adsabs/AstroCLIMB huggingface dataset:
Paper: MHD Simulations of Dense Core Collision
Authors: Shinichi W. Kinoshita, Fumitaka Nakamura
Figure caption: As in Figure 2, for the model b1-M1-Bz30. Snapshots at 0.21, 0.4, and 0.5 Myr are shown.
Paper: MHD Simulations of Dense Core Collision
Authors: Shinichi W. Kinoshita, Fumitaka Nakamura
Figure caption: As in Figure 2, for the model b1-M1-By30. Snapshots at 0.21, 0.36, and 0.46 Myr are shown.
Paper: MHD Simulations of Dense Core Collision
Authors: Shinichi W. Kinoshita, Fumitaka Nakamura
Figure caption: Temporal evolution of the maximum density normalized to the initial central core density for head-on (b = 0) cases.
Paper: MHD Simulations of Dense Core Collision
Authors: Shinichi W. Kinoshita, Fumitaka Nakamura
Figure caption: As in Figure 2, for the model b1-M1-By10. Snapshots at 0.21, 0.3, and 0.4 Myr are shown.
Paper: MHD Simulations of Dense Core Collision
Authors: Shinichi W. Kinoshita, Fumitaka Nakamura
Figure caption: As in Figure 2, for the model b1-M1-Bz10. Snapshots at 0.21, 0.3, and 0.4 Myr are shown.
Paper: The Galactic Nova Rate: Estimates from the ASAS-SN and Gaia Surveys
Authors: A. Kawash, L. Chomiuk, J. Strader, K. V. Sokolovsky, E. Aydi, C. S. Kochanek, K. Z. Stanek, Z. Kostrzewa-Rutkowska, S. T. Hodgkin, K. Mukai, B. Shappee, T. Jayasinghe, M. Rizzo Smith, T. W.-S. Holoien, J. L. Prieto, T. A. Thompson
Figure caption: Galactic nova rate predictions as a function of the year published, compared with the number of novae confirmed each year since 1980. The rate predictions made using the Galactic or direct method are shown as red circles, and those using the extragalactic or indirect method are shown as black diamonds, along with error bars if the uncertainty was estimated. The estimate from this work is shown as the magenta square. The number of discovered and confirmed Galactic novae each year is plotted as a blue histogram and was derived using Koji Mukai’s List of Galactic Novae, Bill Gray’s Database of Galactic Novae, and AAVSO’s VSX. Citations for published rates from left to right are as follows: Liller & Mayer (1987), Ciardullo et al. (1990), van den Bergh (1991b), della Valle & Livio (1994b), Shafter (1997), Hatano et al. (1997), Shafter et al. (2000), Shafter (2002), Darnley et al. (2006), Shafter et al. (2014), Shafter (2017), Özdönmez et al. (2018), De et al. (2021b), and Rector et al. (2022).
Paper: The Galactic Nova Rate: Estimates from the ASAS-SN and Gaia Surveys
Authors: A. Kawash, L. Chomiuk, J. Strader, K. V. Sokolovsky, E. Aydi, C. S. Kochanek, K. Z. Stanek, Z. Kostrzewa-Rutkowska, S. T. Hodgkin, K. Mukai, B. Shappee, T. Jayasinghe, M. Rizzo Smith, T. W.-S. Holoien, J. L. Prieto, T. A. Thompson
Figure caption: Distribution of the peak absolute magnitude vs. time to decline by 2 mag from maximum (t 2) for 10,000 model novae (black circles). The peak absolute magnitudes are sampled from a normal distribution, and the t 2 values are sampled from a lognormal distribution. The patchiness in the t 2 distribution is the result of a limited number of nova light-curve templates. The allowed values in this parameter space are shown below the blue dashed line, and this is compared to real Galactic nova values estimated from Gaia distances (Schaefer 2018; denoted with green stars), extragalactic measurements (pink diamonds, cyan crosses, and orange diamonds; Shafter et al. 2011; Kasliwal et al. 2011; Shara et al. 2016), and the MMRD correlation derived in della Valle & Livio (1995; shown as the red shaded region).
