adsabs/AstroCLIMB huggingface dataset:
Paper: Early Emission from Double Detonation Type Ia Supernovae
Authors: Anthony L. Piro, Ehud Nakar
Figure caption: Diagram of a quadrant of a DD, highlighting the key velocities considered in this model. The total system is broken into two regions: (1) the detonating He surface layer with mass m (orange) and (2) the detonating CO WD with mass M (blue). For velocities v > vt (dotted line), the core is imparted with a steep gradient ρ ∝ v−n due to the detonation shock propagating into the edge of the star. In contrast, the prior He detonation moves roughly perpendicular in the layer and thus produces a shallower velocity gradient with ﹩{v}_{1,{\rm{\max }}}\sim 2{v}_{1}﹩, where v1 ≈ 1.3 × 109 cm s−1 is the characteristic velocity of the layer. During the collision, roughly only the outer m of the CO core participates, which defines the velocity v2 (dashed line).
Paper: Early Emission from Double Detonation Type Ia Supernovae
Authors: Anthony L. Piro, Ehud Nakar
Figure caption: Contours of constant luminosity (blue) and timescale (red) expected for shock cooling emission from a DD as a function of the WD mass M and the He surface layer mass m. The initial He-detonation velocity is set to v1 = 1.3 × 109 cm s−1 with a delay of Δt = 3 s from the initiation of the He detonation to the unbinding of the core. We fix the explosion energy of the core detonation to E = 1051 erg and use an opacity of κ = 0.1 cm2 g−1 for the cooling emission. Recombination occurs above the dashed black line for Trec = 7000 K. Unlike the numerical scalings summarized in Section 2.3, we do not approximate v2 ≫ v1 for this plot.
Paper: Consistent Gas-phase C/O Abundances from UV and Optical Emission Lines: A Robust Scale for Chemical Evolution across Cosmic Time
Authors: Paige M. Kelly, Tucker Jones, Yuguang Chen, Ryan L. Sanders, Danielle A. Berg, Peter Senchyna, Fabio Bresolin, Daniel Stark
Figure caption: Rest-frame HST/COS spectra of C III] λλ1907,1909 and O III] λλ1660,1666 emission lines. The spectra are binned by 6 pixels and scaled arbitrarily for display purposes. Dashed blue lines show the expected wavelengths of each transition, and best-fit Gaussian profiles to each emission line are shown in red. NGC 5408 shows a complex C III] profile that could not be fit well with a single Gaussian.
Paper: TESS Subgiant and Lower-red-giant Asteroseismology in the Continuous Viewing Zones
Authors: Sophia Grusnis, Jamie Tayar, Diego Godoy-Rivera
Figure caption: We show for comparison (gray) the full sample from the APOGEE DR17 spectroscopic survey in this temperature and metallicity regime. left: our data is circled in black and color coded by [α/M]. [M/H] plotted against ages given by the MIST stellar models. We see no strong correlation between [M/H] and age. Right: our data is circled in black and color coded by [M/H]. [α/M] plotted against ages given by the MIST stellar model. In the top-left corner, we can see our young alpha-enhanced (yαr) stars. The α-rich, thick-disk stars are in the top-right quadrant, with the remaining lower half of the chart representing the thin disk. Most of the sample are low-alpha stars. The dotted line shows the age of the universe for reference. Average error bars are shown in the top-right corner.
Paper: TESS Subgiant and Lower-red-giant Asteroseismology in the Continuous Viewing Zones
Authors: Sophia Grusnis, Jamie Tayar, Diego Godoy-Rivera
Figure caption: Asteroseismic masses as a function of temperature and luminosity. Our data is outlined with black circles and compared to previous result from Kepler for dwarfs and subgiants (A. Serenelli et al. 2017), and giants (M. H. Pinsonneault et al. 2018). We also emphasize the location of one unusual star, TIC 366490487 (see Section 3.5) with an x marker at a Teff of 5499 K, and a luminosity of 4.84 L⊙. In general, our seismic results are consistent with previous efforts, but populate a regime undersampled in Kepler.
Paper: TESS Subgiant and Lower-red-giant Asteroseismology in the Continuous Viewing Zones
Authors: Sophia Grusnis, Jamie Tayar, Diego Godoy-Rivera
Figure caption: Surface gravity vs. the temperature difference between the model and our observables, color coded by metallicity, for each set of models: GARSTEC, DSEP, YREC, and MIST. The first gray line from the linear regression line shows a 1σ error. The gray box is showing where the bulk of the data is. The horizontal line is at ΔTeff = 0 and the vertical line is at ﹩{\rm{log}}(g)=3.5﹩ roughly separating the giants on the left and the subgiants on the right. Our observed errors are shown in the bottom-left corner of each subplot.
