Pith. sign in

REVIEW 2 major objections 6 minor 286 references

X-ray polarization of Z-type neutron star low-mass X-ray binaries -- II. Spectropolarimetric analysis

T0 review · 2 major / 6 minor · reviewed 2026-08-01 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗ Review JSON

Pith's one-line read For most Z-type neutron star X-ray binaries, the dominant polarized signal is Comptonized emission, reaching about 6% on the horizontal branch — higher than spreading-layer models predict.

desk verdict Careful, useful branch-resolved spectropolarimetric analysis with a real discovery claim, but the component-level polarization values inherit fixed priors that need a sensitivity test before the headline should be taken at face value. read the letter →

arxiv 2607.16140 v1 pith:7MF2N3CT submitted 2026-07-17 astro-ph.HE

Andrea Gnarini , Francesco Ursini , Giorgio Matt , Stefano Bianchi , Fiamma Capitanio , Massimo Cocchi , Sergio Fabiani , Ruben Farinelli
show 3 more authors
Philip Kaaret Lorenzo Marra Antonella Tarana
This is my paper · ORCID
classification astro-ph.HE
keywords X-raypolarimetryZ-sourcesneutronstarlow-massbinariesComptonizationaccretiondiskreflectionspectropolarimetryIXPE
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

Using imaging X-ray polarimetry together with NICER and NuSTAR spectra, the paper builds the first branch-resolved spectropolarimetric picture of six Z-type neutron star X-ray binaries as they move along their color–color diagrams. It tries to establish that Comptonized emission is the main source of both flux and polarization for most sources and branches: the 2–8 keV polarization degree is about 6% on the horizontal branch and falls to 3–4% on the normal branch. Those numbers exceed theoretical expectations for spreading-layer or boundary-layer geometries, so the authors argue the Comptonizing region is not a simple spreading layer. The disk component is less polarized (below 3%) but still above the plane-parallel scattering-atmosphere prediction, and its polarization angle is generally not perpendicular to the Comptonized angle, suggesting a non-axisymmetric system.

What carries the argument

The analysis uses a single spectral baseline for all sources — a thermal accretion disk model plus thermal Comptonization of a blackbody seed, with a relativistic reflection model (and occasionally an extra hard tail) added where needed — and fits the IXPE, NICER, and NuSTAR spectra separately for each branch of the color–color diagram. Polarization is then assigned component by component with a constant-polarization multiplicative model (polconst), with the reflected component's polarization degree fixed at 10% and its angle tied to the Comptonized component. This decomposition is the load-bearing device: it turns measured total Stokes parameters into per-component polarization degrees and

What would settle it

Take a bright Z-source (e.g., Cyg X-2) and leave the reflected component's polarization degree and angle free instead of fixing them at 10% and parallel to the Comptonized angle; if the best fit yields a reflection PD far below 10% or a PA that is not parallel to the Comptonized PA, the headline Comptonized PD values would not be reproduced. A second, weaker test: obtain high-signal branch-resolved data (e.g., with a more sensitive future polarimeter) and check whether the disk PA remains misaligned when it is not frozen to Comptonization+90°.

Watch

Extended reading notes

Core claim

The central claim is that, for most of the sources and branches, the main contribution to the X-ray emission and polarization is due to Comptonization: moving from the horizontal branch to the normal branch, the polarization degree in the 2–8 keV band varies from about 6% to 3–4%, while the flaring branch is loosely constrained. These values are significantly higher than theoretical expectations for typical spreading or boundary layer configurations. The disk polarization is generally lower (below 3%) but still higher than the prediction for an electron scattering-dominated, plane-parallel atmosphere at the corresponding inclination. The polarization angle of the disk appears significantly m

Load-bearing premise

The component-level polarization results depend on the assumed spectral decomposition and on fixing the reflected component's polarization degree at 10% with its angle tied to the Comptonized angle; if the degeneracy between Comptonized and reflected emission is resolved differently, or the reflection polarization differs, the reported per-component degrees and angle misalignment would not hold.

Editorial extensions

If this is right

  • If the high Comptonized polarization degrees (up to about 6–7% in the horizontal branch) are real, standard optically thick spreading-layer geometries, which predict only a few percent, are ruled out for most Z-sources and branches.
  • The non-orthogonal disk and Comptonized polarization angles imply broken axial symmetry in the inner accretion flow, so inclination alone is insufficient to predict the observed polarization.
  • Because the disk contribution rises as sources move from the horizontal to the normal branch, the branch-to-branch drop in total polarization can be explained partly by dilution from a weakly and misaligned polarized disk component.
  • Including the reflected component in the polarization budget matters: even at 5–20% of the photon flux, highly polarized reflected photons can shift the inferred Comptonized polarization if omitted.

Reading between the lines

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

  • If the fixed 10% reflection polarization and the parallel PA assumption are wrong — for example, if the reflection PA follows a warped disk's local normal — the quoted Comptonized polarization degrees would change; a future fit that frees the reflection PA on a bright source would settle this.
  • The paper's claim that the disk is more polarized than a plane-parallel scattering atmosphere could be tested independently with spectropolarimetric atmosphere models that include absorption, since the measured values are still consistent with those.
  • A natural extension is to model the Z-track as a continuous sequence of spreading-layer opening angles or covering fractions; if the covering fraction varies systematically along the track, the polarization evolution observed here may be reproduced without invoking an extra wind component.
  • The strong HB-to-NB contrast suggests that dedicated observations of currently unobserved branches in Sco X-1-like sources could decide whether the two Z-source subclasses differ in polarization or only in sampling.
Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 6 minor

Summary. This paper presents the first branch-resolved spectropolarimetric analysis of a sample of six Z-type neutron star low-mass X-ray binaries observed with IXPE, NICER, and NuSTAR. The authors fit a common spectral model — TBabs*(diskbb+thcomp*bbodyrad), plus relxillNS reflection for all sources except GX 5–1 — to each branch of the Z-track, then fix the spectral parameters and apply polconst component-by-component to the IXPE Stokes spectra. They report a Comptonized-component PD of roughly 3–6% in the HB/NB, a disk PD generally below 3%, and a disk PA that is often not perpendicular to the Comptonization PA. They interpret the high Comptonized PD as evidence that the Comptonizing region is not a simple spreading layer, and they compare the disk PD with plane-parallel atmosphere predictions. They also find no correlation between polarization and inclination or reflection fraction.

Significance. If the component-level polarization values are robust, this is a valuable step: it is the first uniform, branch-resolved spectropolarimetric study of Z-sources, it includes a reflection component in the polarimetric decomposition, and it provides a direct observational test of spreading-layer/boundary-layer geometries. The paper also makes useful connections to ADC systems and winds. However, the central quantitative claims rest on priors for the reflection polarization and on only a subset of rows with free disk polarization angles. The paper itself acknowledges the Comptonization/reflection degeneracy and the difficulty of estimating component PD/PA. The significance of the results therefore depends on sensitivity checks that are not currently presented.

major comments (2)
  1. [§4, Table 2, Appendix A] The component-resolved PD/PA values in Table 2 are derived by fixing the spectral model and assigning polarization with polconst under three priors: reflection PD is fixed to 10%, reflection PA is tied to the Comptonization PA for every source and branch, and in several rows the disk PA is frozen to Comp+90 (Cyg X-2 HB/FB, XTE J1701–462 FB, Sco X-1 FB, GX 340+0 NB/FB). The central claim in the abstract and §4 — that the Comptonized PD is 3–6% and significantly above spreading-layer expectations of ~2% — is sensitive to these priors. Reflection contributes 5–32% of the 2–8 keV flux in the Appendix tables; e.g., Cyg X-2 HB has N_relxillNS/N_Tot = 17.8% and Table 2 gives Comp PD = 4.2±0.9. If the true reflection PD were 20% (a value the paper itself cites from Matt 1993 and Podgorný et al. 2025) with PA aligned to the Comptonization, the inferred Comptonized PD would shift downward by sever
  2. [§4, Table 2, §5] The claim that the disk PA is 'significantly misaligned and not perpendicular' to the Comptonization PA is only testable in rows where the disk PA was left free. In several rows the disk PA is frozen to Comp+90, so those rows cannot provide evidence for misalignment. Among the free rows, some are actually consistent with perpendicular orientation within the quoted 90% errors: for example, Cyg X-2 NB has disk PA = 54±15 and Comp PA = −42±7, giving ΔPA≈96°, consistent with 90° within errors. Moreover, the reflection PA is tied to the Comptonization PA in §4 under the assumption of an axisymmetric configuration, but the paper later invokes a possible break in axial symmetry to explain the absence of an inclination trend and the non-orthogonal PAs. In a non-axisymmetric geometry, the reflection PA would not in general be locked to the Comptonization PA. The present treatment therefore preclu
minor comments (6)
  1. [Table 1] The header 'XTE J1071–461' is a typo; the source is XTE J1701–462 throughout the text.
  2. [§3.5] There is a repeated word in 'also simultaneously observed the the source'; please correct.
  3. [§4, Table 2] The notation '=PA Comp +90' and bracketed values such as '[10]' should be defined explicitly in the table notes as frozen priors, not as measured quantities. This will avoid confusion about which entries are constraints and which are assumptions.
  4. [§3.4] The gray-filter correction E^{−ΔΓ} for Sco X-1 is mentioned but ΔΓ is not defined or described in terms of how it was constrained. Please clarify whether this factor is applied to the model I, Q, and U consistently and what value of ΔΓ was used.
  5. [Figures 2 and 4] The legend states that empty markers correspond to 'values frozen during the fits,' but it is not always clear whether the PD or the PA was frozen. Please make the legend more explicit, e.g., 'PD frozen' vs 'PA frozen'.
  6. [§4] The uncertainties in Table 2 are statistical only, since the spectral parameters are fixed to their best-fit values. The paper should state explicitly that the quoted errors do not include covariance with the spectral parameters, especially given the Comptonization/reflection degeneracy.

