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REVIEW 4 major objections 5 minor 29 references

A new shock in the pre-merging cluster pair 1E2215-2216

T0 review · 4 major / 5 minor · reviewed 2026-08-07 · deepseek-v4-flash

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Pith's one-line read New X-ray observations reveal a shock front 2.3 arcminutes south of the X-ray peak of cluster 1E2215, with a Mach number of about 1.2 confirmed independently from surface brightness and temperature jumps.

desk verdict New X-ray shock candidate in 1E2215-2216 is real but its claimed significance is weakened by a post-hoc sector choice. read the letter →

arxiv 2505.24323 v1 pith:LQH4GWEH submitted 2025-05-30 astro-ph.CO

Yanling Chen , Liyi Gu , Aurora Simionescu , Chunyang Jiang , Rui Huang , Wei Cui This is my paper
classification astro-ph.CO
keywords galaxyclustermergersshockfrontintraclustermediumRankine-HugoniotconditionsX-raysurfacebrightnessMachnumber1E2215-2216XMM-NewtonChandraanalysis
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper reports the detection of a new shock front in the early-stage merging galaxy cluster pair 1E2215-2216, located about 2.3 arcminutes south of the X-ray brightness peak of the cluster 1E2215. The claim rests on a combined XMM-Newton and Chandra analysis showing a surface brightness jump of 1.33±0.07 and a temperature jump of 1.22 +0.13/−0.14, with both jumps independently giving a Mach number of about 1.2. The authors argue that because the shock's age, speed, and location resemble those of the previously identified equatorial shock in the same system, the new front is likely a spatial extension of that shock rather than an unrelated feature. If correct, the detection adds a second shock diagnostic to a system caught in a rarely observed early pre-merger phase, helping to map how kinetic energy is dissipated in cluster outskirts.

What carries the argument

The central object is the shock front itself, identified through a projected broken power-law model of the surface brightness profile fitted with pyproffit, which yields the density jump n_in/n_out = 1.33±0.07. The Rankine-Hugoniot jump conditions (Eqs. 3 and 4) then convert the measured surface brightness and temperature jumps into independent Mach number estimates, and the agreement between the two estimates is the argument that the edge is a genuine adiabatic shock. The sector choice (230–280 degrees) and the comparison between XMM-Newton and Chandra are the empirical supports that locate the discontinuity.

What would settle it

A deep X-ray observation of the 230–280 degree sector that resolves the 2.3-arcmin edge and measures the pre- and post-shock temperatures with uncertainty below about 10 percent would settle the claim: the Rankine-Hugoniot prediction is a temperature ratio of about 1.22 for a brightness ratio of 1.33, so a measured ratio consistent with 1.0 at that precision would falsify the shock interpretation.

Watch

Extended reading notes

Core claim

The paper claims that a previously undetected shock front exists at approximately 2.3 arcminutes (about 251.5 kpc) south of the X-ray peak of 1E2215, visible as a steepened surface-brightness edge in the 230–280 degree sector and as a corresponding temperature jump in spectra extracted on either side of the edge. The surface brightness ratio measured with XMM-Newton is 1.33±0.07 and with Chandra 1.19±0.13, and the XMM-Newton temperature ratio is 1.22 +0.13/−0.14. Applying the Rankine-Hugoniot jump conditions to the brightness jump gives M = 1.22±0.05, and applying them to the temperature jump gives M = 1.25 +0.11/−0.17; the agreement indicates the temperature jump is adiabatic and supports the shock interpretation. Based on the pre-shock sound speed, the shock speed is roughly 1500 km/s and the age roughly 280 Myr, which the authors interpret as consistent with the previously known equatorial shock at about 1740 km/s and 250 Myr, making a common physical origin the favored explanation.

Load-bearing premise

The interpretation that the observed edge is a genuine shock assumes that the surface brightness and temperature jumps trace a single adiabatic Rankine-Hugoniot discontinuity along the line of sight, and are not contaminated by line-of-sight projection or unrelated foreground gas; the Chandra brightness profile alone does not statistically prefer the broken power-law model (BIC difference +1.64), and the XMM-Newton temperature jump is modest.