Paper: TESS Subgiant and Lower-red-giant Asteroseismology in the Continuous Viewing Zones
Authors: Sophia Grusnis, Jamie Tayar, Diego Godoy-Rivera
Figure caption: Cumulative distribution function for our solar-like oscillator detections vs. the probability of detecting oscillators given by M. Schofield et al. (2019) and D. Hey et al. (2024). Overall, the ranking of predictions was accurate, but we were less likely to detect oscillations than expected.
Paper: TESS Subgiant and Lower-red-giant Asteroseismology in the Continuous Viewing Zones
Authors: Sophia Grusnis, Jamie Tayar, Diego Godoy-Rivera
Figure caption: Age estimates from the MIST stellar-model tracks. We show our ages (blue) normalized in comparison to the ages from A. Serenelli et al. (2017; red) and can see that the ages for the TESS stars are quite consistent with previous studies from Kepler, perhaps because both sample a local population. The average observed error bar is in the upper right corner.
Paper: TESS Subgiant and Lower-red-giant Asteroseismology in the Continuous Viewing Zones
Authors: Sophia Grusnis, Jamie Tayar, Diego Godoy-Rivera
Figure caption: Our seismic results compare well to spectroscopic surface gravities from APOGEE (left) and radii from Gaia (right, D. Godoy-Rivera et al. (2021). For each plot we show error bars for all points, but may be smaller than the markers.
Paper: TESS Subgiant and Lower-red-giant Asteroseismology in the Continuous Viewing Zones
Authors: Sophia Grusnis, Jamie Tayar, Diego Godoy-Rivera
Figure caption: We show that there is a definite trend that brighter and redder stars are more likely to be detected as solar-like oscillators. Our SCVZ stars (light blue) that showed oscillations covered a wider range of colors but were brighter than the NCVZ oscillators (dark blue). The red x markers show stars with no detected oscillators.
Paper: TESS Subgiant and Lower-red-giant Asteroseismology in the Continuous Viewing Zones
Authors: Sophia Grusnis, Jamie Tayar, Diego Godoy-Rivera
Figure caption: The background-corrected power spectrum for TIC 366490487. Here we do not have a Gaussian envelope of power but instead we can see multiple large power spikes throughout a large range of frequencies.
Paper: TESS Subgiant and Lower-red-giant Asteroseismology in the Continuous Viewing Zones
Authors: Sophia Grusnis, Jamie Tayar, Diego Godoy-Rivera
Figure caption: Mass distribution for our sample. As expected, these subgiants tend to be low mass stars (1M⊙–1.3M⊙) near the solar age. The values range from 0.75 to 1.90 M⊙, with an average uncertainty of 0.21 M⊙.
Paper: The Effects of Linear Matter Power Spectrum Enhancement on Dark Matter Substructure
Authors: Ethan O. Nadler, Vera Gluscevic, Andrew Benson
Figure caption: Ratio of the differential SHMF relative to CDM (Equation (5)). Results are shown for Bump + Cutoff (solid purple), Bump (dotted–dashed blue), and Cutoff (dashed red) models with k0 = 22.8, 32.1, and 41.8 Mpc−1, from lightest to darkest shade. Shaded bands show 1σ Poisson uncertainties for the Bump results.
Paper: The Effects of Linear Matter Power Spectrum Enhancement on Dark Matter Substructure
Authors: Ethan O. Nadler, Vera Gluscevic, Andrew Benson
Figure caption: Ratio of the differential SHMF in our models with P(k) enhancement relative to CDM divided by the corresponding ratio for isolated halos (Equation (6)). Results are shown for Bump + Cutoff (solid purple) and Bump (dotted–dashed blue) models with k0 = 22.8, 32.1, and 41.8 Mpc−1, from lightest to darkest shade. Shaded bands show 1σ Poisson uncertainties for the Bump results. The differences in subhalo vs. isolated halo abundances shown here are small compared to the differences in SHMFs relative to CDM that are imprinted by P(k) (see Figure 4).
