Spatial structure of the WMAP-Planck haze. (arXiv:1812.05228v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Rubtsov_G/0/1/0/all/0/1">G. Rubtsov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhezher_Y/0/1/0/all/0/1">Y. Zhezher</a>
It was proposed that the two phenomena, WMAP-Planck haze and Fermi bubbles,
may have a common origin. In the present paper we analyze the spatial structure
of the haze using the Planck 2018 data release. It is found that the spatial
dimensions and locations of WMAP-Planck haze and Fermi bubbles are compatible
within the experimental uncertainties. No substructures similar to the Fermi
bubbles cocoon are identified in the Planck data. Comparison with the spatial
extent of possible synchrotron emission caused by the electron-positron pair
emitted by the Galactic center pulsar population and by the decay of dark
matter particles in the Galactic center region are performed. Both galactic
pulsars and dark matter decay remain viable explanations of the WMAP-Planck
haze.
It was proposed that the two phenomena, WMAP-Planck haze and Fermi bubbles,
may have a common origin. In the present paper we analyze the spatial structure
of the haze using the Planck 2018 data release. It is found that the spatial
dimensions and locations of WMAP-Planck haze and Fermi bubbles are compatible
within the experimental uncertainties. No substructures similar to the Fermi
bubbles cocoon are identified in the Planck data. Comparison with the spatial
extent of possible synchrotron emission caused by the electron-positron pair
emitted by the Galactic center pulsar population and by the decay of dark
matter particles in the Galactic center region are performed. Both galactic
pulsars and dark matter decay remain viable explanations of the WMAP-Planck
haze.
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