adsabs/AstroCLIMB huggingface dataset:
Paper: The First Catalog of Candidate White Dwarf–Main-sequence Binaries in Open Star Clusters: A New Window into Common Envelope Evolution
Authors: Steffani M. Grondin, Maria R. Drout, Jason Nordhaus, Philip S. Muirhead, Joshua S. Speagle, 佳士 沈, Ryan Chornock
Figure caption: Photometric properties of our catalog of 52 high-probability (P > 0.9) candidate WD+MS binaries (stars). Each system is colored by its SVM probability. Four high-probability candidates with spectroscopy and/or a light curve discussed in Section 5 in this paper are numbered (1) Alessi12-c1, (2) Pleiades-c1, (3) Pleiades-c2, and (4) Pleiades-c3. The MS cluster training data (gray) and the A. Rebassa-Mansergas et al. (2010) SDSS WD+MS sample (purple) are also shown for reference. Note that the WD+MS training data used in our SVM (only Class 1 WD+MS binaries; see Section 3.2.2) is indicated in plum, whereas the full A. Rebassa-Mansergas et al. (2010) sample (including both Class 1 and Class 2 WD+MS systems) is indicated in light purple. While the systems in our catalog generally overlap with the SDSS binaries, our candidates lie closer on average to the ZAMS in a Gaia CMD and some example color–color spaces.
Paper: The First Catalog of Candidate White Dwarf–Main-sequence Binaries in Open Star Clusters: A New Window into Common Envelope Evolution
Authors: Steffani M. Grondin, Maria R. Drout, Jason Nordhaus, Philip S. Muirhead, Joshua S. Speagle, 佳士 沈, Ryan Chornock
Figure caption: Color–color and color–magnitude spaces of a variety of astrophysical sources with similar photometry to SDSS WD+MS binaries in A. Rebassa-Mansergas et al. (2010). Here, we show rapidly rotating M dwarfs (red-filled triangles) from E. Kado-Fong et al. (2016), CVs (gold-filled hexagons) from K. Inight et al. (2023), and single WDs (blue-filled diamonds) from N. P. Gentile Fusillo et al. (2021) relative to our high-probability candidate WD+MS binaries (orange stars) and our training samples (SDSS WD+MS binaries from A. Rebassa-Mansergas et al. 2010 and a set of MS cluster members from T. Cantat-Gaudin et al. 2020 as purple- and gray-filled circles, respectively). We conclude that our catalog is unlikely to have any significant contamination from single WDs, but our sample may contain CVs (in addition to detached WD+MS binaries). Some contamination from young, active M dwarfs is possible for systems in our catalog that lie close the the ZAMS.
Paper: The First Catalog of Candidate White Dwarf–Main-sequence Binaries in Open Star Clusters: A New Window into Common Envelope Evolution
Authors: Steffani M. Grondin, Maria R. Drout, Jason Nordhaus, Philip S. Muirhead, Joshua S. Speagle, 佳士 沈, Ryan Chornock
Figure caption: The proposed effect of a CE natal velocity kick on the spatial position and kinematics of candidate NGC 1342-c1. Left: spatial location of NGC 1342-c1 (star) relative to high-probability cluster stars from T. Cantat-Gaudin et al. (2020; gray). Each circle represents the distance NGC 1342-c1 would be located if it received a natal kick for various kick magnitudes and travel times. Right: similar to the left panel, however with proper motion. Each circle here represents the change in NGC 1342-c1's proper motion (Δμ) upon receiving a velocity kick completely imparted into the tangential direction (for simplicity).
