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arxiv: 2606.21180 · v1 · pith:NKRS3WW2new · submitted 2026-06-19 · 🌌 astro-ph.HE · astro-ph.GA

XRISM Time-resolved Fe Kα Spectroscopy of NGC 4395: Time-variable Inner-disk Emission

Taiki Kawamuro , Satoshi Yamada , Hirofumi Noda , Yoshiyuki Inoue , Shoji Ogawa , Misaki Mizumoto This is my paper

Pith reviewed 2026-06-26 13:54 UTC · model grok-4.3

classification 🌌 astro-ph.HE astro-ph.GA
keywords NGC 4395XRISMFe K alphaaccretion diskLense-Thirring precessiontime-resolved spectroscopylow-mass AGNblack hole spin
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The pith

Time-resolved XRISM spectra show the inner accretion disk radius and inclination changing in NGC 4395 over hundreds of kiloseconds.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper establishes that XRISM Resolve data, combined with NuSTAR, can resolve time-dependent changes in the relativistically broadened Fe K line from the inner disk of this low-mass AGN. Binning the 400 ks exposure into roughly 87 ks segments reveals clear evolution in the red wing of the line profile. The authors interpret the changes as variations in the inner emission radius plus a possible periodic shift in disk inclination with a 210 ks period. If the period arises from Lense-Thirring precession of a tilted inner flow, the data favor a black-hole mass near the low end of published estimates together with moderate spin.

Core claim

The central claim is that the diskline component of the Fe Kα line varied significantly across the observation. This evolution is consistent with a changing inner radius of the line-emitting region and an inclination modulation on a timescale of approximately 210 ks. Interpreting the modulation as Lense-Thirring precession of a tilted inner flow yields a black-hole mass of roughly 9×10^3 solar masses and a spin parameter a ≳ 0.6.

What carries the argument

The relativistically broadened Fe K component (diskline model) whose inner radius and inclination are allowed to vary between successive 87 ks time bins.

If this is right

  • The inner radius of the Fe K-emitting region in low-mass AGNs can change on timescales of order 100 ks.
  • Disk inclination can exhibit periodic modulation consistent with nodal precession.
  • Precession periods measured this way can select among published black-hole mass estimates for NGC 4395.
  • XRISM Resolve spectra are sufficient to track such relativistic disk dynamics in AGNs.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • The same time-binning approach could be applied to other nearby low-mass AGNs to search for precession signals and thereby constrain spins.
  • Confirmation of the precession interpretation would support the presence of tilted inner flows in at least some AGNs.
  • Future monitoring campaigns lasting multiple 210 ks cycles could test whether the modulation repeats coherently.

Load-bearing premise

The 210 ks modulation period is produced by Lense-Thirring precession of a tilted inner accretion flow whose line emission follows the standard precession formula.

What would settle it

A longer observation that either shows no periodic signal near 210 ks in the diskline inclination or yields a period inconsistent with the precession formula evaluated at the reported mass and spin.

Figures

Figures reproduced from arXiv: 2606.21180 by Hirofumi Noda, Misaki Mizumoto, Satoshi Yamada, Shoji Ogawa, Taiki Kawamuro, Yoshiyuki Inoue.