Editorial extensions

If this is right

  • The new shock adds a second, independent Mach number estimate (M ≈ 1.2) for the southern part of 1E2215, reinforcing that shocks in early-stage cluster mergers can be weak and sub-radio-loud.
  • Because the shock speed (~1500 km/s) and age (~280 Myr) are close to those of the equatorial shock identified by Gu et al. 2019, a common origin implies the equatorial shock front extends over a large opening angle, as the paper notes such fronts can be wide.
  • The weak Mach number (M ≈ 1.2) is below the ~2.2 threshold for efficient particle acceleration, explaining the absence of significant radio emission near the new front.
  • If the shock is a physical extension, the merger shock structure in 1E2215-2216 is more extended than previously mapped, providing a direct probe of how kinetic energy is dissipated in the outskirts during the early merger phase.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • If the common-origin interpretation holds, the merger geometry of 1E2215-2216 may be more complex than a simple two-body collision; an independent merger within 1E2215 could be tested with deeper observations looking for a cold front or a second brightness edge on the opposite side of the cluster.
  • A testable extension would be to search for a Sunyaev-Zeldovich decrement or a polarization signal at the shock location, which would trace the gas pressure jump independently of X-ray emission and break degeneracies in the line-of-sight projection.
  • The paper's sensitivity-map treatment of the cosmic X-ray background could be applied to other faint cluster outskirts to reduce background-driven biases, but whether the modest temperature jump survives even larger CXB variations is not established by this paper.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

4 major / 5 minor

Summary. The paper reports the detection of a new X-ray shock front in the pre-merging cluster pair 1E2215-2216, located about 2.3 arcmin south of the X-ray peak of 1E2215. Using XMM-Newton and Chandra data, the authors fit projected broken power-law surface brightness profiles and extract X-ray spectra in a 230-280 degree sector. They measure a surface brightness ratio of 1.33 +/- 0.07 and a temperature ratio of 1.22 +0.13/-0.14 with XMM-Newton, from which they derive Mach numbers of M = 1.22 +/- 0.05 (density jump) and M = 1.25 +0.11/-0.17 (temperature jump), and argue these are consistent with a common origin with the previously identified equatorial shock. The manuscript includes a BIC comparison of broken power-law versus beta models for six sectors, spectral fits with three CXB normalizations, and detailed background modeling.

Significance. If the detection is robust, this would add a new shock to the still-small sample of merger shocks in the early pre-merger phase, and the consistency of Mach numbers derived from independent jump conditions would be a useful confirmation of the Rankine-Hugoniot interpretation. The paper's strengths include the use of new ~300 ks XMM-Newton observations, the explicit BIC table for all sectors (Table 5), the stability of the temperature jump against CXB normalization variations, and the care taken with background modeling. However, the central claim currently rests on a single sector chosen after inspecting the data, and the statistical significance is substantially weakened once that selection is accounted for. The result is scientifically interesting but needs additional validation before it can be regarded as an established detection.

