adsabs/AstroCLIMB huggingface dataset:
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) when using the model without 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: Real vs. synthetic images during a flare (2011-02-15 02:00:00) when using the model without 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: Evaluating the Plausible Range of N2O Biosignatures on Exo-Earths: An Integrated Biogeochemical, Photochemical, and Spectral Modeling Approach
Authors: Edward W. Schwieterman, Stephanie L. Olson, Daria Pidhorodetska, Christopher T. Reinhard, Ainsley Ganti, Thomas J. Fauchez, Sandra T. Bastelberger, Jaime S. Crouse, Andy Ridgwell, Timothy W. Lyons
Figure caption: A concept image illustrating the interpretability of N2O as a biosignature in the context of the planetary environment. The left panel illustrates a scenario like the modern Earth, with a high-oxygen atmosphere and N2O generated overwhelmingly via partial biological denitrification. In this case, the simultaneous presence of O2, O3, N2O, and CH4 indicates a strong chemical disequilibrium. The middle panel illustrates a weakly oxygenated planetary environment like the Proterozoic Earth, with N2O generated both by partial biological denitrification and by chemodenitrification of nitrogenous intermediates (likely substantially biogenic) in a redox stratified ocean. In this case, molecular oxygen (O2) and methane may have concentrations that are too low to detect directly, but detectable N2O and O3 would be a strong biosignature. A false positive is unlikely, because an abiotic O2 atmosphere would be unstable in combination with a reducing ocean. The right panel illustrates the most likely false-positive scenario, where an active star splits N2 via SPEs, resulting in photochemically produced N2O. This scenario would predict additional photochemical products, such as HCN, that would be indicative of abiotic origins. Stellar characterization would confirm the magnitude of the stellar activity. Vigorous atmospheric production of NOx species could be inferred from spectrally active NO2.
Paper: Evaluating the Plausible Range of N2O Biosignatures on Exo-Earths: An Integrated Biogeochemical, Photochemical, and Spectral Modeling Approach
Authors: Edward W. Schwieterman, Stephanie L. Olson, Daria Pidhorodetska, Christopher T. Reinhard, Ainsley Ganti, Thomas J. Fauchez, Sandra T. Bastelberger, Jaime S. Crouse, Andy Ridgwell, Timothy W. Lyons
Figure caption: Gas mixing ratio profiles for (from top to bottom): the Earth orbiting the Sun, an Earthlike planet orbiting the late K-dwarf star HD85512 (K6V), an Earthlike Proxima Centauri b, and an Earthlike TRAPPIST-1e. The N2O profiles assuming fluxes of 1, 10, and 100 Tmol yr−1 are shown. For brevity, not all species are included. All runs assume pO2 = 100% PAL.
Paper: Evaluating the Plausible Range of N2O Biosignatures on Exo-Earths: An Integrated Biogeochemical, Photochemical, and Spectral Modeling Approach
Authors: Edward W. Schwieterman, Stephanie L. Olson, Daria Pidhorodetska, Christopher T. Reinhard, Ainsley Ganti, Thomas J. Fauchez, Sandra T. Bastelberger, Jaime S. Crouse, Andy Ridgwell, Timothy W. Lyons
Figure caption: Simulated thermal emission spectra of (a) an Earth–Sun scenario, (b) an Earth orbiting the late K-dwarf star HD85512 (K6V), (c) an Earthlike Proxima Centauri b, and (d) an Earthlike TRAPPIST-1e. Each figure shows variations in the spectra according to N2O surface fluxes of 1, 10, and 100 Tmol yr−1, using the temperature and gas mixing ratio profiles shown in Figure 9 and assuming 50% cloud cover.
Paper: Evaluating the Plausible Range of N2O Biosignatures on Exo-Earths: An Integrated Biogeochemical, Photochemical, and Spectral Modeling Approach
Authors: Edward W. Schwieterman, Stephanie L. Olson, Daria Pidhorodetska, Christopher T. Reinhard, Ainsley Ganti, Thomas J. Fauchez, Sandra T. Bastelberger, Jaime S. Crouse, Andy Ridgwell, Timothy W. Lyons
Figure caption: Sensitivity test showing the atmospheric mixing ratios of N2O as a function of surface flux for an Earthlike atmosphere with pO2 = 100% PAL and total pressures of 0.5 bar (dotted lines), 1 bar (solid lines), and 10 bar (dashed lines). The total pressures are adjusted by changing the N2 partial pressures, while the O2 partial pressure is fixed at 0.21 bar. N2O mixing ratios are recalculated to reflect the effective mixing ratio if the total pressure were 1 bar.
