adsabs/AstroCLIMB huggingface dataset:
Paper: Asteroseismic Calibration of the Rossby Number and Its Connection to the Stellar Dynamo and Fundamental Properties
Authors: Alfio M. Bonanno, Enrico Corsaro, Travis S. Metcalfe, Sylvain N. Breton, Orlagh L. Creevey, Christopher J. Lindsay
Figure caption: Convective velocities vconv and convective turnover time τc as a function of Gaia DR3 color index ﹩{\left({G}_{{\rm{BP}}}-{G}_{{\rm{RP}}}\right)}_{0}﹩, surface gravity ﹩\mathrm{log}g﹩, metallicity ﹩\left[{\rm{Fe}}/{\rm{H}}\right]﹩, and temperature Teff for both samples (main sequence and early subgiants from LEGACY + KOI in blue, late subgiants and early RGB from C. J. Lindsay et al. 2024 in orange). Spearman’s rank correlation coefficients are also indicated for each sample using the same color-coding. The dashed vertical line represents the cut in ﹩\mathrm{log}g﹩ applied to distinguish ﹩{{ \mathcal S }}_{1}﹩ from ﹩{{ \mathcal S }}_{2}﹩, as described in Section 5.
Paper: Asteroseismic Calibration of the Rossby Number and Its Connection to the Stellar Dynamo and Fundamental Properties
Authors: Alfio M. Bonanno, Enrico Corsaro, Travis S. Metcalfe, Sylvain N. Breton, Orlagh L. Creevey, Christopher J. Lindsay
Figure caption: Dispersion plots showing the τc predictions from model ﹩{{ \mathcal M }}_{1}﹩. The data points are shown in color (open symbols), while the model predictions are represented by gray (filled) bullets. A panel showing the residuals of the fit in the form ﹩\mathrm{ln}{\tau }_{c}-\mathrm{ln}{\tau }_{c}^{{\rm{predict}}}﹩ is also shown for each observable. Also indicated are a polynomial fit with its 1σ confidence region (dotted line with light blue shading), the average value of the residuals (dotted–dashed red line), and the indices ﹩{\sigma }_{{\rm{res}}}﹩, sdev, Davg, and Iabs.
Paper: Discovery of 79 δ Scuti Stars in NGC 3532 Suggests a Decrease of Pulsator Occurrence with Age
Authors: Ian Berry, Daniel Huber, Yaguang Li, Daniel Hey, Timothy R. Bedding, Simon J. Murphy
Figure caption: Top: amplitude spectrum for TIC 304561736 with the 10 highest pulsation modes used for Δν measurement marked with red points. Bottom left: the autocorrelation function (ACF, red), fast fourier transform (FFT, blue) and histogram of frequency differences (HFD, black). The gray dotted line shows the measured Δν = 6.8 day−1. Bottom right: échelle diagram using the found Δν. The blue circles show the locations of the 10 marked modes in the amplitude spectrum.
Paper: Asteroseismic Calibration of the Rossby Number and Its Connection to the Stellar Dynamo and Fundamental Properties
Authors: Alfio M. Bonanno, Enrico Corsaro, Travis S. Metcalfe, Sylvain N. Breton, Orlagh L. Creevey, Christopher J. Lindsay
Figure caption: Similar description as for Figure 2 but for model ﹩{{ \mathcal M }}_{5}﹩.
Paper: Asteroseismic Calibration of the Rossby Number and Its Connection to the Stellar Dynamo and Fundamental Properties
Authors: Alfio M. Bonanno, Enrico Corsaro, Travis S. Metcalfe, Sylvain N. Breton, Orlagh L. Creevey, Christopher J. Lindsay
Figure caption: Similar description as for Figure 2 but for model ﹩{{ \mathcal M }}_{6}﹩.
Paper: Asteroseismic Calibration of the Rossby Number and Its Connection to the Stellar Dynamo and Fundamental Properties
Authors: Alfio M. Bonanno, Enrico Corsaro, Travis S. Metcalfe, Sylvain N. Breton, Orlagh L. Creevey, Christopher J. Lindsay
Figure caption: Similar description as for Figure 2 but for model ﹩{{ \mathcal M }}_{4}﹩.
Paper: Asteroseismic Calibration of the Rossby Number and Its Connection to the Stellar Dynamo and Fundamental Properties
Authors: Alfio M. Bonanno, Enrico Corsaro, Travis S. Metcalfe, Sylvain N. Breton, Orlagh L. Creevey, Christopher J. Lindsay
Figure caption: Similar description as for Figure 2 but for model ﹩{{ \mathcal M }}_{2}﹩.
