adsabs/AstroCLIMB huggingface dataset:
Paper: Spherical Harmonic Representation of Energetic Neutral Atom Flux Components Observed by IBEX
Authors: P. Swaczyna, M. A. Dayeh, E. J. Zirnstein
Figure caption: GDF maps reconstructed from the spherical harmonic representation for energy steps 0.7, 1.1, 1.7, 2.7, and 4.3 keV (left to right panels). Rows from top to bottom show the results from the time-combined maps and single-year maps from 2009 to 2019.
Paper: Spherical Harmonic Representation of Energetic Neutral Atom Flux Components Observed by IBEX
Authors: P. Swaczyna, M. A. Dayeh, E. J. Zirnstein
Figure caption: Role of the regularization for spherical harmonic decomposition shown for the IBEX map at energy step 1.7 keV observed in 2016, which includes a significant gap in the data (top left panel). The top middle and right panels show the L-curve and the curvature as a function of the regularization parameter, respectively. The three bottom panels show the reconstructed maps for three values of the regularization parameter: α = 0.000079, 0.002815, and 0.125893. The middle panel shows the result for optimal regularization. The maps shown here and in other figures in this paper use the equirectangular projection in ecliptic coordinates where the top and bottom edges correspond to the north and south ecliptic poles, respectively. The left and right edges correspond to ecliptic longitude of 72°.
Paper: Spherical Harmonic Representation of Energetic Neutral Atom Flux Components Observed by IBEX
Authors: P. Swaczyna, M. A. Dayeh, E. J. Zirnstein
Figure caption: Grid of time-series plots of the GDF and ribbon flux observed from the entire sky and six regions around the nose, tail, north and south ecliptic pole, starboard, and port directions (left to right). Rows show results for energy steps 0.7, 1.1, 1.7, 2.7, and 4.3 keV (top to bottom). The ribbon flux is multiplied by 4 to facilitate comparison with the GDF. The bands in this figure show 1σ uncertainties.
Paper: Spherical Harmonic Representation of Energetic Neutral Atom Flux Components Observed by IBEX
Authors: P. Swaczyna, M. A. Dayeh, E. J. Zirnstein
Figure caption: Optimization of the maximum degree of spherical harmonics. The top panel shows the mean statistical significance of spherical harmonic contributions for all orders as a function of the degree. The bottom panel shows the AIC used to select among models with various numbers of parameters. The optimal maximum degree ranges from ℓ = 17 to 22. The top scale shows the angular size of structures that can be reconstructed.
Paper: Spherical Harmonic Representation of Energetic Neutral Atom Flux Components Observed by IBEX
Authors: P. Swaczyna, M. A. Dayeh, E. J. Zirnstein
Figure caption: Separation for the 2016 map in energy step 1.7 keV. The top panels show the original map and the reconstructed fluxes from the spherical harmonic representations of the total, GDF, and ribbon flux (left to right). The middle and bottom rows show the uncertainties obtained from Equations (12) and (15)–(16), respectively. The uncertainty map for the original map is the same in both rows.
Paper: Spherical Harmonic Representation of Energetic Neutral Atom Flux Components Observed by IBEX
Authors: P. Swaczyna, M. A. Dayeh, E. J. Zirnstein
Figure caption: Ribbon maps reconstructed from the spherical harmonic representation for energy steps 0.7, 1.1, 1.7, 2.7, and 4.3 keV (left to right panels). Rows from top to bottom show the results from the time-combined maps and single-year maps from 2009 to 2019.
Paper: Spherical Harmonic Representation of Energetic Neutral Atom Flux Components Observed by IBEX
Authors: P. Swaczyna, M. A. Dayeh, E. J. Zirnstein
Figure caption: Spherical harmonic reconstruction of the time-combined IBEX map at energy step 1.7 keV. The top panel shows the original map, and the middle panels show the reconstruction for the maximum degree of spherical harmonics ﹩{{\ell }}_{\max }=﹩ 14, 22, and 30 (left to right). The bottom panels show the residual signal normalized by the original map uncertainties.
Paper: Spherical Harmonic Representation of Energetic Neutral Atom Flux Components Observed by IBEX
Authors: P. Swaczyna, M. A. Dayeh, E. J. Zirnstein
Figure caption: Results of the GDF and ribbon separation for combined ENA flux observed in 2009–2011 in energy step 1.7 keV and three possible mask widths of 36°, 45°, and 60° (top to bottom). The maps from left to right show the original IBEX map, with the white outlines showing the extent of the mask, the reconstructed total flux map, the GDF map, and the ribbon map.