Paper: Evaluating the Plausible Range of N2O Biosignatures on Exo-Earths: An Integrated Biogeochemical, Photochemical, and Spectral Modeling Approach
Authors: Edward W. Schwieterman, Stephanie L. Olson, Daria Pidhorodetska, Christopher T. Reinhard, Ainsley Ganti, Thomas J. Fauchez, Sandra T. Bastelberger, Jaime S. Crouse, Andy Ridgwell, Timothy W. Lyons
Figure caption: Photochemical reaction rates for the two major N2O destruction pathways as a function of stellar type. The solid lines represent the N2O photolysis rates, while the dotted lines represent the destruction of N2O by singlet oxygen O(1D). The calculations assume pO2 = 100% PAL.
Paper: Evaluating the Plausible Range of N2O Biosignatures on Exo-Earths: An Integrated Biogeochemical, Photochemical, and Spectral Modeling Approach
Authors: Edward W. Schwieterman, Stephanie L. Olson, Daria Pidhorodetska, Christopher T. Reinhard, Ainsley Ganti, Thomas J. Fauchez, Sandra T. Bastelberger, Jaime S. Crouse, Andy Ridgwell, Timothy W. Lyons
Figure caption: A simulated transmission spectrum of TRAPPIST-1e with N2O surface fluxes of 1, 10, and 100 Tmol yr−1, assuming the same gas profiles as shown in Figure 8(d), simulated with PSG. Major spectral features are noted. The top panel shows wavelengths accessible to the JWST NIRSpec instrument, while the bottom panel shows wavelengths accessible to the JWST MIRI instrument.
Paper: Evaluating the Plausible Range of N2O Biosignatures on Exo-Earths: An Integrated Biogeochemical, Photochemical, and Spectral Modeling Approach
Authors: Edward W. Schwieterman, Stephanie L. Olson, Daria Pidhorodetska, Christopher T. Reinhard, Ainsley Ganti, Thomas J. Fauchez, Sandra T. Bastelberger, Jaime S. Crouse, Andy Ridgwell, Timothy W. Lyons
Figure caption: The same as Figures 7 and 8, but for an Earthlike planet with pO2 = 10% PAL.
Paper: Evaluating the Plausible Range of N2O Biosignatures on Exo-Earths: An Integrated Biogeochemical, Photochemical, and Spectral Modeling Approach
Authors: Edward W. Schwieterman, Stephanie L. Olson, Daria Pidhorodetska, Christopher T. Reinhard, Ainsley Ganti, Thomas J. Fauchez, Sandra T. Bastelberger, Jaime S. Crouse, Andy Ridgwell, Timothy W. Lyons
Figure caption: A simulated transmission spectrum of the Earthlike TRAPPIST-1e case, with a flux of 100 Tmol yr−1 N2O. The top panel shows simulated 5σ error envelopes, as calculated with PSG, assuming 40 coadded transits with the JWST NIRSpec instrument. The bottom panel shows the influence of N2O on the spectral features of the top panel.
Paper: Evaluating the Plausible Range of N2O Biosignatures on Exo-Earths: An Integrated Biogeochemical, Photochemical, and Spectral Modeling Approach
Authors: Edward W. Schwieterman, Stephanie L. Olson, Daria Pidhorodetska, Christopher T. Reinhard, Ainsley Ganti, Thomas J. Fauchez, Sandra T. Bastelberger, Jaime S. Crouse, Andy Ridgwell, Timothy W. Lyons
Figure caption: The same as Figure 7, but for an Earthlike planet with pO2 = 50% PAL.