Paper: The First Catalog of Candidate White Dwarf–Main-sequence Binaries in Open Star Clusters: A New Window into Common Envelope Evolution
Authors: Steffani M. Grondin, Maria R. Drout, Jason Nordhaus, Philip S. Muirhead, Joshua S. Speagle, 佳士 沈, Ryan Chornock
Figure caption: Raw and phase-folded light curves for three high-probability WD+MS binary candidates. Left panels: Alessi12-c1; r-band light curve obtained from the ZTF. The period of 0.29 day is computed using a a Lomb–Scargle periodogram where the phase-folded light curve corresponds to the period of maximum power in the periodogram. Middle panels: Pleiades-c2; light curve obtained from Kepler/K2 archival data. The period of 0.29 day is computed from a periodogram with default LightKurve settings. Right panels: Pleiades-c3; light curve obtained from TESS archival data. The period of 6.41 days is also computed from a periodogram with default LightKurve settings.
Paper: The First Catalog of Candidate White Dwarf–Main-sequence Binaries in Open Star Clusters: A New Window into Common Envelope Evolution
Authors: Steffani M. Grondin, Maria R. Drout, Jason Nordhaus, Philip S. Muirhead, Joshua S. Speagle, 佳士 沈, Ryan Chornock
Figure caption: A 3D spatial and 2D kinematic χ 2 association for two candidate WD+MS binaries in NGC 2287. NGC 2287-c1 (filled triangle) and NGC 2287-c2 (filled hexagon) are shown relative to high-probability cluster members in T. Cantat-Gaudin et al. (2020). Each source is colored by its χ 2 value, where the spatial χ 2 is computed using R.A. (α), decl. (δ), and parallax (π), whereas the kinematic χ 2 is computed from proper motions (μ  α , μ  δ ). Both of these candidates fall into the “Tier 1” category for cluster membership since they are both spatially and kinematically consistent with their host cluster.
Paper: The First Catalog of Candidate White Dwarf–Main-sequence Binaries in Open Star Clusters: A New Window into Common Envelope Evolution
Authors: Steffani M. Grondin, Maria R. Drout, Jason Nordhaus, Philip S. Muirhead, Joshua S. Speagle, 佳士 沈, Ryan Chornock
Figure caption: Photometric errors of the high-probability candidate WD+MS binaries in this catalog.
Paper: The First Catalog of Candidate White Dwarf–Main-sequence Binaries in Open Star Clusters: A New Window into Common Envelope Evolution
Authors: Steffani M. Grondin, Maria R. Drout, Jason Nordhaus, Philip S. Muirhead, Joshua S. Speagle, 佳士 沈, Ryan Chornock
Figure caption: NGC 2682: a cluster with no identified high-probability or mid-probability candidate WD+MS binaries.
Paper: The First Catalog of Candidate White Dwarf–Main-sequence Binaries in Open Star Clusters: A New Window into Common Envelope Evolution
Authors: Steffani M. Grondin, Maria R. Drout, Jason Nordhaus, Philip S. Muirhead, Joshua S. Speagle, 佳士 沈, Ryan Chornock
Figure caption: Alessi 12: a cluster with both high-probability and mid-probability candidate WD+MS binaries.
Paper: Whole-disk Sampling of Molecular Clouds in M83
Authors: Akihiko Hirota, Jin Koda, Fumi Egusa, Tsuyoshi Sawada, Kazushi Sakamoto, Mark Heyer, Amanda M Lee, Fumiya Maeda, Samuel Boissier, Daniela Calzetti, Bruce G. Elmegreen, Nanase Harada, Luis C. Ho, Masato I. N. Kobayashi, Nario Kuno, Barry F. Madore, Sergio Martín, Jennifer Donovan Meyer, Kazuyuki Muraoka, Yoshimasa Watanabe
Figure caption: Scaling relations of cloud properties. In each plot, the density distribution of the clouds at the 20% level of the maximum density is shown for M83 clouds with the black contour and for the Galactic clouds of S87, R16, and M17 with green, purple, and blue contours, respectively. For the Galactic catalogs of S87, R16, and M17, we excluded the clouds with the Galactocentric of R gal > 8.5 kpc and the Galactic longitude l within ∣l∣ < 5°. The former filtering is made to compare clouds among molecular-dominated environments, as in the disk of M83. The latter is to exclude the Galactic Center clouds. In the top and bottom rows, the Galactic clouds with the kinematic distance at D kin < 8.5 kpc and D kin > 8.5 kpc are shown, respectively. (a), (e) σ v–R eff relationship. The black dashed line indicates the σ v–R eff relation of S87, which is Equation (9) with C = 0.72 km s−1 pc−1/2. The purple and blue dotted lines indicate the relations reported in R16 and M17, respectively. (b), (f) M vir–L CO relationship. The dotted and dashed–dotted lines indicate α vir of 1 and 4, respectively. (c), (g) M cl–R eff relationship. The dotted lines indicate the lines for Σ of 1, 10, 100, and 1000 M ⊙ pc−2, respectively. (d), (h) ﹩{\sigma }_{{\rm{v}}}/{R}_{\mathrm{eff}}^{1/2}﹩–Σ relationship. The dotted and dashed–dotted lines indicate α vir of 1 and 4, respectively.
