adsabs/AstroCLIMB huggingface dataset:
Paper: An Inclusive Library for Quantitative Analysis of the Laser-induced Breakdown Spectra Acquired by the Zhurong Mars Rover
Authors: Shuai-Yi Qu, Jianxun Shen, Luning Li, Zhicheng Cui, Xuesen Xu, Ziyi Liu, Chengxiang Huang, Haohuan Li, Honglei Lin, Wei Lin, Yangting Lin
Figure caption: LIBS spectral acquisition setup and samples. (A) The overall view of the MarSDEEP platform. (B) The sample plate with clamped samples inside of MarSDEEP, a maximum of 16 samples can be placed on each tray. (C) Pressed powder samples.
Paper: An Inclusive Library for Quantitative Analysis of the Laser-induced Breakdown Spectra Acquired by the Zhurong Mars Rover
Authors: Shuai-Yi Qu, Jianxun Shen, Luning Li, Zhicheng Cui, Xuesen Xu, Ziyi Liu, Chengxiang Huang, Haohuan Li, Honglei Lin, Wei Lin, Yangting Lin
Figure caption: Categories of laboratory samples prepared for the MarSCoDe calibration database. A total of 322 samples are included in the database, comprising terrestrial natural samples, standard minerals and reagents, Martian meteorites, and Martian simulant samples. The proportions of each sample type within the database are represented by different colors.
Paper: An Inclusive Library for Quantitative Analysis of the Laser-induced Breakdown Spectra Acquired by the Zhurong Mars Rover
Authors: Shuai-Yi Qu, Jianxun Shen, Luning Li, Zhicheng Cui, Xuesen Xu, Ziyi Liu, Chengxiang Huang, Haohuan Li, Honglei Lin, Wei Lin, Yangting Lin
Figure caption: Comparison of rms error of prediction (RMSEP) for different models. (A) RMSEPs comparison of BPNN, GBR, PLS1, and PLS2 based on this database, with BPNN achieving the lowest RMSEP; (B) RMSEP comparison between BPNN based on this database and models from previous studies using existing databases, demonstrating the comparable RMSEPs of BPNN and supporting the feasibility of quantitative modeling with this database; (C) RMSEPs of major oxides in selected quantitative regression models tested with representative samples containing hydrous minerals; (D) RMSEPs of major element predictions for two Martian meteorites (NWA 7034 and Dhofar 019) using BPNN.
Paper: An Inclusive Library for Quantitative Analysis of the Laser-induced Breakdown Spectra Acquired by the Zhurong Mars Rover
Authors: Shuai-Yi Qu, Jianxun Shen, Luning Li, Zhicheng Cui, Xuesen Xu, Ziyi Liu, Chengxiang Huang, Haohuan Li, Honglei Lin, Wei Lin, Yangting Lin
Figure caption: Scanning μXRF graphs of Si, Ti, Al, Fe, Mg, Ca, Na, and K distributions in the sample BA03, showing their relative concentrations as indicated by the color scale bar on the right-hand side of each panel. The particle size of the sample is less than 48 μm.
Paper: An Inclusive Library for Quantitative Analysis of the Laser-induced Breakdown Spectra Acquired by the Zhurong Mars Rover
Authors: Shuai-Yi Qu, Jianxun Shen, Luning Li, Zhicheng Cui, Xuesen Xu, Ziyi Liu, Chengxiang Huang, Haohuan Li, Honglei Lin, Wei Lin, Yangting Lin
Figure caption: Comparison of major element predictions based on the BPNN model with XRF measurement results. Seven-fold cross-validation was employed to sequentially select test sets for evaluation, and the results for all spectra are presented in the figure. RE (relative error) represents the percentage deviation of the predicted value from the reference value.
Paper: An Inclusive Library for Quantitative Analysis of the Laser-induced Breakdown Spectra Acquired by the Zhurong Mars Rover
Authors: Shuai-Yi Qu, Jianxun Shen, Luning Li, Zhicheng Cui, Xuesen Xu, Ziyi Liu, Chengxiang Huang, Haohuan Li, Honglei Lin, Wei Lin, Yangting Lin
Figure caption: The LIBS spectrum of boric acid obtained in this experiment. Boric acid exhibits no characteristic peaks in the LIBS spectrum and does not interfere with the LIBS analysis of the samples.