Paper: The Effects of Linear Matter Power Spectrum Enhancement on Dark Matter Substructure
Authors: Ethan O. Nadler, Vera Gluscevic, Andrew Benson
Figure caption: Differential SHMFs in CDM (black) and Bump + Cutoff (purple) models with k0 = 22.8, 32.1, and 41.8 Mpc−1, from lightest to darkest shade. The bottom panel shows the ratio to CDM (Equation (5)). In both panels, shaded bands show 1σ Poisson uncertainties.
Paper: The Effects of Linear Matter Power Spectrum Enhancement on Dark Matter Substructure
Authors: Ethan O. Nadler, Vera Gluscevic, Andrew Benson
Figure caption: Projected DM density maps for our CDM (top left), Bump + Cutoff (top right), Bump (bottom left), and Cutoff (bottom right) simulations; for all non-CDM models, we show the k0 = 22.8 Mpc−1 result. Each visualization is centered on the host, spans 1.5 times its virial radius, and is created using MESHOID (https://github.com/mikegrudic/meshoid).
Paper: The Effects of Linear Matter Power Spectrum Enhancement on Dark Matter Substructure
Authors: Ethan O. Nadler, Vera Gluscevic, Andrew Benson
Figure caption: Left: ratio of the linear matter power spectrum in our Bump + Cutoff (solid purple) and WDM (dashed orange) scenarios relative to CDM (black dotted). Models are shown with k0 = 22.8, 32.1, and 41.8 Mpc−1, corresponding to khm for 3, 4, and 5 keV WDM, from lightest to darkest shade. Right: examples of Bump + Cutoff (solid purple), Bump (dotted–dashed blue), and Cutoff (dashed red) transfer functions with different values of k0. In both panels, top ticks show halo masses associated with wavenumbers in linear theory (E. O. Nadler et al. 2025a).
Paper: OTI on FIRE: Testing the Efficacy of Orbital Torus Imaging to Recover the Galactic Potential
Authors: Micah Oeur, Sarah R. Loebman, Adrian M. Price-Whelan, Arpit Arora, Lina Necib, Danny Horta
Figure caption: Selecting volumes of stars across the disk and analyzing within individual volumes enables us to explore how diverse disk environments impact OTI inferences. Left: the background displays a face-on view of the stellar surface mass density for the FIRE-2 simulated galaxy, m12i, at the present day. In the foreground, we plot open, colored circles indicating 16 solar-analog volumes, each centered at a galactocentric radius of 8 kpc, with a radius of 1.4 kpc and a height constraint of ∣z∣ ≤ 3.5 kpc, containing the stellar populations analyzed in our OTI study. Right: edge-on view of the stellar surface mass density reveals a slight warp in the outer region of the disk where we carry out OTI analysis. Refer to Figure B2 in Appendix B for the edge-on view of the individual volumes.
Paper: OTI on FIRE: Testing the Efficacy of Orbital Torus Imaging to Recover the Galactic Potential
Authors: Micah Oeur, Sarah R. Loebman, Adrian M. Price-Whelan, Arpit Arora, Lina Necib, Danny Horta
Figure caption: The vertical metallicity gradient slope in m12i at the present day is nonzero in all solar volumes, a requirement for OTI analysis. We plot the mean line of best fit across 16 solar-analog volumes (black solid line), showing a slope of ﹩\bar{m}=-0.15﹩  dex kpc−1, as well as the best-fit line in all 16 solar volumes (colored translucent lines). See Figure A2 in Appendix A for the measured slopes of each individual volume. For reference, we include the black dashed line representing the mean vertical [Fe/H] profile across all stars in 11 FIRE-2 MW-mass galaxies at the present day at R = 8 kpc, and the 1σ interval (black shaded region; R. L. Graf et al. 2025). For comparison, the MW has vertical metallicity gradient slope estimates from −0.1 to −0.3 dex kpc−1 (Ž. Ivezić et al. 2008; K. Carrell et al. 2012; M. R. Hayden et al. 2014; J. Imig et al. 2023). See Section 2 for further discussion.
Paper: OTI on FIRE: Testing the Efficacy of Orbital Torus Imaging to Recover the Galactic Potential
Authors: Micah Oeur, Sarah R. Loebman, Adrian M. Price-Whelan, Arpit Arora, Lina Necib, Danny Horta
Figure caption: The average mean [Fe/H] across all 16 volumes in bins of z–vz. Mean [Fe/H] systematically decreases from central to outer regions, as seen in the MW; this strong vertical metallicity gradient improves the OTI fit for parameterized orbital shapes. Such a gradient enables accurate orbital modeling, as it maps more distinct orbital paths to the vertical distribution. See Section 2 for further discussion and Figure A1 in Appendix A for individual vertical metallicity gradients within each volume.
