adsabs/AstroCLIMB huggingface dataset:
Paper: Self-similar Cosmic-Ray Transport in High-resolution Magnetohydrodynamic Turbulence
Authors: Philipp Kempski, Drummond B. Fielding, Eliot Quataert, Robert J. Ewart, Philipp Grete, Matthew W. Kunz, Alexander A. Philippov, James Stone
Figure caption: PDFs of particle collision times P(τc/L) multiplied by τc/L (thus showing the probability per logarithmic interval). We consider two types of spatial scattering events, (1) ﹩{\boldsymbol{v}}\,\cdot \,\hat{{\boldsymbol{b}}}﹩ changing sign (top panel) and (2) ﹩{\boldsymbol{v}}\,\cdot \,\widehat{{\boldsymbol{z}}}﹩ changing sign (bottom panel), and we define the associated collision times τb and τz, respectively. The locations of the peaks in the PDFs of τz are set by the gyroperiods. For small rL, P(τ) shows clear power-law tails. For comparison, we also plot as dotted lines the τ−1/2 Sparre–Andersen scaling and a τ−1 scaling. If the power law is shallower then τ−1, as is the case over a wide range rL, the global diffusion rate is set not by the mean free path but instead by the longest excursions (the location of the cutoff). In the top panel, the cutoff increases with decreasing rL, indicating that particles are able to avoid higher-curvature regions for increasingly long stretches of time. This is not the case in the bottom panel, as the field-line random walk (dashed line; traced by particles with ﹩{\boldsymbol{v}}=c\hat{{\boldsymbol{b}}}﹩) imposes an upper limit on how far particles can propagate without changing their vz. The different behavior of the two cutoffs is the reason why κz and κ∥ are different functions of rL (Figure 4).
Paper: Self-similar Cosmic-Ray Transport in High-resolution Magnetohydrodynamic Turbulence
Authors: Philipp Kempski, Drummond B. Fielding, Eliot Quataert, Robert J. Ewart, Philipp Grete, Matthew W. Kunz, Alexander A. Philippov, James Stone
Figure caption: Contours show the conditional probability density ﹩P(| \delta B(\ell )\,| /\bar{B}(\ell )\,| \,\ell )﹩ multiplied by ﹩| \delta B(\ell )| /\mathop{B}\limits^{\unicode{x00304}}(\ell )﹩ (to show the probability per logarithmic interval) for our highest-resolution run (L/Δx = 10,240). The thick magenta curve traces the median ﹩| \delta B(\ell )| /\mathop{B}\limits^{\unicode{x00304}}(\ell )﹩ at each separation. Thinner magenta curves give the medians for lower-resolution simulations (L/Δx = 640 and 2560). Their departure from the high-resolution median at small ℓ underscores the need for extreme resolution to capture both the super-Alfvénic (﹩| \delta B(\ell )| \gtrsim \bar{B}(\ell )﹩) and sub-Alfvénic (﹩| \delta B(\ell )| \lesssim \bar{B}(\ell )﹩) portions of the cascade within the resolved range. The transition from super-Alfvénic to sub-Alfvénic turbulence occurs approximately at the location where the magenta line intersects the yellow horizontal dashed line, which happens at ℓA ≃ L/30 (≈300 grid cells). The median lines change to a dashed style at ℓ ≤ 16Δx, where numerical dissipation truncates the inertial range. The white dotted segment indicates a reference power-law scaling ∝ℓ1/2. Although the median fractional fluctuation drops below 1 for ℓ < ℓA, the PDF retains a substantial tail of high-﹩| \delta B(\ell )| /\bar{B}(\ell )﹩[ events; even an order of magnitude below ℓA, a nonnegligible fraction of pairs still satisfy ﹩| \delta B| \gt \mathop{B}\limits^{\unicode{x00304}}﹩. CRs with rL ≪ ℓA therefore encounter strongly perturbed fields despite the globally sub-Alfvénic character of the cascade.