Paper: An Inclusive Library for Quantitative Analysis of the Laser-induced Breakdown Spectra Acquired by the Zhurong Mars Rover
Authors: Shuai-Yi Qu, Jianxun Shen, Luning Li, Zhicheng Cui, Xuesen Xu, Ziyi Liu, Chengxiang Huang, Haohuan Li, Honglei Lin, Wei Lin, Yangting Lin
Figure caption: Comparison of the bulk major element compositions (red) of Martian meteorites (A) NWA 7034 and (B) Dhofar 019 with the BPNN prediction results (blue). The results demonstrate that the BPNN model based on this database provides reliable predictions for major elements.
Paper: An Inclusive Library for Quantitative Analysis of the Laser-induced Breakdown Spectra Acquired by the Zhurong Mars Rover
Authors: Shuai-Yi Qu, Jianxun Shen, Luning Li, Zhicheng Cui, Xuesen Xu, Ziyi Liu, Chengxiang Huang, Haohuan Li, Honglei Lin, Wei Lin, Yangting Lin
Figure caption: Scanning μXRF graphs of Si, Ti, Al, Fe, Mg, Ca, Na, and K distributions in the sample Alluvial fan-1, showing their relative concentrations as indicated by the color scale bar on the right-hand side of each panel. The particle size of the sample is less than 48 μm.
Paper: An Inclusive Library for Quantitative Analysis of the Laser-induced Breakdown Spectra Acquired by the Zhurong Mars Rover
Authors: Shuai-Yi Qu, Jianxun Shen, Luning Li, Zhicheng Cui, Xuesen Xu, Ziyi Liu, Chengxiang Huang, Haohuan Li, Honglei Lin, Wei Lin, Yangting Lin
Figure caption: Scanning μXRF graphs of Si, Ti, Al, Fe, Mg, Ca, Na, and K distributions in the sample Debris flow-1, showing their relative concentrations as indicated by the color scale bar on the right-hand side of each panel. The particle size of the sample is less than 48 μm.
Paper: An Inclusive Library for Quantitative Analysis of the Laser-induced Breakdown Spectra Acquired by the Zhurong Mars Rover
Authors: Shuai-Yi Qu, Jianxun Shen, Luning Li, Zhicheng Cui, Xuesen Xu, Ziyi Liu, Chengxiang Huang, Haohuan Li, Honglei Lin, Wei Lin, Yangting Lin
Figure caption: Scanning μXRF graphs of Si, Ti, Al, Fe, Mg, Ca, Na, and K distributions in the sample Yardang-1, showing their relative concentrations as indicated by the color scale bar on the right-hand side of each panel. The particle size of the sample is less than 48 μm.
Paper: An Inclusive Library for Quantitative Analysis of the Laser-induced Breakdown Spectra Acquired by the Zhurong Mars Rover
Authors: Shuai-Yi Qu, Jianxun Shen, Luning Li, Zhicheng Cui, Xuesen Xu, Ziyi Liu, Chengxiang Huang, Haohuan Li, Honglei Lin, Wei Lin, Yangting Lin
Figure caption: Scanning μXRF graphs of Si, Ti, Al, Fe, Mg, Ca, Na, and K distributions in the sample SER-2, showing their relative concentrations as indicated by the color scale bar on the right-hand side of each panel. The particle size of the sample is less than 48 μm.
Paper: An Inclusive Library for Quantitative Analysis of the Laser-induced Breakdown Spectra Acquired by the Zhurong Mars Rover
Authors: Shuai-Yi Qu, Jianxun Shen, Luning Li, Zhicheng Cui, Xuesen Xu, Ziyi Liu, Chengxiang Huang, Haohuan Li, Honglei Lin, Wei Lin, Yangting Lin
Figure caption: Standard deviations (SD) of LIBS spectral patterns between 20 laser shots of a single point (i.e., intrasample SD) and those between different measurement points on the surface (i.e., intersample SD) of 16 representative samples (A)–(P).