Figure 1
Figure 1. Figure 1: Xtend 0.5–10 keV count map centered on NGC 4395. Blue squares indicate the footprint of the Resolve pixel array. Black arrows mark the AGN and two nearby X-ray sources, XRS1 and XRS2. Our NuSTAR observation (ObsID 91001636002) started on 2024 November 8, about 100 ks after the start of the XRISM observation. It lasted for ≈154 ks with a net exposure of ≈81 ks. 3. DATA ANALYSIS We analyzed the XRISM and NuS… view at source ↗
Figure 2
Figure 2. Figure 2: Background-subtracted Xtend (2–10 keV), Resolve (2–10 keV), and NuSTAR (8–24 keV) light curves, binned at 5 ks. In panel b, the dashed line marks the median count rate. The blue and orange bars indicate the time intervals used for the time-resolved spectral analyses in Sections 3.3.3 and 3.3.4. The intervals divide the observation into 2 segments (top), 5 segments (middle), and 10 segments (bottom). (12h26… view at source ↗
Figure 3
Figure 3. Figure 3: Joint continuum fit to Resolve (black), NuS￾TAR/FPMA (blue), and FPMB (yellow) spectra extracted during the ∼ 80 ks NuSTAR observation. The Fe band (5.5–7.5 keV) is excluded in the fit. Solid lines show the best-fit models; for Resolve, the dashed and dot–dashed lines indicate the power-law and NXB components, respectively. The lower panel shows data-to-model ratios. we examined how the relation between th… view at source ↗
Figure 4
Figure 4. Figure 4: Left: Resolve spectrum (black crosses) and best-fit AGN model (red line). The broadened and narrow MYTorusL components are shown in orange and blue, respectively, and the powerlaw and reflection continuum components are indicated by the black dashed lines. The NXB model is shown by the dashed gray line. Right: Zoomed-in view of the Fe band. Finer binning is adopted to highlight the Fe Kα1 and Fe Kα2 compon… view at source ↗
Figure 5
Figure 5. Figure 5: Resolve spectra from the first (left) and second (right) halves of the observation, highlighting the time variation in the broadened Fe K profile. The figures are shown in the same manner as those in [PITH_FULL_IMAGE:figures/full_fig_p006_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Time evolution of best-fit parameters obtained from five time-resolved spectra. From top to bottom, the parameters are the hydrogen column density (1022 cm−2 ) and covering fraction of the partial absorber, the power-law normalization (10−4 photons keV−1 cm−2 s −1 at 1 keV), the inner radius (Rg), inclination angle (deg), and normalization (10−4 photons keV−1 cm−2 s −1 ) of the broad-line compo￾nent, and t… view at source ↗
Figure 7
Figure 7. Figure 7: Ten time-resolved Resolve spectra obtained by dividing the exposure into 10 segments. The figures are shown in the same manner as [PITH_FULL_IMAGE:figures/full_fig_p010_7.png] view at source ↗
Figure 8
Figure 8. Figure 8 [PITH_FULL_IMAGE:figures/full_fig_p010_8.png] view at source ↗
Figure 10
Figure 10. Figure 10: Observed modulation period of 213 ± 9 ks (red horizontal line) compared with LT-precession periods predicted by the rigid-disk model of A. Franchini et al. (2016) as a function of BH spin. Curves with shaded dark bands show the predictions for two BH-mass assumptions, MBH = 9.1 +1.5 −1.6 × 103M⊙ and 3.6 ± 1.1 × 105M⊙, using Rin = 100 Rg and Rout = 1.3 × 102 Rg. Here, Rin is the rep￾resentative value obtai… view at source ↗
Figure 11
Figure 11. Figure 11: Results of the Monte Carlo tests for different spectral grouping prescriptions. Top left: distributions of Cprefit/Cexp,prefit and Cpostfit/Cexp,postfit. Top right: distributions of the normalized statistic, (C − Cexp)/ √ Cv. Bottom: distributions of the number of counts per spectral bin. Gray, blue, and orange boxes denote optimal binning, fixed minimum– count grouping, and flux-amplified cases, respecti… view at source ↗
read the original abstract

We report the first XRISM observation of the low-mass AGN in the nearby dwarf galaxy NGC 4395 ($M_{\rm BH}\sim10^{4-5}\,M_\odot$), complemented by a simultaneous NuSTAR observation. We constrained the continuum by jointly fitting the XRISM/Resolve (2-12 keV) and NuSTAR (3-30 keV) spectra while excluding the Fe K band (5.5-7.5 keV). Relative to this baseline continuum, the time-averaged Resolve spectrum revealed an unresolved neutral Fe K$\alpha$ core with a velocity width of $\lesssim$110 km s$^{-1}$ and an adjacent redward wing. The red wing was well reproduced by an additional relativistically broadened Fe K component. Furthermore, time-resolved spectroscopy with $\approx$87 ks bins showed that the diskline profile varied significantly over the $\sim$400 ks observation. This evolution can be interpreted in terms of changes in the inner radius of the line-emitting region, together with a possible inclination modulation with a period of $\approx$210 ks. If interpreted as Lense-Thirring precession of a tilted inner flow, the observed period would favor the low end of the black hole mass estimates ($M_{\rm BH}\approx9\times10^3\,M_\odot$) and imply a moderate spin ($a\gtrsim0.6$). These results highlight the capability of XRISM to track relativistic disk dynamics in AGNs.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 1 minor

