adsabs/AstroCLIMB huggingface dataset:
Paper: IRIS2+: A Comprehensive Database of Stratified Thermodynamic Models in the Low Solar Atmosphere
Authors: Alberto Sainz Dalda, Aaryan Agrawal, Bart De Pontieu, Milan Gošić
Figure caption: First row: Spectroheliogram map for Mg II h and k k 3, Ti I 2785.46 Å, the photospheric continuum at 2832.04 Å, and a map of the various types of features that were identified: umbra (light blue), penumbra (green), plage (orange), and quiet Sun (brown). The other rows are the results of an inversion for the location marked with a white cross on the map “Selected areas” to the right of the top row. From the second to the sixth row, from left to right, the observed (solid dotted in fuchsia) and the inverted profile (black) are shown. The value in parentheses is the average height (in megameters) at optical depth equal to 1. The gray shaded areas around the inverted lines show the spectral ranges considered for the calculation of the uncertainties. The bottom row shows the temperature (T, orange), the logarithm of the electron density (n e, blue), velocity of turbulent motions or microturbulent (v turb, green), and the line of sight (v los, violet). The colored shaded area in these panels represents the uncertainty of each variable as described in the text (see Equation (2)).
Paper: IRIS2+: A Comprehensive Database of Stratified Thermodynamic Models in the Low Solar Atmosphere
Authors: Alberto Sainz Dalda, Aaryan Agrawal, Bart De Pontieu, Milan Gošić
Figure caption: Top: Average profile of the quiet Sun at the disk center showing the spectrum around the Mg II h and k lines observed by IRIS in its near-ultraviolet camera. The core of the photospheric and chromospheric lines selected in this investigation are marked by dashed lines. The photospheric lines are labeled in orange, while the chromospheric are in violet. The values in parentheses indicate the approximate height (in megameters) above the optical depth at 500 nm equal to 1 sampled by the velocity line shifts, and the uncertainty associated with the fact that the formation occurs in a corrugated layer, as obtained by Pereira et al. (2013). Bottom: The spectrum as seen on the detector is shown for a better comparison with the IRIS linelist files, e.g., v36_01, which show all the spectral ranges selected for a given observation. It should be noted that the wavelength increases toward the left in this panel.
Paper: IRIS2+: A Comprehensive Database of Stratified Thermodynamic Models in the Low Solar Atmosphere
Authors: Alberto Sainz Dalda, Aaryan Agrawal, Bart De Pontieu, Milan Gošić
Figure caption: Left: Response function (RF) of the intensity to perturbations in T of the selected lines in an RP of the IRIS2+ database. The intensity profiles (white) are shown as a reference. The meanings of the values in parentheses are given in the caption of Figure 2. Right: Optical depth ranges where these lines are on average sensitive to a perturbation in T for the solar features included in the IRIS2+ database. These ranges may slightly vary for each solar feature and for the other physical parameters in the database.
Paper: IRIS2+: A Comprehensive Database of Stratified Thermodynamic Models in the Low Solar Atmosphere
Authors: Alberto Sainz Dalda, Aaryan Agrawal, Bart De Pontieu, Milan Gošić
Figure caption: Distribution of the selected data in the IRIS2+ database with respect the observation date (left), ﹩\mu =\cos (\theta )﹩—with θ being the heliocentric angle (middle), and the exposure time (right).
Paper: Stellar Loci. VII. Photometric Metallicities of 5 Million FGK Stars Based on GALEX GR6+7 AIS and Gaia EDR3
Authors: Xue Lu, Haibo Yuan, Shuai Xu, Ruoyi Zhang, Kai Xiao, Yang Huang, Timothy C. Beers, Jihye Hong
Figure caption: H-R diagram of the training samples, color coded by [Fe/H]. The dwarfs and giants are separated by the black-dashed line (Xu et al. 2022a): M  G  = −(BP − RP)2 + 6.5 × (BP − RP) −1.8.
Paper: Stellar Loci. VII. Photometric Metallicities of 5 Million FGK Stars Based on GALEX GR6+7 AIS and Gaia EDR3
Authors: Xue Lu, Haibo Yuan, Shuai Xu, Ruoyi Zhang, Kai Xiao, Yang Huang, Timothy C. Beers, Jihye Hong
Figure caption: Distributions of the dwarf (top panel) and giant (bottom panel) training samples after cutting in the [Fe/H] vs. (BP − RP)0 plane, color coded by M  G .