Paper: Whole-disk Sampling of Molecular Clouds in M83
Authors: Akihiko Hirota, Jin Koda, Fumi Egusa, Tsuyoshi Sawada, Kazushi Sakamoto, Mark Heyer, Amanda M Lee, Fumiya Maeda, Samuel Boissier, Daniela Calzetti, Bruce G. Elmegreen, Nanase Harada, Luis C. Ho, Masato I. N. Kobayashi, Nario Kuno, Barry F. Madore, Sergio Martín, Jennifer Donovan Meyer, Kazuyuki Muraoka, Yoshimasa Watanabe
Figure caption: (a) ﹩{\sigma }_{{\rm{v}}}/\sqrt{{R}_{\mathrm{eff}}}﹩–Σ relationship for clouds in M83. Cyan and gray markers indicate the clouds with T peak above and below 2 K, respectively. White circle markers with black outline indicate the running median of ﹩{\sigma }_{{\rm{v}}}/\sqrt{{R}_{\mathrm{eff}}}﹩–Σ. The dotted line indicates a state of virial equilibrium, α vir = 1. The red thick line shows the expected range of variation for clouds that have α vir = 1 and a constant intrinsic surface density Σ0 of 160 M ⊙ pc−2 but are affected by the beam dilution with f of <1. (b) α vir–M cl relationship for clouds in M83. The running median of α vir and fitted to the median values are displayed similarly to (a). The red line indicates the minimum α vir expected from Equation (C1) by setting σ v to be 1 / ﹩\sqrt{12}﹩ km s−1, which is the instrumental limit of the data, and T peak of 0.5 K, which is the near the detection limit of the clouds. Most clouds are located well above the line, indicating that the velocity resolution is not driving the observed M cl-dependence of α vir. The marker colors are coded to express the variation in ﹩{\sigma }_{{\rm{v}}}^{2}/{{\rm{\Sigma }}}^{1/2}﹩.
Paper: Whole-disk Sampling of Molecular Clouds in M83
Authors: Akihiko Hirota, Jin Koda, Fumi Egusa, Tsuyoshi Sawada, Kazushi Sakamoto, Mark Heyer, Amanda M Lee, Fumiya Maeda, Samuel Boissier, Daniela Calzetti, Bruce G. Elmegreen, Nanase Harada, Luis C. Ho, Masato I. N. Kobayashi, Nario Kuno, Barry F. Madore, Sergio Martín, Jennifer Donovan Meyer, Kazuyuki Muraoka, Yoshimasa Watanabe
Figure caption: Simulation results of the source injection test made with the noise-only setup, which uses a CO emission-free portion of the data cube. (a) Integrated CO intensity image of the data used in one of the 40 rounds of the test. In the image, five sources with M cl of 0.5, 1, 2, 4, and 8 × 105 M ⊙ are injected. The red dotted markers indicate the positions of the input sources. Yellow ellipses indicate the output FWHM sizes of the detected sources. (b) Detection rate as a function of the input M cl. (c) Output-to-input ratios of M cl for the detected sources as a function of the input M cl. The black dotted horizontal line indicates the output-to-input ratio of 1. Gray dots indicate each of the detected clouds in each round. Open markers indicate the median output-to-input ratios for each input M cl with error bars showing the 16th-to-84th percentiles range. (d) Same as (c), but for R eff. The blue dashed line indicates the line of θ b/θ source, where θ b and θ source are the FWHM sizes of the beam (∼46 pc) and the input model sources, respectively. (e) Same as (c), but for σ v. (f) α vir–Σ relationship of the detected sources. The vertical and horizontal dotted lines indicate Σ of 100 M ⊙ pc−2 and α vir of 1.5 uniformly assigned to all the input sources. The dashed line indicates the relation of α vir ∝ Σ−0.5.
