adsabs/AstroCLIMB huggingface dataset:
Paper: Measuring the Mean Free Path of H I Ionizing Photons at 3.2 ≤ z ≤ 4.6 with DESI Y1 Quasars
Authors: Anning Gao, J. Xavier Prochaska, Zheng Cai, Siwei Zou, Cheng Zhao, Zechang Sun, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, Arjun Dey, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, S. Juneau, A. Kremin, P. Martini, A. Meisner, R. Miquel, J. Moustakas, A. Muñoz-Gutiérrez, J. A. Newman, I. Pérez-Ràfols, G. Rossi, E. Sanchez, M. Schubnell, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: Left: examples of the composite spectra from the bootstrap technique (gray), together with the composite spectra from the normal stacking procedure (red). Right: comparisons between the SED templates and our composite spectra at 700 Å ≤ λr ≤ 2000 Å.
Paper: Interpreting the Extremely Diffuse Stellar Distribution of the Nube Galaxy through Fuzzy Dark Matter
Authors: Yu-Ming Yang, Zhao-Chen Zhang, Xiao-Jun Bi, Peng-Fei Yin
Figure caption: Radial FDM profiles for the three models under consideration are shown. The blue, green, and red solid lines represent the target FDM profiles ρin(r) used as input for generating the initial wave functions. The squares represent the reproduced density profiles ρout(r) obtained from the derived initial wave functions. The dashed lines represent the initial stellar density profiles. Note that the lines representing the stellar density profiles of Model-2 and Model-3 overlap in the figure. The light blue and light orange lines represent the spherical-averaged FDM density profiles of Model-1 at various snapshots during the first 9.2 Gyr and final 1 Gyr of evolution, respectively. Each snapshot is separated by a 50 Myr interval.
Paper: Interpreting the Extremely Diffuse Stellar Distribution of the Nube Galaxy through Fuzzy Dark Matter
Authors: Yu-Ming Yang, Zhao-Chen Zhang, Xiao-Jun Bi, Peng-Fei Yin
Figure caption: Left panel: FDM density field ρ = ma∣ψ∣2 in the z = 0 plane (top row) and the projected positions of the star particles onto the x–y plane (bottom row) at four snapshots throughout the entire simulation duration. The red dots and circles in the bottom row represent the position of the stellar mass center and the locations at a distance of R = 13 kpc from the mass center, corresponding to the maximum observational range. Right panel: relative coordinate of the soliton center and stellar mass center concerning the halo mass center throughout the simulation duration. Gray, orange, and purple distinguish the x, y, and z coordinates, while solid and dashed lines differentiate between the soliton and the stellar component. All the results in this figure are derived from the analysis of Model-1.
Paper: Interpreting the Extremely Diffuse Stellar Distribution of the Nube Galaxy through Fuzzy Dark Matter
Authors: Yu-Ming Yang, Zhao-Chen Zhang, Xiao-Jun Bi, Peng-Fei Yin
Figure caption: Left panel: initial (dashed lines) and final (solid lines) 2D stellar density profiles of the three models under consideration. The color scheme aligns with the colors used in Figure 1. The black points with error bars represent the observational stellar distribution of Nube (M. Montes et al. 2024). The gray shaded region delineates the approximate range covered by the profiles of dwarf galaxies from N. Chamba et al. (2020) with stellar masses (1–5 × 108 M⊙) similar to that of Nube. For comparison, the profile of DF 44, a prototypical UDG, is illustrated by the gray square symbols (M. Montes et al. 2024). Right panel: the blue, red, and green solid lines, as well as the black points with error bars, are the same as in the left panel. However, the horizontal axis is set to a logarithmic scale to more intuitively display the profiles at small radii. The cyan and pink solid lines represent the results of Model-﹩1^{\prime} ﹩ and Model-1″, respectively.