Paper: Stellar Loci. VII. Photometric Metallicities of 5 Million FGK Stars Based on GALEX GR6+7 AIS and Gaia EDR3
Authors: Xue Lu, Haibo Yuan, Shuai Xu, Ruoyi Zhang, Kai Xiao, Yang Huang, Timothy C. Beers, Jihye Hong
Figure caption: Photometric metallicities for the dwarf training sample. (a) Histogram distribution of the residuals Δ[Fe/H], with the Gaussian fitting profile overplotted in black. (b) Comparison of photometric metallicity estimates from GALEX and Gaia data with high-resolution spectroscopic metallicities from SAGA or PASTEL. (c)–(g) Δ[Fe/H] as a function of BP − RP color, [Fe/H]H-R, M  G , E(B − V), and NUV, respectively. The red solid lines indicate the median values and standard deviations. The black-dashed line indicates the zero level. (h) The color–magnitude diagram, color coded by Δ[Fe/H].
Paper: Stellar Loci. VII. Photometric Metallicities of 5 Million FGK Stars Based on GALEX GR6+7 AIS and Gaia EDR3
Authors: Xue Lu, Haibo Yuan, Shuai Xu, Ruoyi Zhang, Kai Xiao, Yang Huang, Timothy C. Beers, Jihye Hong
Figure caption: Test results for 633,807 dwarfs. (a) Histogram distribution of the residuals Δ[Fe/H], with the mean and standard deviation values labeled. (b) [Fe/H]GALEX as a function of [Fe/H]LAMOST, color coded by number density. (c)–(g) Δ[Fe/H] as a function of BP − RP color, [Fe/H]LAMOST, M  G , E(B − V), and NUV, respectively. The black solid lines indicate the median values and standard deviations. The black-dashed line indicates the zero level. (h) Distributions of the dwarfs in the (NUV − BP) vs. (BP − RP) plane, color coded by [Fe/H] values from LAMOST, as indicated by the right color bar. The expression for the black-dashed line is (NUV − BP) < −1.56 × (BP − RP)2 + 10.87 × (BP − RP) − 4.78 for dwarfs. The [Fe/H]GALEX values of stars below the black-dashed line are considered unreliable and assigned “flag = 1.”
Paper: Stellar Loci. VII. Photometric Metallicities of 5 Million FGK Stars Based on GALEX GR6+7 AIS and Gaia EDR3
Authors: Xue Lu, Haibo Yuan, Shuai Xu, Ruoyi Zhang, Kai Xiao, Yang Huang, Timothy C. Beers, Jihye Hong
Figure caption: (a) Distributions of the dwarf training sample in the NUV − BP vs. BP − RP plane (stellar loci), color coded by [Fe/H] as shown in the right color bar. (b) When M  G  = 4.5, the variations of stellar loci for different metallicities (as shown in the label) relative to the one at [Fe/H] = −0.5. (c)–(g) Fitting residuals as a function of BP − RP color, [Fe/H], M  G , E(B − V), and NUV, respectively. The red solid lines indicate the median values and standard deviations. The black-dashed line indicates the zero level. (h) Histogram distribution of the fitting residuals, with the Gaussian fitting profile overplotted in black.
Paper: Stellar Loci. VII. Photometric Metallicities of 5 Million FGK Stars Based on GALEX GR6+7 AIS and Gaia EDR3
Authors: Xue Lu, Haibo Yuan, Shuai Xu, Ruoyi Zhang, Kai Xiao, Yang Huang, Timothy C. Beers, Jihye Hong
Figure caption: Same as Figure 7, but for the giant training sample.
Paper: Stellar Loci. VII. Photometric Metallicities of 5 Million FGK Stars Based on GALEX GR6+7 AIS and Gaia EDR3
Authors: Xue Lu, Haibo Yuan, Shuai Xu, Ruoyi Zhang, Kai Xiao, Yang Huang, Timothy C. Beers, Jihye Hong
Figure caption: Same as Figure 9, but for 72,911 giants. The expression for the black-dashed line is (NUV − BP) < −7.20 × (BP − RP)2 + 27.69 × (BP − RP) −16.63.
Paper: Stellar Loci. VII. Photometric Metallicities of 5 Million FGK Stars Based on GALEX GR6+7 AIS and Gaia EDR3
Authors: Xue Lu, Haibo Yuan, Shuai Xu, Ruoyi Zhang, Kai Xiao, Yang Huang, Timothy C. Beers, Jihye Hong
Figure caption: The spatial distribution (R.A. and decl.) of the residuals Δ[Fe/H]. The top row of panels are for the test-with-LAMOST sample of 633,807 dwarfs and 72,911 giants, respectively. The bottom row of panels are the subsample of these stars with ∣Z∣ > 300 pc (441,141 dwarfs and 64,696 giants, respectively.)
