adsabs/AstroCLIMB huggingface dataset:
Paper: Machine Learning Inference of Stellar Properties Using Integrated Photometric and Spectroscopic Data
Authors: Ilay Kamai, Alex M. Bronstein, Hagai B. Perets
Figure caption: Results of age prediction. The dark blue lines represent a 72% confidence interval. Colors represent Teff.
Paper: Solar Eruption Onset and Particle Acceleration in Nested-null Topologies
Authors: Pankaj Kumar, Judith T. Karpen, Peter F. Wyper, David Lario, Spiro K. Antiochos, C. Richard DeVore
Figure caption: Kinematics of the flux rope and associated fast and slow EUV waves during E1. (a1)–(a2) AIA 304 Å images showing remote ribbons R4 and R5 during the flux rope eruption. The first image is overlaid with HMI magnetogram contours (scale = ±100 G), representing positive (cyan) and negative (black) polarities. (b1)–(b4) AIA 211 Å running-difference images capturing the fast and slow EUV waves during the eruption. LE denotes the leading edge of the flux rope. The solid black curve traces the solar limb. (c1) RHESSI X-ray flux profiles (4 s cadence) in five different energy channels. (c2) AIA 304 Å peak counts (12 s cadence) extracted from ribbons R4 and R5 within the boxes outlined in (a2). The vertical dashed line indicates the onset of energy release near N2. The time intervals of energy release at N1 and N2 are indicated by arrows. (c3) RSTN radio flux-density profile (410 MHz, 1 s cadence) from the Sagamore Hill Solar Observatory. (d1)–(d2) TD intensity plots along slices R3S3 (see Figure 3(c1)) and R4S4 (see panel (b3)), derived from AIA 94 Å and 211 Å images.
Paper: Solar Eruption Onset and Particle Acceleration in Nested-null Topologies
Authors: Pankaj Kumar, Judith T. Karpen, Peter F. Wyper, David Lario, Spiro K. Antiochos, C. Richard DeVore
Figure caption: Formation and eruption of the flux rope and associated X1.0 flare for E1. (a1)–(a4) AIA 304 Å images showing a filament and multiple ribbons (R1, R2, R3, and R4) prior to and during the eruption. The first image is overlaid with HMI magnetogram contours (scale = ±200 G) representing positive (white) and negative (black) polarities. RHESSI contours (12–25 keV, 25–50 keV, and 100–300 keV) are overlaid on the AIA 304 Å image in panel (a3), with contour levels at 50%, 70%, and 90% of the peak intensity. (b1)–(b4) and (c1)–(c4) AIA 131 Å and 94 Å images showing the flux rope (FR), leading edge (LE), and associated plasma sheet (PS). FA represents the flare arcade, while SA1 and SA2 indicate the side arcades. R3S3 marks a slice used to generate the TD intensity map in Figure 4(d1). (d1)–(d4) RHESSI contours (6–12 keV, 12–25 keV, 25–50 keV, and 100–300 keV) overlaid on AIA 94 Å images during the preeruption, eruption, and posteruption phases. The contour levels in panels (d1)–(d3) are 50%, 70%, and 90% of the peak intensity, whereas in panel (d4), the contour levels are 30%, 50%, 70%, and 90% of the peak intensity.
Paper: Solar Eruption Onset and Particle Acceleration in Nested-null Topologies
Authors: Pankaj Kumar, Judith T. Karpen, Peter F. Wyper, David Lario, Spiro K. Antiochos, C. Richard DeVore
Figure caption: Kinematics of the flux rope and associated fast and slow EUV wavefronts during E2. (a1)–(a3) AIA 304 and 211 Å images showing the filament and multiple ribbons. (b1)–(b3) AIA 211 Å running-difference images illustrating the fast and slow EUV waves. The red box indicates the field of view for the top-row panels. (c1)–(c3) TD intensity plots along slits P1Q1, P2Q2, and P3Q3 (LE=leading edge, FR=flux rope). (d1)–(d3) GOES soft X-ray flux (1–8 Å) and AIA 94 Å peak counts (red dashed curve) extracted from the eruption site (red box in (b1)). The vertical dashed line indicates the onset of energy release at N2. The AIA 211 Å peak counts in (d2) are extracted from the breakout ribbons (R3 and R4) within the white box shown in (a3). The RSTN radio flux density (1 s cadence) at 245 MHz shows quasiperiodic Type III radio bursts.