major comments (4)
  1. [§3.1, Table 5] The claimed detection is based on the 230-280 degree sector, which is the only one of six XMM-Newton sectors where the broken power-law model is preferred (Delta BIC = -6.23), while the other five sectors strongly favor the beta model. The text in §3.1 states that this is 'the sector where the new shock front is detected,' indicating that the sector was selected after inspecting the profiles. The reported 'strong evidence' is therefore the minimum of six independent model comparisons, and no multiple-trial correction is applied. A single-sector Delta BIC of -6.23 corresponds to modest evidence when interpreted as a single test; after accounting for the six sector choices, the effective significance drops further. The paper should either report a trial-corrected significance, present a pre-specified or independent confirmation sector, or explicitly acknowledge that the current evidence is not sufficient to claim a robust detection from the surface brightness profile alone.
  2. [§3.1, Table 2 and Table 5] The Chandra data in the same 230-280 degree sector favor the beta model over the broken power law (Delta BIC = +1.64), and the Chandra density jump of 1.19 +/- 0.13 is consistent with no jump at about 1.5 sigma. The paper attributes this to low signal-to-noise (end of §3.1), but this is not quantified. Since the abstract and conclusion state that the shock is 'confirmed' and that the XMM-Newton and Chandra results are 'consistent,' the current wording overstates the evidence. A joint fit or a stacked XMM-Newton plus Chandra profile would provide a more honest estimate of the combined significance; at minimum, the text should state explicitly that Chandra provides only a weak upper limit on the density jump and does not independently prefer a discontinuity.
  3. [§3.2, Tables 3 and 4] The temperature jump T_in/T_out = 1.22 +0.13/-0.14 from XMM-Newton has a lower 1-sigma bound of 1.08, so it is only marginally inconsistent with no temperature jump (about 1.6 sigma). Moreover, the temperature ratio is extracted from exactly the same 230-280 degree sector that was selected based on the surface brightness edge, so it is not an independent confirmation of the shock. The claim in §3.2 that the temperature jump 'strongly supports our high-confidence conclusion' is not supported by the statistical significance. The authors should provide the significance of the temperature ratio relative to unity and explicitly discuss the selection effect shared with the brightness edge.
  4. [§4.2 and §5] The conclusion states that the new shock 'shares a common physical origin with the previously identified equatorial shock,' but the discussion in §4.2 presents this only as a possibility and also offers an alternative explanation (an ongoing merger within 1E2215). The age and speed similarities are suggestive, but no quantitative criterion distinguishes the common-origin scenario from coincidence. The conclusion should be reworded to match the weaker, more hedged language used in the discussion, or the authors should provide a more detailed comparison (e.g., geometry, propagation direction, and expected shock age across the system) to support the common-origin claim.
minor comments (5)
  1. [Introduction and §4.2] There is a typo in the Introduction: 'accerlerated' should be 'accelerated'.
  2. [Appendix B] The text refers to 'Huang et al. in prep.' for the sensitivity map method; since this is a key part of the CXB estimate, the authors should either provide more details in the appendix or cite a publicly available description.
  3. [§3.1 and Table 5] Table 5 does not include the excluded 120-170 degree sector. Adding that sector (or stating why it is omitted from the table) would make the sector-by-sector comparison complete.
  4. [§3.1] The significance thresholds of BIC are quoted only informally ('strong evidence' and 'definitive'). It would be useful to state the Kass & Raftery thresholds in the text so that the reader can interpret the numbers in Table 5 without external reference.
  5. [Figure 1] In the right panel of Figure 1, the annotations are described as being the same as in the left panel, but the magenta sectors and numbered regions are not visible in the Chandra panel. Please clarify which annotations apply to the Chandra image.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the Mach numbers are algebraic transforms of independently fitted density and temperature jumps, and the common-origin claim is interpretive rather than derived.

full rationale

The central derivation chain is self-contained. The break radius and density jump are obtained by fitting the 230-280 degree sector brightness profile with a projected broken power law; the Mach number from Eq. 3 is an algebraic transformation of the fitted density jump n_in/nout, and the Mach number from Eq. 4 uses an independently fitted temperature jump from the same sector. Neither quantity is fitted to force the other, and the paper presents their agreement as a consistency check. The comparison with the previously identified equatorial shock (Gu et al. 2019) is interpretive, explicitly offers an alternative explanation (infall of a group), and is not needed for the detection claim. The a posteriori sector choice and absent trial correction, visible in Table 5 where only one of six XMM sectors favors the broken power law and Chandra favors the beta model in that same sector, are a statistical robustness concern rather than circularity: the model comparison statistics are reported as measured values, not as predictions derived from the model or from the fitted Mach numbers. I therefore find no step in which a claimed result reduces by construction to its inputs.

Assumptions & free parameters 4 free parameters · 5 assumptions · 0 invented entities

All inputs to the Mach number calculation are either fitted profile or spectral parameters or standard physical constants. No new particles, mediators, or ad hoc quantities are introduced. The most fragile inputs are the geometric depth assumption and the unpublished CXB sensitivity map.