Paper: Gravitational Wave Sources in Our Galactic Backyard: Predictions for BHBH, BHNS, and NSNS Binaries Detectable with LISA
Authors: T. Wagg, F. S. Broekgaarden, S. E. de Mink, N. Frankel, L. A. C. van Son, S. Justham
Figure caption: Fraction of each DCO type that is formed through different formation channels for all physics variations. Channels are described in detail in Broekgaarden et al. (2021). The classic, single-core common-envelope event and double-core common-envelope event channels all require at least one common-envelope event, while only “only stable” consists of only stable mass transfer, and “other” contains the remaining binaries, which are mainly formed from case A classic binaries as well as lucky SN kicks that shrink the binary. </>
Paper: Gravitational Wave Sources in Our Galactic Backyard: Predictions for BHBH, BHNS, and NSNS Binaries Detectable with LISA
Authors: T. Wagg, F. S. Broekgaarden, S. E. de Mink, N. Frankel, L. A. C. van Son, S. Justham
Figure caption: As the bottom panels of Figure 2, but without the density distributions, and scatter points are colored by their eccentricity. We show that eccentric sources are located in an offshoot below the 30 kpc around 2 mHz. </>
Paper: Gravitational Wave Sources in Our Galactic Backyard: Predictions for BHBH, BHNS, and NSNS Binaries Detectable with LISA
Authors: T. Wagg, F. S. Broekgaarden, S. E. de Mink, N. Frankel, L. A. C. van Son, S. Justham
Figure caption: As Figure 3, but for the properties of the detectable systems at DCO formation. </>
Paper: CLEAR: The Ionization and Chemical-enrichment Properties of Galaxies at 1.1 < z < 2.3
Authors: Casey Papovich, Raymond C. Simons, Vicente Estrada-Carpenter, Jasleen Matharu, Ivelina Momcheva, Jonathan R. Trump, Bren E. Backhaus, Gabriel Brammer, Nikko J. Cleri, Steven L. Finkelstein, Mauro Giavalisco, Zhiyuan Ji, Intae Jung, Lisa J. Kewley, David C. Nicholls, Norbert Pirzkal, Marc Rafelski, Benjamin Weiner
Figure caption: The stellar-mass, ionization relation (MQR) for CLEAR galaxies at 1.1 < z < 2.3. The top plot shows the MQR with the CLEAR galaxies color-coded by redshift. Large squares show medians in bins of stellar mass. The error bars show the scatter in each bin. The shaded region denotes the SDSS galaxy distribution of ionization parameters derived using our analysis (identical to that applied to the CLEAR galaxies). The solid lines show analytic fits to the data for the SDSS (black), CLEAR z = 1.3 (blue), and CLEAR z = 1.8 samples. The bottom panels show the MQR with galaxies color-coded by specific SFR (bottom left; log sSFR ) and gas-phase metallicity, ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩.
Paper: CLEAR: The Ionization and Chemical-enrichment Properties of Galaxies at 1.1 < z < 2.3
Authors: Casey Papovich, Raymond C. Simons, Vicente Estrada-Carpenter, Jasleen Matharu, Ivelina Momcheva, Jonathan R. Trump, Bren E. Backhaus, Gabriel Brammer, Nikko J. Cleri, Steven L. Finkelstein, Mauro Giavalisco, Zhiyuan Ji, Intae Jung, Lisa J. Kewley, David C. Nicholls, Norbert Pirzkal, Marc Rafelski, Benjamin Weiner
Figure caption: Comparison of the properties of galaxies in the high-ionization subsample (﹩\mathrm{log}q/[\mathrm{cm}\,{{\rm{s}}}^{-1}]\gt 7.8)﹩ compared to the low-ionization subsample (﹩\mathrm{log}q/[\mathrm{cm}\,{{\rm{s}}}^{-1}]\lt 7.8)﹩. The top panel shows the stacked G102 and G141 spectra for each sample (as labeled). Prominent emission features are indicated. All galaxies were selected to have stellar mass ﹩9.3\lt \mathrm{log}M/{M}_{\odot }\lt 9.7﹩ and ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})\gt 8.3﹩. The bottom panels show distributions of the galaxy properties in each subsample from this selection, including stellar masses and specific SFRs (derived from SED fitting), the gas-phase metallicities (derived from the emission-line analysis), and extinction (derived from the observed Hα/Hβ ratios). The stellar masses and metallicities are similar between the samples, while the sSFR shows differences (see discussion in the text).
