Cited by 116Astrophysical Phenomena and ObservationsAstrophysics and Cosmic PhenomenaGalaxies: Formation, Evolution, Phenomena

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AN XMM-NEWTON SURVEY OF THE SOFT X-RAY BACKGROUND. III. THE GALACTIC HALO X-RAY EMISSION

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Henley, David B., Shelton, Robin L.·2013·The Astrophysical Journal

DOI 10.1088/0004-637x/773/2/92

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Abstract

We present measurements of the Galactic halo's X-ray emission for 110 XMM-Newton sight lines selected to minimize contamination from solar wind charge exchange emission. We detect emission from few million degree gas on ∼4/5 of our sight lines. The temperature is fairly uniform (median = 2.22 × 10 6 K, interquartile range = 0.63 × 10 6 K), while the emission measure and intrinsic 0.5–2.0 keV surface brightness vary by over an order of magnitude (∼(0.4–7) × 10 −3 cm −6 pc and ∼(0.5–7) × 10 −12 erg cm −2 s −1 deg −2 , respectively, with median detections of 1.9 × 10 −3 cm −6 pc and 1.5 × 10 −12 erg cm −2 s −1 deg −2 , respectively). The high-latitude sky contains a patchy distribution of few million degree gas. This gas exhibits a general increase in emission measure toward the inner Galaxy in the southern Galactic hemisphere. However, there is no tendency for our observed emission measures to decrease with increasing Galactic latitude, contrary to what is expected for a disk-like halo morphology. The measured temperatures, brightnesses, and spatial distributions of the gas can be used to place constraints on models for the dominant heating sources of the halo. We provide some discussion of such heating sources, but defer comparisons between the observations and detailed models to a later paper.

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CONTRIBUTION OF UNRESOLVED POINT SOURCES TO THE DIFFUSE X-RAY BACKGROUND BELOW 1 keV
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A Nearby Repeating Fast Radio Burst in the Direction of M81
Bhardwaj, M., Gaensler, B. M., Kaspi, V. M., Landecker, T. L., Mckinven, R., Michilli, D., Pleunis, Z., Tendulkar, S. P., Andersen, B. C., Boyle, P. J., et al. (2021) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/abeaa6 · Cited by 247
Cooler and smoother – the impact of cosmic rays on the phase structure of galactic outflows
Girichidis, P., Naab, T., Hanasz, M., & Walch, S. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty1653 · Cited by 152
The Extended Distribution of Baryons around Galaxies
Bregman, J. N., Anderson, M. E., Miller, M. J., Hodges-Kluck, E., Dai, X., Li, J.-T., Li, Y., & Qu, Z. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aacafe · Cited by 157
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Donahue, M. E., & Voit, G. M. (2022) · Physics Reports · doi:10.1016/j.physrep.2022.04.005 · Cited by 140

See all 116

Authors: Henley, D. B., & Shelton, R. L.
Affiliations: University of Georgia (US)
ORCID: Henley, David B.
Shelton, Robin L.
Venue: The Astrophysical Journal
Publisher: American Astronomical Society
Published: 2013-07-29
Volume: 773
Issue: 2
Pages: 92
ISSN: 0004-637X (ISSN-L)
1538-4357
DOI: 10.1088/0004-637x/773/2/92
OpenAlex: W2027993584
Cited by: 116
References: 95
Citations by year: 2026: 6 · 2025: 13 · 2024: 6 · 2023: 8 · 2022: 8 · 2021: 11 · 2020: 8 · 2019: 9 · 2018: 11 · 2017: 7 · 2016: 10 · 2015: 13 · 2014: 5 · 2013: 1
FWCI: 5.21
Type: journal article
Language: en
Open access: bronze
doi.org
Licence: iopscience.iop.org/info/page/text-and-data-mining (tdm)
iopscience.iop.org/page/copyright (vor)
Locations: The Astrophysical Journal (publishedVersion)
arXiv (Cornell University) (submittedVersion)
arXiv (Cornell University)
Topics: Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysical Phenomena and Observations
Physical Sciences › Physics and Astronomy › Nuclear and High Energy Physics › Astrophysics and Cosmic Phenomena
Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
Keywords: Galactic halo, X-ray emission, soft X-ray background, hot gas, emission measure, surface brightness, Galactic latitude distribution, XMM-Newton survey, solar wind charge exchange

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AN XMM-NEWTON SURVEY OF THE SOFT X-RAY BACKGROUND. III. THE GALACTIC HALO X-RAY EMISSION

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