Paper: Self-similar Cosmic-Ray Transport in High-resolution Magnetohydrodynamic Turbulence
Authors: Philipp Kempski, Drummond B. Fielding, Eliot Quataert, Robert J. Ewart, Philipp Grete, Matthew W. Kunz, Alexander A. Philippov, James Stone
Figure caption: Running diffusion coefficients in the 10,2403 simulation with δBrms/B0 = 2. The diffusion coefficients are normalized by cL, where c is the speed of light and L is the size of the turbulent box. Top: running diffusion coefficient along the background guide field for particles with different gyroradii rL. Middle: running diffusion coefficient of particles perpendicular to the guide field. Bottom: running diffusion coefficients perpendicular and parallel to the background guide field of magnetic field lines as traced by particles propagating ballistically along magnetic field lines with velocity ﹩{\boldsymbol{v}}=c\hat{{\boldsymbol{b}}}﹩ (this is described in detail at the end of Section 2). Because of the background guide field, the field lines show late-time ballistic behavior in the z-direction.
Paper: Self-similar Cosmic-Ray Transport in High-resolution Magnetohydrodynamic Turbulence
Authors: Philipp Kempski, Drummond B. Fielding, Eliot Quataert, Robert J. Ewart, Philipp Grete, Matthew W. Kunz, Alexander A. Philippov, James Stone
Figure caption: Left: 2D slice of the magnitude of current density normalized by the grid spacing in the 10,2403 simulation characterized by δBrms/B0 = 2 (Fielding et al. 2025, in preparation). Right: trajectory of a CR with rL/L ≈ 7 × 10−4 in a 6403 subdomain (represented by the yellow square in the left panel) with side lengths approximately twice the Alfvén scale, lA. The trajectory is color-coded using the logarithm of the particle’s magnetic moment μM averaged over a time window 2π/Ω, where Ω is the gyrofrequency computed using the rms magnetic field strength along the particle’s trajectory. The white lines show a collection of magnetic field lines. The CR trajectory shows that there are various scattering mechanisms at play: μM-conserving magnetic mirroring, where the field lines converge, as well as strong scattering events by large field-line curvature in which μM changes rapidly (see also Figure 5). The latter occur in regions where the magnetic field is weaker and more tangled.
Paper: Self-similar Cosmic-Ray Transport in High-resolution Magnetohydrodynamic Turbulence
Authors: Philipp Kempski, Drummond B. Fielding, Eliot Quataert, Robert J. Ewart, Philipp Grete, Matthew W. Kunz, Alexander A. Philippov, James Stone
Figure caption: Track of a particle with gyroradius rL/L ≈ 3 × 10−4. Faint lines show instantaneous values; dark lines show running averages of tracked quantities over a window 2π/Ω, where Ω is the gyrofrequency computed using the rms magnetic field strength along the particle’s trajectory. Changes in the particle’s magnetic moment (top) are very abrupt and occur when the particle experiences regions of large field-line curvature, ﹩K\equiv | \hat{{\boldsymbol{b}}}\,\cdot \,{\boldsymbol{\nabla }}\hat{{\boldsymbol{b}}}| ﹩, i.e., when K2πc/Ω ≳ 1 (bottom).
Paper: Self-similar Cosmic-Ray Transport in High-resolution Magnetohydrodynamic Turbulence
Authors: Philipp Kempski, Drummond B. Fielding, Eliot Quataert, Robert J. Ewart, Philipp Grete, Matthew W. Kunz, Alexander A. Philippov, James Stone
Figure caption: PDF of field-line curvature K normalized by the curvature K* that maximizes KP(K) (i.e., the most volume-filling logarithmic curvature bin) for the 6403 and 10,2403 simulations. In both cases, KP(K) ∝ K−1.5 at high K. However, as the resolution is increased, the width of the PDF near the peak is broadened significantly. At 10,2403, the power law occurs for K ≳ 10K*, which is significantly larger than the corresponding threshold in the 6403 simulation. We speculate that it is this broadening of the PDF that is responsible for the more efficient scattering along the field lines (pink lines in Figure 4) at higher resolution. See D. B. Fielding et al. (2025, in preparation) for more details.