Paper: Mapping the Merging Zone of Late Infall in the AB Aur Planet-forming System
Authors: Jessica Speedie, Ruobing Dong, Richard Teague, Dominique Segura-Cox, Jaime E. Pineda, Josh Calcino, Cristiano Longarini, Cassandra Hall, Ya-Wen Tang, Jun Hashimoto, Teresa Paneque-Carreño, Giuseppe Lodato, Bennedetta Veronesi
Figure caption: Modeling S1, S2, and S3 as infall. (a) Intensity-weighted velocity map of the anti-Keplerian-weighted 12CO J = 2–1 image cube (as in Figure 3(b) inset). We overlay R.A.–decl. trajectories of three streamlines matching S1, S2, and S3, computed with the analytic accretion flow model of S. Mendoza et al. (2009) implemented in J. E. Pineda et al. (2020). The color bar for velocity applies to both the background velocity map and the model streamlines. (b), (c), and (d) PV slices taken along the R.A.–decl. trajectory of each streamline for completely consistent comparison between model and data (one panel per streamline). Within a panel, multiple cubes have been sliced: the full unweighted 12CO cube (color map), the Keplerian-weighted 12CO cube (orange contours), and the anti-Keplerian-weighted 12CO cube (cyan contours). PV slices in the SO JN = 56–45 image cube are overplotted as filled contours in increments of 2σ starting at 3σ. We concatenate arbitrary extensions to the slice paths so that the PV diagrams span r = 0″–8″ in on-sky radial offset, shown as dotted gray lines extending from both ends of the streamline trajectories. Radial and azimuthal PV cross sections providing additional visualizations of S1 and S2 merging with the disk are available in Appendix D Figure 9.
Paper: Mapping the Merging Zone of Late Infall in the AB Aur Planet-forming System
Authors: Jessica Speedie, Ruobing Dong, Richard Teague, Dominique Segura-Cox, Jaime E. Pineda, Josh Calcino, Cristiano Longarini, Cassandra Hall, Ya-Wen Tang, Jun Hashimoto, Teresa Paneque-Carreño, Giuseppe Lodato, Bennedetta Veronesi
Figure caption: ALMA 12CO J = 2–1 moment maps after disentangling the disk and exo-disk emission. (a) Integrated intensity map of 12CO after weighting with a spectrally smoothed Keplerian mask. (b) The same, but after weighting with an anti-Keplerian mask generated with opposite Boolean values prior to spectral smoothing. Views of the masks are provided in Appendix B Figure 7. The cyan points trace S1, S2, and S3 from Table 4 of Y.-W. Tang et al. (2012). Panels (a) and (b) are shown on a ﹩{\mathrm{log}}_{10}﹩ color scale to compare with Figure 1(b). Intensity-weighted velocity maps are shown in the insets. (c) High-pass-filtered integrated intensity map of the Keplerian-weighted 12CO cube in panel (a), highlighting the architecture of spiral structure within the disk. (d) The same as panel (b), but scaled by r (on sky) and presented on a linear color scale.
Paper: Mapping the Merging Zone of Late Infall in the AB Aur Planet-forming System
Authors: Jessica Speedie, Ruobing Dong, Richard Teague, Dominique Segura-Cox, Jaime E. Pineda, Josh Calcino, Cristiano Longarini, Cassandra Hall, Ya-Wen Tang, Jun Hashimoto, Teresa Paneque-Carreño, Giuseppe Lodato, Bennedetta Veronesi
Figure caption: Introducing our ALMA observations. (a) VLT/SPHERE H-band scattered light image at 1.6 μm (A. Boccaletti et al. 2020), shown for scale. (b) ALMA 12CO J = 2–1 integrated intensity map, collapsed uniformly over line-of-sight velocities ±6 km s−1 about vsys. Emission extends ∼20″ (∼3200 au) in diameter, roughly half the diameter of the 12 m antenna FOV in Band 6. (c) ALMA SO JN = 56−45 peak intensity map. The ring takes a brightness peak in the northeast.
Paper: Mapping the Merging Zone of Late Infall in the AB Aur Planet-forming System
Authors: Jessica Speedie, Ruobing Dong, Richard Teague, Dominique Segura-Cox, Jaime E. Pineda, Josh Calcino, Cristiano Longarini, Cassandra Hall, Ya-Wen Tang, Jun Hashimoto, Teresa Paneque-Carreño, Giuseppe Lodato, Bennedetta Veronesi
Figure caption: The influence of the continuum ring substructure on the observed SO ring substructure in peak intensity vs. integrated intensity maps. (a) ALMA continuum image at 233.0 GHz from the program presented in this work. The continuum is overlaid in contours at 1.0, 2.0, 3.0, and 4.0 mJy beam–1 in all other panels. (b) ALMA SO JN = 56−45 peak intensity map before continuum subtraction, and (c) after continuum subtraction (shown in the main text). These two maps are shown on the same color bar scale. (d) ALMA SO JN = 56−45 integrated intensity map before and (e) after continuum subtraction.