Circularity Check

0 steps flagged · score 2.0 of 10

No circular reduction: component-level PD/PA values are conditional on explicit priors, but the headline comparison rests on independent IXPE measurements and published external models.

full rationale

The paper's central derivation is observational: IXPE Stokes spectra are fit with polconst applied to a fixed spectral decomposition, and the resulting component PD/PA are compared with published theoretical models (Chandrasekhar atmospheres, spreading-layer/boundary-layer simulations). The measured total and branch-resolved polarization are external data, not outputs of the theories being tested. The model-dependent component decomposition in Table 2 does involve priors: relxillNS PD is fixed at 10% with PA tied to thcomp*bbodyrad, and in some rows the disk PA is frozen perpendicular to the Comptonization PA. These are assumptions, and the paper explicitly acknowledges the resulting degeneracy: 'it is difficult to estimate the PD and PA for each component due to the limited bandpass of IXPE and the degeneracy of some components' (Sect. 4) and 'Although there is strong degeneracy between the Comptonized and reflected components, as expected...' (Sect. 5). Frozen values are marked in Table 2 and Fig. 2, and the misalignment claim is restricted to rows 'when measurable,' so no prediction is silently forced by construction. Self-citations to G25 are prior data-analysis work (branch GTIs, model-independent PD) and serve as cross-checks, not as an unverified load-bearing premise. Thus the central claim is conditional on modeling choices but not circularly derived from its inputs. The score of 2 reflects these acknowledged model-dependence caveats and minor self-citation, not a circular reduction.

Assumptions & free parameters 15 free parameters · 9 assumptions · 1 invented entities

The central spectropolarimetric results rest on a fairly large number of fitted spectral parameters (disk, Comptonization, reflection, cross-calibration) and on several imposed priors for the polarization of reflection (PD=10%, PA tied) and sometimes the disk. These are standard in the field but mean the component-level PD/PA values are model-dependent rather than pure measurements.

free parameters (15)
  • diskbb kT_in (per source/branch) = 0.65–1.26 keV
    Inner disk temperature; defines the disk spectral component whose polarization is measured.
  • diskbb normalization (R_d sqrt(cos i)) = 10–30 km
    Sets the disk flux contribution in the 2–8 keV band, affecting the decomposition into disk vs Comptonized components.
  • thcomp electron temperature kT_e = 2.6–14.5 keV
    Defines the Comptonized continuum shape; this is the component with the highest PD.
  • thcomp optical depth τ = 7.5–30
    Together with kT_e sets the thcomp spectral shape and flux fraction.
  • thcomp covering fraction f = 0–1 (fixed to 1 or 0 in many branches; free values ~0.2–0.51)
    Controls the fraction of seed photons that are Comptonized; strongly changes the relative flux of the Comptonized component.
  • bbodyrad seed temperature kT = 0.99–1.57 keV
    Seed photon temperature for thcomp, tied to relxillNS seed temperature.
  • bbodyrad normalization / R_bb = 8–29 km
    Sets seed photon flux; affects the Comptonized component normalization.
  • relxillNS inclination i = 30°–62°
    Used for the disk PD comparison to plane-parallel atmosphere predictions; a systematic underestimate would weaken the disk-PD tension.
  • relxillNS inner radius R_in = upper limits; fixed to ISCO in some branches
    Controls the reflection flux and profile.
  • relxillNS ionization log ξ = 1.5–3.0
    Reflection spectral shape; affects the reflected flux normalization.
  • relxillNS iron abundance A_Fe = 1.4–9.7 (often fixed)
    Sets the Fe line/reflection strength.
  • reflection PD (fixed) = 10%
    Chosen from Matt (1993); applied to relxillNS in all sources/branches, directly setting the reflection's contribution to the polarized signal.
  • NICER edge depth D = 0.015–0.079
    Ad hoc multiplicative edge at ~1.839 keV to correct NICER residuals; affects the low-energy spectral shape.
  • GX 5-1 powerlaw normalization N_pl = 0.44–0.47 (or upper limit 0.02)
    Extra hard-tail component for GX 5-1; its polarization is tied to thcomp.
  • Cross-calibration constants (per DU/FPM/NICER) = 0.728–1.392
    Account for inter-instrument normalization; do not directly affect polarization but affect the joint spectral fit.
assumptions (9)
  • domain assumption The spectral model TBabs*(diskbb+thcomp*bbodyrad)+relxillNS adequately describes the 1.5–30 keV spectra of all Z-sources (with source-specific additions like edge, powerlaw, apec).
    Used throughout §3; if the true continuum contains e.g. a separate corona or different seed photon distribution, the component polarization assignments would change.
  • domain assumption The Comptonized component is produced by thcomp applied to bbodyrad seed photons from the NS surface/boundary layer; its covering fraction f is a valid descriptor.
    Baseline model §3; the physical identification of thcomp*bbodyrad with the Comptonizing region underpins the interpretation of its PD.
  • domain assumption relxillNS (single-temperature blackbody illuminating a disk at 45°) describes the reflection component, with spin fixed at 0.1, outer radius 1000 Rg, and reflection fraction −1.
    §3; the reflection normalization and parameters are used in the spectropolarimetric decomposition and inclination estimates.
  • ad hoc to paper Reflected photons have PD = 10% and PA parallel to the Comptonization PA (axisymmetric geometry).
    §4: 'we decided to fix the PD of relxillNS at 10% ... while the PA is tied to that of thcomp*bbodyrad'; this is a prior imposed on the polarimetric fit, not derived from the data.
  • domain assumption Chandrasekhar/Sobolev plane-parallel electron-scattering atmosphere predictions are the correct baseline for disk atmospheric polarization at the measured inclination.
    Used to claim disk PD is higher than predictions (§4, comparing to Chandrasekhar 1960; Sobolev 1963); more detailed atmosphere models (Taverna et al. 2021; Marra et al. 2026) are cited but not used quantitatively.
  • ad hoc to paper NICER residuals below 2 keV are instrumental and can be modeled with an absorption edge at ~1.839 keV (Al edge).
    §2.2; if the edge is astrophysical, the continuum decomposition at low energies changes.
  • ad hoc to paper For Sco X-1, the IXPE gray-filter residuals can be corrected by multiplying the model by E^{-ΔΓ}.
    §3.4; this correction is applied during polarimetric analysis and could bias the component polarization if wrong.
  • domain assumption Branch classifications (HB/NB/FB) from G25 are correct; the GTIs split the data appropriately.
    All branch-resolved results depend on this; incorrect branch assignment would mix states.
  • domain assumption The adopted distances (2.1–11 kpc) used to convert normalizations to physical radii are correct.
    Used for R_d and R_bb values; not central to polarization but used in parameter interpretation.
invented entities (1)
  • Sub-relativistic or fully ionized accretion disk wind
    purpose: Offered as a possible additional source of polarized photons to explain the high Comptonized-component PD without changing the continuum spectrum (§5).
    Mentioned speculatively; no direct detection or falsifiable prediction is provided in this paper, and it is not part of the fitted model.

how reviews work

0 comments
Cite this review

Pith. "Pith review of X-ray polarization of Z-type neutron star low-mass X-ray binaries -- II. Spectropolarimetric analysis." pith.science (2026). https://pith.science/paper/7MF2N3CT

@misc{pith2026260716140,
  author       = {Pith},
  title        = {Pith review of: X-ray polarization of Z-type neutron star low-mass X-ray binaries -- II. Spectropolarimetric analysis},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/7MF2N3CT}},
  note         = {Machine review of arXiv:2607.16140}
}
read the original abstract

IXPE has provided for the first time detailed energy- and time-resolved X-ray polarimetry of Z-type neutron star low-mass X-ray binaries (NS-LMXBs) as they move along their color-color diagrams (CCDs). These sources can reach the highest polarization observed for NS-LXMBs in the 2-8 keV range when they move along the horizontal branch. In a previous paper, we characterized the spectral state of a sample of Z-sources using the CCD and estimated the polarization with model-independent analysis. Here, we present detailed spectropolarimetric analysis for each source on each branch using data from IXPE, NICER, and NuSTAR. The continuum X-ray emission of all the sources is well described with a combination of thermal accretion disk emission plus a harder Comptonized component. In addition, reflection features, in particular the relativistically broadened Fe line, are observed for our sources, except GX 5-1. For most of the sources and branches, the main contribution to the X-ray emission and polarization is due to Comptonization: moving from the horizontal branch (HB) to the normal branch (NB), the polarization degree (PD) in the 2-8 keV band varies from about 6% to 3-4%, while the PD is loosely constrained in the flaring branch (FB), due to the shorter exposures. These PD values are significantly higher than theoretical expectations for typical spreading or boundary layer configurations. The polarization of the disk is generally lower (below 3%) but still higher than predictions for an electron scattering-dominated, plane-parallel atmosphere above the disk observed at the corresponding inclination. Moreover, the polarization angle (PA) of the disk seems to be significantly misaligned and not perpendicular to that of Comptonization. We find no correlation between the polarization signal and the inclination, nor with the contribution of reflected photons throughout the Z-track.

