adsabs/AstroCLIMB huggingface dataset:
Paper: GRB 200826A: A Precursor of a Long Gamma-Ray Burst with Missing Main Emission
Authors: Xiangyu Ivy Wang, Bin-Bin Zhang, Wei-Hua Lei
Figure caption: The E p,z vs. E  γ,iso correlation diagram. The black and gray solid lines are the best linear correlations for long and short GRBs, respectively. GRB 200826A (red star) and the precursor of GRB 160625B (green star) both fall in the long-GRB region. The samples are from Amati et al. 2002 and Zhang et al. (2009).
Paper: GRB 200826A: A Precursor of a Long Gamma-Ray Burst with Missing Main Emission
Authors: Xiangyu Ivy Wang, Bin-Bin Zhang, Wei-Hua Lei
Figure caption: The blue, orange, and green lines represent the evolution of the observed peak flux with the viewing angle when the Lorentz factor Γ = 20, 100, and 200, respectively.
Paper: GRB 200826A: A Precursor of a Long Gamma-Ray Burst with Missing Main Emission
Authors: Xiangyu Ivy Wang, Bin-Bin Zhang, Wei-Hua Lei
Figure caption: The schematic sketch of the precession jet model.
Paper: Radiative Transfer Modeling of Chang’e-4 Spectroscopic Observations and Interpretation of the South Pole-Aitken Compositional Anomaly
Authors: Jian Chen, Zongcheng Ling, Bradley L. Jolliff, Lingzhi Sun, Le Qiao, Jianzhong Liu, Xiaohui Fu, Jiang Zhang, Bo Li, Changqing Liu, Xiaobin Qi, Xuejin Lu, Zhiping He, Rui Xu
Figure caption: Yutu-2 traverse map and mineralogical variations along the path. (A) Traverse path of the Yutu-2 rover and locations of the exploration sites overlaid on the image taken by LROC NAC (frame M1303619844) and the color-coded digital terrain mode (DTM) derived from stereo pairs of NAC images (https://wms.lroc.asu.edu/lroc/view_rdr/NAC_DTM_CHANGE4). Topographic contours are shown as black solid lines with the elevation values labeled. (B) Shallow subsurface stratigraphy along the traverse path. The thicknesses of different deposit layers reflect the mixing ratios. The vertical scale is zoomed 10×. (C) Estimated mineralogy along the traverse path. The solid and dashed lines indicate the mean values and standard deviations of mineral proportions.(The data used to create this figure are available.)
Paper: Radiative Transfer Modeling of Chang’e-4 Spectroscopic Observations and Interpretation of the South Pole-Aitken Compositional Anomaly
Authors: Jian Chen, Zongcheng Ling, Bradley L. Jolliff, Lingzhi Sun, Le Qiao, Jianzhong Liu, Xiaohui Fu, Jiang Zhang, Bo Li, Changqing Liu, Xiaobin Qi, Xuejin Lu, Zhiping He, Rui Xu
Figure caption: Comparison between the modeled and measured data. (A)–(C) LSCC spectra of samples 12001, 64804, and 71061 and their best-matched modeled spectra. (D) Mineral abundances modeled with our LUT vs. measured modal mineralogy of LSCC samples.(The data used to create this figure are available.)
Paper: Radiative Transfer Modeling of Chang’e-4 Spectroscopic Observations and Interpretation of the South Pole-Aitken Compositional Anomaly
Authors: Jian Chen, Zongcheng Ling, Bradley L. Jolliff, Lingzhi Sun, Le Qiao, Jianzhong Liu, Xiaohui Fu, Jiang Zhang, Bo Li, Changqing Liu, Xiaobin Qi, Xuejin Lu, Zhiping He, Rui Xu
Figure caption: Mineralogy of CE-4 VNIS exploration sites. (A) Modal mineralogy plotted on a plagioclase–pyroxene–olivine ternary. (B) Modal mineralogy plotted on a Plg–LCP–HCP ternary (Olv < 10 vol.%). The modeled SPA impact melt differentiation and mineralogic evolution are indicated by arrows (Hurwitz & Kring 2014).(The data used to create this figure are available.)