free parameters (4)
  • r_break (XMM-Newton) = 2.32 +/- 0.08 arcmin
    Location of the surface brightness edge; used to set shock radius, speed, and age.
  • density jump nin/nout (XMM-Newton) = 1.33 +/- 0.07
    Fitted surface brightness discontinuity; directly enters Eq. 3 for the Mach number.
  • temperature jump T_in/T_out (XMM-Newton) = 1.22 +0.13/-0.14
    Derived from fitted kT values in adjacent spectral sectors; enters Eq. 4 for the independent Mach number.
  • broken power-law slopes alpha_in, alpha_out (XMM-Newton) = 0.28 +/- 0.08 and 1.29 +/- 0.04
    Shape parameters of the projected brightness model; they characterize the profile but do not directly set the jump ratio.
assumptions (5)
  • standard math Rankine-Hugoniot jump conditions for adiabatic shocks
    Used in Eqs. 3 and 4 to convert measured brightness and temperature discontinuities into Mach numbers.
  • domain assumption Gamma = 5/3 for the ICM plasma
    Assumed in Eq. 3 for a monoatomic gas; standard for cluster plasma but an idealization.
  • domain assumption Projected broken power-law model and cylindrical geometry with line-of-sight depth equal to the cluster diameter
    Used in Sections 3.1 and 3.2 to convert projected brightness and APEC normalization into densities and a density jump.
  • domain assumption The LHB, GH, CXB, and NXB model components accurately represent the sky background
    Appendix B; only CXB flux is varied over its statistical range, while foreground spectral shapes and the sensitivity map are fixed.
  • domain assumption The shock propagates outward at constant speed from the cluster center
    Used in Section 4.1 to estimate the shock age of about 280 Myr from radius and speed; stated explicitly but unverified.

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Cite this review

Pith. "Pith review of A new shock in the pre-merging cluster pair 1E2215-2216." pith.science (2026). https://pith.science/paper/LQH4GWEH

@misc{pith2026250524323,
  author       = {Pith},
  title        = {Pith review of: A new shock in the pre-merging cluster pair 1E2215-2216},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/LQH4GWEH}},
  note         = {Machine review of arXiv:2505.24323}
}
abstract

The galaxy cluster pair 1E2216.0-0401 and 1E2215.7-0404 represents a major cluster merger in its early stages, a phase that has been scarcely explored in previous studies. Within this system, both axial and equatorial merger shocks have been identified. Recent XMM-Newton observations of the southern region of the cluster pair have increased the total exposure time to approximately 300 ks, enhancing the sensitivity to detect faint shock features in the cluster outskirts. Through a combined analysis of XMM-Newton and Chandra data, including both imaging and spectral techniques, a new shock front has been identified at approximately 2'.3 south of the X-ray brightness peak of 1E2215. This shock front exhibits a surface brightness ratio of $1.33 \pm 0.07$ and a temperature ratio of $1.22^{+0.13}_{-0.14}$ in XMM-Newton, consistent with Chandra results. The Mach number, independently calculated from both the temperature and surface brightness discontinuities, yields consistent values of $\mathcal{M} \approx 1.2$ . The age, velocity, and spatial distribution of this shock suggest that it shares a common physical origin with the previously identified equatorial shock.

Figures

Figures reproduced from arXiv: 2505.24323 by the authors.

Figure 1
Figure 1. Left panel: Zoom-in XMM-Newton image in the [0.5-2.0] keV band (extracted from the red box region in Fig.6), with white contours indicating 235 MHz radio intensity observed by GMRT. Cyan dashed curves mark surface brightness edges identified through surface brightness profile analysis in this work, yellow dashed curves denote edges from previous studies, green ellipses outline point source exclusion regions, and mag… view at source ↗
Figure 2
Figure 2. The surface brightness radial profiles were extracted from azimuthal sectors centered on the 1E2215 brightness peak using XMM-Newton data (left panel) and Chandra data (right panel), with all profiles extracted in the [0.5-2.0] keV energy band. Black data points represent profiles from the 230◦ -280◦ sector, which is marked by a magenta sector in figure 1. The inset in the left panel shows the opening angle of the s… view at source ↗
Figure 3
Figure 3. The kT spatial distribution (left) and density spatial distribution (right) were obtained by fitting spectra extracted from the magenta sectors from XMM-Newton and Chandra. The black dashed line marks the location of the shock front, approximately 2.3′ from the X-ray brightness peak of 1E2215, where a temperature and density jump can be observed. The fitted values are represented by black, red, and blue points with … view at source ↗
Figures from the paper (4 more)
Figure 4
Figure 4. Figure 4: The fitted spectra for the source and sky background regions of XMM-Newton for CXB fixed at middle value. The data points are shown in black with corresponding error bars. The fitted models consist of multiple components, each represented by a different color curve. Th…
Figure 5
Figure 5. Figure 5: The fitted spectra for the source and sky background regions of Chandra observation 20778. The line labels are the same as in Fig.4 [PITH_FULL_IMAGE:figures/full_fig_p012_5.png]
Figure 6
Figure 6. Figure 6: The [0.5-2.0] keV XMM-Newton image of the entire dataset is shown, with particle background subtracted and vignetting effects corrected. The magenta sectors indicate the regions used for spectral fitting in XMM-Newton data, while the pink solid sector marks the sky bac…
Figure 7
Figure 7. Figure 7: Left: The XMM-Newton sensitivity map of 1E2215/2216. Right: The logN-logS curve in the XMM-Newton FoV. In the left panel, the sensitivity Slimit improves from the edge to the center of the FoV, but deteriorates in the cluster region. In the right panel, the black stair…