Paper: The Galactic Nova Rate: Estimates from the ASAS-SN and Gaia Surveys
Authors: A. Kawash, L. Chomiuk, J. Strader, K. V. Sokolovsky, E. Aydi, C. S. Kochanek, K. Z. Stanek, Z. Kostrzewa-Rutkowska, S. T. Hodgkin, K. Mukai, B. Shappee, T. Jayasinghe, M. Rizzo Smith, T. W.-S. Holoien, J. L. Prieto, T. A. Thompson
Figure caption: The recovery fraction of model novae in ASAS-SN and Gaia as a function of peak absolute magnitude and t 2. The recovery fraction values are calculated on a grid of 0.5 mag by 0.25 ﹩{\mathrm{log}}_{10}({t}_{2})﹩ days and are shown in each square, with darker gray scale indicating a higher recovery fraction. While novae that adhere to the supposed MMRD relation are on average easier to detect, they are only recovered about twice as efficiently as faint, fast novae, implying that all-sky surveys would have detected a substantial population of faint, fast novae if they were present.
Paper: The Galactic Nova Rate: Estimates from the ASAS-SN and Gaia Surveys
Authors: A. Kawash, L. Chomiuk, J. Strader, K. V. Sokolovsky, E. Aydi, C. S. Kochanek, K. Z. Stanek, Z. Kostrzewa-Rutkowska, S. T. Hodgkin, K. Mukai, B. Shappee, T. Jayasinghe, M. Rizzo Smith, T. W.-S. Holoien, J. L. Prieto, T. A. Thompson
Figure caption: The positions of simulated novae that are discovered in our model (blue circles) compared to the real sample discovered between 2019 and 2021 (orange stars). The simulated positions are derived assuming that novae trace the stellar density of the Galaxy. The elongated bulge, oriented at a roughly 20° angle from the Sun–Galactic center line, appears to place more recoverable bulge novae at l > 0° compared to l < 0°.
Paper: The Galactic Nova Rate: Estimates from the ASAS-SN and Gaia Surveys
Authors: A. Kawash, L. Chomiuk, J. Strader, K. V. Sokolovsky, E. Aydi, C. S. Kochanek, K. Z. Stanek, Z. Kostrzewa-Rutkowska, S. T. Hodgkin, K. Mukai, B. Shappee, T. Jayasinghe, M. Rizzo Smith, T. W.-S. Holoien, J. L. Prieto, T. A. Thompson
Figure caption: The normalized distributions of peak apparent magnitude of 10,000 simulated novae in the g-band filter (blue) and G-band filter (red) The dashed vertical lines indicate the limiting magnitude of ASAS-SN (blue) and Gaia (red). Also shown is the distribution with zero extinction with the peak scaled to fit (black dashed line). This demonstrates that dust is a much larger factor than the luminosity or distance in determining the peak apparent magnitude of a nova.
Paper: The Galactic Nova Rate: Estimates from the ASAS-SN and Gaia Surveys
Authors: A. Kawash, L. Chomiuk, J. Strader, K. V. Sokolovsky, E. Aydi, C. S. Kochanek, K. Z. Stanek, Z. Kostrzewa-Rutkowska, S. T. Hodgkin, K. Mukai, B. Shappee, T. Jayasinghe, M. Rizzo Smith, T. W.-S. Holoien, J. L. Prieto, T. A. Thompson
Figure caption: Three examples of simulated novae in ASAS-SN (left) and Gaia (right). The detections are shown in blue for ASAS-SN and red for Gaia, with nondetections shown as black triangles. The epoch of eruption is denoted by the vertical dashed line, and the peak apparent magnitude and t 2 are listed in each panel. The top row shows a fast reddened nova, the middle row shows a nearby and slow nova (the nondetections shortly after the eruption indicate that the transient has saturated the ASAS-SN detectors), and the bottom row shows a reddened nova that was only detected by Gaia.
Paper: The Galactic Nova Rate: Estimates from the ASAS-SN and Gaia Surveys
Authors: A. Kawash, L. Chomiuk, J. Strader, K. V. Sokolovsky, E. Aydi, C. S. Kochanek, K. Z. Stanek, Z. Kostrzewa-Rutkowska, S. T. Hodgkin, K. Mukai, B. Shappee, T. Jayasinghe, M. Rizzo Smith, T. W.-S. Holoien, J. L. Prieto, T. A. Thompson
Figure caption: The predicted Galactic nova rate based on 1000 Monte Carlo trials, from ASAS-SN (blue histogram), Gaia (red histogram), and a combination of both surveys (purple histogram). We give the median values of the distributions as the most likely Galactic nova rate and include the 16% and 84% confidence regions. The results are all consistent at the 1σ level, with the most likely rate from both surveys predicting a Galactic nova rate of R = 26 ± 5 yr−1.