Paper: An Inclusive Library for Quantitative Analysis of the Laser-induced Breakdown Spectra Acquired by the Zhurong Mars Rover
Authors: Shuai-Yi Qu, Jianxun Shen, Luning Li, Zhicheng Cui, Xuesen Xu, Ziyi Liu, Chengxiang Huang, Haohuan Li, Honglei Lin, Wei Lin, Yangting Lin
Figure caption: LIBS spectra of JMSS-1 with 20 wt% nontronite, acquired at three different sampling locations. The spectrum at each location represents the average of 20 LIBS measurements.
Paper: An Inclusive Library for Quantitative Analysis of the Laser-induced Breakdown Spectra Acquired by the Zhurong Mars Rover
Authors: Shuai-Yi Qu, Jianxun Shen, Luning Li, Zhicheng Cui, Xuesen Xu, Ziyi Liu, Chengxiang Huang, Haohuan Li, Honglei Lin, Wei Lin, Yangting Lin
Figure caption: Scanning μXRF graphs of Si, Ti, Al, Fe, Mg, Ca, Na, and K distributions in the sample JMSS-1 with 1% NaClO4·H2O, 1% NaClO3, 1% NaCl, and 1% NaNO3, showing their relative concentrations as indicated by the color scale bar on the right-hand side of each panel. The particle size of the sample is less than 1 mm.
Paper: An Inclusive Library for Quantitative Analysis of the Laser-induced Breakdown Spectra Acquired by the Zhurong Mars Rover
Authors: Shuai-Yi Qu, Jianxun Shen, Luning Li, Zhicheng Cui, Xuesen Xu, Ziyi Liu, Chengxiang Huang, Haohuan Li, Honglei Lin, Wei Lin, Yangting Lin
Figure caption: Statistics of the number of outlier spectra removed from quantitative regression analysis against the order of LIBS shot during the measurement of each sample. The first six-shot spectra and the last two-shot spectra were mostly considered outliers, while the other shot spectra were generally more typical.
Paper: Ultrahigh-energy Cosmic Rays from Neutrino-emitting Tidal Disruption Events
Authors: Pavlo Plotko, Walter Winter, Cecilia Lunardini, Chengchao Yuan,  成 超 袁
Figure caption: Best-fit prediction for the UHECR and diffuse neutrino fluxes for the fitted composition case of the diverse scenario, in comparison to data. Contributions from the aalc and fdr groups are shown with corresponding gold dashed–dotted and red dashed curves, respectively. UHECR spectrum: the upper left plot displays the predicted spectra against the Auger spectrum. The region where spectrum data are considered as upper limits is indicated in gray; UHECR composition: the bottom plots detail the mean (﹩\langle {X}_{{\rm{\max }}}\rangle ﹩, left) and standard deviation (﹩\sigma ({X}_{{\rm{\max }}})﹩, right) of the UHECR composition. The gray regions mark the data range that is excluded from the fits; neutrino diffuse flux: the upper right plot presents the predicted (all-flavor) diffuse source neutrino flux from TDEs in comparison to the HESE neutrino data from IceCube (M. G. Aartsen et al. 2015). In addition, we show sensitivity curves of Auger  (magenta, E. Zas & Pierre Auger Collaboration 2017), and for future neutrino telescopes, IceCube-Gen2  (black; M. G. Aartsen et al. 2019), RNO-G  (olive; J. Aguilar et al. 2021), and GRAND200k  (red; J. Álvarez Muiz et al. 2019). Table 6 provides detailed parameter values for this best-fit case.
Paper: Ultrahigh-energy Cosmic Rays from Neutrino-emitting Tidal Disruption Events
Authors: Pavlo Plotko, Walter Winter, Cecilia Lunardini, Chengchao Yuan,  成 超 袁
Figure caption: Top: the predicted number of muon neutrinos as a function of the production region radius for three TDEs/candidates: AT2019dsg, AT2019fdr, and AT2019aalc. The thickness of each curve accounts for maximum rigidity and CR composition. The minimum and maximum numbers of neutrinos for each radius value are calculated by scanning over the possible range of the maximum rigidity and CR injection. Bottom: the allowed region of the production region radius for all three TDEs based on the expected number of muon neutrinos from the top plot. Gray arrows mark the upper limits on the production region’s radius derived from IR observations (see Table 1 and corresponding references).