Paper: Stellar Loci. VII. Photometric Metallicities of 5 Million FGK Stars Based on GALEX GR6+7 AIS and Gaia EDR3
Authors: Xue Lu, Haibo Yuan, Shuai Xu, Ruoyi Zhang, Kai Xiao, Yang Huang, Timothy C. Beers, Jihye Hong
Figure caption: Same as Figure 5, but for the giant training sample.
Paper: Stellar Loci. VII. Photometric Metallicities of 5 Million FGK Stars Based on GALEX GR6+7 AIS and Gaia EDR3
Authors: Xue Lu, Haibo Yuan, Shuai Xu, Ruoyi Zhang, Kai Xiao, Yang Huang, Timothy C. Beers, Jihye Hong
Figure caption:  R NUV−BP, as a function of BP − RP, for dwarfs (dashed lines) and giants (solid lines) at different extinction values.
Paper: Stellar Loci. VII. Photometric Metallicities of 5 Million FGK Stars Based on GALEX GR6+7 AIS and Gaia EDR3
Authors: Xue Lu, Haibo Yuan, Shuai Xu, Ruoyi Zhang, Kai Xiao, Yang Huang, Timothy C. Beers, Jihye Hong
Figure caption: The differences in BP − RP vs. NUV − BP color loci between dwarfs (blue dots) and giants (red dots).
Paper: Stellar Loci. VII. Photometric Metallicities of 5 Million FGK Stars Based on GALEX GR6+7 AIS and Gaia EDR3
Authors: Xue Lu, Haibo Yuan, Shuai Xu, Ruoyi Zhang, Kai Xiao, Yang Huang, Timothy C. Beers, Jihye Hong
Figure caption: Comparisons of [Fe/H]GALEX with spectroscopic measurements for VMP/EMP stars (taken from the compilation of Hong et al. 2023), color coded by [C/Fe]. From left to right, the panels show the full sample, the subsample of stars with [C/Fe] > +0.7, and the subsample of stars with [C/Fe] ≤ +0.7, respectively. The mean and standard deviation values of the residuals Δ[Fe/H] are labeled in the upper left of each panel. Note that, in all three panels, there are stars with [Fe/H]GALEX that straddle the black solid one-to-one lines; they are not uniformly biased high due to the effect of carbon, as has been seen to occur for several previous photometric metallicity techniques (see the text).
Paper: Stellar Loci. VII. Photometric Metallicities of 5 Million FGK Stars Based on GALEX GR6+7 AIS and Gaia EDR3
Authors: Xue Lu, Haibo Yuan, Shuai Xu, Ruoyi Zhang, Kai Xiao, Yang Huang, Timothy C. Beers, Jihye Hong
Figure caption: From left to right, the columns of panels represent comparisons with the LAMOST DR8 value-added catalog of Wang et al. (2022), the SEGUE DR12 (Alam et al. 2015) catalog, and the VMP catalogs of Li et al. (2018) and Li et al. (2022), respectively. The left column of panels is color coded by the source number density. In the right column of panels, the gray and red dots are from Li et al. (2018) and Li et al. (2022), respectively. The dwarfs are plotted in the top row of panels and the giants in the bottom row of panels. The mean and standard deviation values of the residuals Δ[Fe/H] are labeled in the lower right of each panel.
Paper: Stellar Loci. VII. Photometric Metallicities of 5 Million FGK Stars Based on GALEX GR6+7 AIS and Gaia EDR3
Authors: Xue Lu, Haibo Yuan, Shuai Xu, Ruoyi Zhang, Kai Xiao, Yang Huang, Timothy C. Beers, Jihye Hong
Figure caption: Histograms of [Fe/H]GALEX for the open cluster NGC 2682 (panel (a)) and the globular cluster NGC 104 (panel (b)), NGC 362 (panel (c)), NGC 4590 (panel (d)), with the Gaussian fitting profile overplotted in black, and the mean and standard deviation values labeled. The values [Fe/H]S04 and [Fe/H]H10 are referenced from Salaris et al. (2004) and Harris (2010), respectively, and are indicated with dashed vertical lines. See the text for values of the biweight estimates of location and dispersion.