Paper: The Warm Neptune GJ 3470b Has a Polar Orbit
Authors: Guđmundur Stefànsson, Suvrath Mahadevan, Cristobal Petrovich, Joshua N. Winn, Shubham Kanodia, Sarah C. Millholland, Marissa Maney, Caleb I. Cañas, John Wisniewski, Paul Robertson, Joe P. Ninan, Eric B. Ford, Chad F. Bender, Cullen H. Blake, Heather Cegla, William D. Cochran, Scott A. Diddams, Jiayin Dong, Michael Endl, Connor Fredrick, Samuel Halverson, Fred Hearty, Leslie Hebb, Teruyuki Hirano, Andrea S. J. Lin, Sarah E. Logsdon, Emily Lubar, Michael W. McElwain, Andrew J. Metcalf, Andrew Monson, Jayadev Rajagopal, Lawrence W. Ramsey, Arpita Roy, Christian Schwab, Heidi Schweiker, Ryan C. Terrien, Jason T. Wright
Figure caption: Constraints on the parameters of a potential outer perturber for the two models considered: a) the ZKL/nodal precession model and b) the disk-driven model of Petrovich et al. (2020). For the former, the red and blue regions show where ﹩{\psi }_{\max }\gt 80^\circ ﹩ for i bc = 45° and i bc = 60°, respectively. For the ZKL/nodal precession case, we assume a current Love number of k 2 = 0.01, leading to J 2 ∼ 2 × 108. For the disk-driven model of Petrovich et al. (2020), we assume that GJ 3470 had a radius of R ⋆ = 0.9R ⊙ and a rotation period of 10 days and Love number of k 2 = 0.2 during the disk dispersal phase. For this case, we follow Petrovich et al. (2020) and assume a disk mass-loss law of M disk = 50M J/(1 + t/1 Myr)1/2. The gray regions in b) highlight regions excluded from the conservation of angular momentum deficit (AMD). The green regions show the nominal region consistent with the RV slope from Section 5, where we have assumed i  c  ≤ 90°, e = 0.4 (the green dashed line shows the i  c  = 90° case).
Paper: The Warm Neptune GJ 3470b Has a Polar Orbit
Authors: Guđmundur Stefànsson, Suvrath Mahadevan, Cristobal Petrovich, Joshua N. Winn, Shubham Kanodia, Sarah C. Millholland, Marissa Maney, Caleb I. Cañas, John Wisniewski, Paul Robertson, Joe P. Ninan, Eric B. Ford, Chad F. Bender, Cullen H. Blake, Heather Cegla, William D. Cochran, Scott A. Diddams, Jiayin Dong, Michael Endl, Connor Fredrick, Samuel Halverson, Fred Hearty, Leslie Hebb, Teruyuki Hirano, Andrea S. J. Lin, Sarah E. Logsdon, Emily Lubar, Michael W. McElwain, Andrew J. Metcalf, Andrew Monson, Jayadev Rajagopal, Lawrence W. Ramsey, Arpita Roy, Christian Schwab, Heidi Schweiker, Ryan C. Terrien, Jason T. Wright
Figure caption: Results from the tidal model fit to the observed properties of GJ 3470b. Top panel: comparison of the envelope mass fraction (f env ≡ M env/M  p ) when tides are included and when they are ignored. The gray solid line and banding indicate the mean and standard deviation of the tide-free estimate, f env = 14.0% ± 1.4%. The blue solid region indicates the 2σ contours of the posterior distribution of the planet’s reduced tidal quality factor, ﹩Q^{\prime} ﹩, and f env when accounting for tides. Bottom panel: the degree of radius inflation, parameterized as the ratio of the radius of the planet when tides are accounted for compared to the radius the planet would have if tides were absent. The blue solid region indicates the 2σ contours of the posterior distribution. ﹩Q^{\prime} ﹩ is highly uncertain but most likely in the range ﹩Q^{\prime} \approx {10}^{4}\mbox{--}{10}^{5}﹩, indicating tidal inflation by a factor of ∼1.5–1.7.
