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Diffuse X‐Ray Emission in a Deep Chandra Image of the Galactic Center
Open accessAbstract
We examine the spectrum of diffuse emission detected in the 17' × 17' field around Sgr A* during 625 ks of Chandra observations. The spectrum exhibits He-like and H-like lines from Si, S, Ar, Ca, and Fe that are consistent with an origin in a two-temperature plasma, as well as a prominent low-ionization Fe Kα line. The cooler, kT ≈ 0.8 keV plasma differs in surface brightness across the image in the range (0.2-1.8) × 10 -13 ergs cm -2 s -1 arcmin -2 (observed, 2-8 keV). This soft plasma is probably heated by supernovae, along with a small contribution from the winds of massive Wolf-Rayet (W-R) and O stars. The radiative cooling rate of the soft plasma within the inner 20 pc of the Galaxy could be balanced by 1% of the kinetic energy of one supernova every 3 × 10 5 yr. The hotter, kT ≈ 8 keV component is more spatially uniform, with a surface brightness of (1.5-2.6) × 10 -13 ergs cm -2 s -1 arcmin -2 (observed, 2-8 keV). The intensity of the hard plasma is correlated with that of the soft, but they are probably only indirectly related, because neither supernova remnants nor W-R/O stars are observed to produce thermal plasma hotter than kT ≈ 3 keV. Moreover, a kT ≈ 8 keV plasma would be too hot to be bound to the Galactic center and therefore would form a slow wind or fountain of plasma. The energy required to sustain such a freely expanding plasma within the inner 20 pc of the Galaxy is ~10 40 ergs s -1 . This corresponds to the entire kinetic energy of one supernova every 3000 yr, which is unreasonably high. However, alternative explanations for the kT ≈ 8 keV diffuse emission are equally unsatisfying. The hard X-rays are unlikely to result from undetected point sources, because no known population of stellar objects is numerous enough to account for the observed surface brightness. Neither is there evidence that nonthermal mechanisms for producing the hard emission are operating, as the expected shifts in the line energies and ratios from their collisional-equilibrium values are not observed. We are left to conclude either that there is a significant shortcoming in our understanding of the mechanisms that heat the interstellar medium or that a population of faint (<10 31 ergs s -1 ) hard X-ray sources that is a factor of 10 more numerous than cataclysmic variables remains to be discovered.
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“The x-ray emitting hot gas is found to have a density of 2 cm -3 and a temperature of 0 . 7 -1 keV.”
From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Muno et al. 2004
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“Therefore, the pressure and the total energy are ∼ 2 × 10 7 K cm -3 and E 15pc ∼ 6 × 10 50 erg, respectively (Muno et al. 2004; Ponti et al. 2019).”
From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Muno et al. 2004
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Cites
Warner, B. D. (1995) · Cambridge University Press eBooks · doi:10.1017/cbo9780511586491 · Cited by 2,532
Soft X-ray spectrum of a hot plasma
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MethodTHE GALACTIC CENTER ENVIRONMENT
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Self-citationSchlickeiser, R. (2002) · Astronomy and astrophysics library · doi:10.1007/978-3-662-04814-6 · Cited by 905
Chandra X‐Ray Spectroscopic Imaging of Sagittarius A* and the Central Parsec of the Galaxy
Baganoff, F. K., Maeda, Y., Morris, M., Bautz, M. W., Brandt, W. N., Cui, W., Doty, J. P., Feigelson, E. D., Garmire, G. P., Pravdo, S. H., et al. (2003) · The Astrophysical Journal · doi:10.1086/375145 · Cited by 809 · cited 1×
“It is likely that these represent an outflow from the central parsec (Baganoff et al. 2003; Morris et al. 2003).”
BackgroundSelf-citationWind from a starburst galaxy nucleus
Chevalier, R. A., & Clegg, A. W. (1985) · Nature · doi:10.1038/317044a0 · Cited by 770 · cited 1×
“Although computing the energy loss rate rigorously would require a full solution of wind equations such as those in Chevalier & Clegg (1985), we can make a rough estimate of it by assuming Ẇexp = PdV/dt ≈ PV 2/3cs.”
MethodAn Overview of the Performance and Scientific Results from theChandra X‐Ray Observatory
Weisskopf, M. C., Brinkman, B., CANIZARES, C. R., GARMIRE, G. P., Murray, S. S., & Speybroeck, L. P. V. (2002) · Publications of the Astronomical Society of the Pacific · doi:10.1086/338108 · Cited by 753 · cited 1×
“The inner 20 pc of the Galaxy have been observed on twelve occasions as of June 2002 (Table 1) using the Advanced CCD Imaging Spectrometer imaging array (ACISI) aboard the Chandra X-ray Observatory (Weisskopf et al. 2002).”