Paper: Whole-disk Sampling of Molecular Clouds in M83
Authors: Akihiko Hirota, Jin Koda, Fumi Egusa, Tsuyoshi Sawada, Kazushi Sakamoto, Mark Heyer, Amanda M Lee, Fumiya Maeda, Samuel Boissier, Daniela Calzetti, Bruce G. Elmegreen, Nanase Harada, Luis C. Ho, Masato I. N. Kobayashi, Nario Kuno, Barry F. Madore, Sergio Martín, Jennifer Donovan Meyer, Kazuyuki Muraoka, Yoshimasa Watanabe
Figure caption: Scaling relations of cloud properties. In each plot, the filling-factor corrected data points for the M83 clouds are shown with the gray markers. The blue and purple contour lines indicate the data densities for the corrected and uncorrected cloud properties in M83 at the level of 20% of the maximum density for each. The green contour is the same for S87's Galactic samples. The correction for f is made by assuming α vir,0 of 1, and only the clouds with T eq > 0.5 K are shown for M83 clouds. (a) Velocity dispersion to radius relationship. The dashed line indicates the σ v–R eff relation of S87. (b) Mass to radius relationship. The dashed line indicates Σ = 200 M ⊙ pc−2, the constant Σ implied from S87's scaling relations. Also, the dotted lines indicate the lines for Σ of 10, 100, and 1000 M ⊙ pc−2, respectively.
Paper: Strong Nongravitational Accelerations and the Potential for Misidentification of Near-Earth Objects
Authors: Aster G. Taylor, Darryl Z. Seligman, Matthew J. Holman, Peter Vereš, Davide Farnocchia, Nikole Lewis, Marco Micheli, Jason T. Wright
Figure caption: The change in the on-sky position (as seen from Earth) of 2003 RM (top) and 1998 KY26 (bottom) as a function of time for the three components of nongravitational acceleration. The magnitude of the nongravitational acceleration is set to ∣A  i ∣ = 1 × 10−10 au day−2 and we show the radial A 1 (red), transverse A 2 (blue), and out-of-plane A 3 (purple) components. Since the ephemerides are linear in the nongravitational acceleration magnitude, stronger accelerations have the same functional form. The nongravitational accelerations are of the form given in Equation (1), and the change in position ΔΘ between the perturbed and unperturbed orbits is calculated using Equation (2).
Paper: Strong Nongravitational Accelerations and the Potential for Misidentification of Near-Earth Objects
Authors: Aster G. Taylor, Darryl Z. Seligman, Matthew J. Holman, Peter Vereš, Davide Farnocchia, Nikole Lewis, Marco Micheli, Jason T. Wright
Figure caption: The fraction of NEOs that would exhibit a given change in sky position (or larger) over an approximate apparition period as a function of magnitude and direction of nongravitational acceleration. The ephemerides are calculated for ∣A  i ∣ = 1 × 10−10 au day−2 and linearly scaled for other nongravitational acceleration magnitudes.
