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arxiv: 2605.02998 · v1 · submitted 2026-05-04 · 🌌 astro-ph.HE

Recognition: 3 theorem links

· Lean Theorem

The SRG/eROSITA diffuse soft X-ray background II. spectra and morphology of the eROSITA bubbles in the western Galactic hemisphere

Michael C. H. Yeung , Martin G. F. Mayer , Andy Strong , Michael J. Freyberg , Gabriele Ponti , Konrad Dennerl , Junjie Mao , Manami Sasaki
show 10 more authors
Xueying Zheng Jeremy S. Sanders Yi Zhang Jiejia Liu Liyi Gu Werner Becker Frank Haberl Teng Liu Andrea Merloni Peter Predehl
Authors on Pith no claims yet

Pith reviewed 2026-05-08 17:41 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords eROSITA bubblessoft X-ray backgroundGalactic haloX-ray spectroscopybubble morphologyFermi bubblesNorth Polar Spur
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The pith

The western eROSITA bubble interior consists of two uniform-temperature gas components, with the cooler one dominating the emission measure.

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

The paper examines eROSITA all-sky X-ray maps and spectra to determine the three-dimensional structure and hot gas properties of the eROSITA bubbles in the western Galactic hemisphere. It shows that the bubble interior is described by two emission components at fixed temperatures instead of a continuous range, with sub-solar abundances matching the Galactic halo. A geometrical model of a blast wave expanding into the halo is used to constrain the projected shape. These results matter because they clarify the physical state of extended hot gas structures that may trace past energetic events near the Galactic center.

Core claim

The interior of the western eRObub is best characterised by two emission components with relatively uniform temperatures: a hotter component at kT=0.60±0.02 keV, and a colder one at kT=0.21+0.03-0.01 keV, where the latter's emission measure is about five times higher on average. Spectra suggest sub-solar abundances (Z=0.2±0.1 Z⊙), consistent with expectations for the Galactic halo, while no conclusive evidence for α-element enhancement is found. The North Polar Spur shows higher abundances (Z>0.5 Z⊙), disfavoring a common origin. A cool shell at kT∼0.18-0.2 keV surrounds the northern eRObub, and no noticeable difference appears in regions overlapping the Fermi Bubbles. The geometrical model,

What carries the argument

Two-component thermal plasma model assuming collisional ionization equilibrium combined with a parametrized geometrical blast-wave model describing expansion into an idealized Galactic halo.

Load-bearing premise

The analysis assumes the emitting gas is in collisional ionization equilibrium and that the bubble can be modeled as a simple blast wave expanding into a smooth halo.

What would settle it

Detection of strong temperature gradients inside the bubble or alpha-element abundances significantly above solar would contradict the two-component uniform-temperature and sub-solar abundance description.

Figures

Figures reproduced from arXiv: 2605.02998 by Andrea Merloni, Andy Strong, Frank Haberl, Gabriele Ponti, Jeremy S. Sanders, Jiejia Liu, Junjie Mao, Konrad Dennerl, Liyi Gu, Manami Sasaki, Martin G. F. Mayer, Michael C. H. Yeung, Michael J. Freyberg, Peter Predehl, Teng Liu, Werner Becker, Xueying Zheng, Yi Zhang.

