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
MetadataShow full item record
Showing items related by title, author, creator and subject.
The H alpha galaxy survey. I. The galaxy sample, H alpha narrow-band observations and star formation parameters for 334 galaxies James, P.A.; Shane, N.S.; Beckman, J.E.; Cardwell, A.; Collins, C.A.; Etherton, J.; de Jong, R.S.; Fathi, K.; Knapen, J.; Peletier, R.F.; Percival, S.M.; Pollacco, D.L.; Seigar, M.S.; Stedman, S. (2004)We discuss the selection and observations of a large sample of nearby galaxies, which we are using to quantify the star formation activity in the local Universe. The sample consists of 334 galaxies across all Hubble types ...
Metallicity distributions of elliptical galaxies and globular cluster systems - Absorption line strength gradients in elliptical galaxies Arimoto, N; Kobayashi, Chiaki (1999)Gradients of absorption line indices are studied and mean stellar metallicities are estimated for 46 elliptical galaxies. The mean stellar metallicities range from [[Fe/H]] similar or equal to -0.8 to +0.2 and ellipticals ...
On the Key Processes that Drive Galaxy Evolution: the Role of Galaxy Mergers, Accretion, Local Environment and Feedback in Shaping the Present-Day Universe Martin, Garreth (2019-07-17)The study of galaxy evolution is a fundamental discipline in modern astrophysics, dealing with how and why galaxies of all types evolve over time. The diversity of present-day galaxies is a reflection of the processes ...