Paper: Strong Nongravitational Accelerations and the Potential for Misidentification of Near-Earth Objects
Authors: Aster G. Taylor, Darryl Z. Seligman, Matthew J. Holman, Peter Vereš, Davide Farnocchia, Nikole Lewis, Marco Micheli, Jason T. Wright
Figure caption: The median change in the on-sky position ΔΘ after 10 yr of integration as a function of the magnitude of the transverse nongravitational acceleration A 2, semimajor axis, and eccentricity. Each grid cell shows the median change in position of all objects in a given bin. The white contour corresponds to ΔΘ = 103 arcsec.
Paper: Whole-disk Sampling of Molecular Clouds in M83
Authors: Akihiko Hirota, Jin Koda, Fumi Egusa, Tsuyoshi Sawada, Kazushi Sakamoto, Mark Heyer, Amanda M Lee, Fumiya Maeda, Samuel Boissier, Daniela Calzetti, Bruce G. Elmegreen, Nanase Harada, Luis C. Ho, Masato I. N. Kobayashi, Nario Kuno, Barry F. Madore, Sergio Martín, Jennifer Donovan Meyer, Kazuyuki Muraoka, Yoshimasa Watanabe
Figure caption: Same as Figure 17, but for the blended setup.
Paper: An Elemental Abundance Diagnostic for Coordinated Solar Orbiter/SPICE and Hinode/EIS Observations
Authors: David H. Brooks, Harry P. Warren, Deborah Baker, Sarah A. Matthews, Stephanie L. Yardley
Figure caption: Loops segments selected for the EM analysis. The Fe VIII 185.213 Å image is from an EIS raster scan that started at 00:19:27 UT on 2007 December 10. The loop segments are shown by the dark-blue-, dark-red-, and pink-colored boxes. These colors are also used in Figures 3 and 4 to cross-reference the loops with their corresponding EM distributions and empirical test results.
Paper: An Elemental Abundance Diagnostic for Coordinated Solar Orbiter/SPICE and Hinode/EIS Observations
Authors: David H. Brooks, Harry P. Warren, Deborah Baker, Sarah A. Matthews, Stephanie L. Yardley
Figure caption: Loop EM distributions. The histograms show the best-fit EM solutions from the MCMC algorithm. They are color coded dark-blue, dark-red, and pink for cross-referencing with the selected segments shown in Figure 2 and the empirical test results of Figure 4. The light-blue solid and dotted lines are EM loci curves that constrain where the EM distribution can go. They represent emission lines from various ionization stages of Fe VIII–Fe XIII, O IV–O VI, and Mg VII, and Si VII. The dotted curves indicate that the cross-loop intensity profile is not well correlated with that of Fe VIII 185.213 Å. The shaded area around the EM distribution indicates the uncertainty, based on a comparison of the observed and predicted intensities (see the text for discussion).
Paper: An Elemental Abundance Diagnostic for Coordinated Solar Orbiter/SPICE and Hinode/EIS Observations
Authors: David H. Brooks, Harry P. Warren, Deborah Baker, Sarah A. Matthews, Stephanie L. Yardley
Figure caption: Fe VIII 185.213 Å/Ne VIII 770.428 Å abundance diagnostic ratio. First panel: Fe VIII 185.213 Å contribution function plotted against temperature and density. Second panel: Ne VIII 770.428 Å contribution function plotted against temperature and density. Third panel: ratio plotted against temperature for densities of log (n/cm−3) = 8–10. The ratio shows ∼40% variation in the range of log (T/K) = 5.65–6.05 (delineated by the vertical dotted lines). Fourth panel: ratio plotted against temperature for densities of log (n/cm−3) = 8–10 after the Fe VIII 185.213 Å contribution function has been convolved with an idealized DEM (see text). Variations are reduced by a factor of 2 in the range of log (T/K) = 5.75–6.05.