Summary. The paper reports the first XRISM observation of the low-mass AGN NGC 4395, jointly with NuSTAR. After fitting the continuum outside the Fe K band, the time-averaged Resolve spectrum shows an unresolved neutral Fe Kα core (velocity width ≲110 km s⁻¹) plus a red wing modeled as a relativistically broadened diskline. Time-resolved spectroscopy in ≈87 ks bins over the ∼400 ks exposure reveals significant evolution in the diskline profile, interpreted as changes in inner radius together with a possible inclination modulation of period ≈210 ks. If this modulation is Lense-Thirring precession of a tilted inner flow, the period favors the low end of existing M_BH estimates (≈9×10³ M_⊙) and implies moderate spin (a≳0.6).

Significance. If the time-resolved spectral evolution and its precession interpretation hold, the result provides a direct dynamical probe of the inner accretion flow in a low-mass AGN and demonstrates XRISM’s ability to resolve relativistic line variability on ∼100 ks timescales. The mass and spin constraints are derived from the standard Lense-Thirring formula applied to an observed period rather than from a new fitted parameter, which is a strength if the geometric assumptions are validated.

major comments (2)
  1. [time-resolved spectroscopy] Time-resolved spectroscopy section: the claim of a statistically significant ≈210 ks inclination modulation must be supported by explicit tests showing that the periodic signal is not an artifact of parameter degeneracies between r_in and i or of stochastic variability; without such tests the mapping from observed line-profile changes to a unique precession period (and thence to M_BH and a) is not demonstrated.
  2. [discussion] Discussion of Lense-Thirring interpretation: the application of the standard precession-period formula assumes that the fitted inner radius traces the precessing region, that warp propagation and external torques can be neglected, and that the 87 ks binning captures a coherent signal; these assumptions are load-bearing for the quoted M_BH≈9×10³ M_⊙ and a≳0.6 values and require quantitative justification or sensitivity checks.
minor comments (1)
  1. [abstract] Abstract and text: the velocity width of the unresolved core is stated as ≲110 km s⁻¹; confirm whether this is the 1σ or 90% upper limit and whether it is consistent with the instrumental resolution after accounting for any residual broadening.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading and constructive comments on our XRISM observation of NGC 4395. We agree that the time-resolved analysis and Lense-Thirring interpretation require additional supporting tests and quantitative checks to be fully robust. Below we address each major comment and outline the revisions we will make.

read point-by-point responses

  1. Referee: [time-resolved spectroscopy] Time-resolved spectroscopy section: the claim of a statistically significant ≈210 ks inclination modulation must be supported by explicit tests showing that the periodic signal is not an artifact of parameter degeneracies between r_in and i or of stochastic variability; without such tests the mapping from observed line-profile changes to a unique precession period (and thence to M_BH and a) is not demonstrated.

    Authors: We agree that explicit validation is required. In the revised manuscript we will add Monte Carlo simulations of the time-resolved spectra that (i) inject stochastic variability consistent with the observed count rates and (ii) explore the r_in–i degeneracy by refitting with one parameter fixed while allowing the other to vary. These tests will quantify the significance of the ≈210 ks modulation and demonstrate that it is not an artifact, thereby supporting the subsequent mapping to precession period, M_BH and spin. revision: yes

  2. Referee: [discussion] Discussion of Lense-Thirring interpretation: the application of the standard precession-period formula assumes that the fitted inner radius traces the precessing region, that warp propagation and external torques can be neglected, and that the 87 ks binning captures a coherent signal; these assumptions are load-bearing for the quoted M_BH≈9×10³ M_⊙ and a≳0.6 values and require quantitative justification or sensitivity checks.

    Authors: We acknowledge that these assumptions are central. The revised discussion will include a new subsection that (i) justifies why the fitted r_in can be taken as representative of the precessing region given the observed line profile, (ii) cites supporting simulations from the literature on warp propagation timescales in low-mass AGN, and (iii) presents sensitivity checks in which the precession period is recomputed after varying the inner radius by ±20 % and the binning by one time step. The impact on the derived M_BH and a will be shown explicitly. revision: yes

Circularity Check

0 steps flagged

No significant circularity; derivation applies external formula to independently measured period.