Paper: Lightning: An X-Ray to Submillimeter Galaxy SED-fitting Code with Physically Motivated Stellar, Dust, and AGN Models
Authors: Keith Doore, Erik B. Monson, Rafael T. Eufrasio, Bret D. Lehmer, Kristen Garofali, Antara Basu-Zych
Figure caption: Maps of the derived spatially resolved properties of M81. The values of each pixel are the median value from the corresponding posterior distribution (excluding the p-value, which is a single value, in panel (f)). The properties from the upper left to bottom right are (a) the SFR of the last 100 Myr, (b) the stellar mass, (c) the sSFR of the last 100 Myr, (d) the diffuse V-band optical depth, (e) the L TIR, and (f) the p-value estimated from the PPC. From these maps, it can be seen that the attenuation and recent star formation are concentrated in the spiral arms, while the stellar mass is concentrated in the bulge. This age stratification is clear in the sSFR map, which uses a different color scheme to highlight younger populations in blue and older populations in red.
Paper: Lightning: An X-Ray to Submillimeter Galaxy SED-fitting Code with Physically Motivated Stellar, Dust, and AGN Models
Authors: Keith Doore, Erik B. Monson, Rafael T. Eufrasio, Bret D. Lehmer, Kristen Garofali, Antara Basu-Zych
Figure caption: (Left) Composite SDSS g, r, i color image of M81 after being convolved to a common PSF of 25″ and rebinned to a pixel scale of 10″. Overlaid are the 25 mag arcsec−2 B-band isophotal ellipse as given by HyperLeda in blue and one-half of the 20 mag arcsec−2 K  s -band isophotal ellipse as given by Jarrett et al. (2003) in orange. (Middle) Total best-fit model spectra and component SEDs of the outer (upper plot) and inner (lower plot) regions of the galaxy derived by summing the individual pixels, where the outer region is all pixels between the B-band ellipse and the half of the K  s -band ellipse (i.e., between blue and orange ellipses) and the inner region is all pixels within the half of the K  s -band ellipse (i.e., inside orange ellipse). (Right) Resulting SFH with uncertainty ranges for the outer and inner regions as the blue and orange lines, respectively. From the SEDs and SFHs, it can be seen that the outer region has comparatively higher UV emission and lower NIR emission, which is distinguished by the fit as an overall younger population compared to the inner region.
Paper: Lightning: An X-Ray to Submillimeter Galaxy SED-fitting Code with Physically Motivated Stellar, Dust, and AGN Models
Authors: Keith Doore, Erik B. Monson, Rafael T. Eufrasio, Bret D. Lehmer, Kristen Garofali, Antara Basu-Zych
Figure caption: The X-ray-to-IR SED fit for J033226.49−274035.5. In the left panels, we show the instrumental X-ray spectrum (in terms of count-rate density) with its best-fit model and residuals. In the right panels, we show the observed UV-to-IR SED (in terms of luminosity), its best-fitting model, and residuals. The best-fit model minimizes the total X-ray and UV-to-IR ﹩-\mathrm{log}({P}_{\mathrm{post}})﹩. The Lightning X-ray model implementation can provide rudimentary X-ray spectral fits and directly connect them to the UV-to-IR SED fit.
Paper: Lightning: An X-Ray to Submillimeter Galaxy SED-fitting Code with Physically Motivated Stellar, Dust, and AGN Models
Authors: Keith Doore, Erik B. Monson, Rafael T. Eufrasio, Bret D. Lehmer, Kristen Garofali, Antara Basu-Zych
Figure caption: Panels (a)–(e) are the same as Figure 9 except the values correspond to the best-fit values derived from the MPFIT algorithm. The p-values in panel (f) are estimated from a χ 2 goodness-of-fit test. The color bar minimum and maximum ranges have been truncated to match those in Figure 9. Comparing these maps to those in Figure 9, it can be seen that some of these maps, particularly the SFR and sSFR, are not nearly as smooth, due to the use of best-fit values rather than the posterior median.
