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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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Citations
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
RAYMOND, J. C., & Smith, B. W. (1977) · The Astrophysical Journal Supplement Series · doi:10.1086/190486 · Cited by 1,353 · cited 1×
“The plasma model we used (apec7 in XSPEC; see also, e.g., Raymond & Smith 1977; Mewe, Lemen, & van den Oord 1986; Borkowski, Sarazin, & Blondin 1994) assumes that it is in collisional ionization equilibrium, and is able to self-consistently account for both the continuum emission and the lines from…”
MethodTHE GALACTIC CENTER ENVIRONMENT
Morris, M., & Serabyn, E. (1996) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev.astro.34.1.645 · Cited by 930
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?
Koyama, K., Maeda, Y., Sonobe, T., Takeshima, T., Tanaka, Y., & Yamauchi, S. (1996) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/48.2.249 · Cited by 435 · cited 13×
“These widths are lower than those reported from ASCA data by Koyama et al. (1996) (75 ± 10 eV).”
BackgroundMethodResultInfluential
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Cited by
Sorted by citations
The Galactic Center massive black hole and nuclear star cluster
Genzel, R., Eisenhauer, F., & Gillessen, S. (2010) · Reviews of Modern Physics · doi:10.1103/revmodphys.82.3121 · Cited by 1,236
Nuclear Activity in Nearby Galaxies
Ho, L. C. (2008) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev.astro.45.051806.110546 · Cited by 1,198
“…& Wilson 2003b; Pellegrini 2005; Rinn, Sambruna & Gliozzi 2005; Cappi et al. 2006; González-Mart́ın et al. 2006; Soria et al. 2006), including our own (Muno et al. 2004) and our close neighbor M31 (Garcia et al. 2005), but quantitative, statistical properties of the gas are now becoming available.”
BackgroundGIANT GAMMA-RAY BUBBLES FROM FERMI-LAT: ACTIVE GALACTIC NUCLEUS ACTIVITY OR BIPOLAR GALACTIC WIND?
Su, M., Slatyer, T., & Finkbeiner, D. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/724/2/1044 · Cited by 756
“Diffuse X-ray Emission— Muno et al. (2004) studied the diffuse X-ray emission within ∼ 20 pc of the GC in detail using Chandra observations.”
MethodCharge separation induced by -odd bubbles in QCD matter
Kharzeev, D. E., & ZHITNITSKY, A. R. (2007) · Nuclear Physics A · doi:10.1016/j.nuclphysa.2007.10.001 · Cited by 519
A strong magnetic field around the supermassive black hole at the centre of the Galaxy
Eatough, R. P., Falcke, H. D., Karuppusamy, R., Lee, K., Champion, D. J., Keane, E. F., Desvignes, G., Schnitzeler, D. H. F. M., Spitler, L. G., Krämer, M., et al. (2013) · Nature · doi:10.1038/nature12499 · Cited by 468
“Further away at the 40 pc scale 28 ( 17 ′ ), the density has decreased to 0.1–0.5 cm − 3 and we can roughly describe the central parsecs with a density profile of the form n ( r ) ≃ 26 cm − 3 ( r/ 0 .”
Influential
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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