Charge Exchange X-ray Emission of M82: Kα triplets of O VII, Ne IX, and Mg XI

Details Charge Exchange X-ray Emission of M82: Kα triplets of O VII, Ne IX, and Mg XI Charge Exchange X-ray Emission of M82: Kα triplets of O VII, Ne IX, and Mg XI

2011-05-18

arxiv.org/abs/1105.3539v2

Astronomy and Astrophysics

Astrophysics

Galaxy Astrophysics

5 pages, 5 figs, to appear on MNRAS Letter

Scientific paper

Starburst galaxies are primary feedback sources of mechanical energy and metals, which are generally measured from associated X-ray emission lines assuming that they are from the thermal emission of the outflowing hot gas. Such line emission, however, can also arise from the charge exchange X-ray emission (CXE) between highly ionized ions and neutral species. To understand the feedback of energy and metals, it is crucial to determine the origin of the X-ray emission lines and to distinguish the contributions from the CXE and the thermal emission. The origin of the lines can be diagnosed by the K{\alpha} triplets of He-like ions, because the CXE favors the inter-combination and forbidden lines, while the thermal emission favors the resonance line. We analyze the triplets of O VII, Ne IX, and Mg XI observed in the XMM- Newton reflection grating spectra of the starburst galaxy M82. The flux contribution of the CXE is 90%, 50%, and 30% to the O VII, Ne IX, and Mg XI triplet, respectively. Averaged over all the three triplets, the contribution of the CXE is \sim 50% of the total observed triplet flux. To correctly understand the hot outflow of starburst galaxies, it is necessary to include the CXE. Based on the measured CXE contributions to the O VII, Ne IX, and Mg XI triplets, we estimate the relative abundances of O, Ne, and Mg of the outflow and find they are similar to the solar ratios.

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