Paper: CLEAR: The Ionization and Chemical-enrichment Properties of Galaxies at 1.1 < z < 2.3
Authors: Casey Papovich, Raymond C. Simons, Vicente Estrada-Carpenter, Jasleen Matharu, Ivelina Momcheva, Jonathan R. Trump, Bren E. Backhaus, Gabriel Brammer, Nikko J. Cleri, Steven L. Finkelstein, Mauro Giavalisco, Zhiyuan Ji, Intae Jung, Lisa J. Kewley, David C. Nicholls, Norbert Pirzkal, Marc Rafelski, Benjamin Weiner
Figure caption: Relation between the specific SFR derived from SED fitting (see Section 2.5) and the gas-phase ionization for CLEAR galaxies (see Section 4.2). The right axis shows the equivalent dimensionless ionization parameter, U ≡ q/c. The CLEAR galaxies are color-coded by redshift; large squares show medians binned by sSFR (error bars show errors on the median). The CLEAR sample includes all galaxies with stellar masses, ﹩\mathrm{log}M/{M}_{\odot }=[9.2,10.2]﹩. The dashed line is a linear fit to the CLEAR galaxies. The thick, solid line shows the fit to a subsample with an additional, log sSFR/yr−1 > −9.5 (the light solid lines show 500 random draws from the posterior). The large yellow pentagons show measurements for higher–mass galaxies at z ∼ 1.5 (﹩\mathrm{log}{M}_{* }/{M}_{\odot }=10.4\mbox{--}11﹩; Kaasinen et al. 2018). There is evidence of a correlation between sSFR and gas ionization. The trend becomes stronger when considering sSFR as traced by the Hβ emission EW (Section 6.4).
Paper: CLEAR: The Ionization and Chemical-enrichment Properties of Galaxies at 1.1 < z < 2.3
Authors: Casey Papovich, Raymond C. Simons, Vicente Estrada-Carpenter, Jasleen Matharu, Ivelina Momcheva, Jonathan R. Trump, Bren E. Backhaus, Gabriel Brammer, Nikko J. Cleri, Steven L. Finkelstein, Mauro Giavalisco, Zhiyuan Ji, Intae Jung, Lisa J. Kewley, David C. Nicholls, Norbert Pirzkal, Marc Rafelski, Benjamin Weiner
Figure caption: Comparison between Hβ EW and gas ionization parameter, ﹩\mathrm{log}q﹩, for CLEAR galaxies in the high-ionization (﹩\mathrm{log}q\gt 7.8﹩) and low-ionization subsamples (﹩\mathrm{log}q\lt 7.8﹩). The left panel shows the measured [O III]/[O II] emission-line ratio against the Hβ EW measured from the stacks (large red squares), and individual points (gray downward/upward triangles show galaxies in the low-/high-ionization subsamples, respectively). The contours encompass 50th and 84th percentiles for each sample. The other large symbols show values derived from Hγ, scaled by the Case-B ratio to Hβ. The dashed line is a linear fit to the stacked measurements. The right panel shows the same distribution against the ionization parameter ﹩\mathrm{log}q﹩. Because the Balmer emission EW scales with specific SFR, the plots show strong evidence between ionization (and ionization parameter) and specific SFR galaxies at z ∼ 1–2.
Paper: CLEAR: The Ionization and Chemical-enrichment Properties of Galaxies at 1.1 < z < 2.3
Authors: Casey Papovich, Raymond C. Simons, Vicente Estrada-Carpenter, Jasleen Matharu, Ivelina Momcheva, Jonathan R. Trump, Bren E. Backhaus, Gabriel Brammer, Nikko J. Cleri, Steven L. Finkelstein, Mauro Giavalisco, Zhiyuan Ji, Intae Jung, Lisa J. Kewley, David C. Nicholls, Norbert Pirzkal, Marc Rafelski, Benjamin Weiner
Figure caption: Examples of galaxies in CLEAR at 1.1 < z < 1.5 that have gas-phase metallicities derived using [O II], [O III], Hβ, Hα+[N II], and [S II] that are substantially lower than those derived using [O II], [O III], and Hβ alone. Each row shows one galaxy in our sample (with ID, spectroscopic redshift from the grism data, and stellar mass as indicated). The left panel in each row shows the WFC3 G102 (blue) and G141 (red) 1D extracted spectra. The dashed lines indicate strong emission lines (Hα includes [N II], which is blended at the grism resolution). The middle and right panels show the posterior likelihoods for the gas-phase metallicity, P(12 + logO/H), and ionization parameter, ﹩P(\mathrm{log}q)﹩, derived using only [O II], [O III], and Hβ (shown in tan) compared to those derived using [O II], [O III], Hβ, Hα+[N II], and [S II] (shown in light blue). The likelihoods on the ionization parameters are nearly identical, showing these are strongly constrained by [O II] and [O III]. The posterior likelihood for metallicity for these galaxies shifts to the “lower branch” of the relation when Hα+[N II] and [S II] are included.
