We use the energy-balance code MAGPHYS to determine stellar and dust masses , and dust corrected star-formation rates for over 200,000 GAMA galaxies , 170,000 G10-COSMOS galaxies and 200,000 3D-HST galaxies .
Our values agree well with previously reported measurements and constitute a representative and homogeneous dataset spanning a broad range in stellar mass ( 10 ^ { 8 } — 10 ^ { 12 } M _ { \odot } ) , dust mass ( 10 ^ { 6 } — 10 ^ { 9 } M _ { \odot } ) , and star-formation rates ( 0.01 — 100 M _ { \odot } yr ^ { -1 } ) , and over a broad redshift range ( 0.0 < z < 5.0 ) .
We combine these data to measure the cosmic star-formation history ( CSFH ) , the stellar-mass density ( SMD ) , and the dust-mass density ( DMD ) over a 12 Gyr timeline .
The data mostly agree with previous estimates , where they exist , and provide a quasi-homogeneous dataset using consistent mass and star-formation estimators with consistent underlying assumptions over the full time range .
As a consequence our formal errors are significantly reduced when compared to the historic literature .
Integrating our cosmic star-formation history we precisely reproduce the stellar-mass density with an ISM replenishment factor of 0.50 \pm 0.07 , consistent with our choice of Chabrier IMF plus some modest amount of stripped stellar mass .
Exploring the cosmic dust density evolution , we find a gradual increase in dust density with lookback time .
We build a simple phenomenological model from the CSFH to account for the dust mass evolution , and infer two key conclusions : ( 1 ) For every unit of stellar mass which is formed 0.0065 — 0.004 units of dust mass is also formed ; ( 2 ) Over the history of the Universe approximately 90 to 95 per cent of all dust formed has been destroyed and/or ejected .