Paper: Asteroseismic Calibration of the Rossby Number and Its Connection to the Stellar Dynamo and Fundamental Properties
Authors: Alfio M. Bonanno, Enrico Corsaro, Travis S. Metcalfe, Sylvain N. Breton, Orlagh L. Creevey, Christopher J. Lindsay
Figure caption: Similar description as for Figure 2 but for model ﹩{{ \mathcal M }}_{3}﹩.
Paper: Hyperaccretion-driven Relativistic Jets from Massive Collapsars in Active Galactic Nucleus Disks
Authors: Yun-Feng Wei, Tong Liu, Bao-Quan Huang
Figure caption: Time evolution of the mass accretion rate onto the newborn BH. The black, red, and blue curves correspond to the cases of progenitors with metallicities of Z/Z⊙ = 0, 0.01, and 1, respectively. For each color, the dotted lines represent the jet propagation inside the star, the solid lines indicate the jet propagation inside the AGN disk, and the dashed lines indicate the phase after the jet breaks out from the AGN disk. The dashed lines give the information of the duration and energetics of AGN GRBs. The left, middle, and right panels correspond to progenitor masses of Mpro/M⊙ = 20, 30, and 40, respectively, with an SMBH mass of 106M⊙. In top panels and bottom panels, the radial locations from the SMBH are 104Rg and 105Rg, respectively.
Paper: Hyperaccretion-driven Relativistic Jets from Massive Collapsars in Active Galactic Nucleus Disks
Authors: Yun-Feng Wei, Tong Liu, Bao-Quan Huang
Figure caption: Light curves of the prompt emission of AGN GRBs with different progenitors. The flux is calculated at the Swift BAT energy range (15−150 keV). The black, red, and blue curves correspond to the cases of progenitors with metallicity of Z/Z⊙ = 0, 0.01, and 1, respectively. The solid, dashed, and dotted lines represent the progenitor masses of Mpro/M⊙ = 20, 30, and 40, respectively. The gray dotted lines indicates the BAT sensitivities fsen(Δtobs) with the integration times of Δtobs = 104 s. The SMBH mass is 106M⊙. In panels (a) and (b), the radial locations from the SMBH are 104Rg and 105Rg, respectively.
Paper: Asteroseismic Calibration of the Rossby Number and Its Connection to the Stellar Dynamo and Fundamental Properties
Authors: Alfio M. Bonanno, Enrico Corsaro, Travis S. Metcalfe, Sylvain N. Breton, Orlagh L. Creevey, Christopher J. Lindsay
Figure caption: Dynamo model obtained for the Sun (left) and Iota Horologii (right). In each case, the top panel shows the magnetic diffusivity profile η (blue), the α-effect profile (orange), and the convective velocity (yellow). The black dots highlight where the τc profile intersects the convective turnover time computed using the prescription from E. Corsaro et al. (2021). The bottom panels show the evolution of the mean toroidal field obtained for each model, at r = 0.78 R⊙ and r = 0.8 R⋆, respectively. The magnetic field in the regions in red has an opposite sign with respect to the regions in blue.
Paper: Hyperaccretion-driven Relativistic Jets from Massive Collapsars in Active Galactic Nucleus Disks
Authors: Yun-Feng Wei, Tong Liu, Bao-Quan Huang
Figure caption: Same as Figure 2 but for an SMBH mass of 108M⊙. The radial location from the SMBH is 103Rg.
Paper: Hyperaccretion-driven Relativistic Jets from Massive Collapsars in Active Galactic Nucleus Disks
Authors: Yun-Feng Wei, Tong Liu, Bao-Quan Huang
Figure caption: Density profiles of the progenitor stars investigated, with different masses and metallicities. The black, red, and blue curves correspond to progenitor metallicities of Z/Z⊙ = 0, 0.01, and 1, respectively. The solid, dashed, and dotted lines represent the progenitor masses of Mpro/M⊙ = 20, 30, and 40, respectively.
Paper: Hyperaccretion-driven Relativistic Jets from Massive Collapsars in Active Galactic Nucleus Disks
Authors: Yun-Feng Wei, Tong Liu, Bao-Quan Huang
Figure caption: Same as Figure 2 but for an SMBH mass of 107M⊙. The top and bottom panels correspond to radial locations of 103Rg and 104Rg from the SMBH, respectively.
