pith. sign in

arxiv: 2606.28915 · v1 · pith:XV7DVZP5new · submitted 2026-06-27 · 🌌 astro-ph.HE · astro-ph.SR

Tracing the Orbital Motion of the Accreting White Dwarf in EX~Hydrae with XRISM/Resolve

Yuken Ohshiro , Yukikatsu Terada , Taichi Ichikawa , Yugo Motogami , Manabu Ishida , Koji Mukai , Masayoshi Nobukawa , Takayuki Hayashi
show 2 more authors
Mariko Kimura Mai Takeo
This is my paper

Pith reviewed 2026-06-30 08:52 UTC · model grok-4.3

classification 🌌 astro-ph.HE astro-ph.SR
keywords white dwarfsX-ray spectroscopyorbital motionFe K linesaccretionintermediate polarsEX Hydrae
0
0 comments X

The pith

High-resolution X-ray spectroscopy traces the white dwarf's orbital motion in EX Hydrae using iron line centroids.

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

The paper establishes that the centroids of Fe XXV Kα lines in EX Hydrae modulate coherently with the binary orbital period. This modulation directly measures the white dwarf's radial velocity amplitude as 58.1 ± 8.5 km/s. The result agrees with optical and UV measurements and leads to a white dwarf mass of 0.79 ± 0.04 solar masses when combined with other orbital parameters. A reader would care because it shows a new X-ray method to determine masses of accreting white dwarfs.

Core claim

The Fe XXV Kα components show coherent orbital modulation, yielding K1 = 58.1 ± 8.5 km s^{-1}. This is the first detection of orbital modulation in individual Fe K-shell lines from an accreting WD. Combining this X-ray measurement with literature orbital parameters derives a WD mass of M1 = 0.79 ± 0.04 M⊙.

What carries the argument

The orbital modulation of the centroids of individual Fe K-shell emission lines, which provides a Doppler tracer of the white dwarf's motion.

Load-bearing premise

The observed Fe K-shell line centroids are formed in material that moves with the white dwarf and are not significantly contaminated by other emission sources.

What would settle it

A measurement showing that the Fe line centroids do not vary with the known orbital period or produce a K1 inconsistent with optical data would falsify the claim.

Figures

Figures reproduced from arXiv: 2606.28915 by Koji Mukai, Mai Takeo, Manabu Ishida, Mariko Kimura, Masayoshi Nobukawa, Taichi Ichikawa, Takayuki Hayashi, Yugo Motogami, Yuken Ohshiro, Yukikatsu Terada.

Figure 1
Figure 1. Figure 1: (a) Light curves in the 1.7–10 keV band with 64 s bins, color-coded by orbital phase for clarity. Gray shaded regions mark the good-time intervals (GTIs); only 64 s bins fully contained within GTIs are plotted. The orbital phase is defined using the BJD(TDB) eclipse ephemeris described in the text. (b) Folded light curve in the 1.7–10 keV band of EX Hya with 256 phase bins per cycle. The data are repeated … view at source ↗
Figure 2
Figure 2. Figure 2: Count-rate maps in the Fe K band as a function of energy and orbital phase. The maps are constructed with an energy bin size of 0.5 eV and an orbital-phase bin size of 0.0625 (16 bins per cycle), and are displayed after Gaussian smoothing for visual clarity, with σ = 2 bins in both directions, corresponding to 1.0 eV in energy and 0.125 in orbital phase. The orbital phase is shown over two cycles on the ve… view at source ↗
Figure 3
Figure 3. Figure 3: Phase-resolved spectra in the Fe K band (6.2–7.2 keV) with the best-fit models. Residuals are shown as (data − model)/error. The vertical gray lines indicate the rest-frame energies of the labeled transitions (G. H¨olzer et al. 1997; V. A. Yerokhin & V. M. Shabaev 2015; V. A. Yerokhin & A. Surzhykov 2019) [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Orbital modulation of the four spectral com￾ponents used in the velocity-modulation fit, shown over two cycles by repeating the phase-binned velocities. Gray dashed curves and dotted horizontal lines show independent sinu￾soidal fits and their fitted mean velocities for each compo￾nent. Orange solid curves and dashed horizontal lines are shown only for the two Fe xxv tracers, bvcempow and zgauss 1, and rep… view at source ↗
Figure 5
Figure 5. Figure 5: Line-of-sight component of the XRISM spacecraft velocity toward EX Hya evaluated for screened events. Positive values correspond to spacecraft motion toward EX Hya. Points are colored by the orbital phase bins used for the phase-resolved spectroscopy, and horizontal dashed lines show the phase-bin averages. APPENDIX A. CHECKS ON PHASE-DEPENDENT SYSTEMATICS A.1. Sampling of the projected spacecraft velocity… view at source ↗
Figure 6
Figure 6. Figure 6: Spin-phase sampling within the orbital phase bins for the 1.7–10 keV screened events. The bar height gives the event counts in each orbital phase bin ibin, and the stacked colored segments show the contributions from the WD spin-phase bins jbin. Both sets of bins use the centered-bin definition adopted for the phase-resolved spectroscopy. The orbital phase is calculated with the eclipse ephemeris of J. Ech… view at source ↗
read the original abstract

