fernández-Rodríguez
Figure caption: Detrended WIRC light curves for TOI-1266 b night 1 (left) and 2 (middle) and TOI-1266 c (right). The best-fit transit models are overplotted as red lines, with red shading to indicate the 1σ uncertainties.
Paper: Tidally Heated Sub-Neptunes, Refined Planetary Compositions, and Confirmation of a Third Planet in the TOI-1266 System
Authors: Michael Greklek-McKeon, Shreyas Vissapragada, Heather A. Knutson, Akihiko Fukui, Morgan Saidel, Jonathan Gomez Barrientos, W. Garrett Levine, Aida Behmard, Konstantin Batygin, Yayaati Chachan, Gautam Vasisht, Renyu Hu, Ryan Cloutier, David Latham, Mercedes López-Morales, Andrew Vanderburg, Carolyn Heffner, Paul Nied, Jennifer Milburn, Isaac Wilson, Diana Roderick, Kathleen Koviak, Tom Barlow, John F. Stone, Rocio Kiman, Judith Korth, Jerome P. de Leon, Izuru Fukuda, Yuya Hayashi, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Yugo Kawai, Kiyoe Kawauchi, Nobuhiko Kusakabe, John H. Livingston, Mayuko Mori, Norio Narita, Motohide Tamura, Noriharu Watanabe, Gareb Fernández-Rodríguez
Figure caption: Phase-folded RV data with best-fit model results from our joint TTV+RV fit for TOI-1266 b (left), TOI-1266 c (middle), and TOI-1266 d (right).
Paper: Real-time Collision-free Motion Planning for Next-generation Fiber Positioners in LAMOST
Authors: Guifeng Chen, Zhen Zhang, Chunhui Su, YongGang Gu, Chao Zhai
Figure caption: Schematic of trajectory collision: S1 represents the starting collision position in the first trajectory, S2 represents the starting collision position in the second trajectory, E1 represents the ending collision position in the first trajectory, E2 represents the ending collision position in the second trajectory. The red and blue parts, respectively, represent the parts where the two trajectories will collide. For example, when the trajectory is divided into 1000 segments, the starting point is represented as 1, the endpoint as 1000, and a point halfway along the trajectory as 500.
Paper: Real-time Collision-free Motion Planning for Next-generation Fiber Positioners in LAMOST
Authors: Guifeng Chen, Zhen Zhang, Chunhui Su, YongGang Gu, Chao Zhai
Figure caption: Schematic of a theta-phi positioner: θ represents the rotational angle of central arm, ϕ represents the rotational angle of eccentrical arm, lθ is the length of central arm, lϕ is the length of eccentric arm, the outermost circle represents the patrol area, and the red and blue colors represents different configurations achieving same target. (x0, y0) is the center point, (x1, y1) is the elbow joint and (x2, y2) is the fiber tip.
Paper: Real-time Collision-free Motion Planning for Next-generation Fiber Positioners in LAMOST
Authors: Guifeng Chen, Zhen Zhang, Chunhui Su, YongGang Gu, Chao Zhai
Figure caption: The left panel shows the mean errors between actual trajectories and cubic spline interpolation curves. The right panel shows the mean errors between predicted and actual trajectories in constant-speed method and real-time method.
Paper: Real-time Collision-free Motion Planning for Next-generation Fiber Positioners in LAMOST
Authors: Guifeng Chen, Zhen Zhang, Chunhui Su, YongGang Gu, Chao Zhai
Figure caption: Architectural overview of the real-time control: images of backlighted fibers are captured by calibrated MCS and fed into PS. Then images are transmitted to the image processing module through VDMA. After that, calculated positions are sent to PS via BRAM. PS sends CAN messages to positioners based on calculated positions.
Paper: Real-time Collision-free Motion Planning for Next-generation Fiber Positioners in LAMOST
Authors: Guifeng Chen, Zhen Zhang, Chunhui Su, YongGang Gu, Chao Zhai
Figure caption: The left panel shows the configuration of robot positioners on a focal plane with different colors indicating the coverage. ΦD represents diameter of focal plane, Φd1 represents diameter of patrol area, and d2 represents distance between adjacent positioners. The right panel shows an 84 positioner hexagonal array installed on the focal plane in midterm test. The positioners are installed and disassembled in groups.
Paper: Real-time Collision-free Motion Planning for Next-generation Fiber Positioners in LAMOST
Authors: Guifeng Chen, Zhen Zhang, Chunhui Su, YongGang Gu, Chao Zhai
Figure caption: Schematic showing a collision involving three positioners: O1,O2 and O3 denote the center points of positioners 1, 2 and 3, respectively. S1 represents the collision zone between positioners 1 and 2. S2 represents the collision zone involving positioner 3 with either positioner 1 or 2. R denotes the radius of the patrol circle for each positioner.