Figures

Figures reproduced from arXiv: 2607.16140 by the authors.

Figure 1
Figure 1. Deconvolved spectra for each Z-source with the resulting best-fit model and the corresponding residuals in units of [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Polarization degree of Comptonized (top) and disk (mid [PITH_FULL_IMAGE:figures/full_fig_p008_2.png] view at source ↗
Figure 4
Figure 4. Polarization degree of Comptonized (left) and disk (right) emission for each Z-source as a function of the inclination. Empty [PITH_FULL_IMAGE:figures/full_fig_p009_4.png] view at source ↗

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

286 extracted references · 1 canonical work pages

  1. [1]

    Model-independent, time-resolved X-ray polarimetry

    X-ray polarization of Z-type neutron star low-mass X-ray binaries: I. Model-independent, time-resolved X-ray polarimetry. , year = 2025, month = jul, volume =

    2025

  2. [2]

    Galaxies , year = 2024, month = aug, volume =

    The IXPE View of Neutron Star Low-Mass X-ray Binaries. Galaxies , year = 2024, month = aug, volume =. doi:10.3390/galaxies12040043 , archivePrefix =. 2409.07161 , primaryClass =

    arXiv 2024

  3. [3]

    Constraining the Size of the Corona with Fully Relativistic Calculations of Spectra of Extended Coronae. I. The Monte Carlo Radiative Transfer Code. , year = 2019, month = apr, volume =

    2019

  4. [4]

    and Dovčiak, M

    Zhang, W. and Dovčiak, M. and Bursa, M. and Karas, V. and Matt, G. and Ursini, F. , title = ". Monthly Notices of the Royal Astronomical Society , volume =. 2022 , month =

    2022

  5. [5]

    and Ursini, F

    Gnarini, A. and Ursini, F. and Matt, G. and Bianchi, S. and Capitanio, F. and Cocchi, M. and Farinelli, R. and Zhang, W. , title = ". , volume =. 2022 , month =

    2022

  6. [6]

    Black Holes (Les Astres Occlus) , year = 1973, month = jan, pages =

    Astrophysics of black holes. Black Holes (Les Astres Occlus) , year = 1973, month = jan, pages =

    1973

  7. [7]

    , year = 1980, month = jan, volume =

    Polarization features of X-ray radiation emitted near black holes. , year = 1980, month = jan, volume =

    1980

  8. [8]

    , year = 2000, month = mar, volume =

    Light Curves of Rapidly Rotating Neutron Stars. , year = 2000, month = mar, volume =

    2000

Show all 286 references
  1. [9]

    Patruno and B

    A. Patruno and B. Haskell and N. Andersson , title =. doi:10.3847/1538-4357/aa927a , year = 2017, month =

    2017 doi

  2. [10]

    , year = 2021, month = mar, volume =

    Spectral and polarization properties of black hole accretion disc emission: including absorption effects. , year = 2021, month = mar, volume =

    2021

  3. [11]

    , year = 1987, month = may, volume =

    The light curves of low-mass X-ray binaries. , year = 1987, month = may, volume =

    1987

  4. [12]

    , year = 1988, month = jan, volume =

    The X-Ray Spectral Properties of Accretion Disks in X-Ray Binaries. , year = 1988, month = jan, volume =

    1988

  5. [13]

    , year = 1984, month = jan, volume =

    Energy spectra of low-mass binary X-ray sources observed from Tenma. , year = 1984, month = jan, volume =

    1984

  6. [14]

    , year = 1989, month = jan, volume =

    Luminosity-related changes of the energy spectrum of X 1608-522. , year = 1989, month = jan, volume =

    1989

  7. [15]

    , year = 1989, month = nov, volume =

    Two patterns of correlated X-ray timing and spectral behaviour in low-mass X-ray binaries. , year = 1989, month = nov, volume =

    1989

  8. [16]

    , year = 1989, month = jan, volume =

    Quasi-periodic oscillations and noise in low-mass X-ray binaries. , year = 1989, month = jan, volume =

    1989

  9. [17]

    , year = 1990, month = sep, volume =

    Correlation of X-Ray Burst Properties with Source State in the ``Atoll'' Source 4U/MXB 1636-53. , year = 1990, month = sep, volume =

    1990

  10. [18]

    , title =

    van der Klis, M. , title =. X-ray Binaries , editor =

  11. [19]

    , year = 1995, month = dec, volume =

    X-Ray Spectra of Z Sources. , year = 1995, month = dec, volume =

    1995

  12. [20]

    , editor=

    van der Klis, M. , editor=. Rapid X-ray variability , DOI=. Compact stellar X-ray sources , publisher =. 2006 , pages=

    2006

  13. [21]

    , year = 2010, month = mar, volume =

    On the nature of the Cygnus X-2 like Z-track sources. , year = 2010, month = mar, volume =

    2010

  14. [22]

    , year = 2012, month = jan, volume =

    Dipping - versus flaring in Z-track sources: resolving the controversy. , year = 2012, month = jan, volume =

    2012

  15. [23]

    , year = 2012, month = oct, volume =

    Spectral investigations of the nature of the Scorpius X-1 like sources. , year = 2012, month = oct, volume =

    2012

  16. [24]

    , year = 2003, month = oct, volume =

    Boundary layer, accretion disk and X-ray variability in the luminous LMXBs. , year = 2003, month = oct, volume =

    2003

  17. [25]

    10.1051/0004-6361:20053964

    Boundary layer emission and Z-track in the color-color diagram of luminous LMXBs , DOI= "10.1051/0004-6361:20053964", journal =

    doi

  18. [26]

    Revnivtsev, M. G. and Suleimanov, V. F. and Poutanen, J. , title = ". , volume =. 2013 , month =

    2013

  19. [27]

    Everything you always wanted to know about accretion but were afraid to ask

    Modelling the behaviour of accretion flows in X-ray binaries. Everything you always wanted to know about accretion but were afraid to ask. , year = 2007, month = dec, volume =

    2007

  20. [28]

    , year = 2011, month = may, volume =

    BeppoSAX view of the NS-LMXB GS 1826-238. , year = 2011, month = may, volume =

    2011

  21. [29]

    , year = 1994, month = jun, volume =

    Similarities in Neutron Star and Black Hole Accretion. , year = 1994, month = jun, volume =

    1994

  22. [30]

    , year = 2006, month = feb, volume =

    Jets in neutron star X-ray binaries: a comparison with black holes. , year = 2006, month = feb, volume =

    2006

  23. [31]

    Handbook of X-ray and Gamma-ray Astrophysics , publisher =

    Low-Magnetic-Field Neutron Stars in X-ray Binaries. Handbook of X-ray and Gamma-ray Astrophysics , publisher =

  24. [32]

    , year = 1977, month = jan, volume =

    Soft X-ray emission from dwarf novae. , year = 1977, month = jan, volume =

    1977

  25. [33]

    Astronomy Letters , year = 1999, month = may, volume =

    Spread of matter over a neutron-star surface during disk accretion. Astronomy Letters , year = 1999, month = may, volume =

    1999

  26. [34]

    and Poutanen, J

    Suleimanov, V. and Poutanen, J. , title = ". , volume =. 2006 , month =

    2006

  27. [35]

    , year = 2001, month = jan, volume =

    Accretion Disk Boundary Layers around Neutron Stars: X-Ray Production in Low-Mass X-Ray Binaries. , year = 2001, month = jan, volume =

    2001

  28. [36]

    , year = 1985, month = feb, volume =

    Comptonization of low-frequency radiation in accretion disks Angular distribution and polarization of hard radiation. , year = 1985, month = feb, volume =

    1985

  29. [37]

    A treatise on radiative transfer

  30. [38]

    , year = 2024, month = apr, volume =

    The polarization of the boundary layer around weakly magnetized neutron stars in X-ray binaries. , year = 2024, month = apr, volume =

    2024

  31. [39]

    , year = 2025, month = oct, volume =

    A Monte Carlo spectropolarimetric model for the high-soft state of neutron star low-mass X-ray binaries. , year = 2025, month = oct, volume =

    2025

  32. [40]

    , year = 2025, month = apr, volume =

    Polarized radiation from the spreading layer of weakly magnetized neutron stars. , year = 2025, month = apr, volume =

    2025

  33. [41]

    , year = 1982, month = jun, volume =

    Accretion disk coronae. , year = 1982, month = jun, volume =

    1982

  34. [42]

    , year = 1988, month = jan, volume =

    X-ray orbital modulations from low-mass X-ray binaries. , year = 1988, month = jan, volume =

    1988

  35. [43]