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Works this paper leans on

29 extracted references · 4 canonical work pages

  1. [1]

    2010, PASJ, 62, 335, doi: 10.1093/pasj/62.2.335

    Akahori, T., & Yoshikawa, K. 2010, PASJ, 62, 335, doi: 10.1093/pasj/62.2.335

    doi:10.1093/pasj/62.2.335 2010

  2. [2]

    W., et al

    Akamatsu, H., Gu, L., Shimwell, T. W., et al. 2016, A&A, 593, L7, doi: 10.1051/0004-6361/201629275

    doi:10.1051/0004-6361/201629275 2016

  3. [3]

    J., & Scott, P

    Asplund, M., Grevesse, N., Sauval, A. J., & Scott, P. 2009, Annual Review of Astronomy and Astrophysics, 47, 481–522, doi: 10.1146/annurev.astro.46.060407.145222

    arXiv 2009

  4. [4]

    2018, MNRAS, 476, 5591, doi: 10.1093/mnras/sty598 De Luca, A., & Molendi, S

    Botteon, A., Gastaldello, F., & Brunetti, G. 2018, MNRAS, 476, 5591, doi: 10.1093/mnras/sty598 De Luca, A., & Molendi, S. 2004, A&A, 419, 837, doi: 10.1051/0004-6361:20034421 De Plaa, J. 2017, CXBTools, Zenodo, doi: 10.5281/ZENODO.2575495 de Plaa, J. 2023, Pyspextools, Zenodo, doi: 10.5281/ZENODO.10158621

    doi:10.1093/mnras/sty598 2018

  5. [5]

    2020, The Open Journal of Astrophysics, 3, 12, doi: 10.21105/astro.2009.13944

    Eckert, D., Finoguenov, A., Ghirardini, V., et al. 2020, The Open Journal of Astrophysics, 3, 12, doi: 10.21105/astro.2009.13944

    arXiv 2020

  6. [6]

    2014, A&A, 570, A119, doi: 10.1051/0004-6361/201424259

    Eckert, D., Molendi, S., Owers, M., et al. 2014, A&A, 570, A119, doi: 10.1051/0004-6361/201424259

    doi:10.1051/0004-6361/201424259 2014

  7. [7]

    2012, A&A Rv, 20, 54, doi: 10.1007/s00159-012-0054-z

    Feretti, L., Giovannini, G., Govoni, F., & Murgia, M. 2012, A&A Rv, 20, 54, doi: 10.1007/s00159-012-0054-z

    doi:10.1007/s00159-012-0054-z 2012

  8. [8]

    W., et al

    Gu, L., Akamatsu, H., Shimwell, T. W., et al. 2019, Nature Astronomy, 3, 838, doi: 10.1038/s41550-019-0798-8

    doi:10.1038/s41550-019-0798-8 2019

Show all 29 references
  1. [9]

    2018, ApJ, 857, 26, doi: 10.3847/1538-4357/aab4a2

    Ha, J.-H., Ryu, D., & Kang, H. 2018, ApJ, 857, 26, doi: 10.3847/1538-4357/aab4a2

    2018 doi

  2. [10]

    E., Gottl¨ ober, S., et al

    Hoeft, M., Nuza, S. E., Gottl¨ ober, S., et al. 2011, Journal of Astrophysics and Astronomy, 32, 509, doi: 10.1007/s12036-011-9127-z

    2011 doi

  3. [11]

    J., Liu, W., & Buote, D

    Humphrey, P. J., Liu, W., & Buote, D. A. 2009, ApJ, 693, 822, doi: 10.1088/0004-637X/693/1/822