Paper: Stellar Loci. VII. Photometric Metallicities of 5 Million FGK Stars Based on GALEX GR6+7 AIS and Gaia EDR3
Authors: Xue Lu, Haibo Yuan, Shuai Xu, Ruoyi Zhang, Kai Xiao, Yang Huang, Timothy C. Beers, Jihye Hong
Figure caption: The [Fe/H] distribution of the final sample (with flag = 0). The left and right panels are for the dwarfs and giants, respectively. For dwarfs, there are 14,522 VMP and 2962 EMP stars, respectively. For giants, there are 18,245 VMP and 3582 EMP stars, respectively. Note that the increase in the number of stars at the lowest metallicities is due to the limitations of our model and the likely presence of stellar activity (see the text).
Paper: Stellar Loci. VII. Photometric Metallicities of 5 Million FGK Stars Based on GALEX GR6+7 AIS and Gaia EDR3
Authors: Xue Lu, Haibo Yuan, Shuai Xu, Ruoyi Zhang, Kai Xiao, Yang Huang, Timothy C. Beers, Jihye Hong
Figure caption: Color–magnitude (observed color and apparent magnitude) diagram for subsamples of the VMP/EMP stars shown in Figure 14, represented by the red ([C/Fe] ≤ +0.7) and blue ([C/Fe] > +0.7) symbols, respectively. The squares and circles represent dwarfs and giants, respectively.
Paper: Stellar Loci. VII. Photometric Metallicities of 5 Million FGK Stars Based on GALEX GR6+7 AIS and Gaia EDR3
Authors: Xue Lu, Haibo Yuan, Shuai Xu, Ruoyi Zhang, Kai Xiao, Yang Huang, Timothy C. Beers, Jihye Hong
Figure caption: The G-magnitude distribution of the final sample (with flag = 0). The left and right panels are for the dwarfs and giants, respectively.
Paper: Stellar Loci. VII. Photometric Metallicities of 5 Million FGK Stars Based on GALEX GR6+7 AIS and Gaia EDR3
Authors: Xue Lu, Haibo Yuan, Shuai Xu, Ruoyi Zhang, Kai Xiao, Yang Huang, Timothy C. Beers, Jihye Hong
Figure caption: The spatial distributions in the Z − R plane of the final sample, color coded by [Fe/H]GALEX. The left and right panels are for the dwarfs and giants, respectively. The Sun is located at (R, Z) = (8.178, 0.0) kpc.
Paper: Stellar Loci. VII. Photometric Metallicities of 5 Million FGK Stars Based on GALEX GR6+7 AIS and Gaia EDR3
Authors: Xue Lu, Haibo Yuan, Shuai Xu, Ruoyi Zhang, Kai Xiao, Yang Huang, Timothy C. Beers, Jihye Hong
Figure caption: The spatial distributions in the Z − R plane of the final sample, color coded by number densities. The left and right panels are for the dwarfs and giants, respectively. The Sun is located at (R, Z) = (8.178, 0.0) kpc.
Paper: Stellar Loci. VII. Photometric Metallicities of 5 Million FGK Stars Based on GALEX GR6+7 AIS and Gaia EDR3
Authors: Xue Lu, Haibo Yuan, Shuai Xu, Ruoyi Zhang, Kai Xiao, Yang Huang, Timothy C. Beers, Jihye Hong
Figure caption: Color–magnitude diagram of the final sample, color coded by source number density.
Paper: Stellar Loci. VII. Photometric Metallicities of 5 Million FGK Stars Based on GALEX GR6+7 AIS and Gaia EDR3
Authors: Xue Lu, Haibo Yuan, Shuai Xu, Ruoyi Zhang, Kai Xiao, Yang Huang, Timothy C. Beers, Jihye Hong
Figure caption: Color–magnitude diagram of the LAMOST DR8 test sample. Dwarfs are shown in the upper row of panels and giants are shown in the lower row of panels. The plots are color coded by [Fe/H]LAMOST (left column of panels), Δ[Fe/H] (old model without M  G ) (middle column of panels), and Δ[Fe/H] (new model with M  G  considered) (right column of panels). In the lower middle panel, the shaded region indicates possible blue horizontal branch stars or stars situated near the boundary between dwarfs and giants.