Paper: Lightning: An X-Ray to Submillimeter Galaxy SED-fitting Code with Physically Motivated Stellar, Dust, and AGN Models
Authors: Keith Doore, Erik B. Monson, Rafael T. Eufrasio, Bret D. Lehmer, Kristen Garofali, Antara Basu-Zych
Figure caption: (Left) Histograms of the posterior distribution functions of the SFR of the last 100 Myr for NGC 4631, which are area normalized. The Calzetti et al. (2000) models are shown in the upper panel and the inclination-dependent models are shown in the lower panel. (Right) The total best-fit model spectrum to the observed SED for each of the four models. Inlaid in the SED plot are the posterior distributions of inclination (in terms of ﹩1-\cos i﹩, where ﹩1-\cos i=1﹩ is edge on) for the inclination-dependent models. This inlay shows that the models are correctly predicting a close to edge-on view. In all plots, the inclination-dependent model with and without X-rays and the Calzetti et al. (2000) model with and without X-rays are shown as the blue, green, orange, and red lines, respectively. While the best-fit model spectra are practically identical for each model, the resulting SFR distributions vary depending on the attenuation model and the inclusion of X-ray emission.
Paper: Lightning: An X-Ray to Submillimeter Galaxy SED-fitting Code with Physically Motivated Stellar, Dust, and AGN Models
Authors: Keith Doore, Erik B. Monson, Rafael T. Eufrasio, Bret D. Lehmer, Kristen Garofali, Antara Basu-Zych
Figure caption: (Lower left) A corner plot of the derived parameters for NGC 628. These parameters include the stellar mass (M ⋆), the recent SFR of the last 100 Myr, the sSFR of the last 100 Myr, the V-band attenuation (A  V ), and the L TIR for each SED-fitting code. (Upper right) The median SFH with the 16th and 84th percentile uncertainty range given as the offset vertical lines for each SED-fitting code. For all plots, the results from Lightning, Prospector, and BAGPIPES are given as the blue, green, and orange lines, respectively. From these plots, it can be seen that the results from Lightning and Prospector are highly consistent, while the BAGPIPES results vary in consistency, especially for the SFH.
Paper: Lightning: An X-Ray to Submillimeter Galaxy SED-fitting Code with Physically Motivated Stellar, Dust, and AGN Models
Authors: Keith Doore, Erik B. Monson, Rafael T. Eufrasio, Bret D. Lehmer, Kristen Garofali, Antara Basu-Zych
Figure caption: A corner plot of the AGN model parameters for J033226.49−274035.5, fit with and without an X-ray component as the blue and orange lines, respectively. The X-ray emission is modeled with the theoretical qsosed model and their addition to the SED results in a highly consistent UV-to-IR AGN bolometric luminosity and inclination parameters compared to the fit without X-rays. In addition, the theoretical qsosed model also provides indirect estimates of the SMBH mass M SMBH and Eddington ratio ﹩\dot{m}=\dot{M}/{\dot{M}}_{\mathrm{edd}}﹩.
Paper: Lightning: An X-Ray to Submillimeter Galaxy SED-fitting Code with Physically Motivated Stellar, Dust, and AGN Models
Authors: Keith Doore, Erik B. Monson, Rafael T. Eufrasio, Bret D. Lehmer, Kristen Garofali, Antara Basu-Zych
Figure caption: The total best-fit model spectra to the observed SED of NGC 628 and the associated residuals as generated by Lightning, Prospector, and BAGPIPES as the blue, green, and orange lines, respectively. For each code, the p-value from a PPC is shown in the upper left of each residual plot. In general, it can be seen that all three codes model the data well, both from the PPC and the residuals.
Paper: Lightning: An X-Ray to Submillimeter Galaxy SED-fitting Code with Physically Motivated Stellar, Dust, and AGN Models
Authors: Keith Doore, Erik B. Monson, Rafael T. Eufrasio, Bret D. Lehmer, Kristen Garofali, Antara Basu-Zych
Figure caption: Composite SDSS g, r, i (M81, NGC 4631, and NGC 628) and HST F435W, F606W, and F850LP (J033226.49−274035.5) postage-stamp images for the galaxies used in the example applications of Lightning in Section 4.