Paper: CLEAR: The Ionization and Chemical-enrichment Properties of Galaxies at 1.1 < z < 2.3
Authors: Casey Papovich, Raymond C. Simons, Vicente Estrada-Carpenter, Jasleen Matharu, Ivelina Momcheva, Jonathan R. Trump, Bren E. Backhaus, Gabriel Brammer, Nikko J. Cleri, Steven L. Finkelstein, Mauro Giavalisco, Zhiyuan Ji, Intae Jung, Lisa J. Kewley, David C. Nicholls, Norbert Pirzkal, Marc Rafelski, Benjamin Weiner
Figure caption: Comparison of [Ne III]/[O II] emission-line ratios and gas-phase metallicity (12 ﹩+\mathrm{log}﹩ O/H) derived for CLEAR galaxies and published relations from the literature. The data points show mean metallicities for the CLEAR samples and emission-line ratios derived from the stacked spectra. The filled circles show values derived for galaxies in bins of stellar mass (see Section 3). The large squares show values derived for mass-matched samples at high and low ionization (﹩\mathrm{log}q/[\mathrm{cm}\,{{\rm{s}}}^{-1}]\gt 7.8﹩ and <7.8, respectively; see Section 6.3), where there is no indication the [Ne III]/[O II] ratios are substantially different in these samples (as would be expected if they had significantly different metallicities; see, e.g., Sanders et al. 2021). The models also include analogs of z ∼ 2 galaxies (Bian et al. 2018), calibrations to SDSS at z ∼ 0 and higher redshifts (Maiolino et al. 2008; Curti et al. 2017; Pérez-Montero et al. 2021).
Paper: CLEAR: The Ionization and Chemical-enrichment Properties of Galaxies at 1.1 < z < 2.3
Authors: Casey Papovich, Raymond C. Simons, Vicente Estrada-Carpenter, Jasleen Matharu, Ivelina Momcheva, Jonathan R. Trump, Bren E. Backhaus, Gabriel Brammer, Nikko J. Cleri, Steven L. Finkelstein, Mauro Giavalisco, Zhiyuan Ji, Intae Jung, Lisa J. Kewley, David C. Nicholls, Norbert Pirzkal, Marc Rafelski, Benjamin Weiner
Figure caption: Gas-phase metallicities and ionization parameters for CLEAR galaxies. The top panel shows the data with large squares denoting the CLEAR galaxies (colored by specific SFR). Smaller points show measurements from MOSDEF (Topping et al. 2020). The dashed lines show the range of parameter space covered by nearby H II regions Pérez-Montero (2014). The thick solid lines shows measurements for resolved H II regions in CALIFA galaxies (Espinosa-Ponce et al. 2022). The right axis shows the equivalent dimensionless ionization parameter, U ≡ q/c. The bottom panel shows the same information with a KDE derived distribution (for both the MOSDEF and CLEAR samples).
Paper: CLEAR: The Ionization and Chemical-enrichment Properties of Galaxies at 1.1 < z < 2.3
Authors: Casey Papovich, Raymond C. Simons, Vicente Estrada-Carpenter, Jasleen Matharu, Ivelina Momcheva, Jonathan R. Trump, Bren E. Backhaus, Gabriel Brammer, Nikko J. Cleri, Steven L. Finkelstein, Mauro Giavalisco, Zhiyuan Ji, Intae Jung, Lisa J. Kewley, David C. Nicholls, Norbert Pirzkal, Marc Rafelski, Benjamin Weiner
Figure caption: Comparison of gas-phase metallicities (12 + log O/H) (left) and ionization parameters, ﹩\mathrm{log}q﹩, (right) derived using [O II], [O III], Hβ, Hα+[N II] (which are blended at the resolution of the WFC3 grism) and [S II] (if present) (on the abscissa), vs. fits using only with [O II], [O III], and Hβ (on the ordinate). The data points show the mode of the metallicity likelihood function, and the error bars show the inter-68th percentile derived from the HDI. The dashed line shows the unity relation. The majority of data points have metallicities and ionization parameters that are consistent between the two methods. In a small number of cases (10 out of 87), the metallicities derived including Hα+[N II] and [S II] favor lower gas-phase metallicities. This illustrates that for objects on the lower branch of the R 23 relation, additional information may be required to understand their gas-phase metallicities.