Paper: An Elemental Abundance Diagnostic for Coordinated Solar Orbiter/SPICE and Hinode/EIS Observations
Authors: David H. Brooks, Harry P. Warren, Deborah Baker, Sarah A. Matthews, Stephanie L. Yardley
Figure caption: Results from the empirical tests. The histograms show the difference between the ground truth and inverted FIP bias as a percentage of the ground truth for 1100 experiments. They are color coded dark-blue, dark-red, and pink for cross-referencing with the selected segments shown in Figure 2 and their corresponding EM distributions shown in Figure 3. We also show the standard deviation (σ) and centroid of the peak of the distributions (X 0) in the legends.
Paper: An Elemental Abundance Diagnostic for Coordinated Solar Orbiter/SPICE and Hinode/EIS Observations
Authors: David H. Brooks, Harry P. Warren, Deborah Baker, Sarah A. Matthews, Stephanie L. Yardley
Figure caption: Coordinated Hinode and Solar Orbiter observations from 2023 March 30. Left to right: EIS Fe VIII 185.213 Å intensity from the raster that started at 18:25:56 UT, AIA 171 Å coaligned filter image taken at 20:10:57 UT, EUI 174 Å coaligned filter image taken at 20:10:55 UT, and SPICE Ne VIII 770.428 Å coaligned wave band intensity from the raster scan that started at 19:29:28 UT overlaid on the EUI image. The data were coaligned as described in Section 5.
Paper: Spectropolarimetric Inversion in Four Dimensions with Deep Learning (SPIn4D). I. Overview, Magnetohydrodynamic Modeling, and Stokes Profile Synthesis
Authors: Kai E. Yang, 凯 杨, Lucas A. Tarr, Matthias Rempel, S. Curt Dodds, Sarah A. Jaeggli, Peter Sadowski, Thomas A. Schad, Ian Cunnyngham, Jiayi Liu, 嘉奕 刘, Yannik Glaser, Xudong Sun, 旭东 孙
Figure caption: The power spectra of the normalized continuum intensity I/I 0, V  Z , and B  Z  at the surface ﹩{\mathrm{log}}_{10}\tau =0﹩, displayed from top to bottom. The left panels (a), (d), and (g) present the direct power spectra for the six cases, each offset vertically by a factor of 3 for better visualization. The vertical dashed lines in panels (a), (d), and (g) mark the local power spectrum peak for Case 1. The middle panels (b), (e), and (h) depict the power spectra ratios of Cases 2–6 to Case 1, with the vertical dashed lines in (b) and (e) indicating the local peak and saddle point for Case 2 at smaller scales, and in (h) the local peak for Case 2 at larger scales. Panels (c), (f), and (i) show lines marking the typical scales of the peak values in their respective spectra overlaid on a representative subregion for each variable. The dashed red box in (i) highlights the FOV seen in panels (c) and (f), to enhance the visualization of the typical spatial scale derived from the power spectrum.
Paper: Spectropolarimetric Inversion in Four Dimensions with Deep Learning (SPIn4D). I. Overview, Magnetohydrodynamic Modeling, and Stokes Profile Synthesis
Authors: Kai E. Yang, 凯 杨, Lucas A. Tarr, Matthias Rempel, S. Curt Dodds, Sarah A. Jaeggli, Peter Sadowski, Thomas A. Schad, Ian Cunnyngham, Jiayi Liu, 嘉奕 刘, Yannik Glaser, Xudong Sun, 旭东 孙
Figure caption: The oscillation in temperature in the vertical slice in the middle of the simulation box. Panels (a) and (b) show Case 5 and an additional test case with an added uniform field as large as 400 G. The three dotted curves are for ﹩{\mathrm{log}}_{1}0\tau =0﹩, −2, and −4.