Paper: Lightning: An X-Ray to Submillimeter Galaxy SED-fitting Code with Physically Motivated Stellar, Dust, and AGN Models
Authors: Keith Doore, Erik B. Monson, Rafael T. Eufrasio, Bret D. Lehmer, Kristen Garofali, Antara Basu-Zych
Figure caption: The total best-fit model spectra to the observed SED of J033226.49−274035.5 and the associated residuals as generated by Lightning and CIGALE as the gray and magenta lines, respectively. The gray and magenta colored data points in the X-rays correspond to each code’s input data since Lightning had inputs in units of observed counts (which are converted to model-dependent luminosities for plotting) and CIGALE had inputs in units of absorption-corrected fluxes. For the Lightning fit, we include each model component as in Figure 12. Additionally, we include the range of the top 64% of best-fit models from the MCMC posterior as the correspondingly colored shaded regions to show the uncertainty range on the component SEDs. For each code, we also show the best-fit χ 2 value in the center of each residual plot. In general, it can be seen that both codes model their data well from the best-fit χ 2 and the residuals.
Paper: Spherical Harmonic Representation of Energetic Neutral Atom Flux Components Observed by IBEX
Authors: P. Swaczyna, M. A. Dayeh, E. J. Zirnstein
Figure caption: Histograms of normalized residual signal between the original IBEX map and truncated GDF estimation (see text). Panels from left to right show energy steps 0.7, 1.1, 1.7, 2.7, and 4.3 keV. The histograms are compared with the normal distribution (solid black line). Green and blue ellipses indicate ranges with systematic deviations from the normal distribution, and red arrows point at outliers discussed in the text.
Paper: Spherical Harmonic Representation of Energetic Neutral Atom Flux Components Observed by IBEX
Authors: P. Swaczyna, M. A. Dayeh, E. J. Zirnstein
Figure caption: Time evolution of the ribbon flux. Left column: polar maps of the ribbon flux averaged over 2009–2011. The dashed circle approximately follows the ribbon’s peaks. Lines of heliographic latitudes are shown with green lines. Right column: evolution of the polar-angle-integrated ribbon flux as a function of the azimuth. Rows from top to bottom correspond to energy steps 0.7, 1.1, 1.7, 2.7, and 4.3 keV. The bands in this figure show 1σ uncertainties.
Paper: Spherical Harmonic Representation of Energetic Neutral Atom Flux Components Observed by IBEX
Authors: P. Swaczyna, M. A. Dayeh, E. J. Zirnstein
Figure caption: As Figure 6, except the GDF flux is reconstructed with the spherical harmonics up to the maximum degree derived in Section 4.2.
Paper: Spherical Harmonic Representation of Energetic Neutral Atom Flux Components Observed by IBEX
Authors: P. Swaczyna, M. A. Dayeh, E. J. Zirnstein
Figure caption: Positions of the IBEX ribbon’s centers in ecliptic coordinates. The ellipses and points with error bars show the positions obtained using the methodologies presented in Appendix B and by Zirnstein et al. (2023, Appendix), respectively. Panels from the top left to bottom right show results for periods: 2009–2019, 2009–2011, 2012–2013, 2014–2015, 2016–2017, and 2018–2019.
Paper: Spherical Harmonic Representation of Energetic Neutral Atom Flux Components Observed by IBEX
Authors: P. Swaczyna, M. A. Dayeh, E. J. Zirnstein
Figure caption: Power spectra as a function of the spherical harmonic degree of the GDF and ribbon components and their sum (total) for energy steps 0.7, 1.1, 1.7, 2.7, and 4.3 keV (top to bottom).
Paper: Thermodynamic and Magnetic Topology Evolution of the X1.0 Flare on 2021 October 28 Simulated by a Data-driven Radiative Magnetohydrodynamic Model
Authors: J. H. Guo, Y. W. Ni, Z. Zhong, Y. Guo, C. Xia, H. T. Li, S. Poedts, B. Schmieder, P. F. Chen
Figure caption: (a) Remapped HMI vector magnetogram as viewed from the top. The B  z  is plotted in the background (gray scale), and the purple (red) arrows denote the horizontal magnetic fields with positive (negative) polarities. (b) AIA 131 Å image at 15:24 UT on 2021 October 28, where the red dots outline the path of the inserted flux rope. (c) Selected core field lines of the NLFFF model viewed from the top, colored in temperature. The temperature is obtained from the inserted filament and hydrostatic model. (d) Side view of the extrapolated field lines. (e) The constructed flux rope and inserting prominence with a zoomed-in view of the black rectangle in panel (d), where the pink isosurface represents the prominence material where the temperature is lower than 20,000 K.