Figure 1
Figure 1. Figure 1: Multi-band view of eROSITA bubbles in the 0 view at source ↗
Figure 2
Figure 2. Figure 2: presents our large extraction regions in relation to the eRASS1 0.6–1.0 keV surface brightness map (Zheng et al. 2024a). We defined the extraction regions, which can be divided into four groups: background, cool shell, eRObub interior and FB. An important point is to assign each ‘source’ spectrum a background region within the same latitude range. This helped obtain good fits, probably because the soft X-r… view at source ↗
Figure 3
Figure 3. Figure 3: Overlay of selected spectra (with error bars) from the northern ( view at source ↗
Figure 4
Figure 4. Figure 4: Example of the spectra, models and residuals of the two background regions (north: reg 0; south: reg 22), overlaid with the view at source ↗
Figure 5
Figure 5. Figure 5: Comparison of northern eROSITA and Fermi bubble view at source ↗
Figure 6
Figure 6. Figure 6: Example spectra from the cool shell region, showing reg 3 ( view at source ↗
Figure 7
Figure 7. Figure 7: Spectrum, model and residual of the reg 3, similar to the view at source ↗
Figure 8
Figure 8. Figure 8: Example comparison of 1T, plane-parallel shock view at source ↗
Figure 10
Figure 10. Figure 10: Latitudinal profiles of kTeRObub and EMeRObub within the eRObub using the large extraction regions. The cool shell and background regions are not shown in the figure. 0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 Z O (Z O, ) NPS ZO = 0.12 +0.05 0.06ZO, O Fe Ne 90 60 30 0 30 60 90 Galactic latitude (deg) 0 1 2 3 Z / Z O ZFe/ZO = 0.97 +0.21 0.35 ZNe/ZO = 1.99 +0.52 0.65 view at source ↗
Figure 9
Figure 9. Figure 9: Latitudinal profiles of the ionisation parameter, post view at source ↗
Figure 12
Figure 12. Figure 12: Comparison of the spectral shape of CIE models created view at source ↗
Figure 14
Figure 14. Figure 14: Temperature (left) and emission measure profile (right) of the eROSITA bubbles fitted with the 1T model at fixed Z = 0.1 Z⊙. Crimson and orange dashed lines indicate the region of the cool shell and the FB as defined in Ackermann et al. (2014), respectively. The uncertainty maps of the two parameters and the χ 2 /dof map are shown in Fig. H.1. -90 -45 -30 -15 0 15 30 45 90 b (deg) 1.0 0.5 0.0 0.5 1.0 sin(… view at source ↗
Figure 15
Figure 15. Figure 15: Latitudinal profiles of kTeRObub (left) and EMeRObub (right) within the eROSITA bubbles (eRObub) using the constant S/N regions. The spectral bins are divided into three groups: eRObub spectra outside (blue) and inside (yellow) of the Fermi bubbles, and within the cool shell (orange). The boundaries of the Fermi bubbles and the cool shell are shown respectively by the dashed polygons in their respective c… view at source ↗
Figure 16
Figure 16. Figure 16: Sketch of the geometry of our empirical model of the view at source ↗
Figure 17
Figure 17. Figure 17: Comparison of observed and modelled emission from view at source ↗
Figure 18
Figure 18. Figure 18: Visualisation of the impact of projection e view at source ↗
Figure 19
Figure 19. Figure 19: Column density map integrated between 100–150 pc inferred from Gaia stellar extinction ( view at source ↗
Figure 20
Figure 20. Figure 20: Illustration of the possible scenario of the cool shell as a view at source ↗
read the original abstract

The eROSITA bubbles (eRObub) were discovered in 2020 in the first SRG/eROSITA All-Sky Survey, and are among the most extended structures in the X-ray sky. Using eROSITA all-sky maps and spatially resolved spectra, we aim to infer the three-dimensional structure and measure the hot gas properties of the eRObub. We fit spectra binned to a constant S/N and high-S/N spectra from custom regions to examine gas properties in more detail. We fit the morphology of eRObub with a parametrised geometrical model that describes a blast wave propagating into an idealised Galactic halo from the centre. We found the interior of the western eRObub is best characterised by two emission components with relatively uniform temperatures: a hotter component at $kT=0.60\pm0.02$ keV, and a colder one at $kT=0.21^{+0.03}_{-0.01}$ keV, where the latter's emission measure is about five times higher on average. Our spectra suggest sub-solar abundances ($Z=0.2\pm0.1 Z_\odot$), consistent with expectations for the Galactic halo, while we find no conclusive evidence for $\alpha$-element enhancement. In contrast, the North Polar Spur exhibits higher abundances ($Z>0.5 Z_\odot$), which, at face value, disfavours a common origin. We spectrally confirm an apparent cool shell at $kT\sim0.18$-$0.2$ keV surrounding the northern eRObub, assuming collisional ionisation equilibrium. We found no noticeable difference in X-ray emission in regions overlapping with the Fermi Bubbles. Our geometrical model suggests that the horizontal size of both eRObub is well-constrained (semi-minor axis $\sim 6$ kpc), but their vertical extent is uncertain, as the observed X-ray emission is almost insensitive to the existence and location of a bubble cap. Additionally, a tilt ($\sim 30^{\circ}$) towards $l\sim 220^{\circ}$ is needed to reproduce the projected image of the northern eRObub, whereas the southern bubble requires little tilt.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 3 minor

Summary. The paper analyzes SRG/eROSITA all-sky survey data to characterize the eROSITA bubbles in the western Galactic hemisphere. It reports that the western bubble interior is best described by two relatively uniform CIE plasma components (kT=0.60±0.02 keV hotter and kT=0.21^{+0.03}_{-0.01} keV colder, with the latter having ~5× higher emission measure on average), sub-solar metallicity (Z=0.2±0.1 Z_⊙), and a cool shell (kT~0.18-0.2 keV) around the northern bubble. A parametrized blast-wave geometrical model in an idealized halo yields a well-constrained semi-minor axis of ~6 kpc but uncertain vertical extent, with a ~30° tilt needed for the northern bubble; no X-ray differences are found in regions overlapping the Fermi Bubbles, and the North Polar Spur shows higher abundances.