Paper: XRISM/Resolve Spectroscopy of the Central Engine in the Seyfert-1 AGN Mrk 279
Authors: Jon M. Miller, Xin Xiang, Doyee Byun, 도의 변, Ehud Behar, Laura Brenneman, Edward Cackett, Elisa Costantini, Luigi Gallo, Keith Horne, Elias Kammoun, Chen Li, Abderahmen Zoghbi
Figure caption: Light curves of the XRISM/Resolve observation of Mrk 279. The left panel shows the light curve of the full Resolve band, and the right panel shows the light curve of the filtered 6.3–6.5 keV band (6.1–6.3 keV in the observed frame). The red horizontal line in each panel indicates the mean rate in each band (0.27 ± 0.03 counts s−1 for the full band, 0.011 ± 0.003 counts s−1 for 6.1–6.3 keV), and the horizontal dotted lines indicate the rms of the variations in each curve.
Paper: XRISM/Resolve Spectroscopy of the Central Engine in the Seyfert-1 AGN Mrk 279
Authors: Jon M. Miller, Xin Xiang, Doyee Byun, 도의 변, Ehud Behar, Laura Brenneman, Edward Cackett, Elisa Costantini, Luigi Gallo, Keith Horne, Elias Kammoun, Chen Li, Abderahmen Zoghbi
Figure caption: The time-averaged XRISM/Resolve spectrum of Mrk 279. The data are plotted in the rest frame and binned using the “optimal” algorithm for fitting and by a further factor of 4.0. The model shown in red is the best-fit extended physical model, including three components for the neutral Fe K emission lines, photoionized emission contributing an H-like Fe XXVI line at 6.97 keV, and photoionized absorption from tentative fast wind components. The solid gray lines indicate the lab energies of the neutral Fe Kα and Fe Kβ lines. The dashed gray line indicates the lab energy for the Fe XXVI emission line. The blue and purple lines indicate He-like Fe XXV and H-like Fe XXVI line pairs from potential UFOs at v ≃ 0.22c and v ≃ 0.33c. Please see the text and Table 2.
Paper: XRISM/Resolve Spectroscopy of the Central Engine in the Seyfert-1 AGN Mrk 279
Authors: Jon M. Miller, Xin Xiang, Doyee Byun, 도의 변, Ehud Behar, Laura Brenneman, Edward Cackett, Elisa Costantini, Luigi Gallo, Keith Horne, Elias Kammoun, Chen Li, Abderahmen Zoghbi
Figure caption: The zoomed-in spectrum and the best-fit extended physical model (red), including the breakdown of the components for Fe K emission lines and photoionized emission/absorption lines. The data are plotted in the rest frame.
Paper: XRISM/Resolve Spectroscopy of the Central Engine in the Seyfert-1 AGN Mrk 279
Authors: Jon M. Miller, Xin Xiang, Doyee Byun, 도의 변, Ehud Behar, Laura Brenneman, Edward Cackett, Elisa Costantini, Luigi Gallo, Keith Horne, Elias Kammoun, Chen Li, Abderahmen Zoghbi
Figure caption: Simple model of Mrk 279 with Gaussian-broadened “mytorus” components. The full model is plotted in blue, while the continuum is shown in red. The individual “MYTorus” components are shown in orange, magenta, and purple. The data are plotted in the rest frame.
Paper: XRISM/Resolve Spectroscopy of the Central Engine in the Seyfert-1 AGN Mrk 279
Authors: Jon M. Miller, Xin Xiang, Doyee Byun, 도의 변, Ehud Behar, Laura Brenneman, Edward Cackett, Elisa Costantini, Luigi Gallo, Keith Horne, Elias Kammoun, Chen Li, Abderahmen Zoghbi
Figure caption: A comparison of the inner radii measured for Fe Kα line components in a subset of XRISM spectra of local AGN. All of the radii are based on blurred “mytorus” modeling of Resolve spectra; please see the text for details. With several important caveats, this plot suggests that Resolve data are able to separate line emission from the inner disk, BLR, and torus and capable of tracing trends with Eddington fraction.