    Schnittman and Julian H

    Jeremy D. Schnittman and Julian H. Krolik , title =. doi:10.1088/0004-637X/701/2/1175 , year =

    doi

  36. [44]

    , year = 1996, month = dec, volume =

    Green's matrix for Compton reflection of polarized radiation from cold matter. , year = 1996, month = dec, volume =

    1996

  37. [45]

    , year = 1993, month = feb, volume =

    X-ray polarization properties of a centrally illuminated accretion disc. , year = 1993, month = feb, volume =

    1993

  38. [46]

    , year = 1985, month = nov, volume =

    Angular distribution and polarization of X-ray-burster radiation (during stationary and flash phases). , year = 1985, month = nov, volume =

    1985

  39. [47]

    , year = 2024, month = jan, volume =

    Reflecting on accretion in neutron star low-mass X-ray binaries. , year = 2024, month = jan, volume =

    2024

  40. [48]

    , year = 2013, month = apr, volume =

    Irradiation of an accretion disc by a jet: general properties and implications for spin measurements of black holes. , year = 2013, month = apr, volume =

    2013

  41. [49]

    , year = 2014, month = oct, volume =

    The role of the reflection fraction in constraining black hole spin. , year = 2014, month = oct, volume =

    2014

  42. [50]

    , year = 2014, month = feb, volume =

    Improved Reflection Models of Black Hole Accretion Disks: Treating the Angular Distribution of X-Rays. , year = 2014, month = feb, volume =

    2014

  43. [51]

    , year = 2022, month = feb, volume =

    Relativistic X-Ray Reflection Models for Accreting Neutron Stars. , year = 2022, month = feb, volume =

    2022

  44. [52]

    , keywords =

    Reflection spectra from an accretion disc illuminated by a neutron star X-ray burst. , keywords =

  45. [53]

    , year = 2016, month = oct, volume =

    The effects of high density on the X-ray spectrum reflected from accretion discs around black holes. , year = 2016, month = oct, volume =

    2016

  46. [54]

    , year = 2025, month = jun, volume =

    A Persistent Disk Wind and Variable Jet Outflow in the Neutron-star Low-mass X-Ray Binary GX 13+1. , year = 2025, month = jun, volume =

    2025

  47. [55]

    arXiv e-prints , year = 2025, month = jul, eid =

    X-ray polarization of reflected thermal emission. arXiv e-prints , year = 2025, month = jul, eid =

    2025

  48. [56]

    Direct radiation

    Polarization properties of thermal accretion disk emission: I. Direct radiation. , year = 2026, month = jan, volume =

    2026

  49. [57]

    , year = 2001, month = feb, volume =

    High-Energy X-Ray Timing Experiment Detections of Hard X-Ray Tails in Scorpius X-1. , year = 2001, month = feb, volume =

    2001

  50. [58]

    , year = 2006, month = nov, volume =

    Average hard X-ray emission from NS LMXBs: observational evidence of different spectral states in NS LMXBs. , year = 2006, month = nov, volume =

    2006

  51. [59]

    , year = 1966, month = aug, volume =

    Cosmic X-Ray Sources-Galactic and Extragalactic. , year = 1966, month = aug, volume =

    1966

  52. [60]

    , year = 1979, month = jul, volume =

    The halo population X-ray source Cygnus X-2. , year = 1979, month = jul, volume =

    1979

  53. [61]

    , year = 1990, month = aug, volume =

    Optical spectroscopy of V 1341 Cygni, the optical counterpart of Cygnus X-2. , year = 1990, month = aug, volume =

    1990

  54. [62]

    , year = 1998, month = jan, volume =

    The Mass of the Neutron Star in Cygnus X-2 (V1341 Cygni). , year = 1998, month = jan, volume =

    1998

  55. [63]

    , year = 2010, month = feb, volume =

    On the mass of the neutron star in Cyg X-2. , year = 2010, month = feb, volume =

    2010

  56. [64]

    , year = 1999, month = may, volume =

    The optical light curves of Cygnus X-2 (V1341 Cyg) and the mass of its neutron star. , year = 1999, month = may, volume =

    1999

  57. [65]

    , year = 1998, month = feb, volume =

    Discovery of kHz Quasi-periodic Oscillations in the Z Source Cygnus X-2. , year = 1998, month = feb, volume =

    1998

  58. [66]

    , year = 1998, month = may, volume =

    A Type I Burst with Radius Expansion Observed from Cygnus X-2 with the Rossi X-Ray Timing Explorer. , year = 1998, month = may, volume =

    1998

  59. [67]

    , year = 1986, month = aug, volume =

    Spectral Variability of Cygnus X-2: Structure in the Circumsource Material. , year = 1986, month = aug, volume =

    1986

  60. [68]

    , year = 1993, month = jun, volume =

    Resolving the Iron K Line in Cygnus X-2: an Observation with BBXRT. , year = 1993, month = jun, volume =

    1993

  61. [69]

    , year = 1997, month = jul, volume =

    Low-energy line emission from Cygnus X-2 observed with the BeppoSAX LECS. , year = 1997, month = jul, volume =

    1997

  62. [70]

    , year = 2002, month = may, volume =

    On the spectral evolution of Cygnus X-2 along its color-color diagram. , year = 2002, month = may, volume =

    2002

  63. [71]

    , year = 2009, month = may, volume =

    The X-ray spectral evolution of Cygnus X-2 in the framework of bulk Comptonization. , year = 2009, month = may, volume =

    2009

  64. [72]

    , year = 2010, month = sep, volume =

    Relativistic Lines and Reflection from the Inner Accretion Disks Around Neutron Stars. , year = 2010, month = sep, volume =

    2010

  65. [73]

    , year = 2018, month = feb, volume =

    NuSTAR view of the Z-type neutron star low-mass X-ray binary Cygnus X-2. , year = 2018, month = feb, volume =

    2018

  66. [74]

    R. M. Ludlam and E. M. Cackett and J. A. Garc. Radius Constraints from Reflection Modeling of Cygnus X-2 with. , volume =

  67. [75]

    , year = 2013, month = oct, volume =

    Radio and X-ray observations of jet ejection in Cygnus X-2. , year = 2013, month = oct, volume =

    2013

  68. [76]

    , year = 2026, month = jan, volume =

    XRISM Observations of Accretion Disk Corona in Cyg X-2. , year = 2026, month = jan, volume =

    2026

  69. [77]

    Journal of High Energy Astrophysics , year = 2026, month = mar, volume =

    Decoding Cygnus X-2: The critical role of reflection in IXPE data. Journal of High Energy Astrophysics , year = 2026, month = mar, volume =

    2026

  70. [78]

    , year = 2007, month = sep, volume =

    The variable radio counterpart and possible large-scale jet of the new Z source XTE J1701-462. , year = 2007, month = sep, volume =

    2007

  71. [79]

    The Astronomer's Telegram , keywords =

    Radius expansion bursts from the neutron star transient XTE J1701-462; a new distance estimate. The Astronomer's Telegram , keywords =

  72. [80]

    The Astronomer's Telegram , keywords =

    New X-ray Transient, XTE J1701-462. The Astronomer's Telegram , keywords =

  73. [81]

    The Astronomer's Telegram , keywords =

    Continuing RXTE observations of XTE J1701-462: a new ``Z'' in town?. The Astronomer's Telegram , keywords =

  74. [82]

    The Astronomer's Telegram , keywords =

    First detection of a type-I X-ray burst from the transient Z source XTE J1701-462. The Astronomer's Telegram , keywords =

  75. [83]

    The Astronomer's Telegram , keywords =

    Rapid decay of the neutron star transient XTE J1701-462. The Astronomer's Telegram , keywords =

  76. [84]

    and Remillard, R

    Lin, D. and Remillard, R. A. and Homan, J. , title =

  77. [85]

    and Altamirano, D

    Lin, D. and Altamirano, D. and Homan, J. and Remillard, R. A. and Wijnands, R. and Belloni, T. , title =

  78. [86]

    , year = 2010, month = aug, volume =

    XTE J1701-462 and Its Implications for the Nature of Subclasses in Low-magnetic-field Neutron Star Low-mass X-ray Binaries. , year = 2010, month = aug, volume =

    2010

  79. [87]

    Monthly Notices of the Royal Astronomical Society , volume =

    Sanna, Andrea and Méndez, Mariano and Altamirano, Diego and Homan, Jeroen and Casella, Piergiorgio and Belloni, Tomaso and Lin, Dacheng and van der Klis, Michiel and Wijnands, Rudy , title = ". Monthly Notices of the Royal Astronomical Society , volume =. 2010 , month =

    2010

  80. [88]

    , year = 2014, month = jun, volume =

    Cross-correlations between soft and hard light curves depending on luminosity in the transient neutron star XTE J1701-462. , year = 2014, month = jun, volume =

    2014

  81. [89]

    The Astronomer's Telegram , keywords =

    MAXI/GSC detection of a new X-ray outburst from XTE J1701-462. The Astronomer's Telegram , keywords =

  82. [90]

    The Astronomer's Telegram , keywords =

    Swift/XRT confirms outburst of XTE J1701-462. The Astronomer's Telegram , keywords =

  83. [91]