Paper: Solar Eruption Onset and Particle Acceleration in Nested-null Topologies
Authors: Pankaj Kumar, Judith T. Karpen, Peter F. Wyper, David Lario, Spiro K. Antiochos, C. Richard DeVore
Figure caption: Formation and eruption of a flux rope along with breakout reconnection during E2 on 2014 March 30. AIA 131 and 94 Å images depict the flux rope (FR) formation and eruption. “F” denotes the filament. “N” marks the approximate position of the inner null. SA indicates the side arcade, and FA represents the flare arcade. The red ellipse in panel (b2) highlights the sigmoidal structure. The slits P1Q1 and P2Q2 are used to create the TD intensity maps in Figures 7(c1)–(c3).
Paper: Solar Eruption Onset and Particle Acceleration in Nested-null Topologies
Authors: Pankaj Kumar, Judith T. Karpen, Peter F. Wyper, David Lario, Spiro K. Antiochos, C. Richard DeVore
Figure caption: 3D MHD simulation of an eruption in a nested-null topology. (a)–(d) logarithm of normalized current density and magnetic-field lines (gray represents the pseudostreamer, while yellow and green correspond to the inner fan-spine system). N1 and N2 are the inner and outer nulls, respectively (from P. F. Wyper et al. 2025, in preparation).
Paper: Solar Eruption Onset and Particle Acceleration in Nested-null Topologies
Authors: Pankaj Kumar, Judith T. Karpen, Peter F. Wyper, David Lario, Spiro K. Antiochos, C. Richard DeVore
Figure caption: Radio bursts before and during E2. (a) RSTN radio flux density (sfu, 1 s cadence) at 245 MHz. (b)–(c) E-Callisto dynamic radio spectra from the KRIM (Crimean Astrophysical Observatory) and MRT1 (Mongolia) stations. The oval in (b) highlights the faint radio emission during the preeruption phase. The horizontal dashed line in (c) indicates the 150 MHz frequency. (d)–(g) radio flux density (12 s cadence, sfu) extracted from NRH images of the northwest quarter of the Sun at four frequencies between 150 and 327 MHz during 11:45–12:00 UT.
Paper: Solar Eruption Onset and Particle Acceleration in Nested-null Topologies
Authors: Pankaj Kumar, Judith T. Karpen, Peter F. Wyper, David Lario, Spiro K. Antiochos, C. Richard DeVore
Figure caption: Preeruption activities prior to E1 on 2014 March 29. (a1)–(a4) AIA 211 Å images showing a confined filament eruption and an associated C1.1 flare within the inner fan-spine system. N1 denotes the inner null (X-point). (b1)–(b2) and (c1)–(c2) AIA 171 Å and 94 Å images capturing the preeruption phases. R1S1 and R2S2 indicate the slices used to generate the time–distance (TD) intensity maps. (d1)–(d2) TD intensity maps along slices R1S1 and R2S2 during 16:00–18:00 UT. The white dotted line in (d1) displays the GOES soft X-ray flux profile in the 1–8 Å channel (scale on the right y-axis).