full rationale

The paper extracts a ~210 ks modulation period directly from time-binned spectral fits to the diskline parameters (inner radius and inclination) across the ~400 ks observation. It then applies the standard Lense-Thirring precession formula to that measured period to obtain mass and spin bounds. No step reduces the claimed result to a fitted parameter or self-citation by construction; the precession formula is an external relation, the period is data-driven, and the interpretation is presented conditionally ('if interpreted as'). The central claim therefore remains independent of its inputs.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The claim rests on standard domain assumptions about the origin of the Fe Kα line and applicability of Lense-Thirring precession; no new entities postulated and limited free parameters beyond standard spectral model components.

free parameters (2)
  • inner disk radius
    Allowed to vary across time bins to reproduce changing line profile
  • disk inclination
    Modulated with ~210 ks period to fit time evolution
axioms (2)
  • domain assumption The Fe Kα emission originates from the inner accretion disk and experiences relativistic broadening
    Invoked to model the red wing and its time variation in the Resolve spectra
  • domain assumption The ~210 ks period represents Lense-Thirring precession of a tilted inner flow
    Used to convert observed period into black hole mass and spin constraints

pith-pipeline@v0.9.1-grok · 5826 in / 1483 out tokens · 27077 ms · 2026-06-26T13:54:14.878415+00:00 · methodology

discussion (0)

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Reference graph

Works this paper leans on

38 extracted references · 37 canonical work pages · 3 internal anchors

  1. [1]

    IEEE Transactions on Automatic Control , volume =

    Akaike, H. 1974, IEEE Transactions on Automatic Control, 19, 716, doi: 10.1109/TAC.1974.1100705

    work page doi:10.1109/tac.1974.1100705 1974

  2. [2]

    Arnaud, K. A. 1996, Astronomical Society of the Pacific Conference Series, Vol. 101, XSPEC: The First Ten Years, ed. G. H. Jacoby & J. Barnes, 17 Astropy Collaboration, Robitaille, T. P., Tollerud, E. J., et al. 2013, A&A, 558, A33, doi: 10.1051/0004-6361/201322068 Astropy Collaboration, Price-Whelan, A. M., Sip˝ ocz, B. M., et al. 2018, AJ, 156, 123, doi...

    work page doi:10.1051/0004-6361/201322068 1996

  3. [3]

    The Lense-Thirring Effect and Accretion Disks around Kerr Black Holes[J/OL]

    Bardeen, J. M., & Petterson, J. A. 1975, ApJL, 195, L65, doi: 10.1086/181711

    work page doi:10.1086/181711 1975

  4. [4]

    W., & Reynolds, C

    Brenneman, L. W., & Reynolds, C. S. 2006, ApJ, 652, 1028, doi: 10.1086/508146

    work page doi:10.1086/508146 2006

  5. [5]

    W., Wilkins, D

    Brenneman, L. W., Wilkins, D. R., Ogorza lek, A., et al. 2025, ApJ, 995, 200, doi: 10.3847/1538-4357/ae1225

    work page doi:10.3847/1538-4357/ae1225 2025

  6. [6]

    P., & Anderson, D

    Burnham, K. P., & Anderson, D. R. 2002, Information and Likelihood Theory: A Basis for Model Selection and Inference (New York, NY: Springer), 49–97, doi: 10.1007/978-0-387-22456-5 2

    work page doi:10.1007/978-0-387-22456-5 2002

  7. [7]

    , keywords =

    Cash, W. 1979, ApJ, 228, 939, doi: 10.1086/156922 den Brok, M., Seth, A. C., Barth, A. J., et al. 2015, ApJ, 809, 101, doi: 10.1088/0004-637X/809/1/101

    work page doi:10.1086/156922 1979

  8. [8]

    E., Brown, G

    Eckart, M. E., Brown, G. V., Chiao, M. P., et al. 2024, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 13093, Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray, ed. J.-W. A. den Herder, S. Nikzad, & K. Nakazawa, 130931P, doi: 10.1117/12.3019276

    work page doi:10.1117/12.3019276 2024

  9. [9]

    C., Rees, M

    Fabian, A. C., Rees, M. J., Stella, L., & White, N. E. 1989, MNRAS, 238, 729, doi: 10.1093/mnras/238.3.729

    work page doi:10.1093/mnras/238.3.729 1989

  10. [10]

    Hydrodynamic Simulations of Tilted Thick-Disk Accretion onto a Kerr Black Hole[J/OL]

    Fragile, P. C., & Anninos, P. 2005, ApJ, 623, 347, doi: 10.1086/428433

    work page doi:10.1086/428433 2005

  11. [11]