Paper: Asteroseismic Calibration of the Rossby Number and Its Connection to the Stellar Dynamo and Fundamental Properties
Authors: Alfio M. Bonanno, Enrico Corsaro, Travis S. Metcalfe, Sylvain N. Breton, Orlagh L. Creevey, Christopher J. Lindsay
Figure caption: Similar description as for Figure 2 but for model ﹩{{ \mathcal M }}_{8}﹩.
Paper: Asteroseismic Calibration of the Rossby Number and Its Connection to the Stellar Dynamo and Fundamental Properties
Authors: Alfio M. Bonanno, Enrico Corsaro, Travis S. Metcalfe, Sylvain N. Breton, Orlagh L. Creevey, Christopher J. Lindsay
Figure caption: Similar description as for Figure 2 but for model ﹩{{ \mathcal M }}_{7}﹩.
Paper: ODIN: Probing the LAE Lyα Luminosity Function across Cosmic Time and Different Environments
Authors: Gautam Nagaraj, Robin Ciardullo, Caryl Gronwall, Vandana Ramakrishnan, Kyoung-Soo Lee, Eric Gawiser, Nicole Firestone, Govind Ramgopal, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, Arjun Dey, Biprateep Dey, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, H. K. Herrera-Alcantar, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. E. Levi, C. Magneville, M. Manera, P. Martini, A. Meisner, R. Miquel, J. Moustakas, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, G. Rossi, L. Samushia, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, D. Sprayberry, G. Tarlé, F. Valdes, B. A. Weaver, M. White, R. Zhou, H. Zou
Figure caption: Parametric and nonparametric fits to the z ∼ 2.4 (N419) Lyα emission-line luminosity function of ODIN LAEs in the extended COSMOS field. The “triangle plot” that takes up most of the figure shows the 1D and 2D cross sections of the parameter space explored by the MCMC chains used to fit the Schechter parameters. The high degree of correlation is expected given the interdependence of the L*, ϕ*, and α. The red curves in the top-right panel show the range (up to ∼3σ away from the median) of luminosity functions given various MCMC solutions. Their small spread demonstrates the stability of the fit, though the errors may be underestimated due to the assumption that the completeness and contamination fractions are error-free. The cyan squares show the raw Veff results, while the blue triangles include a correction for the shape of the filter transmission curve. We expect the MCMC result to be more accurate, as it is based on a more rigorous mathematical formulation and is less subject to errors in the characterization of faint-end completeness. While the Veff luminosity function does display some bin-to-bin variations (due principally to shot noise), the agreement between the two methods (blue points vs. the red curves) is excellent.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: ODIN: Probing the LAE Lyα Luminosity Function across Cosmic Time and Different Environments
Authors: Gautam Nagaraj, Robin Ciardullo, Caryl Gronwall, Vandana Ramakrishnan, Kyoung-Soo Lee, Eric Gawiser, Nicole Firestone, Govind Ramgopal, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, Arjun Dey, Biprateep Dey, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, H. K. Herrera-Alcantar, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. E. Levi, C. Magneville, M. Manera, P. Martini, A. Meisner, R. Miquel, J. Moustakas, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, G. Rossi, L. Samushia, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, D. Sprayberry, G. Tarlé, F. Valdes, B. A. Weaver, M. White, R. Zhou, H. Zou
Figure caption: Fraction of ODIN sources that are spectroscopically confirmed LAEs as a function of narrowband magnitude in the N419 (left), N501 (middle), and N673 (right). The error bars represent Poisson uncertainties. (These error bars are generally not incorporated into the analysis due to computational and algorithmic constraints.) The N673 data suffers from a relative dearth of confirming spectroscopy, limiting our ability to measure the function. Integrated over all magnitudes, the confirmed fraction of LAEs is over 90% in all three filters. However, at magnitudes brighter than mAB ∼ 24, the purity fraction declines rapidly, and is near zero at mAB ∼ 22 in N419 and N501. The ratio of confirmed LAEs to total ODIN-DESI spectra per bin is displayed above or below each point. We multiply the reciprocal of this function by our photometric completeness curves to determine the effective completeness at each location in the survey.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: ODIN: Probing the LAE Lyα Luminosity Function across Cosmic Time and Different Environments
