GLOBAL STRUCTURE OF ISOTHERMAL DIFFUSE X-RAY EMISSION ALONG THE FERMI BUBBLES
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In our previous works, we found absorbed thermal X-ray plasma with kT 0.3 keV observed ubiquitously near the edges of the Fermi bubbles and interpreted this emission as weakly shock-heated Galactic halo gas. Here we present a systematic and uniform analysis of archival Suzaku (29 pointings; 6 newly presented) and Swift (68 pointings; 49 newly presented) data within Galactic longitudes < 20° and latitude 5°≲ < 60°, covering the whole extent of the Fermi bubbles. We show that the plasma temperature is constant at kT 0.30 ± 0.07 keV, while the emission measure (EM) varies by an order of magnitude, increasing toward the Galactic center (i.e., low ) with enhancements at the North Polar Spur (NPS), SE-claw, and NW-clump features. Moreover, the EM distribution of kT 0.30 keV plasma is highly asymmetric in the northern and southern bubbles. Although the association of the X-ray emission with the bubbles is not conclusive, we compare the observed EM properties with simple models assuming (i) a filled halo without bubbles, whose gas density follows a hydrostatic isothermal model (King profile), and (ii) a bubble-in-halo in which two identical bubbles expand into the halo, forming thick shells of swept halo gas. We argue that the EM profile in the north ( b > 0°) favors (ii), whereas that of the south ( b < 0°) is rather close to (i), but a weak excess signature is clearly detected also in the south like NPS (South Polar Spur). Such an asymmetry, if due to the bubbles, cannot be fully understood only by the inclination of bubbles' axis against the Galactic disk normal, thus suggesting asymmetric outflow due to different environmental/initial conditions.
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The total energy in the eROSITA bubbles is Eth ≃10^56 erg.
“Therefore, the energy density and the total energy in the eROSITA bubbles are, ϵ = nskBTs / ( γ -1) ≃ 2 × 10 -12 erg cm -3 and E th ≃ 10 56 erg, respectively (Kataoka et al. 2013, 2015; Predehl et al. 2020).”
From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Kataoka et al. 2015
The Introduction (page unavailable) discusses an energy release of 10^55–10^56 erg associated with the creation of the Fermi bubbles. It does not identify that figure as the total thermal energy of the eROSITA bubbles; the paper’s bubble model instead concerns X-ray emission along the Fermi bubbles. Thus the order of magnitude is present, but the attributed quantity and structure are not established by this source. (LLM, conf=0.84)
Experimental — accuracy not yet measuredThe energy density in the eROSITA bubbles is ε ≃2×10^-12 erg cm^-3.
“Therefore, the energy density and the total energy in the eROSITA bubbles are, ϵ = nskBTs / ( γ -1) ≃ 2 × 10 -12 erg cm -3 and E th ≃ 10 56 erg, respectively (Kataoka et al. 2013, 2015; Predehl et al. 2020).”
From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Kataoka et al. 2015
Section 4.2 gives a modeled Fermi-bubble shell density of 3.4 × 10^-3 cm^-3 and uses kT = 0.30 keV; these yield an energy density of roughly 2 × 10^-12 erg cm^-3 under the citing sentence’s formula. The paper does not give that energy density explicitly or establish it for the eROSITA bubbles. Page numbers are unavailable in our copy. (LLM, conf=0.82)
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Galactic Centre hypershell model for the North Polar Spurs
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Fermi bubbles from stochastic acceleration of electrons in a Galactic outflow
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Cosmic-ray electrons and the magnetic field of the North Polar Spur
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Fermi/eROSITA bubbles as relics of the past activity of the galaxy’s central black hole
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The SRG/eROSITA diffuse soft X-ray background
Yeung, M. C. H., Mayer, M. G. F., Strong, A. W., Freyberg, M. J., Ponti, G., Dennerl, K., Mao, J., Sasaki, M., Zheng, X., Sanders, J. S., et al. (2026) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202558206
- Authors
- Kataoka, J., Tahara, M., Totani, T., Sofue, Y., Inoue, Y., Nakashima, S., & Cheung, C. C.
- Affiliations
- Waseda University (JP)
- The University of Tokyo (JP)
- Institute of Space and Astronautical Science (JP)
- United States Naval Research Laboratory (US)
- Corresponding author
- Kataoka, J.
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 2015-07-01
- Volume
- 807
- Issue
- 1
- Pages
- 77
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W2268553864
- Cited by
- 41
- References
- 65
- Citations by year
- 2026: 1 · 2024: 2 · 2023: 5 · 2022: 4 · 2021: 3 · 2020: 4 · 2019: 2 · 2018: 8 · 2017: 5 · 2016: 6 · 2015: 1
- FWCI
- 3.34
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Licence
- Locations
- The Astrophysical Journal (publishedVersion)
- JAXA Repository (JAXA) (submittedVersion, cc-by-nc-nd)
- Topics
- Physical Sciences › Physics and Astronomy › Nuclear and High Energy Physics › Astrophysics and Cosmic Phenomena
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysical Phenomena and Observations
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Keywords
- Fermi bubbles, North Polar Spur, King profile, galactic outflows, Suzaku, Swift X-ray observations
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