Paper: Resolving the Collimation Zone of an Intermediate-mass Protostellar Jet
Authors: Adriana R. Rodríguez-Kamenetzky, Carlos Carrasco-González, Luis F. Rodríguez, Tom P. Ray, Alberto Sanna, Luca Moscadelli, Melvin Hoare, Roberto Galván-Madrid, Hsien Shang, Susana Lizano, Jochen Eislöffel, Jeremy Lim, José M. Torrelles, Paul Ho, Anton Feeney-Johansson
Figure caption: Images of the jet core at different frequencies. The upper panels show the same region of the sky, with the same physical scale. The red dashed rectangles indicate the region surrounding the jet that is shown in the bottom panels ((d), (e), and (f)) with the same physical scale. A red star is shown in each panel to indicate the location of the emission peak in the highest angular resolution image obtained (panel (e)). (a) Briggs-weighted (Robust = 0) C-band image (e-MERLIN and VLA-A data combined); contours are [−4, 4, 7, 9, 13, 18, 24, 40] × the rms of 5 μJy beam−1. (b) Superuniform-weighted image from Ku VLA-A data; contours are [−3, 5, 7, 9, 10.5, 11.5, 14, 17, 23, 27, 50, 90, 105, 113] × the rms of 6 μJy beam−1. NW- and SE-jet counterparts are indicated by black dashed arrows. (c) Briggs-weighted (Robust = 0) K-band VLA-A image; contours are [−4, 4, 6, 8, 10, 12, 20, 30, 50, 70, 100, 130] × the rms of 6 μJy beam−1. We draw a parabolic dashed curve for descriptive purposes (see text). (d) Superuniform-weighted Ka-band VLA-A; contours are [5, 6, 7, 10, 12, 14, 16, 18, 20, 25, 30, 32, 33] × the rms = 20 μJy beam−1. We also show the jet direction as identified in panel (b), and the black curve drawn in panel (c). (e) Q-band VLA-A superuniform-weighted image; contours are [−2, 5, 6, 7, 8, 9, 10, 11, 12] × the rms of 50 μJy beam−1. This is the highest physical resolution image achieved (∼15 au). We draw a green parabolic dashed curve for descriptive purposes (see text), in addition to the jet direction identified in panel (b) and the black curve drawn in panel (c). (f) Brightness temperature map corresponding to the 7 mm (Q band) emission (panel (e)) over 8σ; contours are [−2, 8, 9, 10, 11, 12] × the rms of the Q-band emission. The magenta x symbol in panel (e) indicates the position where the jet ionization seems to start.
Paper: Resolving the Collimation Zone of an Intermediate-mass Protostellar Jet
Authors: Adriana R. Rodríguez-Kamenetzky, Carlos Carrasco-González, Luis F. Rodríguez, Tom P. Ray, Alberto Sanna, Luca Moscadelli, Melvin Hoare, Roberto Galván-Madrid, Hsien Shang, Susana Lizano, Jochen Eislöffel, Jeremy Lim, José M. Torrelles, Paul Ho, Anton Feeney-Johansson
Figure caption: Radio continuum observations of the TRS in Serpens. Left panel: We show a VLA-A C-band image above 4× the rms of 10 μJy beam−1. The main sources detected are labeled (C, SE, and NW). Right panel: We show the deepest image of the Serpens jet core obtained by the combination of VLA-A and e-MERLIN data in the same frequency range (from 4.7 to 5.2 GHz). Contours are [−4, 4, 7, 9, 13, 18, 24, 40] × the rms of 5μJy beam−1. Beam sizes and other parameters of the images are listed in Table 2.
