Gamma-Rays and the Far-Infrared-Radio Continuum Correlation Reveal a Powerful 
Galactic Centre Wind

Crocker, Roland; Jones, David I.; Aharonian, Felix; Law, Casey J.; Melia, Fulvio; Ott, Juergen

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Gamma-Rays and the Far-Infrared-Radio Continuum Correlation Reveal a Powerful Galactic Centre Wind

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Crocker, Roland
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

Jones, David I.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

Aharonian, Felix
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;
Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland;

External Resource

http://onlinelibrary.wiley.com/doi/10.1111/j.1745-3933.2010.00983.x/abstract
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フルテキスト (公開)

1009.4340
(プレプリント), 584KB

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引用

Crocker, R., Jones, D. I., Aharonian, F., Law, C. J., Melia, F., & Ott, J. (2011). Gamma-Rays and the Far-Infrared-Radio Continuum Correlation Reveal a Powerful Galactic Centre Wind. Monthly Notices of the Royal Astronomical Society: Letters, 411(1), L11-L15. Retrieved from http://arxiv.org/abs/1009.4340.

引用: https://hdl.handle.net/11858/00-001M-0000-0012-3398-D

要旨

We consider the thermal and non-thermal emission from the inner 200 pc of the Galaxy. The radiation from this almost star-burst-like region is ultimately driven dominantly by on-going massive star formation. We show that this region's radio continuum (RC) emission is in relative deficit with respect to the expectation afforded by the Far- infrared-Radio Continuum Correlation (FRC). Likewise we show that the region's gamma-ray emission falls short of that expected given its star formation and resultant supernova rates. These facts are compellingly explained by positing that a powerful (400-1200 km/s) wind is launched from the region. This wind probably plays a number of important roles including advecting positrons into the Galactic bulge thus explaining the observed ~kpc extension of the 511 keV positron annihilation signal around the GC. We also show that the large-scale GC magnetic field falls in the range ~100-300 microG and that - in the time they remain in the region - GC cosmic rays do not penetrate into the region's densest molecular material.