Paper: Solar Eruption Onset and Particle Acceleration in Nested-null Topologies
Authors: Pankaj Kumar, Judith T. Karpen, Peter F. Wyper, David Lario, Spiro K. Antiochos, C. Richard DeVore
Figure caption: Interplanetary radio bursts and SEPs (electrons and protons) associated with E1. (a) Wind/WAVES dynamic radio spectrum (1 minute average) in the 0.02–13.82 MHz frequency range. The yellow circle highlights faint radio enhancement during CME propagation in the interplanetary medium. The color bar represents the average intensity of the electric field (in dB above the background level). (b)–(c) Electron flux (12 s cadence) measured by Wind 3DP at different energies ranging from 26 to 512 keV. (d) Proton flux (1 minute cadence) detected by SOHO/ERNE at different energies ranging from 14.5 to 90 MeV.
Paper: Solar Eruption Onset and Particle Acceleration in Nested-null Topologies
Authors: Pankaj Kumar, Judith T. Karpen, Peter F. Wyper, David Lario, Spiro K. Antiochos, C. Richard DeVore
Figure caption: Imaging of radio sources during E2. (a1)–(a4) NRH radio sources (Type III bursts) at 327 MHz. (b1)–(b4) NRH radio sources at 150 MHz (Type III and Type II bursts). (c1)–(c4) Contours of radio sources at 150 MHz (red) and 327 MHz (blue) overlaid on AIA 211 Å running-difference images (Δt = 1 minute). The contour levels are 80% and 90% of the peak intensity. The black curve traces the solar limb.
Paper: GATOS. VIII. On the Physical Origin of the Extended Mid-infrared Emission in Active Galactic Nuclei
Authors: Enrique Lopez-Rodriguez, Cristina Ramos Almeida, Miguel Pereira-Santaella, Ismael García-Bernete, Robert Nikutta, Almudena Alonso-Herrero, Anelise Audibert, Enrica Bellocchi, Andrew Bunker, Steph Campbell, Françoise Combes, Richard Davies, Tanio Diaz-Santos, Lindsay Fuller, Poshak Gandhi, Santiago García-Burillo, Omaira González-Martín, Erin K. S. Hicks, Sebastian Hönig, Kohei Ichikawa, Masatoshi Imanishi, Takuma Izumi, Alvaro Labiano, Nancy A. Levenson, Christopher Packham, David Rosario, Dimitra Rigopoulou, Daniel Rouan, Taro Shimizu, Marko Stalevski, Martin Ward, Lulu Zhang, Claudio Ricci, Donaji Esparza-Arredondo, Begoña García-Lorenzo
Figure caption: Steps to extract the emission lines from the MRS observations and to compute the line emission, line-free, and “MIRI-like” (continuum+line) images within an MIRI imaging filter. As an example, we show the MRS observations of NGC 5728 and the F1000W filter. Step 1: Select MRS subchannels within the wavelength range of a given MIRI imaging filter. Step 2: Identify emission lines within the wavelength range of an MIRI imaging filter. The F1000W throughput (orange line), the integrated spectrum (blue line) within the full datacube, and the identified emission lines are shown. Step 3: Extract the emission line per spaxel. The [S IV] emission line (blue line), the wavelength at the peak flux, λobs, and the lower, λl, and upper, λu, wavelengths at which the emission line flux satisfies ﹩{F}_{{\lambda }_{{\rm{l}},{\rm{u}}}}\leqslant {F}_{{\rm{c}}}+1{\sigma }_{{\rm{c}}}﹩ (green dashed line), are shown. The continuum-subtracted line (red solid line) is shown. Step 4: Compute emission line images. The integrated emission lines (e.g., [Ar III], [Fe VII], H20-0S(3), and [S IV]) identified in the F1000W filter of the central 1 kpc of NGC 5728 are shown. Step 5: Compute the total contribution of the emission lines within the MIRI filter. Step 6: Fit the continuum emission. The spectrum of a single spaxel with the third-order spline curve (black line) fitted to the continuum emission (red line) with masked emission lines (blue line) and broad lines (e.g., PAH at 11.3 μm; green line) is shown. Step 7: Compute the total contribution of the continuum emission within the MIRI imaging filter. Step 8: Compute the total (continuum+line) MIR emission within the MIRI imaging filter. For all images, the filter throughput was multiplied by the MRS cube of the line and continuum emission. Contours (white lines) increase in steps of [1, 5, 10, 30, 50, 70]% from the peak flux. The contour at a 10% level (thick white line) from the peak flux is shown for reference. The radio axis (black line), dust lane (blue line), and stellar bar (red line) are shown.