Paper: Resolving the Collimation Zone of an Intermediate-mass Protostellar Jet
Authors: Adriana R. Rodríguez-Kamenetzky, Carlos Carrasco-González, Luis F. Rodríguez, Tom P. Ray, Alberto Sanna, Luca Moscadelli, Melvin Hoare, Roberto Galván-Madrid, Hsien Shang, Susana Lizano, Jochen Eislöffel, Jeremy Lim, José M. Torrelles, Paul Ho, Anton Feeney-Johansson
Figure caption: Comparison of two e-MERLIN C-band images observed 1.4 yr apart. Both images were convolved to the same beam size (0.″140×0.″050; PA 23°) in order to measure the positions of the internal knots through a Gaussian fit to their intensity profiles. We label all of the knots that can be identified in both epochs above 4σ. Red stars indicate the position of the emission peak in the VLA-A Q-band image (Figure 3, panel (e)), considered to be the location of the powering source of the jet (indicated by C). Gray crosses indicate the averaged position of unresolved knots, i.e., S1&S2, N5&N6, and N3&N4. The gray dashed lines join the positions of the knots in the two epochs. EPOCH 2020.1: contours are [4, 5, 7, 8.5, 9.5, 10.4, 13, 15, 20, 25, 35, 40] ×6 μJy beam−1. EPOCH 2021.5: contours are [4, 5, 5.9, 6.7, 8, 10, 13, 15, 20, 30, 40] × 10 μJy beam−1.
Paper: From Pericenter and Back: Full Debris Stream Evolution in Tidal Disruption Events
Authors: Clément Bonnerot, Martin E. Pessah, Wenbin Lu
Figure caption: Evolution of the longitudinal length (upper panel) and transverse widths in the vertical (middle panel) and in-plane (lower panel) directions for stream sections with different orbital energies as specified by their boundness μ. The initial value used as normalization is arbitrarily set to ℓ i for the length and given by ﹩{H}_{{\rm{i}}}={{\rm{\Delta }}}_{{\rm{i}}}={R}_{\star }{\left(1-{\mu }^{2}\right)}^{1/2}﹩ for the two widths. For a given stream section, diamonds and circles represent the initial and final locations, respectively. The thick green dashed line in the upper panel shows the analytical result of Equation (14) for ℓ eq = ℓ i and ﹩{R}_{\mathrm{eq}}^{{\ell }}={R}_{{\rm{t}}}﹩.
Paper: From Pericenter and Back: Full Debris Stream Evolution in Tidal Disruption Events
Authors: Clément Bonnerot, Martin E. Pessah, Wenbin Lu
Figure caption: Elliptical geometry of two bound stream sections in the ballistic (μ = −0.98, left panel) and hydrostatic (μ = −0.1, right panel) regimes displayed in square boxes at nine different locations (red and blue points) along their center-of-mass trajectory (black solid curve). The gray arrows represent the unit vector  e  ∥ pointing along the local direction of stream elongation (shown in orange initially). The purple and green arrows show the velocity vector at the equilibrium point where ﹩\dot{H}=0﹩, which is parallel to the intersection line (dashed lines of the same color) where the orbital planes of the gas inside each section cross. For better visibility, we only show portions of the trajectory with μ = −0.1 separated by small parallel segments because it would otherwise have a much larger apocenter. We use the same scale to depict the elliptical sections for boxes inside the lower inset (points 1, 2, 3, 8, and 9) but a different one for the other boxes (points 4, 5, 6, and 7). These scales also differ between the two panels.
Paper: From Pericenter and Back: Full Debris Stream Evolution in Tidal Disruption Events
Authors: Clément Bonnerot, Martin E. Pessah, Wenbin Lu
Figure caption: Sketch showing the evolution of a bound section of the stream (orange surface) specified by its boundness μ < 0 as it follows an elliptical trajectory (dashed line) around the black hole (black circle) starting from its initial location inside the star at the tidal radius (pericenter). This section remains orthogonal at all times to the unit vector  e  ∥ locally aligned with the longitudinal direction of the stream elongation. The unit vectors  e  ⊥ and  e  z point along the transverse directions aligned and orthogonal to the stellar orbital plane, respectively. The transverse widths of the stream section are given by Δ and H.