Paper: Ultrahigh-energy Cosmic Rays from Neutrino-emitting Tidal Disruption Events
Authors: Pavlo Plotko, Walter Winter, Cecilia Lunardini, Chengchao Yuan,  成 超 袁
Figure caption: The parameter space for maximum rigidity and radius of the production region for individual TDEs from the aalc (left) and fdr groups (right) for the fitted composition case of the diverse scenario. The white marker indicates the best-fit parameters on each plot, as listed in Table 6. The filled gold square and filled red diamond represent the parameters for AT02019aalc and AT2019fdr from W. Winter & C. Lunardini (2023). The yellow and green contours are the 3σ allowed regions constrained by the spectrum and composition, respectively. The purple contour indicates the part of the parameter space that is consistent with the expected number of neutrinos from progenitors AT2019aalc and AT2019fdr.
Paper: Ultrahigh-energy Cosmic Rays from Neutrino-emitting Tidal Disruption Events
Authors: Pavlo Plotko, Walter Winter, Cecilia Lunardini, Chengchao Yuan,  成 超 袁
Figure caption: The escaped spectra of CRs and neutrinos from an AT02219dsg-like event for two radii (5 × 1016 and 1 × 1018 cm), under the same conditions of maximum rigidity (3.68 × 109 GV) and the CR injection (pure silicon-28), integrated over the entire duration of each event. The solid curves represent the total escaped spectrum of CR, with the contribution of individual CR groups shown in different colors. The black dotted curve represents the total neutrino flux.
Paper: Ultrahigh-energy Cosmic Rays from Neutrino-emitting Tidal Disruption Events
Authors: Pavlo Plotko, Walter Winter, Cecilia Lunardini, Chengchao Yuan,  成 超 袁
Figure caption: The escaped spectra of CRs and neutrinos, integrated over the entire duration of TDE, from the aalc (upper) and fdr groups (lower) for the fitted composition case of the diverse scenario. The solid curves represent the escaped spectrum of CR, with the contribution of individual CR groups shown in different colors. The dashed–dotted and dashed curves represent the total neutrino flux.
Paper: Ultrahigh-energy Cosmic Rays from Neutrino-emitting Tidal Disruption Events
Authors: Pavlo Plotko, Walter Winter, Cecilia Lunardini, Chengchao Yuan,  成 超 袁
Figure caption: Top: composition of injected CRs for the best-fit case for TDEs from the aalc (left) and fdr groups (right). Bottom: composition of MS stars (left), CO-WD (center), and ONeMg-WD (right) for comparison. WD composition shown for comparison only; WD disruptions are unlikely for AT2019dsg, AT2019fdr, or AT2019aalc, see the discussion in Section 6. The elements are categorized into different groups, with each group named after the categorized elements.
Paper: Ultrahigh-energy Cosmic Rays from Neutrino-emitting Tidal Disruption Events
Authors: Pavlo Plotko, Walter Winter, Cecilia Lunardini, Chengchao Yuan,  成 超 袁
Figure caption: The mass abundance profiles across different enhancement factor values for the MS star. The elements are categorized into different groups, with each group named after the categorized elements.
Paper: Ultrahigh-energy Cosmic Rays from Neutrino-emitting Tidal Disruption Events
Authors: Pavlo Plotko, Walter Winter, Cecilia Lunardini, Chengchao Yuan,  成 超 袁
Figure caption: χ2 values as a function of the enhancement factor α of the aalc and fdr groups. For each enhancement factor value of a group, a dedicated fit is performed to determine the minimum χ2 value while minimizing all other fitted parameters, including the enhancement factor of the other group.
Paper: Ultrahigh-energy Cosmic Rays from Neutrino-emitting Tidal Disruption Events
Authors: Pavlo Plotko, Walter Winter, Cecilia Lunardini, Chengchao Yuan,  成 超 袁
Figure caption: The best-fit prediction for UHECR and diffuse neutrino flux for the enhancement factor case in comparison with the data. See the caption of Figure 6 for details. Table 6 provides detailed parameter values for this best-fit case.
Paper: Attributing the O’Connell Effect in Contact Binaries to a Cooling Mass-transfer Stream
Authors: Matthias Fabry, Andrej Prša
Figure caption: Posterior distribution densities of the MCMC chains that estimated the errors on the fit parameters in Table 1. The final row, σlnf, is a numerical “fudge” parameter that estimates the fraction with which the errors on the data are underestimated.
