Speaker
Description
Over the last decade, the IR Herschel satellite has allowed to trace the
dust budget up to z ∼4, and the recent ALMA facility
is extending the measurement of the dust production to even early times.
This has rendered particularly urgent the issue of explaining how
the dust mass in galaxies is related to other key galaxy-integrated quantities, i.e. stellar mass andstar-formation rate.
In the present work, I will focus, in detail, on the dust-to-stellar mass
(DTS) ratio, as this quantity represents a true measure of how much dust
per unit stellar mass survives the various destruction processes,
i.e. astration and interstellar shocks.
The observed values of the DTS from z~0 up to z~6 will be compared to
theoretical estimates computed by means of state-of-the art chemical
evolution models for galaxies of different morphological type, showing
the strong dependence of this quantity on two key ingredients,
i.e. the underlying star formation history and the stellar initial
mass function.
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