Paper: GATOS. VIII. On the Physical Origin of the Extended Mid-infrared Emission in Active Galactic Nuclei
Authors: Enrique Lopez-Rodriguez, Cristina Ramos Almeida, Miguel Pereira-Santaella, Ismael García-Bernete, Robert Nikutta, Almudena Alonso-Herrero, Anelise Audibert, Enrica Bellocchi, Andrew Bunker, Steph Campbell, Françoise Combes, Richard Davies, Tanio Diaz-Santos, Lindsay Fuller, Poshak Gandhi, Santiago García-Burillo, Omaira González-Martín, Erin K. S. Hicks, Sebastian Hönig, Kohei Ichikawa, Masatoshi Imanishi, Takuma Izumi, Alvaro Labiano, Nancy A. Levenson, Christopher Packham, David Rosario, Dimitra Rigopoulou, Daniel Rouan, Taro Shimizu, Marko Stalevski, Martin Ward, Lulu Zhang, Claudio Ricci, Donaji Esparza-Arredondo, Begoña García-Lorenzo
Figure caption: Line emission vs. total MIR emission image in the F1000W filter. From left to right and top to bottom, we show the integrated line emission images (color scale) of [Ar III], [Fe VII], H20-0S(3), and [S IV] for ESO137-G034, MCG-05-23-016, NGC 3081, NGC 5506, NGC 5728, and NGC 7172. Line (white) and total MIR emission (black) contours increase in steps of [1, 5, 10, 30, 50, 70]% from the peak flux. The contour at a 10% level (thick line) from the peak flux is shown for reference. The radio jet (black line) and dust lane (blue line) are shown. The integrated flux of the line emission within the 1 kpc FOV is shown at the bottom of each panel.
Paper: GATOS. VIII. On the Physical Origin of the Extended Mid-infrared Emission in Active Galactic Nuclei
Authors: Enrique Lopez-Rodriguez, Cristina Ramos Almeida, Miguel Pereira-Santaella, Ismael García-Bernete, Robert Nikutta, Almudena Alonso-Herrero, Anelise Audibert, Enrica Bellocchi, Andrew Bunker, Steph Campbell, Françoise Combes, Richard Davies, Tanio Diaz-Santos, Lindsay Fuller, Poshak Gandhi, Santiago García-Burillo, Omaira González-Martín, Erin K. S. Hicks, Sebastian Hönig, Kohei Ichikawa, Masatoshi Imanishi, Takuma Izumi, Alvaro Labiano, Nancy A. Levenson, Christopher Packham, David Rosario, Dimitra Rigopoulou, Daniel Rouan, Taro Shimizu, Marko Stalevski, Martin Ward, Lulu Zhang, Claudio Ricci, Donaji Esparza-Arredondo, Begoña García-Lorenzo
Figure caption: Line emission vs. continuum image emission in the F2100W filter. From left to right and top to bottom, we show the integrated line emission images (color scale) of [Fe II], [S III], and [Ne V] for ESO137-G034, MCG-05-23-016, NGC 3081, NGC 5506, NGC 5728, and NGC 7172. Line (white) and total (black) contours increase in steps of [1, 5, 10, 30, 50, 70]% from the peak flux. The contour at a 10% level (thick line) from the peak flux is shown for reference. The radio jet (black line) and dust lane (blue line) are shown. The integrated flux of the line emission within the 1 kpc FOV is shown at the bottom of each panel.
