THE ROTATION OF THE HOT GAS AROUND THE MILKY WAY
Open accessAbstract
The hot gaseous halos of galaxies likely contain a large amount of mass and are an integral part of galaxy formation and evolution. The Milky Way has a K halo that is detected in emission and by absorption in the O vii resonance line against bright background active galactic nuclei (AGNs), and for which the best current model is an extended spherical distribution. Using XMM-Newton Reflection Grating Spectrometer data, we measure the Doppler shifts of the O vii absorption-line centroids toward an ensemble of AGNs. These Doppler shifts constrain the dynamics of the hot halo, ruling out a stationary halo at about and a co-rotating halo at , and leading to a best-fit rotational velocity of km s−1 for an extended halo model. These results suggest that the hot gas rotates and that it contains an amount of angular momentum comparable to that in the stellar disk. We examined the possibility of a model with a kinematically distinct disk and spherical halo. To be consistent with the emission-line X-ray data, the disk must contribute less than 10% of the column density, implying that the Doppler shifts probe motion in the extended hot halo.
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The Milky Way circumgalactic medium is not stationary but is rotating with a speed of approximately 180 ± 40 km/s, very close to co-rotation with the stellar disk.
“The O vii absorption lines in the MW also revealed that the CGM is not stationary but is rotating with a speed of ≈ 180 ± 40 km s -1”
From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Hodges-Kluck et al. 2016
The Abstract reports O VII Doppler shifts consistent with a best-fit halo rotation speed of 183 ± 41 km/s and rules out a stationary halo. However, the Results say a co-rotating halo is marginally rejected at 95% probability and describe the halo as lagging the disk. Thus the added claim that its speed is very close to co-rotation is not supported. (LLM, conf=0.88)
Experimental — accuracy not yet measuredThe shock will be a bit faster along the Galactic axis than in the horizontal direction because of the slightly disk-like nature of the Milky Way circumgalactic medium in the inner about 10 kpc.
“In practice, the shock will be a bit faster along the Galactic axis than the horizontal direction because of the slightly disk-like nature of the Milky-Way CGM in the inner ∼ 10 kpc owing to the gravity of the stellar disk and the CGM rotation (Hodges-Kluck et al. 2016).”
From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Hodges-Kluck et al. 2016
Section 5.3 (page unavailable) reports rotation of the Milky Way’s hot halo, supporting the CGM-rotation part of the attribution. But the paper favors an extended, roughly spherical halo over a disk model; it does not establish a slightly disk-like CGM within ∼10 kpc or predict that a shock travels faster along the Galactic axis because of stellar-disk gravity and rotation. (LLM, conf=0.83)
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References 68 · Cited by 82
Research works printed but not linked: 6
- Faerman, Y., Sternberg, A., & McKee, C. F. 2016, arXiv:1602.00689 · arXiv
- Kuntz, K. D. 2009, in AIP Conf. Ser. 1156, THE LOCAL BUBBLE AND BEYOND II, ed. R. K. Smith, S. L. Snowden, & K. D. Kuntz (Melville, NY: AIP), 3
- Miller, M. J., Hodges-Kluck, E. J., & Bregman, J. N. 2016, arXiv:1601.06797 · arXiv
- Rasmussen, A., Kahn, S. M., & Paerels, F. 2003, Astrophysics and Space Science Library, ed. J. L. Rosenberg, & M. E. Putman, Vol. 281, 109
- Salem, M., Besla, G., Bryan, G., et al. 2015, arXiv:1507.07935 · arXiv
- Smith, R. K., Ackermann, M., Allured, R., et al. 2014, Proc. SPIE, 9144, 4
- Authors
- Hodges-Kluck, E. J., Miller, M. J., & Bregman, J. N.
- Affiliations
- University of Michigan (US)
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 2016-04-27
- Volume
- 822
- Issue
- 1
- Pages
- 21
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W2310387726
- Cited by
- 82
- References
- 68
- Citations by year
- 2026: 4 · 2025: 5 · 2024: 6 · 2023: 6 · 2022: 11 · 2021: 11 · 2020: 13 · 2019: 5 · 2018: 7 · 2017: 11 · 2016: 3
- FWCI
- 4.14
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Licence
- Locations
- The Astrophysical Journal (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- arXiv (Cornell University)
- Funders
- National Aeronautics and Space Administration (NNX11AG55G)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysical Phenomena and Observations
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Keywords
- Doppler shift, active galactic nuclei, angular momentum, halo kinematics, X-ray absorption
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