Measuring the masses of accreting white dwarfs (WDs) is crucial for understanding their evolution and the physics of accretion. High-resolution X-ray spectroscopy can trace the WD motion through Doppler shifts of emission lines formed close to the WD. We report an 83~ks XRISM/Resolve observation of the intermediate polar EX~Hydrae and measure the orbital modulation of individual Fe K-shell line centroids. The Fe~{\sc xxv} K$\alpha$ components show coherent orbital modulation, yielding $K_1 = 58.1 \pm 8.5\ \mathrm{km\ s^{-1}}$. This is the first detection of orbital modulation in individual Fe K-shell lines from an accreting WD, made possible by the high spectral resolution of Resolve and its frequent in-orbit gain calibration. The measured $K_1$ is consistent with optical/UV $K_1$ measurements, providing a cross-check that these distinct tracers follow the WD orbital motion. Combining this X-ray measurement with literature orbital parameters, we derive a WD mass of $M_1 = 0.79 \pm 0.04\ M_\odot$. These results demonstrate that high-resolution X-ray spectroscopy can use individual Fe K-shell line centroids to trace WD orbital motion in accreting WDs.

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

1 major / 1 minor

Summary. The manuscript reports an 83 ks XRISM/Resolve observation of the intermediate polar EX Hydrae. It measures coherent orbital modulation in the centroids of individual Fe XXV Kα line components, yielding K1 = 58.1 ± 8.5 km s^{-1} (first such detection in X-rays), consistent with published optical/UV values. Combining this with literature orbital parameters, it derives a white dwarf mass M1 = 0.79 ± 0.04 M⊙ and argues that high-resolution X-ray spectroscopy can trace WD orbital motion via Fe K-shell lines.

Significance. If the K1 measurement is robust, the result provides an independent X-ray-based mass for an accreting WD and demonstrates a new observational capability enabled by Resolve's spectral resolution and gain calibration. The cross-check against optical K1 strengthens the case that the X-ray lines trace the same motion, with potential extension to other intermediate polars where optical data are limited.

major comments (1)
  1. [Abstract and Fe XXV Kα centroid analysis] The central claim that the measured K1 traces the WD orbital velocity (abstract; implied in the Fe XXV Kα centroid analysis) rests on the assumption that emission from the post-shock accretion column and curtains does not introduce phase-dependent centroid shifts at the orbital phases used for the fit. The manuscript notes consistency with optical K1 but does not quantify the possible contribution of bulk motion or illumination effects in these regions to the observed modulation amplitude.
minor comments (1)
  1. [Results section] The uncertainty on K1 (8.5 km s^{-1}) and the derived mass should be explicitly compared to the range of published optical K1 values to clarify the degree of agreement.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive review and recommendation of minor revision. We address the major comment below.

read point-by-point responses

  1. Referee: [Abstract and Fe XXV Kα centroid analysis] The central claim that the measured K1 traces the WD orbital velocity (abstract; implied in the Fe XXV Kα centroid analysis) rests on the assumption that emission from the post-shock accretion column and curtains does not introduce phase-dependent centroid shifts at the orbital phases used for the fit. The manuscript notes consistency with optical K1 but does not quantify the possible contribution of bulk motion or illumination effects in these regions to the observed modulation amplitude.