Paper: GATOS. VIII. On the Physical Origin of the Extended Mid-infrared Emission in Active Galactic Nuclei
Authors: Enrique Lopez-Rodriguez, Cristina Ramos Almeida, Miguel Pereira-Santaella, Ismael García-Bernete, Robert Nikutta, Almudena Alonso-Herrero, Anelise Audibert, Enrica Bellocchi, Andrew Bunker, Steph Campbell, Françoise Combes, Richard Davies, Tanio Diaz-Santos, Lindsay Fuller, Poshak Gandhi, Santiago García-Burillo, Omaira González-Martín, Erin K. S. Hicks, Sebastian Hönig, Kohei Ichikawa, Masatoshi Imanishi, Takuma Izumi, Alvaro Labiano, Nancy A. Levenson, Christopher Packham, David Rosario, Dimitra Rigopoulou, Daniel Rouan, Taro Shimizu, Marko Stalevski, Martin Ward, Lulu Zhang, Claudio Ricci, Donaji Esparza-Arredondo, Begoña García-Lorenzo
Figure caption: Column density as a function of the Eddington ratio as a proxy of the AGN radiation pressure vs. gravity balance to generate dusty winds. The CO nuclear column density (left) and X-ray nuclear column density (right), the Eddington ratios, and the outflow mass ratio (color scale) are shown in Table 1. The theoretical limit (Equation (3)) between gravitationally bounded and IR radiation pressure bounded (dashed line) is taken from M. Venanzi et al. (2020).
Paper: GATOS. VIII. On the Physical Origin of the Extended Mid-infrared Emission in Active Galactic Nuclei
Authors: Enrique Lopez-Rodriguez, Cristina Ramos Almeida, Miguel Pereira-Santaella, Ismael García-Bernete, Robert Nikutta, Almudena Alonso-Herrero, Anelise Audibert, Enrica Bellocchi, Andrew Bunker, Steph Campbell, Françoise Combes, Richard Davies, Tanio Diaz-Santos, Lindsay Fuller, Poshak Gandhi, Santiago García-Burillo, Omaira González-Martín, Erin K. S. Hicks, Sebastian Hönig, Kohei Ichikawa, Masatoshi Imanishi, Takuma Izumi, Alvaro Labiano, Nancy A. Levenson, Christopher Packham, David Rosario, Dimitra Rigopoulou, Daniel Rouan, Taro Shimizu, Marko Stalevski, Martin Ward, Lulu Zhang, Claudio Ricci, Donaji Esparza-Arredondo, Begoña García-Lorenzo
Figure caption: Normalized correlation coefficients between line, total MIR emission, and continuum images for each object and emission line. The normalized correlation coefficients, ρ, between the line and dust-only (solid line), and line and continuum (dashed line) emission in the F1000W (top), F1500W (middle), and F2100W (bottom) filters for each galaxy as shown in the title. The ranges for strong, moderate, and uncorrelated coefficients are displayed.
Paper: GATOS. VIII. On the Physical Origin of the Extended Mid-infrared Emission in Active Galactic Nuclei
Authors: Enrique Lopez-Rodriguez, Cristina Ramos Almeida, Miguel Pereira-Santaella, Ismael García-Bernete, Robert Nikutta, Almudena Alonso-Herrero, Anelise Audibert, Enrica Bellocchi, Andrew Bunker, Steph Campbell, Françoise Combes, Richard Davies, Tanio Diaz-Santos, Lindsay Fuller, Poshak Gandhi, Santiago García-Burillo, Omaira González-Martín, Erin K. S. Hicks, Sebastian Hönig, Kohei Ichikawa, Masatoshi Imanishi, Takuma Izumi, Alvaro Labiano, Nancy A. Levenson, Christopher Packham, David Rosario, Dimitra Rigopoulou, Daniel Rouan, Taro Shimizu, Marko Stalevski, Martin Ward, Lulu Zhang, Claudio Ricci, Donaji Esparza-Arredondo, Begoña García-Lorenzo
Figure caption: Line emission vs. continuum image emission in the F1500W filter. From left to right and top to bottom, we show the integrated line emission images (color scale) of [Ne II], [Ar V], [Ne V], [Ne III], and H20-0S(1), for ESO137-G034, MCG-05-23-016, NGC 3081, NGC 5506, NGC 5728, and NGC 7172. Line (white) and total MIR emission (black) contours increase in steps of [1, 5, 10, 30, 50, 70]% from the peak flux. The contour at a 10% level (thick line) from the peak flux is shown for reference. The radio jet (black line) and dust lane (blue line) are shown. The integrated flux of the line emission within the 1 kpc FOV is shown at the bottom of each panel.