Paper: Radiative Transfer Modeling of Chang’e-4 Spectroscopic Observations and Interpretation of the South Pole-Aitken Compositional Anomaly
Authors: Jian Chen, Zongcheng Ling, Bradley L. Jolliff, Lingzhi Sun, Le Qiao, Jianzhong Liu, Xiaohui Fu, Jiang Zhang, Bo Li, Changqing Liu, Xiaobin Qi, Xuejin Lu, Zhiping He, Rui Xu
Figure caption: SPA region as seen in different data sets. (A) LOLA color shaded relief map (https://astrogeology.usgs.gov/search/map/Moon/LMMP/LOLA-derived/Lunar_LRO_LOLA_ClrShade_Global_128ppd_v04) centered on Mons Marguerite. The dashed circle is determined by the diameter (820 km) of the transient cavity formed by the SPA impact event from Hurwitz & Kring (2014), that is perfectly outlining the SPACA region identified by Moriarty (2016). The irregular dashed polygon is the extent of the so-called MPA. (B) Impact crater density calculated based on the lunar crater database from Robbins (2019). Note the high-density annulus of the secondary craters surrounding the Imbrian crater Antoniadi. (C) Ejecta thickness distribution of post-SPA impacts (>15 km). (D)–(E) LPGRS Half Degree Abundance Data of FeO and Th (https://pds-geosciences.wustl.edu/missions/lunarp/reduced_special.html). The boundary of SPACA identified by Moriarty (2016) is shown as an irregular polygon. The elliptical lines are the SPA basin ring. The black mask represents mare basalt regions modified from Nelson et al. (2014).(The data used to create this figure are available.)
Paper: Radiative Transfer Modeling of Chang’e-4 Spectroscopic Observations and Interpretation of the South Pole-Aitken Compositional Anomaly
Authors: Jian Chen, Zongcheng Ling, Bradley L. Jolliff, Lingzhi Sun, Le Qiao, Jianzhong Liu, Xiaohui Fu, Jiang Zhang, Bo Li, Changqing Liu, Xiaobin Qi, Xuejin Lu, Zhiping He, Rui Xu
Figure caption: The 820 nm artifact in VNIS spectra and its effects on continuum removal. (A) The artifact (gray region) between 760 nm and 900 nm. (B) The artifact affects the positions of the tie point used for continuum removal of CE-4 VNIS data. (C) VNIR spectra of lunar clinopyroxene, olivine, and orthopyroxene/pigeonite collected and characterized by the Apollo missions (Data are from RELAB database: clinopyroxene (LR-CMP-168 from Apollo 15 sample 15555), olivine (LR-CMP-169 from Apollo 15 sample 15555), and orthopyroxene (LR-CMP-173 from Apollo 15 sample 15058). The endpoint wavelength (2395 nm) of VNIS spectra is marked by a magenta dashed line to illustrate that the 2 μm absorption band was not completely measured by VNIS.(The data used to create this figure are available.)
Paper: Radiative Transfer Modeling of Chang’e-4 Spectroscopic Observations and Interpretation of the South Pole-Aitken Compositional Anomaly
Authors: Jian Chen, Zongcheng Ling, Bradley L. Jolliff, Lingzhi Sun, Le Qiao, Jianzhong Liu, Xiaohui Fu, Jiang Zhang, Bo Li, Changqing Liu, Xiaobin Qi, Xuejin Lu, Zhiping He, Rui Xu
Figure caption: Compositional and mineralogical profile along the section line Zhinyu-CE4-Finsen. (A) Section line overlain on the shaded relief derived from LRO + Kaguya merged topography products (https://astrogeology.usgs.gov/search/map/Moon/LRO/LOLA/Lunar_LRO_LOLAKaguya_Shade_60N60S_512ppd). (B) Compositional and mineralogical variations along the traverse path. FeO and mineralogy data are from Kaguya MI global map products. Three dashed lines indicate the locations of the Zhinyu crater rim, CE-4 landing site, and Finsen crater rim on the section line. The red stars mark the mineralogy derived from CE-4 VNIS data sets. The dark marbles represent the three end-members for mixing, i.e., VKB, FE, and FCP (Finsen central peak).(The data used to create this figure are available.)
