GAMA/H-ATLAS: The Local Dust Mass Function and Cosmic Density as a Function of Galaxy Type - A Benchmark for Models of Galaxy Evolution
Beeston, R. A.
Wright, A. H.
Gomez, H. L.
Driver, S. P.
Clark, C. J. R.
Takeuchi, T. T.
Bremer, M. N.
Moffett, A. J.
Vis, P. De
Eales, S. A.
Holwerda, B. W.
Smith, M. W. L.
Smith, D. J. B.
We present the dust mass function (DMF) of 15 750 galaxies with redshift z <0.1, drawn from the overlapping area of the GAMA and H-ATLAS surveys. The DMF is derived using the density corrected V max method, wherewe estimate V max using: (i) the normal photometric selection limit (pV max) and (ii) a bivariate brightness distribution (BBD) technique, which accounts for two selection effects.We fit the datawith a Schechter function, and find M * = (4.65 ± 0.18) × 10 7 h 2 70M ⊙, a = (-1.22 ± 0.01), ϕ * = (6.26 ± 0.28) × 10 -3 h 3 70 Mpc -3 dex -1. The resulting dust mass density parameter integrated down to 10 4 M ⊙ is ω d = (1.11 ± 0.02) × 10 -6 which implies the mass fraction of baryons in dust is f mb = (2.40 ± 0.04) × 10 -5; cosmic variance adds an extra 7-17 per cent uncertainty to the quoted statistical errors. Ourmeasurements have fewer galaxies with high dust mass than predicted by semi-analytic models. This is because the models include too much dust in high stellar mass galaxies. Conversely, our measurements find more galaxies with high dust mass than predicted by hydrodynamical cosmological simulations. This is likely to be from the long time-scales for grain growth assumed in the models. We calculate DMFs split by galaxy type and find dust mass densities of ω d = (0.88 ± 0.03) × 10 -6 and ω d = (0.060 ± 0.005) × 10 -6 for late types and early types, respectively. Comparing to the equivalent galaxy stellar mass functions (GSMF) we find that the DMF for late types is well matched by the GSMF scaled by (8.07 ± 0.35) × 10 -4.
Published inMonthly Notices of the Royal Astronomical Society
RelationsSchool of Physics, Astronomy and Mathematics
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