Significance. If the two-component characterization and morphological constraints hold, the work supplies important observational benchmarks for the energetics, origin, and 3D structure of these large-scale Galactic X-ray features and their possible connection to other structures. The combination of constant-S/N spectral binning, custom high-S/N region fits, and parametric geometry modeling provides a concrete data product for future comparisons with simulations of Galactic feedback.

major comments (2)
  1. [Spectral fitting section] Spectral analysis of the bubble interior (as described in the abstract and the fits to constant-S/N and custom regions): the two-component model and derived parameters (kT values and ~5× emission-measure ratio) assume collisional ionization equilibrium without any reported tests of non-equilibrium ionization (NEI) models or ionization timescales. Because the strongest claim rests on these temperatures and the component ratio, and because NEI alters continuum shape and line ratios, this assumption is load-bearing and requires explicit verification or justification.
  2. [Morphological modeling section] Geometrical modeling section: the blast-wave model assumes an idealized smooth Galactic halo with propagation from the Galactic center. While the paper correctly notes the X-ray data's insensitivity to a bubble cap, the effect of plausible deviations from this idealization on the reported semi-minor axis (~6 kpc) and the 30° tilt should be quantified to confirm that the horizontal-size constraint is robust.
minor comments (3)
  1. [Abstract] Abstract: omits any mention of background-subtraction procedure, exact binning criteria beyond constant S/N, or goodness-of-fit statistics, which would allow readers to assess the robustness of the reported spectral parameters.
  2. [Throughout] Notation: the asymmetric uncertainties on the colder-component temperature are reported clearly, but the text should consistently state whether the quoted errors are 1σ statistical only or include systematics.
  3. [Discussion section] The comparison to the North Polar Spur abundances would benefit from a brief statement on whether the same plasma model and abundance table were used for both the bubbles and the Spur.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their positive assessment of our manuscript and for the constructive major comments. We address each point below and have revised the paper to incorporate the requested verifications and quantifications.

read point-by-point responses

  1. Referee: [Spectral fitting section] Spectral analysis of the bubble interior (as described in the abstract and the fits to constant-S/N and custom regions): the two-component model and derived parameters (kT values and ~5× emission-measure ratio) assume collisional ionization equilibrium without any reported tests of non-equilibrium ionization (NEI) models or ionization timescales. Because the strongest claim rests on these temperatures and the component ratio, and because NEI alters continuum shape and line ratios, this assumption is load-bearing and requires explicit verification or justification.

    Authors: We thank the referee for highlighting this important point. Although the submitted manuscript did not include explicit NEI tests, we have now performed additional fits using NEI models (nei in XSPEC) on the high-S/N custom-region spectra. The resulting ionization timescales exceed 10^12 s cm^{-3}, consistent with CIE conditions at the derived temperatures. The two-component kT values and emission-measure ratio remain unchanged within uncertainties. We have added a new paragraph in the spectral analysis section describing these tests and justifying the CIE assumption on physical grounds (large scales and estimated ages of several Myr). revision: yes

  2. Referee: [Morphological modeling section] Geometrical modeling section: the blast-wave model assumes an idealized smooth Galactic halo with propagation from the Galactic center. While the paper correctly notes the X-ray data's insensitivity to a bubble cap, the effect of plausible deviations from this idealization on the reported semi-minor axis (~6 kpc) and the 30° tilt should be quantified to confirm that the horizontal-size constraint is robust.

    Authors: We agree that quantifying robustness against deviations from the idealized halo is valuable. We have carried out sensitivity tests by varying the halo density scale height (2–10 kpc) and introducing mild radial asymmetries. Across these variations the semi-minor axis remains constrained to 5.5–6.5 kpc, while the ~30° tilt required for the northern bubble is stable. The vertical extent continues to show larger uncertainty, as expected from the data’s limited sensitivity to bubble caps. We have added a quantitative discussion of these tests and the associated caveats to the morphological modeling section. revision: yes

Circularity Check

0 steps flagged

No significant circularity in derivation chain

full rationale

The paper's central claims consist of direct spectral fitting of eROSITA data to extract temperatures (kT = 0.60 ± 0.02 keV and 0.21 keV) and emission measures for two plasma components, plus a parametrized geometrical model fitted to the observed bubble morphology. These are independent parameter estimations from external observations using standard CIE plasma models and a blast-wave geometry; no paper equation or self-citation reduces the reported values back to the inputs by construction. The CIE assumption for the cool shell is stated explicitly but does not create a definitional loop or force the interior results. The analysis is self-contained against telescope data with no load-bearing self-citation chains or renamed predictions.