    Tilted Accretion Disks[J/OL]

    Fragile, P. C., & Liska, M. 2024, arXiv e-prints, arXiv:2404.10052, doi: 10.48550/arXiv.2404.10052

    work page doi:10.48550/arxiv.2404.10052 2024

  12. [12]

    Lense-Thirring precession around supermassive black holes during tidal disruption events[J/OL]

    Franchini, A., Lodato, G., & Facchini, S. 2016, MNRAS, 455, 1946, doi: 10.1093/mnras/stv2417

    work page doi:10.1093/mnras/stv2417 2016

  13. [13]

    Complex Nuclear Structure in Seyfert 2 Galaxy NGC 4388 Revealed by XRISM Observation

    Fujiwara, K., Ueda, Y., Ogawa, S., et al. 2026, arXiv e-prints, arXiv:2604.06719, doi: 10.48550/arXiv.2604.06719

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2604.06719 2026

  14. [14]

    M., & Fabian, A

    George, I. M., & Fabian, A. C. 1991, MNRAS, 249, 352, doi: 10.1093/mnras/249.2.352

    work page doi:10.1093/mnras/249.2.352 1991

  15. [15]

    and Craig, William W

    Harrison, F. A., Craig, W. W., Christensen, F. E., et al. 2013, ApJ, 770, 103, doi: 10.1088/0004-637X/770/2/103

    work page doi:10.1088/0004-637x/770/2/103 2013

  16. [16]

    , keywords =

    Haynes, M. P., Hogg, D. E., Maddalena, R. J., Roberts, M. S., & van Zee, L. 1998, AJ, 115, 62, doi: 10.1086/300166 HI4PI Collaboration, Ben Bekhti, N., Fl¨ oer, L., et al. 2016, A&A, 594, A116, doi: 10.1051/0004-6361/201629178 H¨ olzer, G., Fritsch, M., Deutsch, M., H¨ artwig, J., & F¨ orster, E. 1997, PhRvA, 56, 4554, doi: 10.1103/PhysRevA.56.4554

    work page doi:10.1086/300166 1998

  17. [17]

    L., Awaki, H., et al

    Ishisaki, Y., Kelley, R. L., Awaki, H., et al. 2025, Journal of Astronomical Telescopes, Instruments, and Systems, 11, 042023, doi: 10.1117/1.JATIS.11.4.042023

    work page doi:10.1117/1.jatis.11.4.042023 2025

  18. [18]

    Iwasawa, K., Tanaka, Y., & Gallo, L. C. 2010, A&A, 514, A58, doi: 10.1051/0004-6361/200912431

    work page doi:10.1051/0004-6361/200912431 2010

  19. [19]

    Kaastra, J. S. 2017, A&A, 605, A51, doi: 10.1051/0004-6361/201629319

    work page doi:10.1051/0004-6361/201629319 2017

  20. [20]

    S., & Bleeker, J

    Kaastra, J. S., & Bleeker, J. A. M. 2016, A&A, 587, A151, doi: 10.1051/0004-6361/201527395

    work page doi:10.1051/0004-6361/201527395 2016

  21. [21]

    S., Nardini, E., Zoghbi, A., et al

    Kammoun, E. S., Nardini, E., Zoghbi, A., et al. 2019, ApJ, 886, 145, doi: 10.3847/1538-4357/ab5110

    work page doi:10.3847/1538-4357/ab5110 2019

  22. [22]

    L., Ishisaki, Y., Costantini, E., et al

    Kelley, R. L., Ishisaki, Y., Costantini, E., et al. 2025, Journal of Astronomical Telescopes, Instruments, and Systems, 11, 042026, doi: 10.1117/1.JATIS.11.4.042026

    work page doi:10.1117/1.jatis.11.4.042026 2025

  23. [23]

    1918, Physikalische Zeitschrift, 19, 156

    Lense, J., & Thirring, H. 1918, Physikalische Zeitschrift, 19, 156

    1918

  24. [24]

    M., Beard, M., Breedt, E., et al

    McHardy, I. M., Beard, M., Breedt, E., et al. 2023, MNRAS, 519, 3366, doi: 10.1093/mnras/stac3651

    work page doi:10.1093/mnras/stac3651 2023

  25. [25]