    , year = 2024, month = jun, volume =

    Constraining the physical parameters of XTE J1701-462 through NuSTAR observations. , year = 2024, month = jun, volume =

    2024

  84. [92]

    , year = 1968, month = jun, volume =

    Celestial Positions of X-Ray Sources in Sagittarius. , year = 1968, month = jun, volume =

    1968

  85. [93]

    Two Topics in X-Ray Astronomy, Volume 1: X Ray Binaries

    Non-Thermal Radio Emission of X-Ray Binaries. Two Topics in X-Ray Astronomy, Volume 1: X Ray Binaries. Volume 2: AGN and the X Ray Background , year = 1989, editor =

    1989

  86. [94]

    , year = 1991, month = jul, volume =

    Two hard X-ray sources in 100 square degrees around the Galactic Center. , year = 1991, month = jul, volume =

    1991

  87. [95]

    , year = 1993, month = dec, volume =

    Three Years of Monitoring GRS 1758-258: an Extremely Hard X-Ray Source near GX 5-1. , year = 1993, month = dec, volume =

    1993

  88. [96]

    , year = 1994, month = sep, volume =

    Spectral and correlated timing behaviour of GX5-1. , year = 1994, month = sep, volume =

    1994

  89. [97]

    , year = 2000, month = jul, volume =

    The infrared counterpart of the Z source GX 5-1. , year = 2000, month = jul, volume =

    2000

  90. [98]

    , year = 2002, month = jul, volume =

    Low- and high-frequency variability as a function of spectral properties in the bright X-ray binary GX 5-1. , year = 2002, month = jul, volume =. doi:10.1046/j.1365-8711.2002.05442.x , archivePrefix =. astro-ph/0202420 , primaryClass =

    2002

  91. [99]

    , year = 2000, month = sep, volume =

    The radio luminosity of persistent X-ray binaries. , year = 2000, month = sep, volume =

    2000

  92. [100]

    , year = 2006, month = sep, volume =

    The X-Ray Halo of GX 5-1. , year = 2006, month = sep, volume =

    2006

  93. [101]

    , year = 2016, month = may, volume =

    New orbital ephemerides for the dipping source 4U 1323-619: constraining the distance to the source. , year = 2016, month = may, volume =

    2016

  94. [102]

    , year = 2018, month = jan, volume =

    Monte Carlo Simulation of the X-Ray Halos of GX 5-1 and GX 13+1 to Test Models of Insterstellar Dust Grains. , year = 2018, month = jan, volume =

    2018

  95. [103]

    , year = 2018, month = feb, volume =

    Absence of Reflection Features in NuSTAR Spectra of the Luminous Neutron Star X-Ray Binary GX 5-1. , year = 2018, month = feb, volume =

    2018

  96. [104]

    , year = 1999, month = jun, volume =

    X-ray reflection spectra from ionized slabs. , year = 1999, month = jun, volume =

    1999

  97. [105]

    and Gursky, H

    Giacconi, R. and Gursky, H. and Paolini, F. R. and Rossi, B. B. , journal =. ``Evidence for X-Rays From Sources Outside the Solar System''. 1962 , publisher =

    1962

  98. [106]

    , year = 1968, month = jun, volume =

    Detection of Radio Emission from Scorpio X-1. , year = 1968, month = jun, volume =

    1968

  99. [107]

    , year = 1979, month = sep, volume =

    The linear X-ray polarization of Scorpius X-1. , year = 1979, month = sep, volume =

    1979

  100. [108]

    , year = 2001, month = may, volume =

    Scorpius X-1: Energy Transfer from the Core to the Radio Lobes. , year = 2001, month = may, volume =

    2001

  101. [109]

    , year = 2001, month = sep, volume =

    Scorpius X-1: The Evolution and Nature of the Twin Compact Radio Lobes. , year = 2001, month = sep, volume =

    2001

  102. [110]

    Spectral Hardening during the Flaring Branch

    X-Ray Spectral and Timing Behavior of Scorpius X-1. Spectral Hardening during the Flaring Branch. , year = 2014, month = jul, volume =

    2014

  103. [111]

    , year = 2021, month = apr, volume =

    Distances to Galactic X-ray binaries with Gaia DR2. , year = 2021, month = apr, volume =

    2021

  104. [112]

    A Significant Detection of X-ray Polarization in Sco X-1 with

    Xiangyun Long and Hua Feng and Hong Li and Jiahuan Zhu and Qiong Wu and Jiahui Huang and Massimo Minuti and Weichun Jiang and Dongxin Yang and Saverio Citraro and Hikmat Nasimi and Jiandong Yu and Ge Jin and Ming Zeng and Peng An and Jiachen Jiang and Enrico Costa and Luca Bal...

  105. [113]

    , year = 2006, month = oct, volume =

    A Hard X-Ray View of Scorpius X-1 with INTEGRAL: Nonthermal Emission?. , year = 2006, month = oct, volume =

    2006

  106. [114]

    , year = 2021, month = oct, volume =

    Fe K and Fe K line detection in the NuSTAR spectrum of the ultra-bright Z source Scorpius X-1. , year = 2021, month = oct, volume =

    2021

  107. [115]

    Science , year = 1967, month = apr, volume =

    Distribution and Variability of Cosmic X-Ray Sources. Science , year = 1967, month = apr, volume =

    1967

  108. [116]

    , year = 1971, month = nov, volume =

    GX 349+2 and GX 340+0: Locations and X-Ray Pulsation Limits. , year = 1971, month = nov, volume =

    1971

  109. [117]

    , year = 1993, month = jan, volume =

    The radio counterpart of the Z source GX 340+0. , year = 1993, month = jan, volume =

    1993

  110. [118]

    , year = 1994, month = jan, volume =

    Simultaneous radio and X-ray observations of GX 340+0. , year = 1994, month = jan, volume =

    1994

  111. [119]

    , year = 1996, month = oct, volume =

    GX340+0 with EXOSAT: its correlated X-ray spectral and timing behaviour. , year = 1996, month = oct, volume =

    1996

  112. [120]

    , year = 2000, month = oct, volume =

    Simultaneous radio and X-ray observations of Galactic Centre low-mass X-ray binaries. , year = 2000, month = oct, volume =

    2000

  113. [121]

    , year = 2000, month = jul, volume =

    The Power Spectral Properties of the Z Source GX 340+0. , year = 2000, month = jul, volume =

    2000

  114. [122]

    Nuclear Physics B Proceedings Supplements , year = 2004, month = jun, volume =

    A BeppoSAX study of the Galactic Z-source GX 340+0. Nuclear Physics B Proceedings Supplements , year = 2004, month = jun, volume =

    2004

  115. [123]

    , year = 2005, month = feb, volume =

    2005

  116. [124]

    , year = 2009, month = mar, volume =

    Disk Reflection Signatures in the Spectrum of the Bright Z-Source GX 340+0. , year = 2009, month = mar, volume =

    2009

  117. [125]

    , year = 2013, month = mar, volume =

    Stability of the Photon Indices in Z-source GX 340+0 for Spectral States. , year = 2013, month = mar, volume =

    2013

  118. [126]

    , year = 2016, month = may, volume =

    An Ultra-fast X-Ray Disk Wind in the Neutron Star Binary GX 340+0. , year = 2016, month = may, volume =

    2016

  119. [127]

    , year = 2025, month = sep, volume =

    The structure of the relativistic Fe line in GX 340+0 as viewed with XRISM/Resolve, NICER, and NuSTAR. , year = 2025, month = sep, volume =

    2025

  120. [128]

    , year = 1998, month = apr, volume =

    GX349+2 (ScoX-2): an odd-ball among the Z sources. , year = 1998, month = apr, volume =

    1998

  121. [129]

    , year = 2001, month = jun, volume =

    Detection of a Hard Tail in the X-Ray Spectrum of the Z Source GX 349+2. , year = 2001, month = jun, volume =

    2001

  122. [130]

    Log(N)-Log(S) and luminosity function of X-ray binaries from RXTE/ASM data

    The Milky Way in X-rays for an outside observer. Log(N)-Log(S) and luminosity function of X-ray binaries from RXTE/ASM data. , year = 2002, month = sep, volume =

    2002

  123. [131]

    , year = 2003, month = dec, volume =

    X-ray spectral evolution of low-mass X-ray binary GX 349+2. , year = 2003, month = dec, volume =

    2003

  124. [132]

    , year = 2004, month = jan, volume =

    Disappearance of Hard X-Ray Emission in the Last BeppoSAX Observation of the Z Source GX 349+2. , year = 2004, month = jan, volume =

    2004

  125. [133]

    , year = 2008, month = feb, volume =

    Relativistic Iron Emission Lines in Neutron Star Low-Mass X-Ray Binaries as Probes of Neutron Star Radii. , year = 2008, month = feb, volume =

    2008

  126. [134]

    , year = 2009, month = jan, volume =

    A Search for Iron Emission Lines in the Chandra X-Ray Spectra of Neutron Star Low-Mass X-Ray Binaries. , year = 2009, month = jan, volume =

    2009

  127. [135]

    , year = 2009, month = oct, volume =

    A ionized reflecting skin above the accretion disk of GX 349+2. , year = 2009, month = oct, volume =