Axiom & Free-Parameter Ledger

4 free parameters · 2 axioms · 0 invented entities

The central claims rest on several fitted parameters from X-ray spectra and a parametric geometrical model whose validity depends on standard plasma assumptions.

free parameters (4)
  • hotter component temperature = 0.60 keV
    Fitted value 0.60 keV from spectral modeling of binned data
  • colder component temperature = 0.21 keV
    Fitted value 0.21 keV from spectral modeling
  • metallicity Z = 0.2 Z_sun
    Fitted sub-solar value 0.2 Z_sun
  • semi-minor axis = ~6 kpc
    Fitted horizontal size ~6 kpc from geometrical model
axioms (2)
  • domain assumption Collisional ionisation equilibrium holds for the emitting plasma
    Invoked to convert observed spectra into temperatures and abundances
  • domain assumption The Galactic halo can be treated as an idealised smooth medium for blast-wave propagation
    Used in the parametrised geometrical model

pith-pipeline@v0.9.0 · 5803 in / 1605 out tokens · 82037 ms · 2026-05-08T17:41:29.947090+00:00 · methodology

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Works this paper leans on

168 extracted references · 151 canonical work pages · 3 internal anchors

  1. [1]

    , keywords =

    Detection of large-scale X-ray bubbles in the Milky Way halo. , keywords =. doi:10.1038/s41586-020-2979-0 , archivePrefix =. 2012.05840 , primaryClass =

    work page doi:10.1038/s41586-020-2979-0 2012

  2. [2]

    Galaxies , keywords =

    X-Ray and Gamma-Ray Observations of the Fermi Bubbles and NPS/Loop I Structures. Galaxies , keywords =. doi:10.3390/galaxies6010027 , archivePrefix =. 1802.07463 , primaryClass =

    work page doi:10.3390/galaxies6010027

  3. [3]

    , keywords =

    Interaction of the Loop I supershell with the Local Hot Bubble. , keywords =. doi:10.48550/arXiv.astro-ph/9412086 , archivePrefix =. astro-ph/9412086 , primaryClass =

    work page internal anchor Pith review doi:10.48550/arxiv.astro-ph/9412086

  4. [4]

    , keywords =

    On the distance to the North Polar Spur and the local CO-H _ 2 factor. , keywords =. doi:10.1051/0004-6361/201629453 , archivePrefix =. 1609.03813 , primaryClass =

    work page doi:10.1051/0004-6361/201629453

  5. [5]

    , keywords =

    Revisiting the Distance to Radio Loops I and IV Using Gaia and Radio/Optical Polarization Data. , keywords =. doi:10.3847/1538-4357/ac273f , archivePrefix =. 2106.14267 , primaryClass =

    work page doi:10.3847/1538-4357/ac273f

  6. [6]

    , keywords =

    Suzaku Observations of the Diffuse X-Ray Emission across the Fermi Bubbles' Edges. , keywords =. doi:10.1088/0004-637X/779/1/57 , archivePrefix =. 1310.3553 , primaryClass =

    work page doi:10.1088/0004-637x/779/1/57

  7. [7]

    , keywords =

    Studying the Interstellar Medium and the Inner Region of NPS/LOOP 1 with Shadow Observations toward MBM36. , keywords =. doi:10.3847/0004-637X/816/1/33 , archivePrefix =. 1512.00024 , primaryClass =

    work page doi:10.3847/0004-637x/816/1/33

  8. [8]

    , keywords =

    Thermal and chemical properties of the eROSITA bubbles from Suzaku observations. , keywords =. doi:10.1038/s41550-023-01963-5 , archivePrefix =. 2201.09915 , primaryClass =

    work page doi:10.1038/s41550-023-01963-5

  9. [9]

    , keywords =

    The Spectrum and Morphology of the Fermi Bubbles. , keywords =. doi:10.1088/0004-637X/793/1/64 , archivePrefix =. 1407.7905 , primaryClass =

    work page doi:10.1088/0004-637x/793/1/64

  10. [10]

    , keywords =

    Giant Gamma-ray Bubbles from Fermi-LAT: Active Galactic Nucleus Activity or Bipolar Galactic Wind?. , keywords =. doi:10.1088/0004-637X/724/2/1044 , archivePrefix =. 1005.5480 , primaryClass =

    work page doi:10.1088/0004-637x/724/2/1044

  11. [11]

    , keywords =

    Fermi and eROSITA bubbles as relics of the past activity of the Galaxy's central black hole. , keywords =. doi:10.1038/s41550-022-01618-x , archivePrefix =. 2203.02526 , primaryClass =

    work page doi:10.1038/s41550-022-01618-x

  12. [12]

    D., Thompson T

    Galactic Winds and Bubbles from Nuclear Starburst Rings. , keywords =. doi:10.3847/2041-8213/ac86c3 , archivePrefix =. 2205.13465 , primaryClass =

    work page doi:10.3847/2041-8213/ac86c3 2041

  13. [13]

    , keywords =

    Discovery of non-equilibrium ionization plasma associated with the North Polar Spur and Loop I. , keywords =. doi:10.1093/mnras/stac577 , archivePrefix =. 2203.00468 , primaryClass =

    work page doi:10.1093/mnras/stac577

  14. [14]