Paper: The S-PLUS 12-band Photometry as a Powerful Tool for Discovery and Classification: Ten Cataclysmic Variables in a Proof-of-concept Study
Authors: Raimundo Lopes de Oliveira, Amanda S. de Araújo, Angela C. Krabbe, Claudia L. Mendes de Oliveira, Koji Mukai, Luis A. Gutiérrez-Soto, Antonio Kanaan, Romualdo Eleutério, Marcelo Borges Fernandes, Fredi Quispe-Huaynasi, William Schoenell, Tiago Ribeiro
Figure caption: Optical spectra from the GMOS instrument at Gemini South telescope.
Paper: The S-PLUS 12-band Photometry as a Powerful Tool for Discovery and Classification: Ten Cataclysmic Variables in a Proof-of-concept Study
Authors: Raimundo Lopes de Oliveira, Amanda S. de Araújo, Angela C. Krabbe, Claudia L. Mendes de Oliveira, Koji Mukai, Luis A. Gutiérrez-Soto, Antonio Kanaan, Romualdo Eleutério, Marcelo Borges Fernandes, Fredi Quispe-Huaynasi, William Schoenell, Tiago Ribeiro
Figure caption: X-ray spectra from Swift/XRT: red circles for S-PLUS CV1, green diamonds for S-PLUS CV4, and blue squares for S-PLUS CV6.
Paper: The S-PLUS 12-band Photometry as a Powerful Tool for Discovery and Classification: Ten Cataclysmic Variables in a Proof-of-concept Study
Authors: Raimundo Lopes de Oliveira, Amanda S. de Araújo, Angela C. Krabbe, Claudia L. Mendes de Oliveira, Koji Mukai, Luis A. Gutiérrez-Soto, Antonio Kanaan, Romualdo Eleutério, Marcelo Borges Fernandes, Fredi Quispe-Huaynasi, William Schoenell, Tiago Ribeiro
Figure caption: SED from the S-PLUS photometry.
Paper: Multimission Observations of Relativistic Electrons and High-speed Jets Linked to Shock-generated Transients
Authors: Savvas Raptis, Martin Lindberg, Terry Z. Liu, Drew L. Turner, Ahmad Lalti, Yufei Zhou, Primož Kajdič, Athanasios Kouloumvakos, David G. Sibeck, Laura Vuorinen, Adam Michael, Mykhaylo Shumko, Adnane Osmane, Eva Krämer, Lucile Turc, Tomas Karlsson, Christos Katsavrias, Lynn B. Wilson, Hadi Madanian, Xóchitl Blanco-Cano, Ian J. Cohen, C. Philippe Escoubet
Figure caption: MMS observations of the downstream magnetosheath region. (A) From top to bottom, the panels display the magnetic field resampled in GSE coordinates and averaged with a 150 data point window, ion velocity in GSE coordinates, ion and electron densities, the omnidirectional ion energy spectrum from FPI, ion temperatures parallel and perpendicular to the magnetic field, the high-energy electron differential energy spectrum from FEEPS, and the electron differential energy spectrum from FPI. The red-shaded area indicates a thermalized region associated with the “core” of the transmitted HFAs, while the blue-shaded area reveals localized high-speed jets forming at the transmitted compressive boundaries. (B) corresponds to a detailed plot of the compressive edge/jet and its adjacent heated core region. From top to bottom, the plot includes ion dynamic pressure, with the background value plotted as a 5 min window moving average, the magnetic field resampled in GSE coordinates and averaged over a 150 data point (30 s) window, ion velocity in GSE coordinates, integrated 1D distribution along the Sun–Earth line, ion and electron densities, ion differential energy spectrum, and ion temperature. As demonstrated, the localized jets exhibit a relative increase in both density and speed, resulting in dynamic pressure up to 10 times higher than the magnetosheath background.