Paper: The Galactic Nova Rate: Estimates from the ASAS-SN and Gaia Surveys
Authors: A. Kawash, L. Chomiuk, J. Strader, K. V. Sokolovsky, E. Aydi, C. S. Kochanek, K. Z. Stanek, Z. Kostrzewa-Rutkowska, S. T. Hodgkin, K. Mukai, B. Shappee, T. Jayasinghe, M. Rizzo Smith, T. W.-S. Holoien, J. L. Prieto, T. A. Thompson
Figure caption: The normalized extinction distributions of 10,000 simulated novae in the ASAS-SN g-band filter (blue) and Gaia G-band filter (red). These distributions are estimated from the mwdust package (default values shown as dotted lines), and we add additional extinction if the line of sight is not complete out to the distance of the nova (solid line).
Paper: Changes in the Na D1 Absorption Components of η Carinae Provide Clues on the Location of the Dissipating Central Occulter
Authors: Connor S. Pickett, Noel D. Richardson, Theodore R. Gull, D. John Hillier, Henrik Hartman, Nour Ibrahim, Alexis M. Lane, Emily Strawn, Augusto Damineli, Anthony F. J. Moffat, Felipe Navarete, Gerd Weigelt
Figure caption: A subset of the data taken for η Car, from phase ϕ = 11.975 to ϕ = 14.256 (indicated as numbers below the spectra on the right), which highlights some of the variations seen in the data. The dotted lines represent the multiple absorption features discussed in this paper relative to the Na D1 line, with the +87 km s−1 component also shown as a dashed line for the Na D2 line. We indicate the velocity of the absorptions at the bottom of the figure. The data before phase 12.5 were taken with the lower-resolution fiber-fed echelle spectrograph, while the more recent data were taken with the CHIRON spectrograph. The variable emission on the red side of this plot is from He I λ5876, for which the variability changes the apparent spacing on the left.
Paper: Changes in the Na D1 Absorption Components of η Carinae Provide Clues on the Location of the Dissipating Central Occulter
Authors: Connor S. Pickett, Noel D. Richardson, Theodore R. Gull, D. John Hillier, Henrik Hartman, Nour Ibrahim, Alexis M. Lane, Emily Strawn, Augusto Damineli, Anthony F. J. Moffat, Felipe Navarete, Gerd Weigelt
Figure caption: Velocity profiles of Si II, Si IV, Al II, and Al III resonant lines as recorded by HST/STIS. The three spectra were recorded at similar phases following the periastron passages 11, 13, and 14 when η Car has reentered the high-ionization state. Long-term changes in the Little Homunculus are apparent between −100 and −400 km s−1. The absorption at +87 km s−1 is also present in the low-ionization Si II and Al II profiles.
Paper: Changes in the Na D1 Absorption Components of η Carinae Provide Clues on the Location of the Dissipating Central Occulter
Authors: Connor S. Pickett, Noel D. Richardson, Theodore R. Gull, D. John Hillier, Henrik Hartman, Nour Ibrahim, Alexis M. Lane, Emily Strawn, Augusto Damineli, Anthony F. J. Moffat, Felipe Navarete, Gerd Weigelt
Figure caption: The measured equivalent width strength of the +87 km s−1 feature from the CHIRON spectrograph, where the strength changes slightly near the 2014 periastron, presumably because of the changing ionization in the line of sight.
Paper: Changes in the Na D1 Absorption Components of η Carinae Provide Clues on the Location of the Dissipating Central Occulter
Authors: Connor S. Pickett, Noel D. Richardson, Theodore R. Gull, D. John Hillier, Henrik Hartman, Nour Ibrahim, Alexis M. Lane, Emily Strawn, Augusto Damineli, Anthony F. J. Moffat, Felipe Navarete, Gerd Weigelt
Figure caption: The measured equivalent width strength of the −145 km s−1 feature through the 2009, 2014, and 2020 events, phased to the binary clock. For the 2020 event, the equivalent width of the blended components at −145 and −168 km s−1 were measured, but multiplied by a factor of 3 to be displayed on a similar scale as the previous two periastron passages.