Paper: CLEAR: The Ionization and Chemical-enrichment Properties of Galaxies at 1.1 < z < 2.3
Authors: Casey Papovich, Raymond C. Simons, Vicente Estrada-Carpenter, Jasleen Matharu, Ivelina Momcheva, Jonathan R. Trump, Bren E. Backhaus, Gabriel Brammer, Nikko J. Cleri, Steven L. Finkelstein, Mauro Giavalisco, Zhiyuan Ji, Intae Jung, Lisa J. Kewley, David C. Nicholls, Norbert Pirzkal, Marc Rafelski, Benjamin Weiner
Figure caption: Zoom-in on spectroscopic features in the high-ionization subsample (﹩\mathrm{log}q/[\mathrm{cm}\,{{\rm{s}}}^{-1}]\gt 7.8)﹩ compared to those in the low-ionization subsample (﹩\mathrm{log}q/[\mathrm{cm}\,{{\rm{s}}}^{-1}]\lt 7.8)﹩ from Figure 15. The top panel shows both stacked spectra. The bottom panel shows the percent difference. The Hβ and Hγ features (labeled in bold) are the most isolated at the resolution of the G102 and G141 grisms (i.e., they are not blended with other possible features). These lines all show excess emission of 20%–30% in the high-ionization subsample compared to the low-ionization subsample. This is evidence that higher-ionization galaxies have higher specific SFRs.
Paper: Spatial Scales and Time Variation of Solar Subsurface Convection
Authors: Alexander V. Getling, Alexander G. Kosovichev
Figure caption: Solid curves (in all panels but the last one): the l-variation of the power p  l , based on the above-displayed spectra for different depths (the low-activity period; Figure 5); the dotted curves indicate the standard deviation of p  l  from its running average, while the dashed curves indicate the total power, ﹩{p}_{l}^{{\rm{\Sigma }}}﹩. The depth values are indicated at the top of each panel. The bottom right panel shows the p  l  curves obtained for a velocity divergence field at d = 0.5 Mm, averaged with Gaussians corresponding to the helioseismic averaging kernels of two different widths, w.
Paper: Relationship between Successive Flares in the Same Active Region and SHARP Parameters
Authors: Hao Ran, Ying D. Liu, Yang Guo, Rui Wang
Figure caption: Scatterplot of the average and variance of the correlation coefficients between the SHARP parameters and the flare envelope. The left panel refers to the whole AR case, and the right panel refers to the PIL-modified case. The x-axis represents the average value, and y-axis represents the variance value. A parameter has a better performance if it is closer to the lower right corner of the figure. Inside the blue ellipse are the parameters that we think have the best performance in correlation.
Paper: Spatial Scales and Time Variation of Solar Subsurface Convection
Authors: Alexander V. Getling, Alexander G. Kosovichev
Figure caption: Time variations of the total power of all the harmonics of the unmasked fields (solid curves) and masked fields (dashed curves) for all the depths considered (indicated at the top of each panel). Left: unfiltered; right: filtered by applying the Butterworth filter, with f H = 14, n = 4. The red curve in each panel represents the monthly average sunspot number.
Paper: Spatial Scales and Time Variation of Solar Subsurface Convection
Authors: Alexander V. Getling, Alexander G. Kosovichev
Figure caption: The effect of narrowing the source field sector. The l-averaged (solid curves) and l-summed (dashed curves) spectra are shown for divergence fields at d = 6 Mm, differently chosen for spherical harmonic transform: triplicate 120° wide fields (left); quadruplicate 90° wide fields of the (−45°, +45°) sector (middle); quadruplicate 90° wide field of the (−60°, +30°) sector (right). Top: the low-activity period, from 2019 December 21 to 2020 February 4; bottom: the high-activity period, from 2013 December 21 to 2014 February 4.