Paper: GATOS. VIII. On the Physical Origin of the Extended Mid-infrared Emission in Active Galactic Nuclei
Authors: Enrique Lopez-Rodriguez, Cristina Ramos Almeida, Miguel Pereira-Santaella, Ismael García-Bernete, Robert Nikutta, Almudena Alonso-Herrero, Anelise Audibert, Enrica Bellocchi, Andrew Bunker, Steph Campbell, Françoise Combes, Richard Davies, Tanio Diaz-Santos, Lindsay Fuller, Poshak Gandhi, Santiago García-Burillo, Omaira González-Martín, Erin K. S. Hicks, Sebastian Hönig, Kohei Ichikawa, Masatoshi Imanishi, Takuma Izumi, Alvaro Labiano, Nancy A. Levenson, Christopher Packham, David Rosario, Dimitra Rigopoulou, Daniel Rouan, Taro Shimizu, Marko Stalevski, Martin Ward, Lulu Zhang, Claudio Ricci, Donaji Esparza-Arredondo, Begoña García-Lorenzo
Figure caption: Line emission vs. total MIR emission image in the F1500W filter. From left to right and top to bottom, we show the integrated line emission images (color scale) of [Ne II], [Ar V], [Ne V], [Ne III], and H20-0S(1), for ESO137-G034, MCG-05-23-016, NGC 3081, NGC 5506, NGC 5728, and NGC 7172. Line (white) and total MIR emission (black) contours increase in steps of [1, 5, 10, 30, 50, 70]% from the peak flux. The contour at a 10% level (thick line) from the peak flux is shown for reference. The radio jet (black line) and dust lane (blue line) are shown. The integrated flux of the line emission within the 1 kpc FOV is shown at the bottom of each panel.
Paper: GATOS. VIII. On the Physical Origin of the Extended Mid-infrared Emission in Active Galactic Nuclei
Authors: Enrique Lopez-Rodriguez, Cristina Ramos Almeida, Miguel Pereira-Santaella, Ismael García-Bernete, Robert Nikutta, Almudena Alonso-Herrero, Anelise Audibert, Enrica Bellocchi, Andrew Bunker, Steph Campbell, Françoise Combes, Richard Davies, Tanio Diaz-Santos, Lindsay Fuller, Poshak Gandhi, Santiago García-Burillo, Omaira González-Martín, Erin K. S. Hicks, Sebastian Hönig, Kohei Ichikawa, Masatoshi Imanishi, Takuma Izumi, Alvaro Labiano, Nancy A. Levenson, Christopher Packham, David Rosario, Dimitra Rigopoulou, Daniel Rouan, Taro Shimizu, Marko Stalevski, Martin Ward, Lulu Zhang, Claudio Ricci, Donaji Esparza-Arredondo, Begoña García-Lorenzo
Figure caption: Line emission vs. continuum emission image in the F1000W filter. From left to right and top to bottom, we show the integrated line emission images (color scale) of [Ar III], [Fe VII], H20-0S(3), and [S IV] for ESO137-G034, MCG-05-23-016, NGC 3081, NGC 5506, NGC 5728, and NGC 7172. Line (white) and continuum (black) contours increase in steps of [1, 5, 10, 30, 50, 70]% from the peak flux. The contour at a 10% level (thick line) from the peak flux is shown for reference. The radio jet (black line) and dust lane (blue line) are shown. The integrated flux of the line emission within the 1 kpc FOV is shown at the bottom of each panel.