Paper: Changes in the Na D1 Absorption Components of η Carinae Provide Clues on the Location of the Dissipating Central Occulter
Authors: Connor S. Pickett, Noel D. Richardson, Theodore R. Gull, D. John Hillier, Henrik Hartman, Nour Ibrahim, Alexis M. Lane, Emily Strawn, Augusto Damineli, Anthony F. J. Moffat, Felipe Navarete, Gerd Weigelt
Figure caption: The measured equivalent width strength of the −145 km s−1 feature, in reference to Na D1, through the 2009 and 2014 events, where the strength increases drastically near the two periastron passages. In the interim time, the feature is seen to have a slow decline, which accelerates to higher velocities after the 2014 event.
Paper: Changes in the Na D1 Absorption Components of η Carinae Provide Clues on the Location of the Dissipating Central Occulter
Authors: Connor S. Pickett, Noel D. Richardson, Theodore R. Gull, D. John Hillier, Henrik Hartman, Nour Ibrahim, Alexis M. Lane, Emily Strawn, Augusto Damineli, Anthony F. J. Moffat, Felipe Navarete, Gerd Weigelt
Figure caption: A cartoon diagram showing the geometry of the gas that provides Na D absorption. A detailed discussion of this geometry is in the text.
Paper: Changes in the Na D1 Absorption Components of η Carinae Provide Clues on the Location of the Dissipating Central Occulter
Authors: Connor S. Pickett, Noel D. Richardson, Theodore R. Gull, D. John Hillier, Henrik Hartman, Nour Ibrahim, Alexis M. Lane, Emily Strawn, Augusto Damineli, Anthony F. J. Moffat, Felipe Navarete, Gerd Weigelt
Figure caption: The measured equivalent width strength of the −168 km s−1 feature across the 2020 periastron passage, where the strength increases after the periastron. This measurement is a blend of the bluer component of −145 km s−1 with the −168 km s−1 component.
Paper: Changes in the Na D1 Absorption Components of η Carinae Provide Clues on the Location of the Dissipating Central Occulter
Authors: Connor S. Pickett, Noel D. Richardson, Theodore R. Gull, D. John Hillier, Henrik Hartman, Nour Ibrahim, Alexis M. Lane, Emily Strawn, Augusto Damineli, Anthony F. J. Moffat, Felipe Navarete, Gerd Weigelt
Figure caption: A comparison of the Na D profiles of η Car at ϕ = 13.964, CPD −59° 2628, HD 93204, HD 93205, and HD 303308 at 1′ to the north. η Car, CPD −59° 2628, and HD 303308 clearly have features present at positive velocities similar to that of η Car. Similar interstellar features are denoted with arrows.
Paper: Multi-messenger Observations of Binary Neutron Star Mergers in the O4 Run
Authors: Alberto Colombo, Om Sharan Salafia, Francesco Gabrielli, Giancarlo Ghirlanda, Bruno Giacomazzo, Albino Perego, Monica Colpi
Figure caption:  M 1, M 2 plane showing the mass distribution for our NSNS population. The filled blue colored regions contain 50%, 90%, and 99% of the binaries. The black dashed lines and the gray lines represent, respectively, the contours for the predicted dynamical ejecta and disk mass, assuming the SFHo EoS. Red stars and contours show the best-fit and 90% credible regions for the known Galactic NSNS (Özel & Freire 2016; Farrow et al. 2019) systems that merge within a Hubble time. Yellow and aquamarine lines represent the 50% confidence regions for the component masses in GW190425 (Abbott et al. 2020c) and GW170817 (Abbott et al. 2019b), both constructed using the publicly available low-spin-prior posterior samples.
Paper: Multi-messenger Observations of Binary Neutron Star Mergers in the O4 Run
Authors: Alberto Colombo, Om Sharan Salafia, Francesco Gabrielli, Giancarlo Ghirlanda, Bruno Giacomazzo, Albino Perego, Monica Colpi
Figure caption: Numerical-relativity simulations used to calibrate the ejecta and disk mass fitting formulae compared to our assumed mass distribution on the M 1, M 2 plane. Filled contours show the smallest areas containing 50%, 90%, and 99% of the binaries in our NSNS population (same color coding as in Figure 8). Colored symbols mark the pairs of NS gravitational masses corresponding to the simulations in the calibration set. Different symbols are used for simulations described in different references. The ejecta mass fitting formula (Krüger & Foucart 2020) is calibrated on the data from Hotokezaka et al. (2013), Bauswein et al. (2013), Dietrich et al. (2015), Lehner et al. (2016), Sekiguchi et al. (2016), Dietrich et al. (2017) and Kiuchi et al. (2019); the ejecta velocity fitting formula is calibrated on data from Radice et al. (2018) (using only the simulations with neutrino leakage—LK); the disk mass fitting formula (Barbieri et al. 2021) is calibrated on data from Radice et al. (2018) (both simulations with neutrino leakage—LK—and those with M0 transport—M0), Vincent et al. (2020), Kiuchi et al. (2019), and Bernuzzi et al. (2020).