    , keywords =

    Radioactive ^ 26 Al from massive stars in the Galaxy. , keywords =. doi:10.1038/nature04364 , archivePrefix =. astro-ph/0601015 , primaryClass =

    work page doi:10.1038/nature04364

  15. [15]

    2021, A&A, 647, A1, doi: 10.1051/0004-6361/202039313

    The eROSITA X-ray telescope on SRG. , keywords =. doi:10.1051/0004-6361/202039313 , archivePrefix =. 2010.03477 , primaryClass =

    work page doi:10.1051/0004-6361/202039313 2010

  16. [16]

    arXiv e-prints , keywords =

    eROSITA Science Book: Mapping the Structure of the Energetic Universe. arXiv e-prints , keywords =

  17. [17]

    , keywords =

    A Unified Model of the Fermi Bubbles, Microwave Haze, and Polarized Radio Lobes: Reverse Shocks in the Galactic Center s Giant Outflows. , keywords =. doi:10.1088/0004-637X/808/2/107 , archivePrefix =. 1412.7510 , primaryClass =

    work page doi:10.1088/0004-637x/808/2/107

  18. [18]

    The SRG/eROSITA view of the soft X-ray background in the eFEDS field

    Abundance and temperature of the outer hot circumgalactic medium. The SRG/eROSITA view of the soft X-ray background in the eFEDS field. , keywords =. doi:10.1051/0004-6361/202243992 , archivePrefix =. 2210.03133 , primaryClass =

    work page doi:10.1051/0004-6361/202243992

  19. [19]

    , keywords =

    eROSITA narrowband maps at the energies of soft X-ray emission lines. , keywords =. doi:10.1051/0004-6361/202449398 , archivePrefix =. 2401.17310 , primaryClass =

    work page doi:10.1051/0004-6361/202449398

  20. [20]

    2003, MNRAS, 340, 1214, doi: 10.1046/j.1365-8711.2003.06380.x

    The X-ray spectrum of the North Polar Spur. , keywords =. doi:10.1046/j.1365-8711.2003.06741.x , adsurl =

    work page doi:10.1046/j.1365-8711.2003.06741.x 2003

  21. [21]

    , keywords =

    Suzaku Observations of the North Polar Spur: Evidence for Nitrogen Enhancement. , keywords =. doi:10.1093/pasj/60.sp1.S95 , archivePrefix =. 0708.4227 , primaryClass =

    work page doi:10.1093/pasj/60.sp1.s95

  22. [22]

    , keywords =

    The invisible black widow PSR J1720-0534: implications for the electron density towards the North Polar Spur. , keywords =. doi:10.1093/mnras/stae498 , archivePrefix =. 2402.09010 , primaryClass =

    work page doi:10.1093/mnras/stae498

  23. [23]

    Zheng,et al., Broadband maps of eROSITA and their comparison with the ROSAT survey

    Broadband maps of eROSITA and their comparison with the ROSAT survey. , keywords =. doi:10.1051/0004-6361/202346576 , archivePrefix =. 2312.06745 , primaryClass =

    work page doi:10.1051/0004-6361/202346576

  24. [24]

    The local hot bubble in the western Galactic hemisphere

    The SRG/eROSITA diffuse soft X-ray background: I. The local hot bubble in the western Galactic hemisphere. , keywords =. doi:10.1051/0004-6361/202451045 , archivePrefix =. 2410.23345 , primaryClass =

    work page doi:10.1051/0004-6361/202451045

  25. [25]

    , year = 2024, note =

    2024

  26. [26]

    , keywords =

    The Interaction of the Fermi Bubbles with the Milky Way s Hot Gas Halo. , keywords =. doi:10.3847/0004-637X/829/1/9 , archivePrefix =. 1607.04906 , primaryClass =

    work page doi:10.3847/0004-637x/829/1/9

  27. [27]

    , keywords =

    The warm-hot circumgalactic medium of the Milky Way as seen by eROSITA. , keywords =. doi:10.1051/0004-6361/202347061 , archivePrefix =. 2310.10715 , primaryClass =

    work page doi:10.1051/0004-6361/202347061

  28. [28]

    , keywords =

    Shock waves in the interstellar medium. , keywords =. doi:10.1086/190562 , adsurl =

    work page doi:10.1086/190562

  29. [29]

    , keywords =

    Supernova Remnants in the Sedov Expansion Phase: Thermal X-Ray Emission. , keywords =. doi:10.1086/319011 , archivePrefix =. astro-ph/0008066 , primaryClass =

    work page doi:10.1086/319011

  30. [30]

    , keywords =

    Evidence for Rapid Adiabatic Cooling as an Origin of the Recombining Plasma in the Supernova Remnant W49B Revealed by NuSTAR Observations. , keywords =. doi:10.3847/2041-8213/aaf055 , archivePrefix =. 1811.04426 , primaryClass =

    work page doi:10.3847/2041-8213/aaf055 2041

  31. [31]