Paper: OTI on FIRE: Testing the Efficacy of Orbital Torus Imaging to Recover the Galactic Potential
Authors: Micah Oeur, Sarah R. Loebman, Adrian M. Price-Whelan, Arpit Arora, Lina Necib, Danny Horta
Figure caption: Asymmetric global stellar kinematic conditions are present at the present day in m12i: violet and blue lobes near the solar annulus emphasize variations in stellar velocities. Top: a top-down view of the mean stellar radial velocity. Colored circles mark the solar regions shown in Figure 1. Bottom: similar view of the mean stellar vertical velocity. The asymmetry in velocity distributions provides insights into the kinematic structure across the galactic disk.
Paper: The Effects of Linear Matter Power Spectrum Enhancement on Dark Matter Substructure
Authors: Ethan O. Nadler, Vera Gluscevic, Andrew Benson
Figure caption: Effective concentration (Equation (7)) vs. peak virial mass for subhalos with Mvir > 108 M⊙ in our CDM simulation (black circles), along with our k0 = 22.8 Mpc−1 (light blue squares) and 41.8 Mpc−1 (dark blue triangles) Bump simulations. Thick points show median values, and error bars show 1σ scatter in bins of Mpeak. Subhalo concentrations are enhanced in the Bump and Bump + Cutoff scenarios.
Paper: The Effects of Linear Matter Power Spectrum Enhancement on Dark Matter Substructure
Authors: Ethan O. Nadler, Vera Gluscevic, Andrew Benson
Figure caption: Normalized radial distribution of subhalos with 1.5 × 107 M⊙ < Mpeak < 5 × 108 M⊙ in CDM (black) and Bump + Cutoff models (purple) with k0 = 22.8, 32.1, and 41.8 Mpc−1, from lightest to darkest shade. The dotted–dashed black line shows the CDM result for subhalos with Mpeak > 5 × 108 M⊙. The shaded gray band shows 1σ Poisson uncertainty for the CDM result. Note that the host halo’s virial radius is Rvir,host = 263 kpc in all simulations. Models that enhance P(k) at higher Mpeak yield more centrally concentrated radial distributions.
Paper: The Effects of Linear Matter Power Spectrum Enhancement on Dark Matter Substructure
Authors: Ethan O. Nadler, Vera Gluscevic, Andrew Benson
Figure caption: Same as Figure 3, but comparing the differential SHMF in our LR (dashed) vs. HR (solid) simulations. We show CDM (black) and Bump + Cutoff (purple) models with k0 = 22.8, 32.1, and 41.8 Mpc−1, from lightest to darkest shade. The bottom panel shows the SHMF ratio between each LR/HR pair. In both panels, shaded bands show 1σ Poisson uncertainties for the HR results.
Paper: The Effects of Linear Matter Power Spectrum Enhancement on Dark Matter Substructure
Authors: Ethan O. Nadler, Vera Gluscevic, Andrew Benson
Figure caption: Same as Figure 3, but comparing the differential SHMF in CDM (black) to Cutoff (red) models with k0 = 22.8, 32.1, and 41.8 Mpc−1, from lightest to darkest shade. The bottom panel shows the ratio of the SHMF to CDM in the Cutoff (solid red) and WDM (dashed orange) scenarios. In both panels, shaded bands show 1σ Poisson uncertainties.
Paper: Synthetic Ca II 8542 Å Stokes Profile Associated with Chromospheric Magnetic Reconnection in a Simulated Active Region
Authors: Xinyu Zhou, Takaaki Yokoyama, Haruhisa Iijima, Takuma Matsumoto, Shin Toriumi, Yukio Katsukawa, Masahito Kubo
Figure caption: Stokes signals and simulation data around reconnection event 2 at t = 1748 s organized similar to Figure 4.
Paper: Synthetic Ca II 8542 Å Stokes Profile Associated with Chromospheric Magnetic Reconnection in a Simulated Active Region
Authors: Xinyu Zhou, Takaaki Yokoyama, Haruhisa Iijima, Takuma Matsumoto, Shin Toriumi, Yukio Katsukawa, Masahito Kubo
Figure caption: Temperature of the whole simulation domain at t = 1674 s around reconnection event 2. The yellow box indicates the location of 2D maps in Figure 7.