Paper: Thermodynamic and Magnetic Topology Evolution of the X1.0 Flare on 2021 October 28 Simulated by a Data-driven Radiative Magnetohydrodynamic Model
Authors: J. H. Guo, Y. W. Ni, Z. Zhong, Y. Guo, C. Xia, H. T. Li, S. Poedts, B. Schmieder, P. F. Chen
Figure caption: Comparison between photospheric QSLs (lg Q > 2) and the emission in AIA 1600 Å (a)–(b) and 304 Å (c)–(d). QSLs with a positive (negative) vertical magnetic component are colored in orange and chartreuse (cyan). The black dashed line in panel (a) illustrates a slice crossing the flare ribbons. The blue box shows the observational evidence of the 3D reconnection in Section 3.2. (e) Time–distance diagram of the QSLs and 1600 Å image for slice “S” in panel (a).
Paper: Thermodynamic and Magnetic Topology Evolution of the X1.0 Flare on 2021 October 28 Simulated by a Data-driven Radiative Magnetohydrodynamic Model
Authors: J. H. Guo, Y. W. Ni, Z. Zhong, Y. Guo, C. Xia, H. T. Li, S. Poedts, B. Schmieder, P. F. Chen
Figure caption: Snapshots of the simulated magnetic field lines colored in temperature. The left column shows the evolution of the simulated flux ropes, which are overlaid on the 304 Å images at (a) 15:26, (c) 15:32, and (e) 15:50 UT. The right column shows the evolution of the flux ropes from the side view at the same times as the left column.
Paper: Thermodynamic and Magnetic Topology Evolution of the X1.0 Flare on 2021 October 28 Simulated by a Data-driven Radiative Magnetohydrodynamic Model
Authors: J. H. Guo, Y. W. Ni, Z. Zhong, Y. Guo, C. Xia, H. T. Li, S. Poedts, B. Schmieder, P. F. Chen
Figure caption: Multiwavelength composite images of SDO/AIA at 15:24, 15:32, 15:35, and 15:42 UT on 2021 October 28, showing the evolution of the filament, flare ribbons, and postflare loops. The blue/red contour lines in panel (b) correspond to the positive/negative magnetic polarities.
Paper: Thermodynamic and Magnetic Topology Evolution of the X1.0 Flare on 2021 October 28 Simulated by a Data-driven Radiative Magnetohydrodynamic Model
Authors: J. H. Guo, Y. W. Ni, Z. Zhong, Y. Guo, C. Xia, H. T. Li, S. Poedts, B. Schmieder, P. F. Chen
Figure caption: (a) Synthesized EUV 193 Å image at 15:32 UT. (b) Running-difference image of the EUV 193 Å radiation at 15:32 UT, where the blue solid line outlines the CME leading edge, and the red dashed line outlines the piston-driven shock. (c) Synthesized white-light image at 15:32 UT. (d) Averaged temperature distribution at 15:32 UT.
Paper: Thermodynamic and Magnetic Topology Evolution of the X1.0 Flare on 2021 October 28 Simulated by a Data-driven Radiative Magnetohydrodynamic Model
Authors: J. H. Guo, Y. W. Ni, Z. Zhong, Y. Guo, C. Xia, H. T. Li, S. Poedts, B. Schmieder, P. F. Chen
Figure caption: Reconnection geometries recognized by the field-line connectivity (a)–(c), Q distribution (d)–(f), and J/B distribution (g)–(i). The columns from left to right represent the ar-rf geometry at 15:30 UT, the aa-rf geometry at 15:32 UT, and the breakout-like geometry at 15:34 UT, respectively. (a)–(c) Pre-reconnection (cyan) and post-reconnection (purple) field lines, where the transparent surfaces represent the plasma heated by the reconnection. (d)–(f) Q distributions near the current sheet, which are correspond to three types of reconnection geometries displayed in panels (a)–(c). (g)–(i) J/B distributions at the same plane of the second row.