    Authors: We acknowledge the referee's point that the manuscript relies on the consistency with optical K1 without a quantitative assessment of potential contributions from the post-shock region. The strongest evidence remains the agreement between the X-ray-derived K1 = 58.1 ± 8.5 km s^{-1} and published optical/UV values, which would be unlikely if significant phase-dependent shifts from bulk motions were present. Nevertheless, to strengthen the paper, we will add a short discussion paragraph outlining why such effects are expected to be minimal for the Fe XXV lines formed near the WD surface, and noting the limitation. This constitutes a partial revision to address the concern explicitly. revision: partial

Circularity Check

0 steps flagged

No circularity: K1 measured directly from line centroids; M1 from standard equations with external parameters

full rationale

The derivation extracts K1=58.1±8.5 km s^{-1} by fitting the observed orbital-phase modulation of Fe XXV Kα centroid velocities in the XRISM data. The white-dwarf mass is then obtained from the standard spectroscopic mass function using this K1 together with literature values for P_orb, i, and K2. No quantity is defined in terms of itself, no fitted parameter is relabeled as a prediction, and no load-bearing premise reduces to a self-citation. The optical/UV consistency is presented only as an external cross-check. The assumption that the line-forming gas co-moves with the WD is a correctness concern, not a circularity in the reported chain.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The measurement relies on standard assumptions of binary orbital motion and line formation near the white dwarf. No new free parameters are introduced beyond the usual line-fitting parameters; no new entities are postulated.

axioms (2)
  • domain assumption The observed line centroids trace the orbital motion of the white dwarf without significant velocity contributions from other system components at the sampled phases.
    Invoked when converting measured K1 directly to white dwarf orbital velocity.
  • standard math Standard Keplerian binary orbit equations and published values for orbital period, inclination, and secondary velocity apply without modification.
    Used to convert K1 into white dwarf mass.

pith-pipeline@v0.9.1-grok · 5815 in / 1653 out tokens · 37094 ms · 2026-06-30T08:52:56.430927+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

43 extracted references · 42 canonical work pages · 2 internal anchors

  1. [1]

    1973, Progress of Theoretical Physics, 49, 1184, doi: 10.1143/PTP.49.1184

    Aizu, K. 1973, Progress of Theoretical Physics, 49, 1184, doi: 10.1143/PTP.49.1184

    work page doi:10.1143/ptp.49.1184 1973

  2. [2]

    S., O’Mara, B

    Allan, A., Hellier, C., & Beardmore, A. 1998, Monthly Notices of the Royal Astronomical Society, 295, 167, doi: 10.1046/j.1365-8711.1998.29511353.x

    work page doi:10.1046/j.1365-8711.1998.29511353.x 1998

  3. [3]

    Arnaud, K. A. 1996, in Astronomical Data Analysis Software and Systems V, Vol. 101, 17

    1996

  4. [4]

    2003, The Astrophysical Journal, 587, 373, doi: 10.1086/368180

    Szkody, P. 2003, The Astrophysical Journal, 587, 373, doi: 10.1086/368180

    work page doi:10.1086/368180 2003

  5. [5]

    2008, Astronomy & Astrophysics, 480, 199, doi: 10.1051/0004-6361:20079010

    Beuermann, K., & Reinsch, K. 2008, Astronomy & Astrophysics, 480, 199, doi: 10.1051/0004-6361:20079010

    work page doi:10.1051/0004-6361:20079010 2008

  6. [6]

    2024a, Astronomy & Astrophysics, 686, A304, doi: 10.1051/0004-6361/202244473

    Beuermann, K., & Reinsch, K. 2024a, Astronomy & Astrophysics, 686, A304, doi: 10.1051/0004-6361/202244473

    work page doi:10.1051/0004-6361/202244473

  7. [7]