Paper: XRISM/Resolve Reveals the Complex Iron Structure of NGC 7213: Evidence for Radial Stratification between Inner Disk and Broad-line Region
Authors: E. Kammoun, T. Kawamuro, K. Murakami, S. Bianchi, F. Nicastro, A. Luminari, E. Aydi, M. Eracleous, O. K. Adegoke, E. Bertola, P. G. Boorman, V. Braito, G. Bruni, A. Comastri, P. Condò, M. Dadina, T. Enoto, J. A. García, V. E. Gianolli, F. A. Harrison, G. Lanzuisi, M. Laurenti, A. Marinucci, G. Mastroserio, H. Matsumoto, G. Matt, G. Matzeu, R. Middei, E. Nardini, H. Noda, H. Odaka, S. Ogawa, F. Panessa, E. Piconcelli, C. Pinto, J. M. Piotrowska, G. Ponti, C. Ricci, R. Ricci, R. Serafinelli, F. Shi, D. Stern, A. Tanimoto, Y. Terashima, R. Tomaru, F. Tombesi, A. Tortosa, Y. Ueda, F. Ursini, C. Vignali, S. Yamada, S. Yamada
Figure caption: Left: the DPB Hα profile of NGC 7213 in velocity space modeled by a DISKLINE with an additional Gaussian smoothing. The negative/positive sign corresponds to blue-/redshift with respect to 6562.8 Å. Right: confidence contours of the disk inclination versus inner radius obtained by modeling the broad Fe Kα line in the XRISM/Resolve spectrum. The shaded regions enclose the 68%, 90%, and 95% posterior probability. The solid contours correspond to the contours derived from a grid of ΔC = 2.3, 4.6,  and 10 (black, red, and blue, respectively), which would correspond to 68%, 90%, and 99.5% confidence levels in the χ2 approximation for two parameters of interest. The green circle shows the best fit obtained by modeling the DPB Hα profile on the left.
Paper: XRISM/Resolve Reveals the Complex Iron Structure of NGC 7213: Evidence for Radial Stratification between Inner Disk and Broad-line Region
Authors: E. Kammoun, T. Kawamuro, K. Murakami, S. Bianchi, F. Nicastro, A. Luminari, E. Aydi, M. Eracleous, O. K. Adegoke, E. Bertola, P. G. Boorman, V. Braito, G. Bruni, A. Comastri, P. Condò, M. Dadina, T. Enoto, J. A. García, V. E. Gianolli, F. A. Harrison, G. Lanzuisi, M. Laurenti, A. Marinucci, G. Mastroserio, H. Matsumoto, G. Matt, G. Matzeu, R. Middei, E. Nardini, H. Noda, H. Odaka, S. Ogawa, F. Panessa, E. Piconcelli, C. Pinto, J. M. Piotrowska, G. Ponti, C. Ricci, R. Ricci, R. Serafinelli, F. Shi, D. Stern, A. Tanimoto, Y. Terashima, R. Tomaru, F. Tombesi, A. Tortosa, Y. Ueda, F. Ursini, C. Vignali, S. Yamada, S. Yamada
Figure caption: Modeling the XRISM/Resolve spectrum (focusing on the Fe region). In addition to the continuum (blue dotted line), we also show the narrow and broad Fe Kα lines (yellow and gray, respectively), the Fe XXV emission lines (orange), the Fe XXVI lines (red), and two Gaussian emission lines added at 6.45 and 6.75 keV (green). The left panel shows the best fit assuming that the broad Fe Kα is described with a ZFEKLOR model smoothed with a Gaussian profile. The right panel shows the best fit assuming that the broad Fe Kα is described with a DISKLINE model. The results in the right panel are based on MCMC analysis. The solid lines and the shaded region correspond to the median profile and the 68% and 95% credibility envelopes of each spectral component, respectively.