Paper: Thermodynamic and Magnetic Topology Evolution of the X1.0 Flare on 2021 October 28 Simulated by a Data-driven Radiative Magnetohydrodynamic Model
Authors: J. H. Guo, Y. W. Ni, Z. Zhong, Y. Guo, C. Xia, H. T. Li, S. Poedts, B. Schmieder, P. F. Chen
Figure caption: Twist distributions on the photosphere at (a) 15:26 UT and (b) 15:48 UT. (c) Temporal evolution of the toroidal (black line) and poloidal (red line) flux of the flux rope. The measurement is repeated 10 times to estimate the errors originating from the uncertainties of the selected regions for the toroidal flux calculation. And the uncertainty of the poloidal flux is calculated by the product of the toroidal flux error and the standard deviation of the twist. The error bars at the bottom represent the mean values of the uncertainty during the whole process. The three reconnection stages are divided by two vertical dashed lines.
Paper: Thermodynamic and Magnetic Topology Evolution of the X1.0 Flare on 2021 October 28 Simulated by a Data-driven Radiative Magnetohydrodynamic Model
Authors: J. H. Guo, Y. W. Ni, Z. Zhong, Y. Guo, C. Xia, H. T. Li, S. Poedts, B. Schmieder, P. F. Chen
Figure caption: Panels (a) and (b), respectively, show the synthesized 94 and 171 Å images integrated from x = 7 Mm to 21 Mm, zoomed in on the rectangle region in Figure 10(a). (c) Number density distribution on the plane of x = 14 Mm. (d) Temperature distribution on the plane of x = 14 Mm. (e) v  y  distribution on the plane of x = 14 Mm. (f) v  z  distribution on the plane of x = 14 Mm. (g) The curl of the velocity distribution on the plane of x = 14 Mm. (h) Magnetic field lines colored in temperature near the cusp-shaped structure, where the transparent background slice represents the number density distribution in panel (c).
Paper: Thermodynamic and Magnetic Topology Evolution of the X1.0 Flare on 2021 October 28 Simulated by a Data-driven Radiative Magnetohydrodynamic Model
Authors: J. H. Guo, Y. W. Ni, Z. Zhong, Y. Guo, C. Xia, H. T. Li, S. Poedts, B. Schmieder, P. F. Chen
Figure caption: Comparisons between AIA observations (a)–(c) and synthesized EUV radiative images (d)–(f) observed from the top at 15:32 UT. Panels (a) and (d) show the 131 Å channel images, panels (b) and (e) show the 193 Å channel images, and panels (c) and (f) show the 335 Å channel images.
Paper: Thermodynamic and Magnetic Topology Evolution of the X1.0 Flare on 2021 October 28 Simulated by a Data-driven Radiative Magnetohydrodynamic Model
Authors: J. H. Guo, Y. W. Ni, Z. Zhong, Y. Guo, C. Xia, H. T. Li, S. Poedts, B. Schmieder, P. F. Chen
Figure caption: Side views of the synthesized EUV radiations at 15:28 (a)–(c) and 15:44 UT (d)–(f). The panels from left to right show the 304 Å ((a) and (d)), 171 Å ((b) and (e)), and 94 Å ((c) and (f)) images, respectively.
Paper: Thermodynamic and Magnetic Topology Evolution of the X1.0 Flare on 2021 October 28 Simulated by a Data-driven Radiative Magnetohydrodynamic Model
Authors: J. H. Guo, Y. W. Ni, Z. Zhong, Y. Guo, C. Xia, H. T. Li, S. Poedts, B. Schmieder, P. F. Chen
Figure caption: (a) Q distribution on the plane of x = 10.6 Mm at 15:28 UT. Panels (b) and (c) illustrate the Q distributions zoomed in on the region of the purple rectangle in panel (a) at 15:26 and 15:28 UT, respectively. (d) Time–distance diagram of Q along the slice (red solid line) in panel (a).
Paper: Thermodynamic and Magnetic Topology Evolution of the X1.0 Flare on 2021 October 28 Simulated by a Data-driven Radiative Magnetohydrodynamic Model
Authors: J. H. Guo, Y. W. Ni, Z. Zhong, Y. Guo, C. Xia, H. T. Li, S. Poedts, B. Schmieder, P. F. Chen
Figure caption: Field lines passing through the asterisks in Figure 10(a) (red: CME leading edge; cyan and yellow: CME cavity; and blue: CME core) on the plane of x = 10 Mm. Panel (a) shows the side view, and panel (b) shows the end view overlaid on the 193 Å image.