Authors: Gautam Nagaraj, Robin Ciardullo, Caryl Gronwall, Vandana Ramakrishnan, Kyoung-Soo Lee, Eric Gawiser, Nicole Firestone, Govind Ramgopal, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, Arjun Dey, Biprateep Dey, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, H. K. Herrera-Alcantar, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. E. Levi, C. Magneville, M. Manera, P. Martini, A. Meisner, R. Miquel, J. Moustakas, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, G. Rossi, L. Samushia, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, D. Sprayberry, G. Tarlé, F. Valdes, B. A. Weaver, M. White, R. Zhou, H. Zou
Figure caption: The properties of the N501 filter curve used by ODIN. The N419 and N673 filter behave in a similar fashion. Left panel: the transmission curve of the filter. Middle panel: the filter’s effective redshift width as a function of emission-line luminosity. The value of ﹩{{\rm{L}}}_{{\rm{\min }}}﹩ is taken as roughly the 50% completeness level, since that is the minimum completeness fraction used in our calculations. Bright objects can be detected even if their redshift places them on the filter’s wings. Right panel: the convolution kernel ﹩G({\rm{\Delta }}{ \mathcal L })﹩ used to convert the true luminosity function into the observed function.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: ODIN: Probing the LAE Lyα Luminosity Function across Cosmic Time and Different Environments
Authors: Gautam Nagaraj, Robin Ciardullo, Caryl Gronwall, Vandana Ramakrishnan, Kyoung-Soo Lee, Eric Gawiser, Nicole Firestone, Govind Ramgopal, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, Arjun Dey, Biprateep Dey, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, H. K. Herrera-Alcantar, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. E. Levi, C. Magneville, M. Manera, P. Martini, A. Meisner, R. Miquel, J. Moustakas, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, G. Rossi, L. Samushia, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, D. Sprayberry, G. Tarlé, F. Valdes, B. A. Weaver, M. White, R. Zhou, H. Zou
Figure caption: Effective completeness as a function of luminosity (x-axis) and distance from the center of the Extended COSMOS field (line color) for N419 (left), N501 (middle), and N673 (right). As described in the text, these curves are the product of photometric completeness, as determined through simulations, and “overcompleteness” caused by the inclusion of active galactic nuclei (AGNs) and other foreground interlopers.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: ODIN: Probing the LAE Lyα Luminosity Function across Cosmic Time and Different Environments
Authors: Gautam Nagaraj, Robin Ciardullo, Caryl Gronwall, Vandana Ramakrishnan, Kyoung-Soo Lee, Eric Gawiser, Nicole Firestone, Govind Ramgopal, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, Arjun Dey, Biprateep Dey, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, H. K. Herrera-Alcantar, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. E. Levi, C. Magneville, M. Manera, P. Martini, A. Meisner, R. Miquel, J. Moustakas, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, G. Rossi, L. Samushia, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, D. Sprayberry, G. Tarlé, F. Valdes, B. A. Weaver, M. White, R. Zhou, H. Zou
Figure caption: The log correction factor as a function of luminosity for our N501 measurements. The curve is derived via the Monte Carlo experiments described in the text, and is used to determine the effect that the filter’s transmission curve has on the Veff method. The curve shows the weighted average of our individual experiments. The 1σ uncertainties on the correction are shown in light blue. The corrections increase monotonically from ﹩{\mathrm{log}}\,L({\rm{Ly}}\alpha )\approx 42.0﹩ to ﹩{\mathrm{log}}\,L({\rm{Ly}}\alpha )\approx 43.5﹩. Since our N501 data only goes down to ﹩{\mathrm{log}}\,L({\rm{Ly}}\alpha )\gtrsim 42.3﹩, only the corrections above this limit are used.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: ODIN: Probing the LAE Lyα Luminosity Function across Cosmic Time and Different Environments
Authors: Gautam Nagaraj, Robin Ciardullo, Caryl Gronwall, Vandana Ramakrishnan, Kyoung-Soo Lee, Eric Gawiser, Nicole Firestone, Govind Ramgopal, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, Arjun Dey, Biprateep Dey, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, H. K. Herrera-Alcantar, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. E. Levi, C. Magneville, M. Manera, P. Martini, A. Meisner, R. Miquel, J. Moustakas, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, G. Rossi, L. Samushia, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, D. Sprayberry, G. Tarlé, F. Valdes, B. A. Weaver, M. White, R. Zhou, H. Zou