Paper: GATOS. VIII. On the Physical Origin of the Extended Mid-infrared Emission in Active Galactic Nuclei
Authors: Enrique Lopez-Rodriguez, Cristina Ramos Almeida, Miguel Pereira-Santaella, Ismael García-Bernete, Robert Nikutta, Almudena Alonso-Herrero, Anelise Audibert, Enrica Bellocchi, Andrew Bunker, Steph Campbell, Françoise Combes, Richard Davies, Tanio Diaz-Santos, Lindsay Fuller, Poshak Gandhi, Santiago García-Burillo, Omaira González-Martín, Erin K. S. Hicks, Sebastian Hönig, Kohei Ichikawa, Masatoshi Imanishi, Takuma Izumi, Alvaro Labiano, Nancy A. Levenson, Christopher Packham, David Rosario, Dimitra Rigopoulou, Daniel Rouan, Taro Shimizu, Marko Stalevski, Martin Ward, Lulu Zhang, Claudio Ricci, Donaji Esparza-Arredondo, Begoña García-Lorenzo
Figure caption: Line emission vs. total MIR emission image in the F2100W filter. From left to right and top to bottom, we show the integrated line emission images (color scale) of [Fe II], [S III], and [Ne V] for ESO137-G034, MCG-05-23-016, NGC 3081, NGC 5506, NGC 5728, and NGC 7172. Line (white) and total MIR emission (black) contours increase in steps of [1, 5, 10, 30, 50, 70]% from the peak flux. The contour at a 10% level (thick line) from the peak flux is shown for reference. The radio jet (black line) and dust lane (blue line) are shown. The integrated flux of the line emission within the 1 kpc FOV is shown at the bottom of each panel.
Paper: AI-powered Reconstruction of Dark Matter Velocity Fields from Redshift-space Halo Distribution
Authors: Xu Xiao, Jiacheng Ding, Xiaolin Luo, Sun Ke Lan, Liang Xiao, Shuai Liu, Xin Wang, Le Zhang, Xiao-Dong Li
Figure caption: UNet neural network architecture employed for the reconstruction of the DM density and velocity/momentum fields. A 1283 box with a side length of 300 Mpc h−1 is employed in the UNet architecture as the input. This architecture is comprised of a three-block structure: an up-convolution block, a down-convolution block, and a final convolution block. The output fields have dimensions of 1283, with a volume of ﹩30{0}^{3}\,{(\mathrm{Mpc}\,{h}^{-1})}^{3}﹩. The left panel provides detailed information on the components included in the three blocks of UNet, while the right panel offers detailed descriptions of the “init,” “conv,” “trans,” and “output” layers. In the final convolution block, a dropout layer is employed between the convolutional transformation and BN layers to enhance the performance of UNet and prevent overfitting. The values of N1, N2, N3, and the dropout percentage are automatically provided by a machine learning tool called Optuna (T. Akiba et al. 2019).
Paper: AI-powered Reconstruction of Dark Matter Velocity Fields from Redshift-space Halo Distribution
Authors: Xu Xiao, Jiacheng Ding, Xiaolin Luo, Sun Ke Lan, Liang Xiao, Shuai Liu, Xin Wang, Le Zhang, Xiao-Dong Li
Figure caption: Joint probability distributions of the reconstructed fields and the true fields for velocity magnitude (∣v∣) and momentum magnitude (∣m∣), using the weighting schemes of “with Mhalo weighting” and “without Mhalo weighting” for comparison. For each field, the distributions were calculated using a large box with a side length of 600 Mpc h−1. The predicted distributions are strongly correlated with the true ones, indicating that the model is capable of effective reconstruction. A linear regression fit of the form y = ax + b, where y and x denote the true and reconstructed values, respectively, is also performed for comparison. The coefficients a and b are presented in each plot.