    2009

  128. [136]

    , year = 2018, month = nov, volume =

    A NuSTAR Observation of the Low-mass X-Ray Binary GX 349+2 throughout the Z-track. , year = 2018, month = nov, volume =

    2018

  129. [137]

    , year = 2023, month = aug, volume =

    Broad-band spectro-temporal investigation of neutron star low-mass X-ray binary GX 349+2. , year = 2023, month = aug, volume =

    2023

  130. [138]

    Space Telescopes and Instrumentation 2016: Ultraviolet to Gamma Ray , year = 2016, editor =

    The Imaging X-ray Polarimetry Explorer (IXPE). Space Telescopes and Instrumentation 2016: Ultraviolet to Gamma Ray , year = 2016, editor =. doi:10.1117/12.2235240 , adsurl =

    2016 doi

  131. [139]

    Journal of Astronomical Telescopes, Instruments, and Systems , year = 2020, month = oct, volume =

    In-flight calibration system of imaging x-ray polarimetry explorer. Journal of Astronomical Telescopes, Instruments, and Systems , year = 2020, month = oct, volume =

    2020

  132. [140]

    , year = 2021, month = nov, volume =

    The Instrument of the Imaging X-Ray Polarimetry Explorer. , year = 2021, month = nov, volume =

    2021

  133. [141]

    Weisskopf and Paolo Soffitta and Luca Baldini and Brian D

    Martin C. Weisskopf and Paolo Soffitta and Luca Baldini and Brian D. Ramsey and Stephen L. O'Dell and Roger W. Romani and Giorgio Matt and William D. Deininger and Wayne H. Baumgartner and Ronaldo Bellazzini and Enrico Costa and Jeffery J. Kolodziejczak and Luca Latronico and ...

    2022

  134. [142]

    , keywords =

    An efficient photoelectric X-ray polarimeter for the study of black holes and neutron stars. , keywords =

  135. [143]

    SoftwareX , year = 2022, month = jul, volume =

    ixpeobssim: A simulation and analysis framework for the imaging X-ray polarimetry explorer. SoftwareX , year = 2022, month = jul, volume =

    2022

  136. [144]

    , year = 2022, month = apr, volume =

    A Weighted Analysis to Improve the X-Ray Polarization Sensitivity of the Imaging X-ray Polarimetry Explorer. , year = 2022, month = apr, volume =

    2022

  137. [145]

    , year = 2023, month = apr, volume =

    Handling the Background in IXPE Polarimetric Data. , year = 2023, month = apr, volume =

    2023

  138. [146]

    Science China Physics, Mechanics, and Astronomy , year = 2025, month = sep, volume =

    Observatory science with eXTP. Science China Physics, Mechanics, and Astronomy , year = 2025, month = sep, volume =

    2025

  139. [147]

    , year = 2023, month = mar, volume =

    Accretion geometry of the neutron star low mass X-ray binary Cyg X-2 from X-ray polarization measurements. , year = 2023, month = mar, volume =

    2023

  140. [148]

    10.1051/0004-6361/202346275

    Discovery of strongly variable X-ray polarization in the neutron star low-mass X-ray binary transient XTE J1701-462 , DOI= "10.1051/0004-6361/202346275", url= "https://doi.org/10.1051/0004-6361/202346275", journal =

    doi

  141. [149]

    , year = 2025, month = mar, volume =

    Correlated spectro-polarimetric study along the Z track in XTE J1701 462 puts constraints on its coronal geometry. , year = 2025, month = mar, volume =

    2025

  142. [150]

    10.1051/0004-6361/202347374

    Discovery of a variable energy-dependent X-ray polarization in the accreting neutron star GX 5-1 , DOI= "10.1051/0004-6361/202347374", url= "https://doi.org/10.1051/0004-6361/202347374", journal =

    doi

  143. [151]

    , year =

    Highly Significant Detection of X-Ray Polarization from the Brightest Accreting Neutron Star Sco X-1. , year =

  144. [153]

    , submitted , keywords =

    X-ray and Radio Campaign of the Z-source GX 340+0 II: the X-ray polarization in the normal branch. , submitted , keywords =

  145. [154]

    , year = 2024, month = nov, volume =

    X-ray spectropolarimetric characterization of GX 340+0 in the horizontal branch: A highly inclined source?. , year = 2024, month = nov, volume =

    2024

  146. [155]

    , year = 2025, month = oct, volume =

    X-ray spectropolarimetric characterisation of the Z source GX 340+0 in the normal branch. , year = 2025, month = oct, volume =

    2025

  147. [156]

    , year = 2025, month = jun, volume =

    X-Ray Polarization Study of the Neutron Star Low-mass X-Ray Binary GX 349+2. , year = 2025, month = jun, volume =

    2025

  148. [157]

    , year = 2025, month = oct, volume =

    IXPE view of the Sco-like source GX 349+2 in the normal branch. , year = 2025, month = oct, volume =

    2025

  149. [158]

    , year = 2025, month = dec, volume =

    First X-Ray and Radio Polarimetry of the Neutron Star Low-mass X-Ray Binary GX 17+2. , year = 2025, month = dec, volume =

    2025

  150. [159]

    , year = 2026, month = feb, volume =

    Discovery of High X-Ray Polarization from the Neutron Star Low-mass X-Ray Binary Cyg X-2 on the Horizontal Branch. , year = 2026, month = feb, volume =

    2026

  151. [160]

    , year = 2023, month = feb, volume =

    Polarization Properties of the Weakly Magnetized Neutron Star X-Ray Binary GS 1826-238 in the High Soft State. , year = 2023, month = feb, volume =

    2023

  152. [161]

    , year = 2023, month = aug, volume =

    X-ray polarimetry and spectroscopy of the neutron star low-mass X-ray binary GX 9+9: An in-depth study with IXPE and NuSTAR. , year = 2023, month = aug, volume =

    2023

  153. [162]

    2023 , month =

    First Detection of X-Ray Polarization from the Accreting Neutron Star 4U 1820−303 , journal =. 2023 , month =. doi:10.3847/2041-8213/acec6e , url =

    2023 doi

  154. [163]

    X-Ray Polarimetry of the Dipping Accreting Neutron Star 4U 1624-49. , doi =. 2024 , month =

    2024

  155. [164]

    , year = 2024, month = oct, volume =

    Constraining the geometry of the dipping atoll 4U 1624-49 with X-ray spectroscopy and polarimetry. , year = 2024, month = oct, volume =

    2024

  156. [165]

    , year = 2024, month = oct, volume =

    X-ray spectropolarimetry of the bright atoll Serpens X-1. , year = 2024, month = oct, volume =

    2024

  157. [166]

    , year = 2025, month = may, volume =

    Unveiling the reflection spectrum in the ultracompact LMXB 4U 1820-30. , year = 2025, month = may, volume =

    2025

  158. [167]

    , year = 2024, month = dec, volume =

    First spectropolarimetric observation of the neutron star low-mass X-ray binary GX 3+1. , year = 2024, month = dec, volume =

    2024

  159. [168]

    , year = 2025, month = jun, volume =

    X-ray spectro-polarimetry analysis of the weakly magnetized neutron star X-ray binary GX 9+1. , year = 2025, month = jun, volume =

    2025

  160. [169]

    Kim and Andrea Marinucci and Herman L

    John Rankin and Fabio La Monaca and Alessandro Di Marco and Juri Poutanen and Anna Bobrikova and Vadim Kravtsov and Fabio Muleri and Maura Pilia and Alexandra Veledina and Rob Fender and Philip Kaaret and Dawoon E. Kim and Andrea Marinucci and Herman L. Marshall and Alessandro...

  161. [170]

    , Submitted , keywords =

    Exploring MAXI J1744-294: IXPE insights into a Newly Discovered X-ray Transient. , Submitted , keywords =

  162. [171]

    , Submitted , year = 2025, month = dec, doi =

    The First X-Ray Polarimetry of an Eclipsing Low-Mass X-Ray Binary: Serendipitous IXPE Observation of AX J1745.6-2901. , Submitted , year = 2025, month = dec, doi =

    2025

  163. [172]

    , year = 2015, month = jan, volume =

    On the Fe K absorption - accretion state connection in the Galactic Centre neutron star X-ray binary AX J1745.6-2901. , year = 2015, month = jan, volume =

    2015

  164. [173]

    , year = 2018, month = jan, volume =

    NuSTAR + XMM-Newton monitoring of the neutron star transient AX J1745.6-2901. , year = 2018, month = jan, volume =

    2018

  165. [174]

    , Submitted , year = 2025, month = sep, eid =

    The detection of high X-ray polarization from an accretion disc corona source and its modelling via Monte Carlo radiation transfer simulation. , Submitted , year = 2025, month = sep, eid =

    2025

  166. [175]

    , year = 2012, month = jul, volume =

    Optical and infrared light curves of the eclipsing X-ray binary V395 Car = 2S 0921-630. , year = 2012, month = jul, volume =

    2012

  167. [176]

    , keywords =

    The Nuclear Spectroscopic Telescope Array (NuSTAR) High-energy X-Ray Mission. , keywords =. doi:10.1088/0004-637X/770/2/103 , archivePrefix =. 1301.7307 , primaryClass =

    arXiv

  168. [177]