Paper: Spectropolarimetric Inversion in Four Dimensions with Deep Learning (SPIn4D). I. Overview, Magnetohydrodynamic Modeling, and Stokes Profile Synthesis
Authors: Kai E. Yang, 凯 杨, Lucas A. Tarr, Matthias Rempel, S. Curt Dodds, Sarah A. Jaeggli, Peter Sadowski, Thomas A. Schad, Ian Cunnyngham, Jiayi Liu, 嘉奕 刘, Yannik Glaser, Xudong Sun, 旭东 孙
Figure caption: Illustration of the synthesized Stokes profiles from SIR. (a) Intensity of SIR Stokes I at continuum wavelength, with locations of representative Stokes profiles marked by colored circles. Panels (b)–(e) and (f)–(i) show the Stokes profiles for the 630 nm and 1565 nm lines, respectively. Panels (j)–(m) and (n)–(q) detail the differences between the SIR and DeSIRe synthesized profiles, i.e., ﹩{I}_{\mathrm{SIR}}-{I}_{\mathrm{DeSIRe}}﹩.
Paper: Spectropolarimetric Inversion in Four Dimensions with Deep Learning (SPIn4D). I. Overview, Magnetohydrodynamic Modeling, and Stokes Profile Synthesis
Authors: Kai E. Yang, 凯 杨, Lucas A. Tarr, Matthias Rempel, S. Curt Dodds, Sarah A. Jaeggli, Peter Sadowski, Thomas A. Schad, Ian Cunnyngham, Jiayi Liu, 嘉奕 刘, Yannik Glaser, Xudong Sun, 旭东 孙
Figure caption: Comparison of the Stokes data from SIR and DeSIRe for the 630 nm line from Case 5 with t = 5.6 hr, focusing on the wings and cores. The colors represent the pixel count in the 2D histogram. The dashed red lines denote the line of identity, indicating perfect agreement between the two sets of data. The corresponding Pearson correlation coefficients are marked on each panel.
Paper: JWST Resolves Collision-induced Absorption Features in White Dwarfs
Authors: Simon Blouin, Mukremin Kilic, Loïc Albert, Bianca Azartash-Namin, Patrick Dufour
Figure caption: Color–magnitude diagram of the Pan–STARRS white dwarfs within 100 pc of the Sun and with 10σ Gaia DR3 parallax measurements. Labels indicate the location of the A, B, Q, and IR-faint branches. The stars analyzed in this work are shown in red. The IR-faint branch starts at M g ≃ 15, g − z ≃ 0.5 and extends toward the bottom-left corner of the figure.
Paper: Spectropolarimetric Inversion in Four Dimensions with Deep Learning (SPIn4D). I. Overview, Magnetohydrodynamic Modeling, and Stokes Profile Synthesis
Authors: Kai E. Yang, 凯 杨, Lucas A. Tarr, Matthias Rempel, S. Curt Dodds, Sarah A. Jaeggli, Peter Sadowski, Thomas A. Schad, Ian Cunnyngham, Jiayi Liu, 嘉奕 刘, Yannik Glaser, Xudong Sun, 旭东 孙
Figure caption: Example synthesized spectropolarimetric data computed for a single snapshot of the Case 5 MHD simulation at t = 5.6 hr; the 3D data cubes show a subset of the output for both spectral line pairs and both forward-modeling codes. The red box in panel (a) marks the FOV of the 3D data cubes. Panel (b) shows the zoom-in view of the subset, with the colorized circles indicating locations representative of typical Stokes profiles, as presented in Figure 9.
Paper: Spectropolarimetric Inversion in Four Dimensions with Deep Learning (SPIn4D). I. Overview, Magnetohydrodynamic Modeling, and Stokes Profile Synthesis
Authors: Kai E. Yang, 凯 杨, Lucas A. Tarr, Matthias Rempel, S. Curt Dodds, Sarah A. Jaeggli, Peter Sadowski, Thomas A. Schad, Ian Cunnyngham, Jiayi Liu, 嘉奕 刘, Yannik Glaser, Xudong Sun, 旭东 孙
Figure caption: The same as Figure 10, but for the 1565 nm lines.