Paper: Radiative Transfer Modeling of Chang’e-4 Spectroscopic Observations and Interpretation of the South Pole-Aitken Compositional Anomaly
Authors: Jian Chen, Zongcheng Ling, Bradley L. Jolliff, Lingzhi Sun, Le Qiao, Jianzhong Liu, Xiaohui Fu, Jiang Zhang, Bo Li, Changqing Liu, Xiaobin Qi, Xuejin Lu, Zhiping He, Rui Xu
Figure caption: Spectral and mineralogical profile along the section line Zhinyu-CE4-Finsen. (A). Mosaic of the Zhinyu-CE4-Finsen region at 540 nm from the M3 data sets (https://pdsimage2.wr.usgs.gov/archive/chandrayaan_1/m3/). (B) M3 Standard color composite. (C) Composite of mineral indices. IBD parameters and mineral indices are defined in Table A1 and Chen et al. (2020). (D) M3 RADF reflectance spectra of the Von Kármán basalts (VKB exposed by Zhinyu), CE-4 landing site, Finsen ejecta (FE), and SPACA region (not associated with Finsen). (E) Continuum-removed spectra.(The data used to create this figure are available.)
Paper: Radiative Transfer Modeling of Chang’e-4 Spectroscopic Observations and Interpretation of the South Pole-Aitken Compositional Anomaly
Authors: Jian Chen, Zongcheng Ling, Bradley L. Jolliff, Lingzhi Sun, Le Qiao, Jianzhong Liu, Xiaohui Fu, Jiang Zhang, Bo Li, Changqing Liu, Xiaobin Qi, Xuejin Lu, Zhiping He, Rui Xu
Figure caption: FeO-Th diagrams of lunar materials. (A) FeO-Th compositions of lunar rock samples modified from Jolliff et al. (2006). The fields with different grayscales represent compositional ranges of different lithologies that occurred in Apollo and Luna rock samples. The “A” point represents the highly feldspathic ferroan anorthosite sample 15418. The “C” point represents the regolith composition of the CE-4 landing site and the traverse area as seen by the Lunar Prospector gamma-ray spectrometer. The “D” point represents the Apollo 17 dunite sample 72415–7. The “E” points represent the enriched end-member lithologies for the mixing in SPACA. The “K” point represents the average compositions of Apollo 15 KREEP basalt samples. The “S” point represents the average compositions of SPACA. The dotted curves indicate mixing effects in lunar regolith samples among three end-members (i.e., feldspathic highlands materials, mare basalt, and KREEP-bearing materials). (B) Data used to unmix the Finsen materials (“F” points) and Von Kármán materials (“V” points).(The data used to create this figure are available.)
Paper: Radiative Transfer Modeling of Chang’e-4 Spectroscopic Observations and Interpretation of the South Pole-Aitken Compositional Anomaly
Authors: Jian Chen, Zongcheng Ling, Bradley L. Jolliff, Lingzhi Sun, Le Qiao, Jianzhong Liu, Xiaohui Fu, Jiang Zhang, Bo Li, Changqing Liu, Xiaobin Qi, Xuejin Lu, Zhiping He, Rui Xu
Figure caption: Spectral classification of VNIS images of the first boulder (0015). The circles indicate the FOV of the SWIR detector. (A) BD940 image. (B) Binary classification results with a pixel resolution of ∼600 μm. (C) Mean spectra (normalized at 750 nm) of blue pixels (with mafic absorptions) and red pixels (without mafic absorptions).(The data used to create this figure are available.)