Paper: Stellar Loci. VII. Photometric Metallicities of 5 Million FGK Stars Based on GALEX GR6+7 AIS and Gaia EDR3
Authors: Xue Lu, Haibo Yuan, Shuai Xu, Ruoyi Zhang, Kai Xiao, Yang Huang, Timothy C. Beers, Jihye Hong
Figure caption: Distribution of the Δ[Fe/H] (calculated from the model without M  G ) as a function of M  G  for dwarfs of 0.95 < BP − RP < 1.15 (left panel) and giants of 0.85 < BP − RP < 1 (right panel), respectively. The red solid line indicates the median values.
Paper: Stellar Loci. VII. Photometric Metallicities of 5 Million FGK Stars Based on GALEX GR6+7 AIS and Gaia EDR3
Authors: Xue Lu, Haibo Yuan, Shuai Xu, Ruoyi Zhang, Kai Xiao, Yang Huang, Timothy C. Beers, Jihye Hong
Figure caption: Distribution of the training sample in the (NUV − BP) vs. (BP − RP) plane, color coded by [Fe/H], with dwarfs in the left panel and giants in the right panel. The colored lines represent different [Fe/H] values, ranging from to −3.5 to +0.5, in steps of 0.5 dex.
Paper: Experimental Branching Fractions, Transition Probabilities, and Oscillator Strengths in Sm II 
Authors: Xinghao Wang, Qi Yu, Jiajin Tan, Hongqiang Xie, Zhiming Chen, Xiong Li
Figure caption: Comparison of A values from references to our A values as a function of our gA values. Specifically, the open triangular symbols represent the natural logarithm of the ratios A Xu et al. (2003)/A TW. The open circle symbols represent the natural logarithm of the ratios A Saffman & Whaling (1979)/A TW. The filled circle symbols represent the natural logarithm of the ratios A SL/A TW, while A SL values are derived by combining BFs from Saffman & Whaling (1979) and reliable lifetimes from Lawler et al. (2006). The error bars correspond to uncertainties combined in quadrature. The dashed line corresponds to the equality between them.
Paper: Experimental Branching Fractions, Transition Probabilities, and Oscillator Strengths in Sm II 
Authors: Xinghao Wang, Qi Yu, Jiajin Tan, Hongqiang Xie, Zhiming Chen, Xiong Li
Figure caption: Comparison of A values from Lawler et al. (2006) to our A values as a function of our gA values. The error bars correspond to the greater of the two reported uncertainties due to strong correlation between the two data sets. The dashed line corresponds to the equality between them.
Paper: Physically Motivated Deep Learning to Superresolve and Cross Calibrate Solar Magnetograms
Authors: Andrés Muñoz-Jaramillo, Anna Jungbluth, Xavier Gitiaux, Paul J. Wright, Carl Shneider, Shane A. Maloney, Atılım Güneş Baydin, Yarin Gal, Michel Deudon, Freddie Kalaitzis
Figure caption: Quantitative comparison of the performance of different loss functions trained on MDI magnetograms. We use bicubic upsampling as a comparative baseline (row 1). All loss functions are based on the MSE term, plus up to three additional penalty terms (rows 2–5). The shaded histograms correspond to calculations across the test set for patches within 90% of the solar disk radius. A red vertical line indicates the ideal value for the corresponding performance metric. The two leftmost columns (a) and (b) show calculations performed across patches of 32 × 32 pixels. The two rightmost columns (c) and (d) show calculations performed per pixel in each patch of the test set. Columns left to right show (a) the added difference between the target and output maxima and minima per patch, (b) Pearson correlation per patch, (c) the magnitude of the target and output gradient difference per pixel, and (d) the difference in target and output magnetic flux per pixel. To compare MSE+Grad+Hist+SSIM with the rest, the bottom row is superimposed (nonshaded histogram) on all other rows.
Paper: Physically Motivated Deep Learning to Superresolve and Cross Calibrate Solar Magnetograms
Authors: Andrés Muñoz-Jaramillo, Anna Jungbluth, Xavier Gitiaux, Paul J. Wright, Carl Shneider, Shane A. Maloney, Atılım Güneş Baydin, Yarin Gal, Michel Deudon, Freddie Kalaitzis
Figure caption: Time evolution of HARP 407. (a) Row showing the HMI magnetogram patch associated with HARP 407 at different stages of its lifetime. The different time stamps are indicated as vertical colored lines in the timelines of panels (b) and (c). (b) Total unsigned flux within the whole patch for the HMI target (red triangles) and the SR output of MDI (green dots) or GONG (purple squares). The bicubic baseline is also shown for MDI (beige dots) and GONG (light blue squares). The magnitude and evolution of the unsigned flux of the HMI target region is well reproduced in all cases. (c) Ratio of the unsigned flux between the SR output (or bicubic baseline) and HMI. (d) Magnetograms (top row) and gradients (bottom row) obtained for the same time step and using different upscaling techniques. The center panel is the HMI target.