Paper: Attributing the O’Connell Effect in Contact Binaries to a Cooling Mass-transfer Stream
Authors: Matthias Fabry, Andrej Prša
Figure caption: PHOEBE meshes of different ET modes where parameters ﹩{{ \mathcal T }}_{{\rm{eff}},1}=5500\,{\rm{k}}﹩, ﹩{{ \mathcal T }}_{{\rm{eff}},2}=4400\,{\rm{k}}﹩, F = 0.5, and q = 0.5 are used throughout. (a) No mixing applied. (b) Internal mixing mode. (c) Two quadratures of the lateral-mixing mode. Note the different color scale in panel (b).
Paper: Attributing the O’Connell Effect in Contact Binaries to a Cooling Mass-transfer Stream
Authors: Matthias Fabry, Andrej Prša
Figure caption: PHOEBE models of KIC 6223646 that include larger covariance than the original MCMC estimate in Table 1. The red line is the median of the 200 models from the rescaled distributions, while the shaded area is the 1σ flux range of these models.
Paper: Attributing the O’Connell Effect in Contact Binaries to a Cooling Mass-transfer Stream
Authors: Matthias Fabry, Andrej Prša
Figure caption: LCs of the same binary system with lateral mixing of Figure 1 but viewed under different inclinations. The O’Connell effect is highlighted with dashed lines. The unit of the y-axis is arbitrary.
Paper: Attributing the O’Connell Effect in Contact Binaries to a Cooling Mass-transfer Stream
Authors: Matthias Fabry, Andrej Prša
Figure caption: Corner plot of the reconstructed, scaled multivariate Gaussian posteriors.
Paper: Attributing the O’Connell Effect in Contact Binaries to a Cooling Mass-transfer Stream
Authors: Matthias Fabry, Andrej Prša
Figure caption: LC for KIC 6223646 (blue), with the best-fit PHOEBE model with lateral mixing in red. The lower panel shows the residuals, which have an rms value of 0.0035. For comparison, an equal-temperature model (by internal mixing) is shown in black.
Paper: Misaligned External Gas Acquisition Boosts Central Black Hole Activities
Authors: Yuren Zhou, Yanmei Chen, Yong Shi, Guinevere Kauffmann, Junfeng Wang, Gaoxiang Jin, Lan Wang, Shuai Feng, Min Bao
Figure caption: An example of obscured AGN. (a) SDSS g, r, i-band false-color image with the magenta hexagon marking the position of the MaNGA bundle. (b) [N II]-BPT diagram. Purely AGN and composite regions are separated by the black solid curve (Ke01, L. J. Kewley et al. 2001) while pure star-forming and composite regions are separated by the black dashed curve (Ka03, G. Kauffmann et al. 2003). The color bar shows the d⊥ value, which is the minimal distance between each spaxel and the Ke01 line. d⊥ > 0 corresponds to the [N II]-AGN region. (c) d⊥ map, the half major axis (gray dashed) is set at ϕ = 0°, with increasing values of ϕ in the counterclockwise direction. (d) d⊥ as a function of ϕ. The blue dots are the median value of d⊥ in each sector, and the error bars are the ±1σ scattering region. The blue solid curve is the best-fitting double-Gaussian model. Black and gray dashed lines mark the position angle of minor axes (90° and 270°). Black and gray solid lines are the position angle of each peak component, while the gray shaded region represents the ±1σ scattering range.
Paper: Misaligned External Gas Acquisition Boosts Central Black Hole Activities
Authors: Yuren Zhou, Yanmei Chen, Yong Shi, Guinevere Kauffmann, Junfeng Wang, Gaoxiang Jin, Lan Wang, Shuai Feng, Min Bao
Figure caption: An example of outflow-induced kinematic misalignment. (a) The SDSS g, r, i-band image. (b) Stellar velocity field. (c) The Hα velocity field. (d) The [O III] λ5007 equivalent width (EW[OIII]) map. The photometric half major axis (gray dotted) is set as φ = 0°, with increasing values of φ in the counterclockwise direction. The blue solid line represents the PA of the gas component. The purple dashed line represents the average position of the two peak components of EW[OIII] marked as ﹩{\varphi }_{{{\rm{EW}}}_{[{\rm{OIII}}]}}﹩. (e) EW[OIII] as a function of φ. The blue dots are the median value of EW[OIII] in each sector, and the error bars are the ±1σ scattering regions. The red solid curve is the best-fitting double-Gaussian model. Purple dashed lines mark the PA of two peak components.