    , year = 2004, month = jun, volume =

    Evidence for a multizone warm absorber in the XMM-Newton spectrum of Markarian 304. , year = 2004, month = jun, volume =

    2004

  169. [178]

    Space Telescopes and Instrumentation 2016: Ultraviolet to Gamma Ray , year = 2016, editor =

    The Neutron star Interior Composition Explorer (NICER): design and development. Space Telescopes and Instrumentation 2016: Ultraviolet to Gamma Ray , year = 2016, editor =. doi:10.1117/12.2231304 , adsurl =

    2016 doi

  170. [179]

    , keywords =

    A NICER Spectrum of MAXI J1535-571: Near-maximal Black Hole Spin and Potential Disk Warping. , keywords =. doi:10.3847/2041-8213/aacc61 , archivePrefix =. 1806.04115 , primaryClass =

    arXiv

  171. [180]

    , keywords =

    NICER Discovers mHz Oscillations in the Clocked Burster GS 1826-238. , keywords =

  172. [181]

    10.1051/0004-6361/201527395

    Optimal binning of X-ray spectra and response matrix design , DOI= "10.1051/0004-6361/201527395", url= "https://doi.org/10.1051/0004-6361/201527395", journal =

    doi

  173. [182]

    HEAsoft: Unified Release of FTOOLS and XANADU

  174. [183]

    Astronomical Data Analysis Software and Systems V , year = 1996, series =

    XSPEC: The First Ten Years. Astronomical Data Analysis Software and Systems V , year = 1996, series =

    1996

  175. [184]

    , year = 1994, month = oct, volume =

    Generalized Comptonization Models and Application to the Recent High-Energy Observations. , year = 1994, month = oct, volume =. doi:10.1086/174760 , adsurl =

    1994 doi

  176. [185]

    , year = 2020, month = mar, volume =

    Spectral and temporal properties of Compton scattering by mildly relativistic thermal electrons. , year = 2020, month = mar, volume =

    2020

  177. [186]

    , keywords =

    On the Absorption of X-Rays in the Interstellar Medium. , keywords =

  178. [187]

    Atomic Data for Astrophysics. II. New Analytic FITS for Photoionization Cross Sections of Atoms and Ions. , keywords =

  179. [188]

    2025, , 697, A83

    Anitra , A., Gnarini , A., Di Salvo , T., et al. 2025, , 697, A83

    2025

  180. [189]

    M., Papei , H., Barmby , P., Bahramian , A., & Gorski , M

    Arnason , R. M., Papei , H., Barmby , P., Bahramian , A., & Gorski , M. D. 2021, , 502, 5455

    2021

  181. [190]

    Arnaud , K. A. 1996, in ASP Conf. Ser., Vol. 101, Astronomical Data Analysis Software and Systems V, ed. G. H. Jacoby & J. Barnes (San Francisco: Astron. Soc. Pac.), 17--20

    1996

  182. [191]

    A., Hynes , R

    Ashcraft , T. A., Hynes , R. I., & Robinson , E. L. 2012, , 424, 620

    2012

  183. [192]

    D., et al

    Baldini , L., Bucciantini , N., Lalla , N. D., et al. 2022, SoftwareX, 19, 101194

    2022

  184. [193]

    2024 a , , submitted, arXiv:2405.19324

    Bhargava , Y., Ng , M., Zhang , L., et al. 2024 a , , submitted, arXiv:2405.19324

    2024 arXiv

  185. [194]

    D., Ng , M., et al

    Bhargava , Y., Russell , T. D., Ng , M., et al. 2024 b , , submitted, arXiv:2411.00350

    2024 arXiv

  186. [195]

    2025, , 696, A181

    Bobrikova , A., Poutanen , J., & Loktev , V. 2025, , 696, A181

    2025

  187. [196]

    M., Romani , R

    Braje , T. M., Romani , R. W., & Rauch , K. P. 2000, , 531, 447

    2000

  188. [197]

    M., Miller , J

    Cackett , E. M., Miller , J. M., Ballantyne , D. R., et al. 2010, , 720, 205

    2010

  189. [198]

    2023, , 943, 129

    Capitanio , F., Fabiani , S., Gnarini , A., et al. 2023, , 943, 129

    2023

  190. [199]

    1960, Radiative transfer (New York: Dover Publications)

    Chandrasekhar , S. 1960, Radiative transfer (New York: Dover Publications)

    1960

  191. [200]

    J., Gibiec , A., Ba uci \'n ska-Church , M., & Jackson , N

    Church , M. J., Gibiec , A., Ba uci \'n ska-Church , M., & Jackson , N. K. 2012, , 546, A35

    2012

  192. [201]

    Clark , G. W. 2018, , 852, 121

    2018

  193. [202]

    2023, , 674, L10

    Cocchi , M., Gnarini , A., Fabiani , S., et al. 2023, , 674, L10

    2023

  194. [203]

    M., Cackett , E

    Coughenour , B. M., Cackett , E. M., Miller , J. M., & Ludlam , R. M. 2018, , 867, 64

    2018

  195. [204]

    D'A \` , A., Iaria , R., Di Salvo , T., Matt , G., & Robba , N. R. 2009, , 693, L1

    2009

  196. [205]

    L., Fabian , A

    Dauser , T., Garcia , J., Parker , M. L., Fabian , A. C., & Wilms , J. 2014, , 444, L100

    2014

  197. [206]

    2022, , 163, 170

    Di Marco , A., Costa , E., Muleri , F., et al. 2022, , 163, 170

    2022

  198. [207]

    2023 a , , 953, L22

    Di Marco , A., La Monaca , F., Poutanen , J., et al. 2023 a , , 953, L22

    2023

  199. [208]

    2023 b , , 165, 143

    Di Marco , A., Soffitta , P., Costa , E., et al. 2023 b , , 165, 143

    2023

  200. [209]

    2002, , 386, 535

    Di Salvo , T., Farinelli , R., Burderi , L., et al. 2002, , 386, 535

    2002

  201. [210]

    2024, in Handbook of X-ray and Gamma-ray Astrophysics, ed

    Di Salvo , T., Papitto , A., Marino , A., Iaria , R., & Burderi , L. 2024, in Handbook of X-ray and Gamma-ray Astrophysics, ed. C. Bambi & A. Santangelo (Singapore: Springer), 4031--4103

    2024

  202. [211]

    2024, , 684, A137

    Fabiani , S., Capitanio , F., Iaria , R., et al. 2024, , 684, A137

    2024

  203. [212]

    & Cocchi , M

    Farinelli , R. & Cocchi , M. 2025, , 702, A272

    2025

  204. [213]

    2023, , 519, 3681

    Farinelli , R., Fabiani , S., Poutanen , J., et al. 2023, , 519, 3681

    2023

  205. [214]

    2009, , 498, 509

    Farinelli , R., Paizis , A., Landi , R., & Titarchuk , L. 2009, , 498, 509

    2009

  206. [215]

    2024, , 684, A62

    Farinelli , R., Waghmare , A., Ducci , L., & Santangelo , A. 2024, , 684, A62

    2024

  207. [216]

    Fender , R. P. & Hendry , M. A. 2000, , 317, 1

    2000

  208. [217]

    B., Geldzahler , B

    Fomalont , E. B., Geldzahler , B. J., & Bradshaw , C. F. 2001 a , , 553, L27

    2001

  209. [218]

    B., Geldzahler , B

    Fomalont , E. B., Geldzahler , B. J., & Bradshaw , C. F. 2001 b , , 558, 283

    2001

  210. [219]

    2014, , 782, 76

    Garc \' a , J., Dauser , T., Lohfink , A., et al. 2014, , 782, 76

    2014

  211. [220]

    A., Dauser , T., Ludlam , R., et al

    Garc \' a , J. A., Dauser , T., Ludlam , R., et al. 2022, , 926, 13

    2022

  212. [221]

    2024 a , , 692, A123

    Gnarini , A., Farinelli , R., Ursini , F., et al. 2024 a , , 692, A123

    2024

  213. [222]

    2024 b , , 690, A230

    Gnarini , A., Lynne Saade , M., Ursini , F., et al. 2024 b , , 690, A230

    2024

  214. [223]

    2026, , 997, 299

    Gnarini , A., Ravi , S., Kaaret , P., et al. 2026, , 997, 299

    2026

  215. [224]

    2025, , 699, A230

    Gnarini , A., Ursini , F., Matt , G., et al. 2025, , 699, A230

    2025

  216. [225]

    2022, , 514, 2561

    Gnarini, A., Ursini, F., Matt, G., et al. 2022, , 514, 2561

    2022

  217. [226]

    J., Gilfanov , M., & Sunyaev , R

    Grimm , H. J., Gilfanov , M., & Sunyaev , R. 2002, , 391, 923

    2002

  218. [227]

    & van der Klis , M

    Hasinger , G. & van der Klis , M. 1989, , 225, 79

    1989

  219. [228]

    F., Lin , D., et al

    Homan , J., Steiner , J. F., Lin , D., et al. 2018, , 853, 157

    2018

  220. [229]

    2009, , 505, 1143

    Iaria , R., D'A \' , A., di Salvo , T., et al. 2009, , 505, 1143

    2009

  221. [230]