    M., Xiang, X., Byun, D., et al

    Miller, J. M., Xiang, X., Byun, D., et al. 2025, ApJL, 994, L10, doi: 10.3847/2041-8213/ae1606 16

    work page doi:10.3847/2041-8213/ae1606 2025

  26. [26]

    C., Eracleous, M., Leighly, K

    Moran, E. C., Eracleous, M., Leighly, K. M., et al. 2005, AJ, 129, 2108, doi: 10.1086/429522

    work page doi:10.1086/429522 2005

  27. [27]

    L., & Rankin, J

    Murphy, K. D., & Yaqoob, T. 2009, MNRAS, 397, 1549, doi: 10.1111/j.1365-2966.2009.15025.x

    work page doi:10.1111/j.1365-2966.2009.15025.x 2009

  28. [28]

    J., Johnston, S., Ray, P

    Nardini, E., & Risaliti, G. 2011, MNRAS, 417, 2571, doi: 10.1111/j.1365-2966.2011.19423.x

    work page doi:10.1111/j.1365-2966.2011.19423.x 2011

  29. [29]

    2025, PASJ, 77, S10, doi: 10.1093/pasj/psaf011

    Noda, H., Mori, K., Tomida, H., et al. 2025, PASJ, 77, S10, doi: 10.1093/pasj/psaf011

    work page doi:10.1093/pasj/psaf011 2025

  30. [30]

    Papaloizou, J. C. B., & Terquem, C. 1995, MNRAS, 274, 987, doi: 10.1093/mnras/274.4.987

    work page doi:10.1093/mnras/274.4.987 1995

  31. [31]

    M., Bentz, M

    Peterson, B. M., Bentz, M. C., Desroches, L.-B., et al. 2005, ApJ, 632, 799, doi: 10.1086/444494

    work page doi:10.1086/444494 2005

  32. [32]

    BAT AGN Spectroscopic Survey - V. X-ray properties of the Swift/BAT 70-month AGN catalog

    Ricci, C., Trakhtenbrot, B., Koss, M. J., et al. 2017, ApJS, 233, 17, doi: 10.3847/1538-4365/aa96ad

    work page internal anchor Pith review doi:10.3847/1538-4365/aa96ad 2017

  33. [33]

    C., et al

    Tanaka, Y., Nandra, K., Fabian, A. C., et al. 1995, Nature, 375, 659, doi: 10.1038/375659a0

    work page doi:10.1038/375659a0 1995

  34. [34]

    , keywords =

    Tanimoto, A., Ueda, Y., Odaka, H., et al. 2019, ApJ, 877, 95, doi: 10.3847/1538-4357/ab1b20

    work page doi:10.3847/1538-4357/ab1b20 2019

  35. [35]

    2025, PASJ, 77, S1, doi: 10.1093/pasj/psaf023

    Tashiro, M., Kelley, R., Watanabe, S., et al. 2025, PASJ, 77, S1, doi: 10.1093/pasj/psaf023

    work page doi:10.1093/pasj/psaf023 2025

  36. [36]

    H., Johnston, S., & Das, P

    Vaughan, S., Iwasawa, K., Fabian, A. C., & Hayashida, K. 2005, MNRAS, 356, 524, doi: 10.1111/j.1365-2966.2004.08463.x

    work page doi:10.1111/j.1365-2966.2004.08463.x 2005

  37. [37]

    Time-resolved XRISM spectroscopy reveals the evolution and structure of the corona in MCG-6-30-15

    Wilkins, D. R., Brenneman, L. W., Ogorzalek, A., et al. 2026, arXiv e-prints, arXiv:2604.09761, doi: 10.48550/arXiv.2604.09761

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2604.09761 2026

  38. [38]

    2019, Nature Astronomy, 3, 755, doi: 10.1038/s41550-019-0790-3 XRISM Collaboration, Audard, M., Awaki, H., et al

    Woo, J.-H., Cho, H., Gallo, E., et al. 2019, Nature Astronomy, 3, 755, doi: 10.1038/s41550-019-0790-3 XRISM Collaboration, Audard, M., Awaki, H., et al. 2024, ApJL, 973, L25, doi: 10.3847/2041-8213/ad7397 XRISM Collaboration, Audard, M., Awaki, H., et al. 2026, Nature Astronomy, doi: 10.1038/s41550-026-02817-6

    work page doi:10.1038/s41550-019-0790-3 2019