    2024b, Astronomy & Astrophysics, 687, A273, doi: 10.1051/0004-6361/202450486

    Beuermann, K., & Reinsch, K. 2024b, Astronomy & Astrophysics, 687, A273, doi: 10.1051/0004-6361/202450486

    work page doi:10.1051/0004-6361/202450486

  8. [8]

    1979, The Astrophysical Journal, 228, 939, doi: 10.1086/156922

    Cash, W. 1979, The Astrophysical Journal, 228, 939, doi: 10.1086/156922

    work page doi:10.1086/156922 1979

  9. [9]

    Eastman, J., Siverd, R., & Gaudi, B. S. 2010, Publications of the Astronomical Society of the Pacific, 122, 935, doi: 10.1086/655938 Echevarr´ ıa, J., Ram´ ırez-Torres, A., Michel, R., & Hern´ andez Santisteban, J. V. 2016, Monthly Notices of the Royal Astronomical Society, 461, 1576, doi: 10.1093/mnras/stw1425

    work page doi:10.1086/655938 2010

  10. [10]

    E., Brown, G

    Eckart, M. E., Brown, G. V., Chiao, M. P., et al. 2025, Journal of Astronomical Telescopes, Instruments, and Systems, 11, 042018, doi: 10.1117/1.JATIS.11.4.042018

    work page doi:10.1117/1.jatis.11.4.042018 2025

  11. [11]

    R., Ji, L., Smith, R

    Foster, A. R., Ji, L., Smith, R. K., & Brickhouse, N. S. 2012, The Astrophysical Journal, 756, 128, doi: 10.1088/0004-637X/756/2/128

    work page doi:10.1088/0004-637x/756/2/128 2012

  12. [12]

    2014a, Monthly Notices of the Royal Astronomical Society, 438, 2267, doi: 10.1093/mnras/stt2342

    Hayashi, T., & Ishida, M. 2014a, Monthly Notices of the Royal Astronomical Society, 438, 2267, doi: 10.1093/mnras/stt2342

    work page doi:10.1093/mnras/stt2342

  13. [13]

    2014b, Monthly Notices of the Royal Astronomical Society, 441, 3718, doi: 10.1093/mnras/stu766 12

    Hayashi, T., & Ishida, M. 2014b, Monthly Notices of the Royal Astronomical Society, 441, 3718, doi: 10.1093/mnras/stu766 12

    work page doi:10.1093/mnras/stu766

  14. [14]

    2018, Monthly Notices of the Royal Astronomical Society, 474, 1810, doi: 10.1093/mnras/stx2766

    Hayashi, T., Kitaguchi, T., & Ishida, M. 2018, Monthly Notices of the Royal Astronomical Society, 474, 1810, doi: 10.1093/mnras/stx2766

    work page doi:10.1093/mnras/stx2766 2018

  15. [15]

    2024, in Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray, ed

    Hayashi, T., Boissay-Malaquin, R., Tamura, K., et al. 2024, in Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray, ed. J.-W. A. Den Herder, K. Nakazawa, & S. Nikzad (Yokohama, Japan: SPIE), 58, doi: 10.1117/12.3019600

    work page doi:10.1117/12.3019600 2024

  16. [16]

    V., Eckart, M

    Hell, N., Brown, G. V., Eckart, M. E., et al. 2025, Frequently Used References For Atomic Data In X-ray Spectroscopy, arXiv, doi: 10.48550/arXiv.2506.17106 H¨ olzer, G., Fritsch, M., Deutsch, M., H¨ artwig, J., & F¨ orster, E. 1997, Physical Review A, 56, 4554, doi: 10.1103/PhysRevA.56.4554

    work page doi:10.48550/arxiv.2506.17106 2025

  17. [17]

    S., & Mauche, C

    Hoogerwerf, R., Brickhouse, N. S., & Mauche, C. W. 2004, The Astrophysical Journal, 610, 411, doi: 10.1086/421389

    work page doi:10.1086/421389 2004

  18. [18]