    Kaastra , J. S. & Bleeker , J. A. M. 2016, , 587, A151

    2016

  222. [231]

    J., Ng , M., et al

    Kashyap , U., Maccarone , T. J., Ng , M., et al. 2025 a , , 986, 207

    2025

  223. [232]

    J., Pattie , E

    Kashyap , U., Maccarone , T. J., Pattie , E. C., et al. 2025 b , , 994, 221

    2025

  224. [233]

    1994, , 289, 795

    Kuulkers , E., van der Klis , M., Oosterbroek , T., et al. 1994, , 289, 795

    1994

  225. [234]

    2025 a , , 702, A40

    La Monaca , F., Bobrikova , A., Poutanen , J., et al. 2025 a , , 702, A40

    2025

  226. [235]

    2025 b , , 702, A101

    La Monaca , F., Di Marco , A., Coti Zelati , F., et al. 2025 b , , 702, A101

    2025

  227. [236]

    M., et al

    La Monaca , F., Di Marco , A., Ludlam , R. M., et al. 2024 a , , 691, A253

    2024

  228. [237]

    2024 b , , 960, L11

    La Monaca , F., Di Marco , A., Poutanen , J., et al. 2024 b , , 960, L11

    2024

  229. [238]

    Lapidus , I. I. & Sunyaev , R. A. 1985, , 217, 291

    1985

  230. [239]

    2007, The Astronomer's Telegram, 1183, 1

    Lin , D., Homan , J., Remillard , R., & Wijnands , R. 2007, The Astronomer's Telegram, 1183, 1

    2007

  231. [240]

    2026, Journal of High Energy Astrophysics, 51, 100548

    Liu , H., Jiang , J., Ingram , A., et al. 2026, Journal of High Energy Astrophysics, 51, 100548

    2026

  232. [241]

    2022, , 924, L13

    Long, X., Feng, H., Li, H., et al. 2022, , 924, L13

    2022

  233. [242]

    Ludlam , R. M. 2024, , 369, 16

    2024

  234. [243]

    M., Ballhausen , R., Chakraborty , P., et al

    Ludlam , R. M., Ballhausen , R., Chakraborty , P., et al. 2025, , 77, S117

    2025

  235. [244]

    M., Cackett, E

    Ludlam, R. M., Cackett, E. M., Garc \' a, J. A., et al. 2022, , 927, 112

    2022

  236. [245]

    M., et al

    Marra , L., Miku s incov \'a , R., Vincentelli , F. M., et al. 2025, , Submitted

    2025

  237. [246]

    2026, , 705, A8

    Marra , L., Podgorn \'y , J., Taverna , R., et al. 2026, , 705, A8

    2026

  238. [247]

    1993, , 260, 663

    Matt , G. 1993, , 260, 663

    1993

  239. [248]

    M., Iaria , R., Di Salvo , T., et al

    Mazzola , S. M., Iaria , R., Di Salvo , T., et al. 2021, , 654, A102

    2021

  240. [249]

    2025, , Submitted

    Miku s incov \'a , R., Marra , L., Manikantan , H., et al. 2025, , Submitted

    2025

  241. [250]

    M., Gendreau , K., Ludlam , R

    Miller , J. M., Gendreau , K., Ludlam , R. M., et al. 2018, , 860, L28

    2018

  242. [251]

    M., Raymond , J., Cackett , E., Grinberg , V., & Nowak , M

    Miller , J. M., Raymond , J., Cackett , E., Grinberg , V., & Nowak , M. 2016, , 822, L18

    2016

  243. [252]

    1984, , 36, 741

    Mitsuda , K., Inoue , H., Koyama , K., et al. 1984, , 36, 741

    1984

  244. [253]

    1989, , 41, 97

    Mitsuda , K., Inoue , H., Nakamura , N., & Tanaka , Y. 1989, , 41, 97

    1989

  245. [254]

    2026, , 996, 49

    Mizumoto , M., Takahashi , H., Behar , E., et al. 2026, , 996, 49

    2026

  246. [255]

    Orosz , J. A. & Kuulkers , E. 1999, , 305, 132

    1999

  247. [256]

    2006, , 459, 187

    Paizis , A., Farinelli , R., Titarchuk , L., et al. 2006, , 459, 187

    2006

  248. [257]

    Parmar , A. N. & White , N. E. 1988, , 59, 147

    1988

  249. [258]

    2017, , 850, 106

    Patruno, A., Haskell, B., & Andersson, N. 2017, , 850, 106

    2017

  250. [259]

    2025, arXiv e-prints, arXiv:2507.23687

    Podgorn \'y , J., Dov c iak , M., Goosmann , R., et al. 2025, arXiv e-prints, arXiv:2507.23687

    2025 arXiv

  251. [260]

    2015, , 446, 1536

    Ponti , G., Bianchi , S., Mu \ n oz-Darias , T., et al. 2015, , 446, 1536

    2015

  252. [261]

    2018, , 473, 2304

    Ponti , G., Bianchi , S., Mu \ n oz-Darias , T., et al. 2018, , 473, 2304

    2018

  253. [262]

    N., & Svensson , R

    Poutanen , J., Nagendra , K. N., & Svensson , R. 1996, , 283, 892

    1996

  254. [263]

    K., & Miller , G

    Psaltis , D., Lamb , F. K., & Miller , G. S. 1995, , 454, L137

    1995

  255. [264]

    M., et al

    Rogantini , D., Homan , J., Plotkin , R. M., et al. 2025, , 986, 41

    2025

  256. [265]

    Schnittman, J. D. & Krolik, J. H. 2009, , 701, 1175

    2009

  257. [266]

    Smale , A. P. 1998, , 498, L141

    1998

  258. [267]

    K., Dame , T

    Smith , R. K., Dame , T. M., Costantini , E., & Predehl , P. 2006, , 648, 452

    2006

  259. [268]

    Sobolev , V. V. 1963, A treatise on radiative transfer

    1963

  260. [269]

    E., Rushton , A

    Spencer , R. E., Rushton , A. P., Ba uci \'n ska-Church , M., et al. 2013, , 435, L48

    2013

  261. [270]

    E., Gendreau , K

    Strohmayer , T. E., Gendreau , K. C., Altamirano , D., et al. 2018, , 865, 63

    2018

  262. [271]

    2025, , 698, A245

    Tarana , A., Capitanio , F., Gnarini , A., et al. 2025, , 698, A245

    2025

  263. [272]

    2021, , 501, 3393

    Taverna , R., Marra , L., Bianchi , S., et al. 2021, , 501, 3393

    2021

  264. [273]

    T., Jirawala , K., Gudennavar , S

    Thomas , N. T., Jirawala , K., Gudennavar , S. B., & Bubbly , S. G. 2024, , 531, 2237

    2024

  265. [274]

    2025, , Submitted, arXiv:2509.26147

    Tomaru , R., Done , C., & Odaka , H. 2025, , Submitted, arXiv:2509.26147

    2025

  266. [275]

    2023, , 676, A20

    Ursini , F., Farinelli , R., Gnarini , A., et al. 2023, , 676, A20

    2023

  267. [276]

    2024 a , , 690, A200

    Ursini , F., Gnarini , A., Bianchi , S., et al. 2024 a , , 690, A200

    2024

  268. [277]

    2024 b , Galaxies, 12, 43

    Ursini , F., Gnarini , A., Capitanio , F., et al. 2024 b , Galaxies, 12, 43

    2024

  269. [278]

    1989, , 27, 517

    van der Klis , M. 1989, , 27, 517

    1989

  270. [279]

    A., Ferland , G

    Verner , D. A., Ferland , G. J., Korista , K. T., & Yakovlev , D. G. 1996, , 465, 487

    1996

  271. [280]

    C., Soffitta, P., Baldini, L., et al

    Weisskopf, M. C., Soffitta, P., Baldini, L., et al. 2022, JATIS, 8, 1

    2022

  272. [281]

    White , N. E. & Holt , S. S. 1982, , 257, 318

    1982

  273. [282]

    E., Stella , L., & Parmar , A

    White , N. E., Stella , L., & Parmar , A. N. 1988, , 324, 363

    1988

  274. [283]

    1998, , 493, L87

    Wijnands , R., Homan , J., van der Klis , M., et al. 1998, , 493, L87

    1998

  275. [284]

    2000, , 542, 914

    Wilms , J., Allen , A., & McCray , R. 2000, , 542, 914

    2000

  276. [285]

    2025, , 695, A108

    Yu , W., Bu , Q., Doroshenko , V., et al. 2025, , 695, A108

    2025

  277. [286]

    A., Szanecki , M., Poutanen , J., Gierli \'n ski , M., & Biernacki , P

    Zdziarski , A. A., Szanecki , M., Poutanen , J., Gierli \'n ski , M., & Biernacki , P. 2020, , 492, 5234

    2020

  278. [287]

    2025, Science China Physics, Mechanics, and Astronomy, 68, 119507

    Zhou , P., Mao , J., Zhang , L., et al. 2025, Science China Physics, Mechanics, and Astronomy, 68, 119507

    2025

Pith tools

Reviewed August 1, 2026 · model on record in the stance chip above.