Paper: Multimission Observations of Relativistic Electrons and High-speed Jets Linked to Shock-generated Transients
Authors: Savvas Raptis, Martin Lindberg, Terry Z. Liu, Drew L. Turner, Ahmad Lalti, Yufei Zhou, Primož Kajdič, Athanasios Kouloumvakos, David G. Sibeck, Laura Vuorinen, Adam Michael, Mykhaylo Shumko, Adnane Osmane, Eva Krämer, Lucile Turc, Tomas Karlsson, Christos Katsavrias, Lynn B. Wilson, Hadi Madanian, Xóchitl Blanco-Cano, Ian J. Cohen, C. Philippe Escoubet
Figure caption: (A) Electron phase space density as a function of energy for upstream (Cluster) and downstream (MMS) observations, along with background noise levels for each instrument. Measurements are taken around the energy peak identified by each mission. CL4 data points (blue) are averaged over 1 min [04:45–04:46], while MMS measurements (black) are averaged during 30 s [04:43:30–04:44:00]. Error bars denote standard deviation, and transparent points indicate values near or below noise levels. Low-energy data are taken from MMS’ FPI and Cluster’s PEACE, while the high-energy tail data are from MMS’ FEEPS and Cluster’s RAPID. The 3σ noise levels are shown for both Cluster and MMS high-energy instruments, with Cluster noise taken at [04:47:30–04:49:30] and MMS at [04:00:30–04:09:30]. Red dashed lines depict spectral slopes (p) of −4 and −3. (B) A zoomed-in view of the energetic tail distribution with noise levels subtracted, comparing MMS observations, Cluster observations, and Cluster with betatron acceleration applied. Horizontal error bars show the range of energy gain modeled by betatron acceleration using 1σ variability in the upstream and downstream magnetic field measurements taken concurrently with the electron fluxes intervals. The betatron model used is defined as ﹩{\rm{\Delta }}E/\langle {E}_{0}\rangle =\tfrac{2}{3}{\rm{\Delta }}B/{B}_{0}﹩, where Δ denotes difference between upstream and downstream measurements and B0, E0 the upstream value.
Paper: Multimission Observations of Relativistic Electrons and High-speed Jets Linked to Shock-generated Transients
Authors: Savvas Raptis, Martin Lindberg, Terry Z. Liu, Drew L. Turner, Ahmad Lalti, Yufei Zhou, Primož Kajdič, Athanasios Kouloumvakos, David G. Sibeck, Laura Vuorinen, Adam Michael, Mykhaylo Shumko, Adnane Osmane, Eva Krämer, Lucile Turc, Tomas Karlsson, Christos Katsavrias, Lynn B. Wilson, Hadi Madanian, Xóchitl Blanco-Cano, Ian J. Cohen, C. Philippe Escoubet
Figure caption: High-energy electron differential energy spectrum from the MMS FEEPS instrument between [04:40:30 and 04:43:30]. The red line represents the trend line of ﹩{\left(B/{B}_{0}\right)}^{2/3}﹩, while the white line shows the relationship of B/B0, where B0 denotes the magnetic field value at 04:40:30. Two lines are plotted, starting from different initial energies E0. The magnetic field signal is averaged over a 30 data point window for better visualization. As shown in this plot, the dependence on the exponent of 2/3 aligns closely with the contours of the phase space density (color bar), validating the use of our model across a wide time range.
Paper: Multimission Observations of Relativistic Electrons and High-speed Jets Linked to Shock-generated Transients
Authors: Savvas Raptis, Martin Lindberg, Terry Z. Liu, Drew L. Turner, Ahmad Lalti, Yufei Zhou, Primož Kajdič, Athanasios Kouloumvakos, David G. Sibeck, Laura Vuorinen, Adam Michael, Mykhaylo Shumko, Adnane Osmane, Eva Krämer, Lucile Turc, Tomas Karlsson, Christos Katsavrias, Lynn B. Wilson, Hadi Madanian, Xóchitl Blanco-Cano, Ian J. Cohen, C. Philippe Escoubet
Figure caption: Overview of Cluster observations in the upstream region. From top to bottom, resampled magnetic field in GSE coordinates (averaged over a 150 data point window), ion velocity in GSE coordinates, ion density, ion differential energy spectrum, and differential energy spectra for electrons in high-energy, mid-energy, and low-energy ranges. The red-shaded area approximately denotes the core region of multiple foreshock transients that develop upstream of Earth’s bow shock.