Figure caption: Completeness as a function of N501 magnitude and radial distance from the center of the extended COSMOS field. Within the region’s inner ﹩1\mathop{.}\limits^{^\circ }5﹩ core, the variations in survey depth are small. However, at the extreme edge of the field, the depth is ∼0.5 mag shallower than in the center.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: ODIN: Probing the LAE Lyα Luminosity Function across Cosmic Time and Different Environments
Authors: Gautam Nagaraj, Robin Ciardullo, Caryl Gronwall, Vandana Ramakrishnan, Kyoung-Soo Lee, Eric Gawiser, Nicole Firestone, Govind Ramgopal, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, Arjun Dey, Biprateep Dey, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, H. K. Herrera-Alcantar, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. E. Levi, C. Magneville, M. Manera, P. Martini, A. Meisner, R. Miquel, J. Moustakas, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, G. Rossi, L. Samushia, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, D. Sprayberry, G. Tarlé, F. Valdes, B. A. Weaver, M. White, R. Zhou, H. Zou
Figure caption: Raw emission-line flux distributions in each of the three narrowband filters. The sample of galaxies used in the luminosity function calculations are shown in blue. Galaxies with fluxes below a certain value—approximately the 50% completeness level—are colored light gray, while very bright objects that are likely foreground contaminants are colored gold. The useful data cover ∼1.1 dex in flux.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: ODIN: Probing the LAE Lyα Luminosity Function across Cosmic Time and Different Environments
Authors: Gautam Nagaraj, Robin Ciardullo, Caryl Gronwall, Vandana Ramakrishnan, Kyoung-Soo Lee, Eric Gawiser, Nicole Firestone, Govind Ramgopal, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, Arjun Dey, Biprateep Dey, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, H. K. Herrera-Alcantar, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. E. Levi, C. Magneville, M. Manera, P. Martini, A. Meisner, R. Miquel, J. Moustakas, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, G. Rossi, L. Samushia, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, D. Sprayberry, G. Tarlé, F. Valdes, B. A. Weaver, M. White, R. Zhou, H. Zou
Figure caption: Total narrowband flux recorded in the N501 filter vs. Lyα flux for ODIN LAEs in the Extended COSMOS field. The orthogonal-regression best-fit line is shown in red; this line is consistent with that expected from the LAE’s equivalent width distribution and the filter’s FWHM. We use this relation to translate between narrowband flux and line flux when computing integrals for the luminosity function. For reference, we also provide the one-to-one relation as a black dotted line.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: ODIN: Probing the LAE Lyα Luminosity Function across Cosmic Time and Different Environments
Authors: Gautam Nagaraj, Robin Ciardullo, Caryl Gronwall, Vandana Ramakrishnan, Kyoung-Soo Lee, Eric Gawiser, Nicole Firestone, Govind Ramgopal, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, Arjun Dey, Biprateep Dey, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, H. K. Herrera-Alcantar, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. E. Levi, C. Magneville, M. Manera, P. Martini, A. Meisner, R. Miquel, J. Moustakas, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, G. Rossi, L. Samushia, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, D. Sprayberry, G. Tarlé, F. Valdes, B. A. Weaver, M. White, R. Zhou, H. Zou
Figure caption: Parametric and nonparametric fits to the z ∼ 3.1 (N501) Lyα emission-line luminosity function of LAEs. The panels are the same as in Figure 8. Once again, we find excellent agreement between the two methods.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Spectropolarimetric Inversion in Four Dimensions with Deep Learning (SPIn4D). II. A Physics-informed Machine Learning Method for 3D Solar Photosphere Reconstruction
Authors: Kai E. Yang, 凯 杨, Xudong Sun, 旭东 孙, Lucas A. Tarr, Jiayi Liu, 嘉奕 刘, Peter Sadowski, S. Curt Dodds, Matthias Rempel, Sarah A. Jaeggli, Thomas A. Schad, Ian Cunnyngham, Yannik Glaser, Linnea Wolniewicz
Figure caption: Columns from left to right show the x-, y-, z-components, and the absolute value of the electric current in the plage case. Panels (a)–(d) and (e)–(h) display the top view of the electric current on the ﹩{\mathrm{log}}_{10}\tau =-1﹩ layer of the ground truth and HDD result, respectively. Panels (i)–(l) and (m)–(p) present the electric current distribution on the true and predicted vertical cuts at Y = 12.3 Mm, indicated by the white-dashed line in panel (d).