Paper: Misaligned External Gas Acquisition Boosts Central Black Hole Activities
Authors: Yuren Zhou, Yanmei Chen, Yong Shi, Guinevere Kauffmann, Junfeng Wang, Gaoxiang Jin, Lan Wang, Shuai Feng, Min Bao
Figure caption: Examples of galaxies with different ΔPA. The ΔPA is defined as ΔPA ≡ ∣PAgas − PAstar∣, where PAgas and PAstar are the PAs of gas and stars. The first column shows the Sloan Digital Sky Survey g, r, i-band images with purple hexagons marking the position of the MaNGA bundle. The second and third columns are velocity fields of stellar and gas components, respectively, while the red side moves away from us and the blue side approaches us. The blue solid line represents the PA of the kinematic major axis, while green dashed lines represent the ±1σ error of PAs. The first row shows an example of aligned galaxies (ΔPA = 2﹩\mathop{.}\limits^{\unicode{x000b0}}﹩0) while the second and third rows show examples of prograde galaxies (ΔPA = 77﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5) and retrograde galaxies (ΔPA = 176﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5).
Paper: Misaligned External Gas Acquisition Boosts Central Black Hole Activities
Authors: Yuren Zhou, Yanmei Chen, Yong Shi, Guinevere Kauffmann, Junfeng Wang, Gaoxiang Jin, Lan Wang, Shuai Feng, Min Bao
Figure caption: The global M* vs. Dn4000 diagram. The gray circles and contours are for the entire MaNGA galaxy sample. Red squares represent misaligned galaxies, while blue triangles are the control sample with ﹩| {\rm{\Delta }}\mathrm{log}{M}_{* }| \lt 0.1﹩ and ∣ΔDn4000∣ < 0.05. Blue and red dashed lines separate galaxies into three populations: blue, green, and red galaxies. Panels (b) and (c) show the M* and Dn4000 distribution, respectively. Red histograms are for misaligned galaxies, while blue histograms are for their controls.
Paper: Misaligned External Gas Acquisition Boosts Central Black Hole Activities
Authors: Yuren Zhou, Yanmei Chen, Yong Shi, Guinevere Kauffmann, Junfeng Wang, Gaoxiang Jin, Lan Wang, Shuai Feng, Min Bao
Figure caption: The [S II]-BPT diagram for a Seyfert galaxy. (a) The SDSS g, r, i-band image. (b) The [S II]-BPT diagram. AGN and star-forming (blue) regions are separated by the blue solid line (Ke01, L. J. Kewley et al. 2001), while Seyferts (red) and LINERs (purple) are separated by the green dotted line (Ke06, L. J. Kewley et al. 2006). For the black star, the line ratio is measured from the stacked spectrum of spaxels within a circular aperture of a central 1 kpc radius. (c) The spatially resolved [S II]-BPT diagram, where the colors have the same notation as panel (b).
Paper: 84 and 169 s Rotation of Two Isolated, Ultramassive, Strongly Magnetic White Dwarfs
Authors: Kurtis A. Williams, Zorayda Martinez, Melissa Ornelas
Figure caption: Pulse shapes for SDSS J1557+0411 (left) and PG 1312+099 (right) created by folding observed light curves on the primary frequency of modulation. The black curve in each panel is a sinusoid with the BG40 fit parameters from Table 1. Filled circles with error bars are points are BG40 data, open blue squares with error bars represent g-band data, and red filled triangles are r-band observations. For SDSS J1557+0411, the larger g-band amplitude is apparent.
Paper: 84 and 169 s Rotation of Two Isolated, Ultramassive, Strongly Magnetic White Dwarfs
Authors: Kurtis A. Williams, Zorayda Martinez, Melissa Ornelas
Figure caption: Periodograms for time-series photometry of SDSS J1557+0411 (left panels) and PG 1312+099 (right panels). For each photometric series, an enlargement of the periodogram centered on the detected frequency is also included. A clear monoperiodic signal is detected well above the significance threshold in all cases except the r-band imaging of SDSS J1557+0411.