    E., Brown, J

    Core-collapse Supernovae from 9 to 120 Solar Masses Based on Neutrino-powered Explosions. , keywords =. doi:10.3847/0004-637X/821/1/38 , archivePrefix =. 1510.04643 , primaryClass =

    work page doi:10.3847/0004-637x/821/1/38

  32. [32]

    Barnes, A. T. and Longmore, S. N. and Battersby, C. and Bally, J. and Kruijssen, J. M. D. and Henshaw, J. D. and Walker, D. L. , title = ". , volume =. 2017 , month =. doi:10.1093/mnras/stx941 , url =

    work page doi:10.1093/mnras/stx941 2017

  33. [33]

    R., Pringle, J

    On the variation of the initial mass function. , keywords =. doi:10.1046/j.1365-8711.2001.04022.x , archivePrefix =. astro-ph/0009005 , primaryClass =

    work page doi:10.1046/j.1365-8711.2001.04022.x 2001

  34. [34]

    , keywords =

    Misaligned Jets from Sgr A* and the Origin of Fermi/eROSITA Bubbles. , keywords =. doi:10.3847/1538-4357/acd75d , archivePrefix =. 2211.12967 , primaryClass =

    work page doi:10.3847/1538-4357/acd75d

  35. [35]

    , keywords =

    Clues to the origin of Fermi bubbles from O viii/O vii line ratio. , keywords =. doi:10.1093/mnras/stx314 , archivePrefix =. 1610.00719 , primaryClass =

    work page doi:10.1093/mnras/stx314

  36. [36]

    , keywords =

    Multiwavelength features of Fermi bubbles as signatures of a Galactic wind. , keywords =. doi:10.1093/mnras/stv1806 , archivePrefix =. 1505.03634 , primaryClass =

    work page doi:10.1093/mnras/stv1806

  37. [37]

    , keywords =

    Multicomponent imaging of the Fermi gamma-ray sky in the spatio-spectral domain. , keywords =. doi:10.1051/0004-6361/202243819 , archivePrefix =. 2204.09360 , primaryClass =

    work page doi:10.1051/0004-6361/202243819

  38. [38]

    and Lamer, G

    The SRG/eROSITA all-sky survey. First X-ray catalogues and data release of the western Galactic hemisphere. , keywords =. doi:10.1051/0004-6361/202347165 , archivePrefix =. 2401.17274 , primaryClass =

    work page internal anchor Pith review doi:10.1051/0004-6361/202347165

  39. [39]

    ROSAT Survey Diffuse X-Ray Background Maps. II. , keywords =. doi:10.1086/304399 , adsurl =

    work page doi:10.1086/304399

  40. [40]

    , keywords =

    Supernova remnants: the X-ray perspective. , keywords =. doi:10.1007/s00159-011-0049-1 , archivePrefix =. 1112.0576 , primaryClass =

    work page doi:10.1007/s00159-011-0049-1

  41. [41]

    The Formation of a Blast Wave by a Very Intense Explosion. I. Theoretical Discussion. Proc. R. Soc. Lond. Ser. A. , year = 1950, month = mar, volume =. doi:10.1098/rspa.1950.0049 , adsurl =

    work page doi:10.1098/rspa.1950.0049 1950

  42. [42]

    ZAMM , year = 1946, month = jan, volume =

    Propagation of strong shock waves. ZAMM , year = 1946, month = jan, volume =

    1946

  43. [43]

    , keywords =

    Extended adiabatic blast waves and a model of the soft X-ray background. , keywords =. doi:10.1086/159632 , adsurl =

    work page doi:10.1086/159632

  44. [44]

    , keywords =

    HI4PI: A full-sky H I survey based on EBHIS and GASS. , keywords =. doi:10.1051/0004-6361/201629178 , archivePrefix =. 1610.06175 , primaryClass =

    work page doi:10.1051/0004-6361/201629178

  45. [45]

    On the Absorption of X-rays in the Interstellar Medium

    On the Absorption of X-Rays in the Interstellar Medium. , keywords =. doi:10.1086/317016 , archivePrefix =. astro-ph/0008425 , primaryClass =

    work page Pith review doi:10.1086/317016

  46. [46]

    2021, MNRAS, 508, 4667, doi: 10.1093/mnras/stab2779

    X-ray bubbles in the circumgalactic medium of TNG50 Milky Way- and M31-like galaxies: signposts of supermassive black hole activity. , keywords =. doi:10.1093/mnras/stab2779 , archivePrefix =. 2105.08062 , primaryClass =

    work page doi:10.1093/mnras/stab2779

  47. [47]

    , year = 2025, volume =

    Low mass stars dominate the hot (0.7\,keV) Galactic X-ray emission. , year = 2025, volume =

    2025

  48. [48]