MethodSelf-citationSchlickeiser, R. (2004) · CRC Press eBooks · doi:10.1201/9780367801618-22 · Cited by 582
Launhardt, R., Zylka, R., & Mezger, P. G. (2002) · Astronomy & Astrophysics · doi:10.1051/0004-6361:20020017 · Cited by 477
ASCA View of Our Galactic Center: Remains of Past Activities in X-Rays?
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“These widths are lower than those reported from ASCA data by Koyama et al. (1996) (75 ± 10 eV).”
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3 of the 85 references couldn’t be matched to a known paper.
Research works printed but not linked: 11
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Cited by
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Items 201–220 of 220
Spectrum composition of galactic center X-ray emission with point and diffuse X-ray sources
Nobukawa, M., & Koyama, K. (2021) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psab076 · Cited by 1
News from the year 2006 Galactic Centre workshop
Morris, M., & Nayakshin, S. (2006) · Journal of Physics Conference Series · doi:10.1088/1742-6596/54/1/072 · Cited by 1
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ResultSelf-citationChandra Observations of the Galactic Center: High Energy Processes at Arcsecond Resolution
Wang, Q. D. (2006) · Journal of Physics Conference Series · doi:10.1088/1742-6596/54/1/020 · Cited by 1
“A fraction of these sources have very hard X-ray spectra (e.g., with power law photon indices less than 0; Muno et al. 2004a).”
BackgroundViscous Dissipation in the Galactic Center Region
Bélmont, R., & Tagger, M. (2006) · Journal of Physics Conference Series · doi:10.1088/1742-6596/54/1/024
A Quark Matter Contribution to the Cosmic Ray Spectrum
Lawson, K. (2013) · EPJ Web of Conferences · doi:10.1051/epjconf/20125204008
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Chan, M. H., & Chu, M. C. (2010) · Astrophysics and Space Science · doi:10.1007/s10509-010-0507-7
Cosmic-Ray Production and X-Ray and Gamma-Ray Emission from the Galactic Center
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BackgroundInfluentialHigh Energy Emission from the Galactic Center
Goldwurm, A. (2006) · Journal of Physics Conference Series · doi:10.1088/1742-6596/54/1/016
Unveiling Accreting White Dwarf Binariesin Hard X-Ray Surveys
de Martino, D. (2016) · Astrophysics and space science proceedings · doi:10.1007/978-3-319-19330-4_40
Review of the Galactic X-ray Background Emission and White Dwarf Binaries
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High-energy emission from the Galactic Center
Goldwurm, A., Clavel, M., Stefano Gabici, A., & Terrier, R. (2025) · Reviews of Modern Physics · doi:10.1103/9nww-fclb · Cited by 2
Ferrario, L., de Martino, D., & Gänsicke, B. T. (2016) · Space sciences series of ISSI · doi:10.1007/978-1-4939-3550-5_5
A Quark Matter Contribution to the Cosmic Ray Spectrum
Lawson, K. (2013) · EPJ Web of Conferences · doi:10.1051/epjconf/20135204008
Diffuse Hot Plasma in the Interstellar Medium and Galactic Outflows
Sasaki, M., Ponti, G., & Mackey, J. (2022) · Springer eBooks · doi:10.1007/978-981-16-4544-0_91-1
Niu, S., Xie, F., Sun, W., & Ji, L. (2023) · Research in Astronomy and Astrophysics · doi:10.1088/1674-4527/acd89f
Diffuse Hot Plasma in the Interstellar Medium and Galactic Outflows
Sasaki, M., Ponti, G., & Mackey, J. (2024) · Springer eBooks · doi:10.1007/978-981-19-6960-7_91
Lecian, O. M. (2025) · Journal of AppliedMath · doi:10.59400/jam2741
Metadata
- Authors
- Muno, M. P., Baganoff, F. K., Bautz, M. W., Feigelson, E. D., Garmire, G. P., Morris, M. R., Park, S., Ricker, G. R., & Townsley, L. K.
- Affiliations
- University of California, Los Angeles (US)
- Massachusetts Institute of Technology (US)
- Pennsylvania State University (US)
- ORCID
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 2004-09-20
- Volume
- 613
- Issue
- 1
- Pages
- 326-342
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W1984008682
- Cited by
- 221
- References
- 85
- Citations by year
- 2026: 2 · 2025: 5 · 2024: 6 · 2023: 5 · 2022: 3 · 2021: 3 · 2020: 6 · 2019: 5 · 2018: 2 · 2017: 8 · 2016: 11 · 2015: 17 · 2014: 7 · 2013: 17 · 2012: 9
- FWCI
- 11.21
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- The Astrophysical Journal (publishedVersion)
- arXiv (Cornell University) (acceptedVersion)
- CERN Document Server (European Organization for Nuclear Research) (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 › Astrophysics and Star Formation Studies
- Keywords
- diffuse X-ray emission, Galactic Center, Sgr A*, two-temperature plasma, Fe Kα line, supernova heating, radiative cooling, hard X-ray emission, supernova remnants, stellar winds, X-ray spectra, Chandra X-ray Observatory, surface brightness
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