Paper: Physically Motivated Deep Learning to Superresolve and Cross Calibrate Solar Magnetograms
Authors: Andrés Muñoz-Jaramillo, Anna Jungbluth, Xavier Gitiaux, Paul J. Wright, Carl Shneider, Shane A. Maloney, Atılım Güneş Baydin, Yarin Gal, Michel Deudon, Freddie Kalaitzis
Figure caption: 2D Histogram of pixel-to-pixel comparison for test patches of the MDI → HMI (top two rows) and GONG → HMI (bottom two rows) transformation. The following caption equally applies to the panels belonging to each instrument. In all panels, orange indicates the deep-learning output, while purple indicates the bicubic upsampling baseline. The bold lines denote the median of the quantity and the shaded area is the 25th–75th percentile range. Top row: comparison between the inferred (x-axis) and target magnetic field (y-axis) for all individual pixels in our test set. The y = x line is denoted with a green dotted line. Note that the bold median lines are difficult to see because a simple correlation plot is not ideal for evaluating SR performance. Bottom row: mean relative error in each superresolved 4 × 4 pixel patch (y-axis) as a function of the magnetic field of the corresponding LR input pixel (x-axis). We propose this as a far superior quantity to visually evaluate the performance of SR algorithms. The closer this quantity is to zero, the better.
Paper: Physically Motivated Deep Learning to Superresolve and Cross Calibrate Solar Magnetograms
Authors: Andrés Muñoz-Jaramillo, Anna Jungbluth, Xavier Gitiaux, Paul J. Wright, Carl Shneider, Shane A. Maloney, Atılım Güneş Baydin, Yarin Gal, Michel Deudon, Freddie Kalaitzis
Figure caption: Benefits of SR, compared to bicubic upscaling or ML-based calibration without SR. Time evolution of the (a) and (b) unsigned flux and (c) and (d) average gradient for HARP 407 for superresolved (a)/(c) GONG and (b)/(d) MDI magnetograms. The HMI target is shown with red triangles. In all cases, the closest match is the superresolved ML-4X output. Scatter plots of the (e) and (f) average unsigned flux and (g) and (h) average gradient for all HARPs and all corresponding time stamps during 2011 March. The x-axis always corresponds to the HMI target and the y-axis to the ML output of (e)/(g) GONG and (f)/(h) MDI magnetograms. The closest match to the y = x line (dotted red) is always the superresolved ML-4X output.
Paper: Physically Motivated Deep Learning to Superresolve and Cross Calibrate Solar Magnetograms
Authors: Andrés Muñoz-Jaramillo, Anna Jungbluth, Xavier Gitiaux, Paul J. Wright, Carl Shneider, Shane A. Maloney, Atılım Güneş Baydin, Yarin Gal, Michel Deudon, Freddie Kalaitzis
Figure caption: Quantitative comparison of the performance of different loss functions trained on MDI magnetograms. All loss functions are based on the MSE term, plus up to three additional penalty terms. The gray-shaded histograms correspond to calculations performed across the full solar disk, with the gray solid line showing the distribution average. The blue histograms were calculated for patches that fall within 90% of the solar disk radius, with the blue dashed line showing the distribution average. The first column shows the Pearson correlation calculated for all magnetic field values, while the second column shows the Pearson correlation calculated for magnetic fields with an absolute value above 10 G. In the ideal case, the Pearson correlation is 1 (indicated by the red line).
Paper: Physically Motivated Deep Learning to Superresolve and Cross Calibrate Solar Magnetograms
Authors: Andrés Muñoz-Jaramillo, Anna Jungbluth, Xavier Gitiaux, Paul J. Wright, Carl Shneider, Shane A. Maloney, Atılım Güneş Baydin, Yarin Gal, Michel Deudon, Freddie Kalaitzis
Figure caption: Comparison of the same area of a magnetogram on 2011 March 14 for the input, target, and deep-learning output with different loss functions. The top two rows show MDI magnetograms as input, the bottom two rows show a comparison for the conversion of GONG magnetograms. We chose this particular magnetogram patch as an example for its interesting structure and moderate to high magnetic field strength.