Paper: XRISM/Resolve Reveals the Complex Iron Structure of NGC 7213: Evidence for Radial Stratification between Inner Disk and Broad-line Region
Authors: E. Kammoun, T. Kawamuro, K. Murakami, S. Bianchi, F. Nicastro, A. Luminari, E. Aydi, M. Eracleous, O. K. Adegoke, E. Bertola, P. G. Boorman, V. Braito, G. Bruni, A. Comastri, P. Condò, M. Dadina, T. Enoto, J. A. García, V. E. Gianolli, F. A. Harrison, G. Lanzuisi, M. Laurenti, A. Marinucci, G. Mastroserio, H. Matsumoto, G. Matt, G. Matzeu, R. Middei, E. Nardini, H. Noda, H. Odaka, S. Ogawa, F. Panessa, E. Piconcelli, C. Pinto, J. M. Piotrowska, G. Ponti, C. Ricci, R. Ricci, R. Serafinelli, F. Shi, D. Stern, A. Tanimoto, Y. Terashima, R. Tomaru, F. Tombesi, A. Tortosa, Y. Ueda, F. Ursini, C. Vignali, S. Yamada, S. Yamada
Figure caption: Posteriors of line fluxes obtained from the best fit to the XRISM/Resolve data (in units of 10−6 photon s−1 cm−2). Top: line fluxes of the narrow DISKLINE Fe Kα and their sum (yellow, gray, and blue, respectively). Middle: line fluxes of the forbidden and resonant Fe XXV lines and their sum (gray, red, and blue, respectively). Bottom: line fluxes of the Fe XXVI Kα1,2. The solid and dashed lines show the median and the 90% confidence range of the distributions, respectively. The green circles show the best-fit flux lines of the corresponding lines from Chandra/HETG reported by S. Bianchi et al. (2008).
Paper: XRISM/Resolve Reveals the Complex Iron Structure of NGC 7213: Evidence for Radial Stratification between Inner Disk and Broad-line Region
Authors: E. Kammoun, T. Kawamuro, K. Murakami, S. Bianchi, F. Nicastro, A. Luminari, E. Aydi, M. Eracleous, O. K. Adegoke, E. Bertola, P. G. Boorman, V. Braito, G. Bruni, A. Comastri, P. Condò, M. Dadina, T. Enoto, J. A. García, V. E. Gianolli, F. A. Harrison, G. Lanzuisi, M. Laurenti, A. Marinucci, G. Mastroserio, H. Matsumoto, G. Matt, G. Matzeu, R. Middei, E. Nardini, H. Noda, H. Odaka, S. Ogawa, F. Panessa, E. Piconcelli, C. Pinto, J. M. Piotrowska, G. Ponti, C. Ricci, R. Ricci, R. Serafinelli, F. Shi, D. Stern, A. Tanimoto, Y. Terashima, R. Tomaru, F. Tombesi, A. Tortosa, Y. Ueda, F. Ursini, C. Vignali, S. Yamada, S. Yamada
Figure caption: SOAR spectrum of NGC 7213 in the Hα region. We fit the data assuming a power-law continuum and a series of Gaussian emission lines to model the narrow Hα, a broad symmetric Hα line, two broad red-/blueshifted Hα lines, and narrow [N II] λλ6548, 6583 and [S II] λλ6716, 6731 lines. In addition, the data required broad and blueshifted [N II] λλ6548, 6583 and [S II] λλ6716, 6731, as well as a low-amplitude red-/blueshifted doublet at ∼6682 Å and ∼6472 Å, respectively, with an intermediate broadening of ∼900–1000 km s−1.
Paper: XRISM/Resolve Reveals the Complex Iron Structure of NGC 7213: Evidence for Radial Stratification between Inner Disk and Broad-line Region
Authors: E. Kammoun, T. Kawamuro, K. Murakami, S. Bianchi, F. Nicastro, A. Luminari, E. Aydi, M. Eracleous, O. K. Adegoke, E. Bertola, P. G. Boorman, V. Braito, G. Bruni, A. Comastri, P. Condò, M. Dadina, T. Enoto, J. A. García, V. E. Gianolli, F. A. Harrison, G. Lanzuisi, M. Laurenti, A. Marinucci, G. Mastroserio, H. Matsumoto, G. Matt, G. Matzeu, R. Middei, E. Nardini, H. Noda, H. Odaka, S. Ogawa, F. Panessa, E. Piconcelli, C. Pinto, J. M. Piotrowska, G. Ponti, C. Ricci, R. Ricci, R. Serafinelli, F. Shi, D. Stern, A. Tanimoto, Y. Terashima, R. Tomaru, F. Tombesi, A. Tortosa, Y. Ueda, F. Ursini, C. Vignali, S. Yamada, S. Yamada
Figure caption: Top: XRISM/Resolve (black), XMM-Newton/EPIC-pn, and NuSTAR spectra modeled with an absorbed power law with a high-energy cutoff. We also show the corresponding residuals. Bottom: the high-energy cutoff versus photon index confidence regions at the 68%, 95%, and 99% levels (black, red, and blue, respectively).