    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

  19. [19]

    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

  20. [20]

    Luna, G. J. M., Mukai, K., Orio, M., & Zemko, P. 2018, The Astrophysical Journal Letters, 852, L8, doi: 10.3847/2041-8213/aaa28f

    work page doi:10.3847/2041-8213/aaa28f 2018

  21. [21]

    W., & Suleimanov, V

    Mauche, C. W., & Suleimanov, V. 2015, Astronomy & Astrophysics, 578, A15, doi: 10.1051/0004-6361/201525755

    work page doi:10.1051/0004-6361/201525755 2015

  22. [22]

    R., & Horne, K

    Marsh, T. R., & Horne, K. 1988, Monthly Notices of the Royal Astronomical Society, 235, 269, doi: 10.1093/mnras/235.1.269

    work page doi:10.1093/mnras/235.1.269 1988

  23. [23]

    2021, Journal of Astronomical Telescopes, Instruments, and Systems, 7, 028005, doi: 10.1117/1.JATIS.7.2.028005

    Midooka, T., Tsujimoto, M., Kitamoto, S., et al. 2021, Journal of Astronomical Telescopes, Instruments, and Systems, 7, 028005, doi: 10.1117/1.JATIS.7.2.028005

    work page doi:10.1117/1.jatis.7.2.028005 2021

  24. [24]

    2025, Publications of the Astronomical Society of Japan, 77, S86, doi: 10.1093/pasj/psaf057

    Miura, D., Yamaguchi, H., Ballhausen, R., et al. 2025, Publications of the Astronomical Society of Japan, 77, S86, doi: 10.1093/pasj/psaf057

    work page doi:10.1093/pasj/psaf057 2025

  25. [25]

    L., et al

    Mochizuki, Y., Tsujimoto, M., Kelley, R. L., et al. 2024a, The Astrophysical Journal Letters, 977, L21, doi: 10.3847/2041-8213/ad946d

    work page doi:10.3847/2041-8213/ad946d 2041

  26. [26]

    A., et al

    Mochizuki, Y., Tsujimoto, M., Kilbourne, C. A., et al. 2024b, in Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray, Vol. 13093 (SPIE), 1714–1729, doi: 10.1117/12.3019453

    work page doi:10.1117/12.3019453 2024

  27. [27]

    2017, Publications of the Astronomical Society of the Pacific, 129, 062001, doi: 10.1088/1538-3873/aa6736

    Mukai, K. 2017, Publications of the Astronomical Society of the Pacific, 129, 062001, doi: 10.1088/1538-3873/aa6736

    work page doi:10.1088/1538-3873/aa6736 2017

  28. [28]

    Moran, C. K. J. 2002, Monthly Notices of the Royal Astronomical Society, 337, 1215, doi: 10.1046/j.1365-8711.2002.05795.x

    work page doi:10.1046/j.1365-8711.2002.05795.x 2002

  29. [29]

    F., G¨ ansicke, B

    Pala, A. F., G¨ ansicke, B. T., Belloni, D., et al. 2022, Monthly Notices of the Royal Astronomical Society, 510, 6110, doi: 10.1093/mnras/stab3449 Pek¨ on, Y., & Balman, S ¸. 2011, Monthly Notices of the Royal Astronomical Society, 411, 1177, doi: 10.1111/j.1365-2966.2010.17752.x

    work page doi:10.1093/mnras/stab3449 2022

  30. [30]

    S., Kilbourne, C

    Porter, F. S., Kilbourne, C. A., Chiao, M. P., et al. 2025, Journal of Astronomical Telescopes, Instruments, and Systems, 11, 042016, doi: 10.1117/1.JATIS.11.4.042016

    work page doi:10.1117/1.jatis.11.4.042016 2025

  31. [31]

    2009, Nature, 458, 1142, doi: 10.1038/nature07946 Rodr´ ıguez-Gil, P., G¨ ansicke, B