Paper: Multimission Observations of Relativistic Electrons and High-speed Jets Linked to Shock-generated Transients
Authors: Savvas Raptis, Martin Lindberg, Terry Z. Liu, Drew L. Turner, Ahmad Lalti, Yufei Zhou, Primož Kajdič, Athanasios Kouloumvakos, David G. Sibeck, Laura Vuorinen, Adam Michael, Mykhaylo Shumko, Adnane Osmane, Eva Krämer, Lucile Turc, Tomas Karlsson, Christos Katsavrias, Lynn B. Wilson, Hadi Madanian, Xóchitl Blanco-Cano, Ian J. Cohen, C. Philippe Escoubet
Figure caption: (A) MMS1 and C4 spacecraft locations in the GSE XY and XZ planes are shown. The bow shock and magnetopause boundary surfaces are shown using J. Chao et al.'s (2002) model. The bow shock is color coded based on 1 hr OMNIweb IMF data, indicating regions of quasi-parallel (blue, θBn < 40∘), oblique (magenta, 40∘ < θBn < 50∘), and quasi-perpendicular (red, θBn > 50∘) shock. The blue arrow shows the shock’s normal direction at the closest point of the bow shock model from the MMS location, while the black arrow indicates the direction of the IMF. (B) shows the XY GSE plane and the positions of the L1 solar wind monitors: ACE, DSCOVR, and Wind. The Sun–Earth line is marked with a dashed line for reference. (C) shows the solar wind magnetic field measurements taken before and during the analysis period, highlighting the presence of multiple discontinuities and mesoscale variability even across the  ∼50 earth radii separation between the L1 solar wind monitors. Such magnetic field configurations are expected to generate disturbances at Earth, contributing to the formation of multiple upstream transient phenomena.
Paper: Dominant Role of Coplanar Inflows in Driving Disk Evolution Revealed by Gas-phase Metallicity Gradients
Authors: Cheqiu Lyu, Enci Wang, Hongxin Zhang, Yingjie Peng, Xin Wang, Haixin Li, Chengyu Ma, Haoran Yu, Zeyu Chen, Cheng Jia, Xu Kong
Figure caption: Top panels: metallicity gradient on the disk as a function of stellar mass and gas-phase metallicity at effective radius. Each dot represents an individual galaxy in our sample, with a redder/bluer color corresponding to a steeper negative/flatter or positive metallicity gradient. The black curve and dots indicate the median y-values in each x-bin with a width of 0.2 dex for each galaxy. The top-left panel shows the scatter plot and the top-right panel shows the corresponding smooth results using the locally weighted regression method LOESS (W. S. Cleveland & S. J. Devlin 1988; M. Cappellari et al. 2013) to reveal the underlying trend. Bottom panels: gas-phase metallicity radial profiles in 0.5−1.5Re considered in this work, subdivided into four stellar mass bins (from left to right: ﹩\mathrm{log}({M}_{* }/{M}_{\odot })=9.0-9.6,9.6-10.2,10.2-10.8,10.8-12.0﹩). For each bin, the blue, orange, green, and red curves correspond to median profiles of galaxies in four quantiles of metallicity excess (﹩{\rm{\Delta }}\mathrm{log}({\rm{O}}/{\rm{H}})﹩). The shaded areas indicate the uncertainties of the median values.
Paper: Dominant Role of Coplanar Inflows in Driving Disk Evolution Revealed by Gas-phase Metallicity Gradients
Authors: Cheqiu Lyu, Enci Wang, Hongxin Zhang, Yingjie Peng, Xin Wang, Haixin Li, Chengyu Ma, Haoran Yu, Zeyu Chen, Cheng Jia, Xu Kong
Figure caption: Metallicity gradient on the disk as a function of metallicity excess at the effective radius and local gas turbulence. The top panels show the scatter plot of each galaxy and the corresponding smooth results. The dots and colors are similar to the top panels of Figure 2. The bottom panel depicts the median gas-phase metallicity profiles, each normalized to arbitrary values, within bins of 0.4 dex in ﹩\mathrm{log}({\sigma }_{{\rm{gas}}}/{R}_{{\rm{e}}})﹩ and 0.2 dex in ﹩{\rm{\Delta }}\mathrm{log}({\rm{O}}/{\rm{H}})﹩. Each inset maintains a consistent y-axis range, with the x-axis spanning from 0.5 to 1.5 Re. The color of each profile corresponds to ﹩{\rm{\nabla }}\mathrm{log}({\rm{O}}/{\rm{H}})﹩, denoted in the colorbar with shaded areas indicating the uncertainties of the median values.