Paper: XRISM/Resolve Reveals the Complex Iron Structure of NGC 7213: Evidence for Radial Stratification between Inner Disk and Broad-line Region
Authors: E. Kammoun, T. Kawamuro, K. Murakami, S. Bianchi, F. Nicastro, A. Luminari, E. Aydi, M. Eracleous, O. K. Adegoke, E. Bertola, P. G. Boorman, V. Braito, G. Bruni, A. Comastri, P. Condò, M. Dadina, T. Enoto, J. A. García, V. E. Gianolli, F. A. Harrison, G. Lanzuisi, M. Laurenti, A. Marinucci, G. Mastroserio, H. Matsumoto, G. Matt, G. Matzeu, R. Middei, E. Nardini, H. Noda, H. Odaka, S. Ogawa, F. Panessa, E. Piconcelli, C. Pinto, J. M. Piotrowska, G. Ponti, C. Ricci, R. Ricci, R. Serafinelli, F. Shi, D. Stern, A. Tanimoto, Y. Terashima, R. Tomaru, F. Tombesi, A. Tortosa, Y. Ueda, F. Ursini, C. Vignali, S. Yamada, S. Yamada
Figure caption: Data-to-continuum ratio of the XRISM/Resolve spectrum in the Fe line region in the observed frame. The red dashed lines show the expected energies for the low-ionization Fe Kα1,2 and Kβ lines and the high-ionization Fe XXV (w, x, y, z) and Fe XXVI Kα1,2 lines.
Paper: XRISM/Resolve Reveals the Complex Iron Structure of NGC 7213: Evidence for Radial Stratification between Inner Disk and Broad-line Region
Authors: E. Kammoun, T. Kawamuro, K. Murakami, S. Bianchi, F. Nicastro, A. Luminari, E. Aydi, M. Eracleous, O. K. Adegoke, E. Bertola, P. G. Boorman, V. Braito, G. Bruni, A. Comastri, P. Condò, M. Dadina, T. Enoto, J. A. García, V. E. Gianolli, F. A. Harrison, G. Lanzuisi, M. Laurenti, A. Marinucci, G. Mastroserio, H. Matsumoto, G. Matt, G. Matzeu, R. Middei, E. Nardini, H. Noda, H. Odaka, S. Ogawa, F. Panessa, E. Piconcelli, C. Pinto, J. M. Piotrowska, G. Ponti, C. Ricci, R. Ricci, R. Serafinelli, F. Shi, D. Stern, A. Tanimoto, Y. Terashima, R. Tomaru, F. Tombesi, A. Tortosa, Y. Ueda, F. Ursini, C. Vignali, S. Yamada, S. Yamada
Figure caption: Effect of the COR on the best-fit parameters. The left and right panels correspond to the best-fit parameters obtained for modeling the broad Fe Kα with a DISKLINE and a symmetric Gaussian-broadened line, respectively. Panels (a) and (c) show the inner radius for the DISKLINE and the FWHM of the narrow Fe Kα, respectively. Panels (b) and (d) show the FWHM of the broad and narrow Fe Kα lines, respectively. Panel (e) shows the improvement in fit statistics for a DISKLINE with respect to a Gaussian-broadened line (blue circles) and the improvement obtained by including the emission line at 6.45 keV (red squares) for different COR values. Panel (f) shows the S/N of the full spectrum in the 5.5–7.5 keV range (see the text for details).
