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MEGAFLOW V: The dust/metallicity anisotropy of the CGM

Observations indicate that the CGM along the minor axis is on average more enriched than the gas located along the major axis of galaxies - consistent with outflow and accretion models

Published onMar 21, 2022
MEGAFLOW V: The dust/metallicity anisotropy of the CGM
Dust/metallicity-anisoptropy of the CGM - Martin Wendt

This video explains how Wendt et al. (2021) [1] used background quasars as a probe of the Circum-Galactic Medium (CGM) to find evidence for an anisotropic dust distribution around star-forming galaxies at 0.4 < z < 1.4. The CGM dust content is obtained from either [Zn/Fe] or from the dust depletion pattern of other elements (e.g., the MnII, CrII, ZnII, model of DeCia et al. 2016 [2] ). Given that our [Zn/Fe] is a good proxy for metallicity, these results indicate that the CGM along the minor axis is on average more enriched than the gas located along the major axis of galaxies - consistent with outflow and accretion models. Our findings are in encouraging agreement with recent results from recent hydrodynamical simulations of the CGM.

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