Paper: Multi-messenger Observations of Binary Neutron Star Mergers in the O4 Run
Authors: Alberto Colombo, Om Sharan Salafia, Francesco Gabrielli, Giancarlo Ghirlanda, Bruno Giacomazzo, Albino Perego, Monica Colpi
Figure caption: Component mass probability distribution comparisons. Upper-left panel: NSNS component mass probability distributions (solid lines: primary mass; dashed lines: secondary mass) from our model, assuming three different parameterizations of the chirp mass probability distribution, namely, a power law (purple—the fiducial model described in the text), a decreasing exponential (orange), and a Gaussian tail (light blue). Other panels: comparison of our component mass (top right: primary; bottom right: secondary) and chirp mass (lower left) probability distributions (red lines) with those from a state-of-the-art population synthesis model (the fiducial model from Broekgaarden et al. (2022), blue lines) and of an observational study that combines Galactic and GW NSNS measurements (Galaudage et al. 2021, black lines, obtained considering their median distributions).
Paper: Multi-messenger Observations of Binary Neutron Star Mergers in the O4 Run
Authors: Alberto Colombo, Om Sharan Salafia, Francesco Gabrielli, Giancarlo Ghirlanda, Bruno Giacomazzo, Albino Perego, Monica Colpi
Figure caption: Fermi/GBM (Swift/BAT) observed inverse cumulative distribution of 64 ms (20 ms) binned photon fluxes in the 10–1000 (15–150) keV band (the colored band shows the 90% confidence band due to Poisson and measurement uncertainties) compared with our model (dashed line).
Paper: Multi-messenger Observations of Binary Neutron Star Mergers in the O4 Run
Authors: Alberto Colombo, Om Sharan Salafia, Francesco Gabrielli, Giancarlo Ghirlanda, Bruno Giacomazzo, Albino Perego, Monica Colpi
Figure caption: Cumulative mass ratio probability density in our mass distribution model (blue solid line), compared to the observed Galactic NSNS (with coalescence time less than the Hubble time) mass ratio cumulative distribution (red line: median; pink area: 90% uncertainty region—based on the data from Farrow et al. 2019).
Paper: Multi-messenger Observations of Binary Neutron Star Mergers in the O4 Run
Authors: Alberto Colombo, Om Sharan Salafia, Francesco Gabrielli, Giancarlo Ghirlanda, Bruno Giacomazzo, Albino Perego, Monica Colpi
Figure caption: Viewing angle θ v vs. redshift z for our NSNS population. The filled gray regions contain 50%, 90%, and 99% of the GW O4-detectable binaries. Solid, dashed, and dotted contours contain 50%, 90%, and 99% of the binaries that exceed both the O4 GW S/Nnet limit and any one of the counterpart search limits relevant to the particular counterpart considered (blue: KN; red: GRB afterglow; orange: GRB prompt). The corresponding detection rates are reported in Figure 1.
Paper: Multi-messenger Observations of Binary Neutron Star Mergers in the O4 Run
Authors: Alberto Colombo, Om Sharan Salafia, Francesco Gabrielli, Giancarlo Ghirlanda, Bruno Giacomazzo, Albino Perego, Monica Colpi
Figure caption: Detection rates as a function of the detection threshold limit for our NSNS population. The upper panel refers to GRB Prompt+O4-detectable binaries. The solid line indicates an all-sky field of view with a 100% duty cycle, the dashed and dotted lines account for the Fermi/GBM and Swift/BAT duty cycle and field of view, respectively. The lower panel refers to GRB Afterglow+O4-detectable binaries. The solid, dashed, and dotted lines indicate the radio, optical, and X bands, respectively.
Paper: Multi-messenger Observations of Binary Neutron Star Mergers in the O4 Run
Authors: Alberto Colombo, Om Sharan Salafia, Francesco Gabrielli, Giancarlo Ghirlanda, Bruno Giacomazzo, Albino Perego, Monica Colpi
Figure caption: Same as Figure 2, but for the g band (484 nm, blue) and for the J band (1250 nm, green).