Paper: Dominant Role of Coplanar Inflows in Driving Disk Evolution Revealed by Gas-phase Metallicity Gradients
Authors: Cheqiu Lyu, Enci Wang, Hongxin Zhang, Yingjie Peng, Xin Wang, Haixin Li, Chengyu Ma, Haoran Yu, Zeyu Chen, Cheng Jia, Xu Kong
Figure caption: The residual scatters to the fitting curves of metallicity gradient vs. μα = Y + α(X) with various combinations of physical parameters X and Y (Y, X in logarithmic scale) labeled on the x-axis. The residual scatters are normalized to ﹩{\sigma }_{{M}_{* }}﹩ (X = 0, ﹩Y=\mathrm{log}({M}_{* }/{M}_{\odot })﹩). Different colors indicate the curves for three different gas-phase metallicity estimators or calibrations.
Paper: Dominant Role of Coplanar Inflows in Driving Disk Evolution Revealed by Gas-phase Metallicity Gradients
Authors: Cheqiu Lyu, Enci Wang, Hongxin Zhang, Yingjie Peng, Xin Wang, Haixin Li, Chengyu Ma, Haoran Yu, Zeyu Chen, Cheng Jia, Xu Kong
Figure caption: Metallicity gradient as a function of metallicity excess at the effective radius and gradient of Σ*. The left and right panels show the scatter plot and corresponding smooth results, respectively. The dots and colors are similar to the top panels of Figure 2. The color gradients, indicated by arrows, represent the directions of increasing ﹩{\rm{\nabla }}\mathrm{log}({\rm{O}}/{\rm{H}})﹩.
Paper: Dominant Role of Coplanar Inflows in Driving Disk Evolution Revealed by Gas-phase Metallicity Gradients
Authors: Cheqiu Lyu, Enci Wang, Hongxin Zhang, Yingjie Peng, Xin Wang, Haixin Li, Chengyu Ma, Haoran Yu, Zeyu Chen, Cheng Jia, Xu Kong
Figure caption: Metallicity gradient on the disk as a function of the linear combination of local turbulence and metallicity excess at the effective radius. Each dot represents an individual galaxy in our sample, with α ∼ 2.69 minimizing the residual scatter (σ ∼ 0.088) of the relation. The blue curve indicates the median values, with the shaded area as the uncertainties, and the red curve represents the second polynomial fit of the data.
Paper: Dominant Role of Coplanar Inflows in Driving Disk Evolution Revealed by Gas-phase Metallicity Gradients
Authors: Cheqiu Lyu, Enci Wang, Hongxin Zhang, Yingjie Peng, Xin Wang, Haixin Li, Chengyu Ma, Haoran Yu, Zeyu Chen, Cheng Jia, Xu Kong
Figure caption: Metallicity gradient as a function of σgas/Re and σgas. The left and right panels show the scatter plot and corresponding smooth results, respectively. The dots and colors are similar to the top panels of Figure 2. The color gradients, indicated by arrows, represent the directions of increasing ﹩{\rm{\nabla }}\mathrm{log}({\rm{O}}/{\rm{H}})﹩.
Paper: Dominant Role of Coplanar Inflows in Driving Disk Evolution Revealed by Gas-phase Metallicity Gradients
Authors: Cheqiu Lyu, Enci Wang, Hongxin Zhang, Yingjie Peng, Xin Wang, Haixin Li, Chengyu Ma, Haoran Yu, Zeyu Chen, Cheng Jia, Xu Kong
Figure caption: Relative importance of galaxy physical parameters (labeled on the x-axis) employed for regressing the metallicity gradient in Random Forest models. The metallicity calibration is marked in the top-right corner.
Paper: Dominant Role of Coplanar Inflows in Driving Disk Evolution Revealed by Gas-phase Metallicity Gradients
Authors: Cheqiu Lyu, Enci Wang, Hongxin Zhang, Yingjie Peng, Xin Wang, Haixin Li, Chengyu Ma, Haoran Yu, Zeyu Chen, Cheng Jia, Xu Kong
Figure caption: Relative importance of galaxy physical parameters (labeled on the x-axis) employed for regressing the metallicity gradient in Random Forest models. ﹩{\rm{\nabla }}\mathrm{log}({\rm{O}}/{\rm{H}})﹩ and ﹩{\rm{\Delta }}\mathrm{log}({\rm{O}}/{\rm{H}})﹩ are calculated by alternative estimators or calibrations marked in the top-right corner of each panel.