Paper: XRISM/Resolve Reveals the Complex Iron Structure of NGC 7213: Evidence for Radial Stratification between Inner Disk and Broad-line Region
Authors: E. Kammoun, T. Kawamuro, K. Murakami, S. Bianchi, F. Nicastro, A. Luminari, E. Aydi, M. Eracleous, O. K. Adegoke, E. Bertola, P. G. Boorman, V. Braito, G. Bruni, A. Comastri, P. Condò, M. Dadina, T. Enoto, J. A. García, V. E. Gianolli, F. A. Harrison, G. Lanzuisi, M. Laurenti, A. Marinucci, G. Mastroserio, H. Matsumoto, G. Matt, G. Matzeu, R. Middei, E. Nardini, H. Noda, H. Odaka, S. Ogawa, F. Panessa, E. Piconcelli, C. Pinto, J. M. Piotrowska, G. Ponti, C. Ricci, R. Ricci, R. Serafinelli, F. Shi, D. Stern, A. Tanimoto, Y. Terashima, R. Tomaru, F. Tombesi, A. Tortosa, Y. Ueda, F. Ursini, C. Vignali, S. Yamada, S. Yamada
Figure caption: Confidence contours of the FWHMs of Fe XXV and Fe XXVI. The solid contours correspond to the contours derived from a grid of ΔC = 2.3, 4.6,  and 10 (black, red, and blue, respectively). The green circle shows the corresponding limits reported by S. Bianchi et al. (2008). The dashed gray lines show the FWHM of the symmetric broad Hα line. The solid black line shows the 1:1 relation.
Paper: XRISM/Resolve Reveals the Complex Iron Structure of NGC 7213: Evidence for Radial Stratification between Inner Disk and Broad-line Region
Authors: E. Kammoun, T. Kawamuro, K. Murakami, S. Bianchi, F. Nicastro, A. Luminari, E. Aydi, M. Eracleous, O. K. Adegoke, E. Bertola, P. G. Boorman, V. Braito, G. Bruni, A. Comastri, P. Condò, M. Dadina, T. Enoto, J. A. García, V. E. Gianolli, F. A. Harrison, G. Lanzuisi, M. Laurenti, A. Marinucci, G. Mastroserio, H. Matsumoto, G. Matt, G. Matzeu, R. Middei, E. Nardini, H. Noda, H. Odaka, S. Ogawa, F. Panessa, E. Piconcelli, C. Pinto, J. M. Piotrowska, G. Ponti, C. Ricci, R. Ricci, R. Serafinelli, F. Shi, D. Stern, A. Tanimoto, Y. Terashima, R. Tomaru, F. Tombesi, A. Tortosa, Y. Ueda, F. Ursini, C. Vignali, S. Yamada, S. Yamada
Figure caption: Residual of XRISM/Resolve data after subtracting the power-law continuum (in units of count s−1 cm−2 keV−1), focusing on the observed 6.4–6.9 keV range. The blue line shows the total model fitting the emission lines in the residual. The orange solid and red dashed lines show the Gaussian lines assuming redshifted velocity of ∼8000 km s−1 and ∼4600 km s−1, respectively, assuming Fe XXV and Fe XXVI.
Paper: XRISM/Resolve Reveals the Complex Iron Structure of NGC 7213: Evidence for Radial Stratification between Inner Disk and Broad-line Region
Authors: E. Kammoun, T. Kawamuro, K. Murakami, S. Bianchi, F. Nicastro, A. Luminari, E. Aydi, M. Eracleous, O. K. Adegoke, E. Bertola, P. G. Boorman, V. Braito, G. Bruni, A. Comastri, P. Condò, M. Dadina, T. Enoto, J. A. García, V. E. Gianolli, F. A. Harrison, G. Lanzuisi, M. Laurenti, A. Marinucci, G. Mastroserio, H. Matsumoto, G. Matt, G. Matzeu, R. Middei, E. Nardini, H. Noda, H. Odaka, S. Ogawa, F. Panessa, E. Piconcelli, C. Pinto, J. M. Piotrowska, G. Ponti, C. Ricci, R. Ricci, R. Serafinelli, F. Shi, D. Stern, A. Tanimoto, Y. Terashima, R. Tomaru, F. Tombesi, A. Tortosa, Y. Ueda, F. Ursini, C. Vignali, S. Yamada, S. Yamada
Figure caption: Schematic representation (not to scale), showing the radial stratification of the various emission lines reported in this work, under the assumption of photoionization by centrally concentrated X-ray and UV photons, and showing the broadening of the lines is caused by orbital motion around the SMBH.