    Revnivtsev, M., Sazonov, S., Churazov, E., et al. 2009, Nature, 458, 1142, doi: 10.1038/nature07946 Rodr´ ıguez-Gil, P., G¨ ansicke, B. T., Hagen, H.-J., et al. 2007, Monthly Notices of the Royal Astronomical Society, 377, 1747, doi: 10.1111/j.1365-2966.2007.11743.x

    work page doi:10.1038/nature07946 2009

  32. [32]

    R., Mason, K

    Rosen, S. R., Mason, K. O., & Cordova, F. A. 1988, Monthly Notices of the Royal Astronomical Society, 231, 549, doi: 10.1093/mnras/231.3.549

    work page doi:10.1093/mnras/231.3.549 1988

  33. [33]

    J., & Seitenzahl, I

    Ruiter, A. J., & Seitenzahl, I. R. 2025, The Astronomy and Astrophysics Review, 33, 1, doi: 10.1007/s00159-024-00158-9

    work page doi:10.1007/s00159-024-00158-9 2025

  34. [34]

    Savoury, C. D. J., Littlefair, S. P., Dhillon, V. S., et al. 2011, Monthly Notices of the Royal Astronomical Society, 415, 2025, doi: 10.1111/j.1365-2966.2011.18707.x

    work page doi:10.1111/j.1365-2966.2011.18707.x 2011

  35. [35]

    Raymond, J. C. 2001, The Astrophysical Journal, 556, L91, doi: 10.1086/322992

    work page internal anchor Pith review doi:10.1086/322992 2001

  36. [36]

    F., Doroshenko, V., & Werner, K

    Suleimanov, V. F., Doroshenko, V., & Werner, K. 2019, Monthly Notices of the Royal Astronomical Society, 482, 3622, doi: 10.1093/mnras/sty2952

    work page doi:10.1093/mnras/sty2952 2019

  37. [37]

    R., Schenker, K., Kolb, U., & Davies, M

    Terada, Y., Ishida, M., Makishima, K., et al. 2001, Monthly Notices of the Royal Astronomical Society, 328, 112, doi: 10.1046/j.1365-8711.2001.04878.x

    work page doi:10.1046/j.1365-8711.2001.04878.x 2001

  38. [38]

    2026, The Astrophysical Journal, 1002, 196, doi: 10.3847/1538-4357/ae5f97

    Terada, Y., Mori, K., Hayashi, T., et al. 2026, The Astrophysical Journal, 1002, 196, doi: 10.3847/1538-4357/ae5f97

    work page doi:10.3847/1538-4357/ae5f97 2026

  39. [39]

    2004, MNRAS, 350, 1301, doi: 10.1111/j.1365-2966.2004.07713.x

    Thoroughgood, T. D., Dhillon, V. S., Watson, C. A., et al. 2004, Monthly Notices of the Royal Astronomical Society, 353, 1135, doi: 10.1111/j.1365-2966.2004.08135.x

    work page doi:10.1111/j.1365-2966.2004.08135.x 2004

  40. [40]

    2000, ApJ, 542, 914, doi: 10.1086/317016

    Wilms, J., Allen, A., & McCray, R. 2000, The Astrophysical Journal, 542, 914, doi: 10.1086/317016

    work page internal anchor Pith review doi:10.1086/317016 2000

  41. [41]

    A., & Shabaev, V

    Yerokhin, V. A., & Shabaev, V. M. 2015, Journal of Physical and Chemical Reference Data, 44, 033103, doi: 10.1063/1.4927487

    work page doi:10.1063/1.4927487 2015

  42. [42]

    A., & Surzhykov, A

    Yerokhin, V. A., & Surzhykov, A. 2019, Journal of Physical and Chemical Reference Data, 48, 033104, doi: 10.1063/1.5121413 13

    work page doi:10.1063/1.5121413 2019

  43. [43]

    2010, Astronomy & Astrophysics, 520, A25, doi: 10.1051/0004-6361/201014542

    Yuasa, T., Nakazawa, K., Makishima, K., et al. 2010, Astronomy & Astrophysics, 520, A25, doi: 10.1051/0004-6361/201014542

    work page doi:10.1051/0004-6361/201014542 2010