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Galaxy and Mass Assembly (GAMA): the star formation rate dependence of the stellar initial mass function

Research output: Contribution to journalArticle

  • M. L. P. Gunawardhana
  • Andrew M. Hopkins
  • Robert G. Sharp
  • Sarah Brough
  • Edward N. Taylor
  • Joss Bland-Hawthorn
  • Richard J. Tuffs
  • Cristina C. Popescu
  • D. B. Wijesinghe
  • David Heath Jones
  • Scott M. Croom
  • E. M. Sadler
  • S. Wilkins
  • Simon P. Driver
  • Jochen Liske
  • Peder Norberg
  • Ivan K. Baldry
  • Steven P. Bamford
  • Jon Loveday
  • John A. Peacock
  • Aaron S. G. Robotham
  • D. B. Zucker
  • Q. A. Parker
  • Christopher J. Conselice
  • Ewan Cameron
  • Carlos S. Frenk
  • David T. Hill
  • Lee S. Kelvin
  • Konrad Kuijken
  • B. F. Madore
  • Hannah R. Parkinson
  • Kevin A. Pimbblet
  • Matthew Prescott
  • Will J. Sutherland
  • Eelco Van Kampen
The stellar initial mass function (IMF) describes the distribution in stellar masses produced from a burst of star formation. For more than 50 yr, the implicit assumption underpinning most areas of research involving the IMF has been that it is universal, regardless of time and environment. We measure the high-mass IMF slope for a sample of low-to-moderate redshift galaxies from the Galaxy and Mass Assembly survey. The large range in luminosities and galaxy masses of the sample permits the exploration of underlying IMF dependencies. A strong IMF–star formation rate dependency is discovered, which shows that highly star-forming galaxies form proportionally more massive stars (they have IMFs with flatter power-law slopes) than galaxies with low star formation rates. This has a significant impact on a wide variety of galaxy evolution studies, all of which rely on assumptions about the slope of the IMF. Our result is supported by, and provides an explanation for, the results of numerous recent explorations suggesting a variation of or evolution in the IMF.
Original languageEnglish
Pages (from-to)1647-1662
JournalMonthly Notices of the Royal Astronomical Society
Volume415
Issue number2
DOIs
Publication statusPublished - 1 Aug 2011

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