Paper: Synthetic Ca II 8542 Å Stokes Profile Associated with Chromospheric Magnetic Reconnection in a Simulated Active Region
Authors: Xinyu Zhou, Takaaki Yokoyama, Haruhisa Iijima, Takuma Matsumoto, Shin Toriumi, Yukio Katsukawa, Masahito Kubo
Figure caption: Stokes signals and simulation data around reconnection event 2 at t = 1826 s organized similar to Figure 4.
Paper: A Search for Minute-timescale Flares from the Transient AT 2024wpp
Authors: Eran O. Ofek, Lior Ozer, Ruslan Konno, Nimrod Strasman, Ping Chen, Sagi Ben-Ami, David Polishook, Alexander Krassilchtchikov, Simone Garrappa, Erez A. Zimmermann, Enrico Segre, Asaf Horowicz, Avishay Gal-Yam, Yarin M. Shani, Stanislav Fainer, Michael Engel, Yahel Sofer-Rimalt, Anna Y. Q. Ho, Yossi Shvartzvald, Ofer Yaron, Kris Rybicki, Arie Blumenzweig, Sarah Spitzer, Ron Arad
Figure caption: The distribution of the ZOGY transient detection statistics S of the image-subtraction process (in units of Gaussian σ). The red curves present the null-hypothesis theoretical expectation of a Gaussian with zero mean and unit standard deviation. The right panel shows the distribution for all the data points, while the left panel is for data points obtained more than 40 days after JD 2460579.0. See the main text for discussion.
Paper: A Search for Minute-timescale Flares from the Transient AT 2024wpp
Authors: Eran O. Ofek, Lior Ozer, Ruslan Konno, Nimrod Strasman, Ping Chen, Sagi Ben-Ami, David Polishook, Alexander Krassilchtchikov, Simone Garrappa, Erez A. Zimmermann, Enrico Segre, Asaf Horowicz, Avishay Gal-Yam, Yarin M. Shani, Stanislav Fainer, Michael Engel, Yahel Sofer-Rimalt, Anna Y. Q. Ho, Yossi Shvartzvald, Ofer Yaron, Kris Rybicki, Arie Blumenzweig, Sarah Spitzer, Ron Arad
Figure caption: The ZTF g (blue circles) and r (red circles) light curve of AT 2024wpp. Time is measured relative to JD 2460579, which is the approximate time of zero flux. The triangles mark 3σ upper limits on the magnitude. The red line shows the r-band light curve of AT 2018cow (adopted from D. A. Perley et al. 2019). The light curve is scaled to the distance modulus of AT 2024wpp (added 4.0558 mag) and the time is relative to JD 2458301.7674.
Paper: A Search for Minute-timescale Flares from the Transient AT 2024wpp
Authors: Eran O. Ofek, Lior Ozer, Ruslan Konno, Nimrod Strasman, Ping Chen, Sagi Ben-Ami, David Polishook, Alexander Krassilchtchikov, Simone Garrappa, Erez A. Zimmermann, Enrico Segre, Asaf Horowicz, Avishay Gal-Yam, Yarin M. Shani, Stanislav Fainer, Michael Engel, Yahel Sofer-Rimalt, Anna Y. Q. Ho, Yossi Shvartzvald, Ofer Yaron, Kris Rybicki, Arie Blumenzweig, Sarah Spitzer, Ron Arad
Figure caption: Histogram of the number of LAST visits (a sequence of 20 × 20 s exposures) of AT 2024wpp, as a function of the time relative to the transient approximate zero-flux date (JD = 2460579). Bin size is 5 days. This includes visits that were taken by different telescopes at the same time.
Paper: A Search for Minute-timescale Flares from the Transient AT 2024wpp
Authors: Eran O. Ofek, Lior Ozer, Ruslan Konno, Nimrod Strasman, Ping Chen, Sagi Ben-Ami, David Polishook, Alexander Krassilchtchikov, Simone Garrappa, Erez A. Zimmermann, Enrico Segre, Asaf Horowicz, Avishay Gal-Yam, Yarin M. Shani, Stanislav Fainer, Michael Engel, Yahel Sofer-Rimalt, Anna Y. Q. Ho, Yossi Shvartzvald, Ofer Yaron, Kris Rybicki, Arie Blumenzweig, Sarah Spitzer, Ron Arad
Figure caption: Example of new, reference, and subtraction (D) images (left to right) of AT 2024wpp. The transient position is marked with a 10″ radius red circle.
