Swinburne
Browse

Galaxy And Mass Assembly (GAMA): The galaxy stellar mass function to z = 0.1 from the r-band selected equatorial regions

Download (9.59 MB)
journal contribution
posted on 2024-08-06, 11:02 authored by A. H. Wright, A. S.G. Robotham, S. P. Driver, M. Alpaslan, S. K. Andrews, I. K. Baldry, J. Bland-Hawthorn, S. Brough, M. J.I. Brown, M. Colless, Elisabete Lima Da Cunha, L. J.M. Davies, Alister GrahamAlister Graham, B. W. Holwerda, A. M. Hopkins, P. R. Kafle, L. S. Kelvin, J. Loveday, S. J. Maddox, M. J. Meyer, A. J. Moffett, P. Norberg, S. Phillipps, K. Rowlands, Edward TaylorEdward Taylor, L. Wang, S. M. Wilkins
We derive the low-redshift galaxy stellar mass function (GSMF), inclusive of dust corrections, for the equatorial Galaxy And Mass Assembly (GAMA) data set covering 180 deg 2 . We construct the mass function using a density-corrected maximum volume method, using masses corrected for the impact of optically thick and thin dust. We explore the galactic bivariate brightness plane (M * -μ), demonstrating that surface brightness effects do not systematically bias our mass function measurement above 10 7.5 M ⊙ . The galaxy distribution in the M-μ plane appears well bounded, indicating that no substantial population of massive but diffuse or highly compact galaxies are systematically missed due to the GAMA selection criteria. The GSMF is fitted with a double Schechter function, with M* = 10 10.78±0.01±0.20 M ⊙ , φ 1 * = (2.93 ± 0.40) × 10 -3 h 70 3 Mpc -3 , α1 =-0.62 ± 0.03 ± 0.15, φ 2 * = (0.63 ± 0.10) × 10 -3 h 70 3 Mpc -3 and α2 =-1.50 ± 0.01 ± 0.15. We find the equivalent faint end slope as previously estimated using the GAMA-I sample, although we find a higher value of M*. Using the full GAMA-II sample, we are able to fit the mass function to masses as low as 10 7.5 M ⊙ , and assess limits to 10 6.5 M ⊙ . Combining GAMA-II with data from G10-COSMOS, we are able to comment qualitatively on the shape of the GSMF down to masses as low as 10 6 M ⊙ . Beyond the well-known upturn seen in the GSMF at 10 9.5 , the distribution appears to maintain a single power-law slope from 10 9 to 10 6.5 . We calculate the stellar mass density parameter given our best-estimate GSMF, finding Ω * = 1.66 -0.23 +0.24 ± 0.97 h 70 -1 × 10 -3 , inclusive of random and systematic uncertainties.

Funding

Science and Technology Facilities Council

European Research Council

Alexander Graham Bell Association for the Deaf and Hard of Hearing

History

Available versions

PDF (Published version)

ISSN

1365-2966

Journal title

Monthly Notices of the Royal Astronomical Society

Volume

470

Issue

1

Pagination

19 pp

Publisher

Oxford University Press

Copyright statement

This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

Language

eng

Usage metrics

    Publications

    Categories

    No categories selected

    Keywords

    Exports

    RefWorks
    BibTeX
    Ref. manager
    Endnote
    DataCite
    NLM
    DC