    2009 doi

  4. [12]

    S., & Bleeker, J

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

    2016 doi

  5. [13]

    E., & Raftery, A

    Kass, R. E., & Raftery, A. E. 1995, Journal of the American Statistical Association, 90, 773, doi: 10.1080/01621459.1995.10476572

    1995

  6. [14]

    V., & Borgani, S

    Kravtsov, A. V., & Borgani, S. 2012, ARA&A, 50, 353, doi: 10.1146/annurev-astro-081811-125502 16

    2012 doi

  7. [15]

    D., & Lifshitz, E

    Landau, L. D., & Lifshitz, E. M. 1959, Fluid mechanics

    1959

  8. [16]

    D., Xue, Y

    Lehmer, B. D., Xue, Y. Q., Brandt, W. N., et al. 2012, ApJ, 752, 46, doi: 10.1088/0004-637X/752/1/46

    2012 doi

  9. [17]

    1994, ApJL, 435, L109, doi: 10.1086/187606

    Loeb, A., & Mao, S. 1994, ApJL, 435, L109, doi: 10.1086/187606

    1994 doi

  10. [18]

    2007, PhR, 443, 1, doi: 10.1016/j.physrep.2007.01.001

    Markevitch, M., & Vikhlinin, A. 2007, PhR, 443, 1, doi: 10.1016/j.physrep.2007.01.001

    2007 doi

  11. [19]

    2016, Frontiers in Astronomy and Space Sciences, 2, 7, doi: 10.3389/fspas.2015.00007

    Molnar, S. 2016, Frontiers in Astronomy and Space Sciences, 2, 7, doi: 10.3389/fspas.2015.00007

    2016

  12. [20]

    2009, A&A, 493, 501, doi: 10.1051/0004-6361:200811197

    Moretti, A., Pagani, C., Cusumano, G., et al. 2009, A&A, 493, 501, doi: 10.1051/0004-6361:200811197

    2009 doi

  13. [21]

    2011, ApJ, 726, 17, doi: 10.1088/0004-637X/726/1/17

    Mannheim, K. 2011, ApJ, 726, 17, doi: 10.1088/0004-637X/726/1/17

    2011 doi

  14. [22]

    M., & Sarazin, C

    Ricker, P. M., & Sarazin, C. L. 2001, ApJ, 561, 621, doi: 10.1086/323365

    2001 doi

  15. [23]

    2024, A&A, 686, A68, doi: 10.1051/0004-6361/202348853

    Rossetti, M., Eckert, D., Gastaldello, F., et al. 2024, A&A, 686, A68, doi: 10.1051/0004-6361/202348853

    2024 doi

  16. [24]

    R., Fabian, A

    Russell, H. R., Fabian, A. C., McNamara, B. R., et al. 2014, MNRAS, 444, 629, doi: 10.1093/mnras/stu1469

    2014 doi

  17. [25]

    L., Mushotzky, R

    Snowden, S. L., Mushotzky, R. F., Kuntz, K. D., & Davis, D. S. 2008, A&A, 478, 615, doi: 10.1051/0004-6361:20077930

    2008 doi

  18. [26]

    L., Egger, R., Freyberg, M

    Snowden, S. L., Egger, R., Freyberg, M. J., et al. 1997, ApJ, 485, 125, doi: 10.1086/304399 van Weeren, R. J., de Gasperin, F., Akamatsu, H., et al. 2019, SSRv, 215, 16, doi: 10.1007/s11214-019-0584-z

    1997 doi

  19. [27]

    2014, ApJ, 780, 125, doi: 10.1088/0004-637X/780/2/125

    Vink, J., & Yamazaki, R. 2014, ApJ, 780, 125, doi: 10.1088/0004-637X/780/2/125

    2014 doi

  20. [28]

    Willingale, R., Starling, R. L. C., Beardmore, A. P., Tanvir, N. R., & O’Brien, P. T. 2013, MNRAS, 431, 394, doi: 10.1093/mnras/stt175

    2013 doi

  21. [29]

    Y., et al

    Yoshino, T., Mitsuda, K., Yamasaki, N. Y., et al. 2009, PASJ, 61, 805, doi: 10.1093/pasj/61.4.805

    2009 doi

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