Paper: A Search for Minute-timescale Flares from the Transient AT 2024wpp
Authors: Eran O. Ofek, Lior Ozer, Ruslan Konno, Nimrod Strasman, Ping Chen, Sagi Ben-Ami, David Polishook, Alexander Krassilchtchikov, Simone Garrappa, Erez A. Zimmermann, Enrico Segre, Asaf Horowicz, Avishay Gal-Yam, Yarin M. Shani, Stanislav Fainer, Michael Engel, Yahel Sofer-Rimalt, Anna Y. Q. Ho, Yossi Shvartzvald, Ofer Yaron, Kris Rybicki, Arie Blumenzweig, Sarah Spitzer, Ron Arad
Figure caption: Histogram of the renormalized mean S values in 10 minute time bins.
Paper: A Search for Minute-timescale Flares from the Transient AT 2024wpp
Authors: Eran O. Ofek, Lior Ozer, Ruslan Konno, Nimrod Strasman, Ping Chen, Sagi Ben-Ami, David Polishook, Alexander Krassilchtchikov, Simone Garrappa, Erez A. Zimmermann, Enrico Segre, Asaf Horowicz, Avishay Gal-Yam, Yarin M. Shani, Stanislav Fainer, Michael Engel, Yahel Sofer-Rimalt, Anna Y. Q. Ho, Yossi Shvartzvald, Ofer Yaron, Kris Rybicki, Arie Blumenzweig, Sarah Spitzer, Ron Arad
Figure caption: Histogram of the 5σ Bp limiting magnitude in the 10 minute time bins.
Paper: Learning to Estimate Photospheric Vector Fields from Line-of-sight Magnetograms
Authors: David Fouhey, KD Leka
Figure caption: Left panel: HMI Blos/μ from the hmi.M_720s series for NOAA AR 13667, 2024 May 7. Located in the far northeast of the solar disk, the apparent polarity inversion line cuts across the middle of the sunspot. Continuum image is from the hmi.Ic_noLimbDark_720s series, isocontours indicate a positive/negative line-of-sight field including the “μ-correction.” Middle panel: HMI vector field data from the hmi.B_720s series showing isocontours of the positive/negative radial field BR and the horizontal components Bϕ , Bθ as vectors, with every third vector displayed for visualization. Right panel: SSLOS plotted similarly. Sharp-eyed viewers may notice the bottom-left-pixel of SSLOS has a strong vertically oriented vector; this is a scaling reference, and all comparison plots will include this small artifact, which forces the vector-lengths to be comparable between the two plots. For all, axes are in arcseconds from image center, contours of μ are shown (as labeled), and the gray contours indicate the smoothed “polarity inversion line” where the (line of sight or BR ) field changes from positive to negative. SSLOS produces the full vector field on-par with HMI vector field data, both being significantly different from the HMI Blos/μ field.
Paper: Learning to Estimate Photospheric Vector Fields from Line-of-sight Magnetograms
Authors: David Fouhey, KD Leka
Figure caption: Full vector magnetic field for the 2024 May storm-producing active regions. Top panels: 2024 May 7; bottom panels: 2024 May 10. Left panels: context image showing NOAA ARs 13664 and 13668, with isocontours of Bz blue (negative) and red (positive) over a continuum image (which includes limb-darkening), and contour(s) of μ. A small region of interest (ROI) is outlined in yellow. Middle panels: the full vector field from HMI for the ROI, the same format as Figure 9, except that for clarity, we do not include the underlying continuum image. Right panels: same, for SSLOS. On May 7 (top panel), SSLOS’s reconstruction is largely correct, and recovers the general nonpotential field structures. On May 10 (bottom panel), while SSLOS does indicate the presence of complex magnetic structures, it underestimates the field magnitude as well as the degree of shear (deviation from potential). On the other hand, SSLOS avoids the HMI disambiguation “checkerboard” artifacts visible in the bottom left of the HMIP data.
Paper: Learning to Estimate Photospheric Vector Fields from Line-of-sight Magnetograms
Authors: David Fouhey, KD Leka
Figure caption: Bivariate log-histograms of Bϕ and Bθ produced by SSLOS with input from SDO/HMI (top row) and NSO/GONG (bottom row) Blos. The method largely does a good job with relatively few polarity confusions. Color map: empty bins are colored white; non-empty bins follow lowest  highest density. Following Figure 6, each condition (GONG AR/HMI Plage) is color mapped identically.