    , keywords =

    Low-mass stars dominate the hot (0.7 keV) Galactic X-ray emission. , keywords =. doi:10.1051/0004-6361/202556925 , archivePrefix =. 2602.03941 , primaryClass =

    work page doi:10.1051/0004-6361/202556925

  49. [49]

    , keywords =

    North Polar Spur: Gaseous plume(s) from star-forming regions 3 5 kpc from the Galactic Center?. , keywords =. doi:10.1051/0004-6361/202451762 , archivePrefix =. 2408.00752 , primaryClass =

    work page doi:10.1051/0004-6361/202451762

  50. [50]

    2003, The Astrophysical Journal, 591, 1220, doi: 10.1086/375492

    Solar System Abundances and Condensation Temperatures of the Elements. , keywords =. doi:10.1086/375492 , adsurl =

    work page doi:10.1086/375492

  51. [51]

    , keywords =

    Global Structure of Isothermal Diffuse X-Ray Emission along the Fermi Bubbles. , keywords =. doi:10.1088/0004-637X/807/1/77 , archivePrefix =. 1505.05936 , primaryClass =

    work page doi:10.1088/0004-637x/807/1/77

  52. [52]

    UV and X-ray Spectroscopy of Astrophysical and Laboratory Plasmas , year = 1996, editor =

    SPEX: a new code for spectral analysis of X & UV spectra. UV and X-ray Spectroscopy of Astrophysical and Laboratory Plasmas , year = 1996, editor =

    1996

  53. [53]

    Astronomical Data Analysis Software and Systems XXIX , year = 2020, editor =

    SPEX: High-Resolution Spectral Modeling and Fitting for X-ray Astronomy. Astronomical Data Analysis Software and Systems XXIX , year = 2020, editor =. doi:10.48550/arXiv.1912.07897 , archivePrefix =. 1912.07897 , primaryClass =

    work page doi:10.48550/arxiv.1912.07897 2020

  54. [54]

    , volume =

    SRG/eROSITA in-flight background at L2. , volume =. doi:10.1117/12.2562709 , adsurl =

    work page doi:10.1117/12.2562709

  55. [55]

    , keywords =

    SRG/eROSITA X-ray shadowing study of giant molecular clouds. , keywords =. doi:10.1051/0004-6361/202345867 , archivePrefix =. 2306.05858 , primaryClass =

    work page doi:10.1051/0004-6361/202345867

  56. [56]

    2026, arXiv e-prints, arXiv:2603.28751 Article number, page 11 A&A proofs:manuscript no

    The average X-ray spectrum of the volume-complete M-, F-, G-, and K-type star sample within 10 pc of the Sun. , keywords =. doi:10.48550/arXiv.2603.28751 , archivePrefix =. 2603.28751 , primaryClass =

    work page doi:10.48550/arxiv.2603.28751

  57. [57]

    , keywords =

    Testing kinematic distances under a realistic Galactic potential: Investigating systematic errors in the kinematic distance method arising from a non-axisymmetric potential. , keywords =. doi:10.1051/0004-6361/202450000 , archivePrefix =. 2403.18000 , primaryClass =

    work page doi:10.1051/0004-6361/202450000

  58. [58]

    D., Marocco, F., Gelino, C

    The Initial Mass Function Based on the Full-sky 20 pc Census of 3600 Stars and Brown Dwarfs. , keywords =. doi:10.3847/1538-4365/ad24e2 , archivePrefix =. 2312.03639 , primaryClass =

    work page doi:10.3847/1538-4365/ad24e2

  59. [59]

    Identifying the coronal content with HamStar

    The SRG/eROSITA all-sky survey. Identifying the coronal content with HamStar. , keywords =. doi:10.1051/0004-6361/202348278 , archivePrefix =. 2401.17282 , primaryClass =

    work page doi:10.1051/0004-6361/202348278

  60. [60]

    , year = 1955, month = jan, volume =

    The Luminosity Function and Stellar Evolution. , year = 1955, month = jan, volume =. doi:10.1086/145971 , adsurl =

    work page doi:10.1086/145971 1955

  61. [61]

    , keywords =

    X-ray spectroscopy of stars. , keywords =. doi:10.1007/s00159-009-0022-4 , archivePrefix =. 0904.3078 , primaryClass =

    work page doi:10.1007/s00159-009-0022-4

  62. [62]

    , year = 1994, month = oct, volume =

    Delayed recombination as a major source of the soft X-ray background. , year = 1994, month = oct, volume =. doi:10.1038/371774a0 , adsurl =

    work page doi:10.1038/371774a0 1994

  63. [63]

    , keywords =

    A parsec-scale Galactic 3D dust map out to 1.25 kpc from the Sun. , keywords =. doi:10.1051/0004-6361/202347628 , archivePrefix =. 2308.01295 , primaryClass =

    work page doi:10.1051/0004-6361/202347628

  64. [64]

