Galaxy and Mass Assembly (GAMA): galaxies at the faint end of the Hα luminosity function

Sarah Brough, Andrew M. Hopkins, Robert G. Sharp, M. L. P. Gunawardhana, D. B. Wijesinghe, Aaron S. G. Robotham, Simon P. Driver, Ivan K. Baldry, Steven P. Bamford, Jochen Liske, Jon Loveday, Peder Norberg, John A. Peacock, Joss Bland-Hawthorn, Michael J. I. Brown, Ewan Cameron, Scott M. Croom, Carlos S. Frenk, C. Foster, David T. HillDavid Heath Jones, Lee S. Kelvin, Konrad Kuijken, Robert C. Nichol, Hannah R. Parkinson, Kevin A. Pimbblet, Cristina C. Popescu, Matthew Prescott, Will J. Sutherland, Edward N. Taylor, Daniel Thomas, Richard J. Tuffs, Eelco Van Kampen

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We present an analysis of the properties of the lowest Hα-luminosity galaxies (LHα ≤ 4 × 1032 W; SFR < 0.02 Mʘ yr−1, with SFR denoting the star formation rate) in the Galaxy And Mass Assembly survey. These galaxies make up the rise above a Schechter function in the number density of systems seen at the faint end of the Hα luminosity function. Above our flux limit, we find that these galaxies are principally composed of intrinsically low stellar mass systems (median stellar mass = 2.5 × 108Mʘ) with only 5/90 having stellar masses
M > 1010Mʘ. The low-SFR systems are found to exist predominantly in the lowest-density environments (median density ∼0.02 galaxy Mpc−2) with none in environments more dense than ∼1.5 galaxy Mpc−2. Their current specific SFRs (SSFRs; −8.5 < log [SSFR (yr −1)] < −12) are consistent with their having had a variety of star formation histories. The low-density environments of these galaxies demonstrate that such low-mass, star-forming systems can only remain as low mass and form stars if they reside sufficiently far from other galaxies to avoid being accreted, dispersed through tidal effects or having their gas reservoirs rendered ineffective through external processes.

Original languageEnglish
Pages (from-to)1236-1243
JournalMonthly Notices of the Royal Astronomical Society
Issue number2
Publication statusPublished - 11 May 2011


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