Paper: Exploring the Limits of Synthetic Creation of Solar EUV Images via Image-to-image Translation
Authors: Valentina Salvatelli, Luiz F. G. dos Santos, Souvik Bose, Brad Neuberg, Mark C. M. Cheung, Miho Janvier, Meng Jin, Yarin Gal, Atilim Güneş Baydin
Figure caption: Predicted intensity vs. real intensity for each of the four channels, for all the pixels contained in the 667 images on the test set. From top to bottom: 211, 193, 171, 94 Å channels. For each channel: the top plot shows the error on the predicted count rate as a function of the real count rate in log10. The error band represents the standard deviation and the line corresponds to the median. In green is the standard U-net model. In blue is the same architecture with square root scaling applied to the input images. The bottom plot shows the histogram of the pixel count rate distributions over the test set. The model performs well over 3 orders of magnitude but its accuracy degrades quickly in the extreme regions where fewer pixels are available.
Paper: Exploring the Limits of Synthetic Creation of Solar EUV Images via Image-to-image Translation
Authors: Valentina Salvatelli, Luiz F. G. dos Santos, Souvik Bose, Brad Neuberg, Mark C. M. Cheung, Miho Janvier, Meng Jin, Yarin Gal, Atilim Güneş Baydin
Figure caption: Real vs. synthetic images on a quiet timestamp (2011-02-10 00:00:00 UT) when using the model with root scaling. From left to right: real image, image synthesized by looking at the other three channels, residuals relative to the ground-truth (GT) value, and the difference between the two images. From top to bottom: 211, 193, 171, and 94 Å channels.
Paper: Exploring the Limits of Synthetic Creation of Solar EUV Images via Image-to-image Translation
Authors: Valentina Salvatelli, Luiz F. G. dos Santos, Souvik Bose, Brad Neuberg, Mark C. M. Cheung, Miho Janvier, Meng Jin, Yarin Gal, Atilim Güneş Baydin
Figure caption: Real vs. synthetic images during a flare (2011-02-15 02:00:00 UT) when using the model with root scaling. From left to right: real image, image synthesized by looking at the other three channels, residuals relative to the GT value, and the difference between the two images. From top to bottom: 211, 193, 171, and 94 Å channels.
Paper: Exploring the Limits of Synthetic Creation of Solar EUV Images via Image-to-image Translation
Authors: Valentina Salvatelli, Luiz F. G. dos Santos, Souvik Bose, Brad Neuberg, Mark C. M. Cheung, Miho Janvier, Meng Jin, Yarin Gal, Atilim Güneş Baydin
Figure caption: Reconstruction error on the covariance in correspondence to the Valentine’s Day flare. From left to right: differences between the ground-truth and the predicted images and differences between the real and predicted covariance maps between 211 Å—the predicted channel—and each of the input channels. From top to bottom: each row corresponds to a different timestamp at an interval of 1 hr. The third line is the closest to the time of the flare.
Paper: Exploring the Limits of Synthetic Creation of Solar EUV Images via Image-to-image Translation
Authors: Valentina Salvatelli, Luiz F. G. dos Santos, Souvik Bose, Brad Neuberg, Mark C. M. Cheung, Miho Janvier, Meng Jin, Yarin Gal, Atilim Güneş Baydin
Figure caption: Coronal Holes for channel 193 Å. On the left is the segmentation mask obtained by thresholding; on the right are the histograms showing the difference between the ground truth and the predicted intensities (on a pixel-by-pixel basis) for both the pixels within the CHs and for the full disk.
Paper: Exploring the Limits of Synthetic Creation of Solar EUV Images via Image-to-image Translation
Authors: Valentina Salvatelli, Luiz F. G. dos Santos, Souvik Bose, Brad Neuberg, Mark C. M. Cheung, Miho Janvier, Meng Jin, Yarin Gal, Atilim Güneş Baydin
Figure caption: U-Net based architecture used to synthesize solar EUV images. Each box corresponds to a multichannel feature map. Gray boxes are copied maps. The number of channels is shown on top of the box. Resolution in pixels is indicated on the left of the box. Arrows represent operations. For images of size 512 × 512 pixels, the trainable parameters are 34, 513, and 857. The figure is taken from Salvatelli et al. (2019).