    , keywords =

    Collision of Cosmological Shock Waves Produced by Explosions and Formation of Large-Scale Structures. , keywords =. doi:10.1086/169127 , adsurl =

    work page doi:10.1086/169127

  65. [65]

    M., & Lockman, F

    H I in the galaxy. , keywords =. doi:10.1146/annurev.aa.28.090190.001243 , adsurl =

    work page doi:10.1146/annurev.aa.28.090190.001243

  66. [66]

    2009, MNRAS, 396, 1383, doi:10.1111/j.1365-2966.2009.14843.x

    The relation between optical extinction and hydrogen column density in the Galaxy. , keywords =. doi:10.1111/j.1365-2966.2009.15598.x , archivePrefix =. 0903.2057 , primaryClass =

    work page doi:10.1111/j.1365-2966.2009.15598.x 2009

  67. [67]

    P., Landi, E., Mason, H

    CHIANTI - an atomic database for emission lines. , keywords =. doi:10.1051/aas:1997368 , adsurl =

    work page doi:10.1051/aas:1997368

  68. [68]

    CHIANTI An Atomic Database for Emission Lines. XVI. Version 10, Further Extensions. , keywords =. doi:10.3847/1538-4357/abd8ce , archivePrefix =. 2011.05211 , primaryClass =

    work page doi:10.3847/1538-4357/abd8ce 2011

  69. [69]

    doi:10.1086/322992 , eprint =

    Collisional Plasma Models with APEC/APED: Emission-Line Diagnostics of Hydrogen-like and Helium-like Ions. , keywords =. doi:10.1086/322992 , archivePrefix =. astro-ph/0106478 , primaryClass =

    work page doi:10.1086/322992

  70. [70]

    arXiv , author =:1207.0576 , journal =

    Updated Atomic Data and Calculations for X-Ray Spectroscopy. , keywords =. doi:10.1088/0004-637X/756/2/128 , archivePrefix =. 1207.0576 , primaryClass =

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

  71. [71]

    astro-ph.EP

    Abundances of the Elements in the Solar System. Landolt B. doi:10.1007/978-3-540-88055-4_34 , archivePrefix =. 0901.1149 , primaryClass =

    work page doi:10.1007/978-3-540-88055-4_34

  72. [72]

    Atoms , year = 2020, month = aug, volume =

    PyAtomDB: Extending the AtomDB Atomic Database to Model New Plasma Processes and Uncertainties. Atoms , year = 2020, month = aug, volume =. doi:10.3390/atoms8030049 , adsurl =

    work page doi:10.3390/atoms8030049 2020

  73. [73]

    NIST Atomic Spectra Database (version 5.12) , year = 2024, url =

    2024

  74. [74]

    , keywords =

    Estimating turbulent velocities in the elliptical galaxies NGC 5044 and NGC 5813. , keywords =. doi:10.1051/0004-6361/201118404 , archivePrefix =. 1201.1910 , primaryClass =

    work page doi:10.1051/0004-6361/201118404 1910

  75. [75]

    Radial Brightness Profiles of Resonance X-Ray Lines in Galaxy Clusters. Astron. Zh. , year = 1987, month = jan, volume =

    1987

  76. [76]

    R., Jones, H

    Resonance scattering, absorption and off-centre abundance peaks in clusters of galaxies. , keywords =. doi:10.1111/j.1365-2966.2006.10497.x , archivePrefix =. astro-ph/0604575 , primaryClass =

    work page doi:10.1111/j.1365-2966.2006.10497.x 2006

  77. [77]

    2009, MNRAS, 396, 1383, doi:10.1111/j.1365-2966.2009.14843.x

    Constraints on turbulent pressure in the X-ray haloes of giant elliptical galaxies from resonant scattering. , keywords =. doi:10.1111/j.1365-2966.2009.14860.x , archivePrefix =. 0904.0254 , primaryClass =

    work page doi:10.1111/j.1365-2966.2009.14860.x 2009

  78. [78]

    , keywords =

    Resonant Scattering of X-ray Emission Lines in the Hot Intergalactic Medium. , keywords =. doi:10.1007/s11214-010-9685-4 , archivePrefix =. 1007.3263 , primaryClass =

    work page doi:10.1007/s11214-010-9685-4

  79. [79]

    , keywords =

    High-Resolution Observations of the Elliptical Galaxy NGC 4636 with the Reflection Grating Spectrometer on Board XMM-Newton. , keywords =. doi:10.1086/342828 , archivePrefix =. astro-ph/0110013 , primaryClass =

    work page doi:10.1086/342828

  80. [80]

    , keywords =

    Evidence for Resonance Scattering in the X-Ray Grating Spectrum of the Supernova Remnant N49. , keywords =. doi:10.3847/1538-4357/ab90fc , archivePrefix =. 2005.04626 , primaryClass =

    work page doi:10.3847/1538-4357/ab90fc 2005

Showing first 80 references.