Paper: Radiative Transfer Modeling of Chang’e-4 Spectroscopic Observations and Interpretation of the South Pole-Aitken Compositional Anomaly
Authors: Jian Chen, Zongcheng Ling, Bradley L. Jolliff, Lingzhi Sun, Le Qiao, Jianzhong Liu, Xiaohui Fu, Jiang Zhang, Bo Li, Changqing Liu, Xiaobin Qi, Xuejin Lu, Zhiping He, Rui Xu
Figure caption: Variations of BC1, BC2, and IBDR values with different SG smoothing windows.(The data used to create this figure are available.)
Paper: Radiative Transfer Modeling of Chang’e-4 Spectroscopic Observations and Interpretation of the South Pole-Aitken Compositional Anomaly
Authors: Jian Chen, Zongcheng Ling, Bradley L. Jolliff, Lingzhi Sun, Le Qiao, Jianzhong Liu, Xiaohui Fu, Jiang Zhang, Bo Li, Changqing Liu, Xiaobin Qi, Xuejin Lu, Zhiping He, Rui Xu
Figure caption: Modal analyses of CE-4 soils. (A) Mineralogy. (B) Mixing ratio.(The data used to create this figure are available.)
Paper: Successful Recovery of an Observed Meteorite Fall Using Drones and Machine Learning
Authors: Seamus L. Anderson, Martin C. Towner, John Fairweather, Philip A. Bland, Hadrien A. R. Devillepoix, Eleanor K. Sansom, Martin Cupák, Patrick M. Shober, Gretchen K. Benedix
Figure caption: The DFN 09 meteorite fall at Kybo Station, Western Australia. Clockwise from top: Fireball observations from DFN camera stations at Mundrabilla Station and O’Malley Siding, and their location within WA. The 5 km2, 90% certainty searching area (transparent white), the best-fit fall line (red markers), and the location of the recovered meteorite (yellow star). Preimpact orbit for the DFN 09 meteoroid (a = 2.597 ± 0.017 au, e = 0.7707 ± 0.0018, i = 0.°3567 ± 0.°0053, ω = 85.°862 ± 0.°015, and Ω = 191.90282 ± 0.°00073 39 (1σ uncertainties)).
Paper: Successful Recovery of an Observed Meteorite Fall Using Drones and Machine Learning
Authors: Seamus L. Anderson, Martin C. Towner, John Fairweather, Philip A. Bland, Hadrien A. R. Devillepoix, Eleanor K. Sansom, Martin Cupák, Patrick M. Shober, Gretchen K. Benedix
Figure caption: The four stage process for eliminating false positives and verifying meteorite candidates. From left to right: (1) Grid GUI. (2) Zoom-pan GUI. (3) Drone visit. (4) In-person visit.
Paper: Successful Recovery of an Observed Meteorite Fall Using Drones and Machine Learning
Authors: Seamus L. Anderson, Martin C. Towner, John Fairweather, Philip A. Bland, Hadrien A. R. Devillepoix, Eleanor K. Sansom, Martin Cupák, Patrick M. Shober, Gretchen K. Benedix
Figure caption: Favorable and unfavorable prediction distributions from two images. Given a 70% confidence threshold, Image/Distribution A will return 3 meteorite candidates, while Distribution B will return >100 candidates. B-like images are later used for retraining. For clarity, the number of detections displayed in image B is capped at 50.
Paper: Successful Recovery of an Observed Meteorite Fall Using Drones and Machine Learning
Authors: Seamus L. Anderson, Martin C. Towner, John Fairweather, Philip A. Bland, Hadrien A. R. Devillepoix, Eleanor K. Sansom, Martin Cupák, Patrick M. Shober, Gretchen K. Benedix
Figure caption: Top: four meteorite tiles selected from our training data. Middle: the recovered meteorite. Bottom: the other three meteorite candidates visited for a second time with the Mavic Pro, and later inspected in person.