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Galaxy And Mass Assembly (GAMA): the 0.013 <z <0.1 cosmic spectral energy distribution from 0.1 μm to 1 mm

Research output: Contribution to journalArticle

  • Simon P. Driver
  • Aaron S. G. Robotham
  • Lee S. Kelvin
  • Mehmet Alpaslan
  • Ivan K. Baldry
  • Steven P. Bamford
  • Sarah Brough
  • M. L. Brown
  • Andrew M. Hopkins
  • Jochen Liske
  • Jon Loveday
  • Peder Norberg
  • John A. Peacock
  • Ellen Andrae
  • Joss Bland-Hawthorn
  • N. Bourne
  • Ewan Cameron
  • Matthew Colless
  • Christopher J. Conselice
  • Scott M. Croom
  • L. Dunne
  • Carlos S. Frenk
  • Alister W. Graham
  • M. Gunawardhana
  • David T. Hill
  • David Heath Jones
  • Konrad Kuijken
  • Barry F. Madore
  • Hannah R. Parkinson
  • Kevin A. Pimbblet
  • Steven Phillipps
  • Cristina C. Popescu
  • Matthew Prescott
  • Mark Seibert
  • Robert G. Sharp
  • Will J. Sutherland
  • Edward N. Taylor
  • Richard J. Tuffs
  • Eelco Van Kampen
  • D. B. Wijesinghe
  • S. Wilkins
We use the Galaxy And Mass Assembly survey (GAMA) I data set combined with GALEX, Sloan Digital Sky Survey (SDSS) and UKIRT Infrared Deep Sky Survey (UKIDSS) imaging to construct the low-redshift (z < 0.1) galaxy luminosity functions in FUV, NUV, ugriz and YJHK bands from within a single well-constrained volume of 3.4 × 105 (Mpc h−1)3. The derived luminosity distributions are normalized to the SDSS data release 7 (DR7) main survey to reduce the estimated cosmic variance to the 5 per cent level. The data are used to construct the cosmic spectral energy distribution (CSED) from 0.1 to 2.1 μm free from any wavelength-dependent cosmic variance for both the elliptical and non-elliptical populations. The two populations exhibit dramatically different CSEDs as expected for a predominantly old and young population, respectively. Using the Driver et al. prescription for the azimuthally averaged photon escape fraction, the non-ellipticals are corrected for the impact of dust attenuation and the combined CSED constructed. The final results show that the Universe is currently generating (1.8 ± 0.3) × 1035 h W Mpc−3 of which (1.2 ± 0.1) × 1035 h W Mpc−3 is directly released into the inter-galactic medium and (0.6 ± 0.1) × 1035 h W Mpc−3 is reprocessed and reradiated by dust in the far-IR. Using the GAMA data and our dust model we predict the mid- and far-IR emission which agrees remarkably well with available data. We therefore provide a robust description of the pre- and post-dust attenuated energy output of the nearby Universe from 0.1 μm to 0.6 mm. The largest uncertainty in this measurement lies in the mid- and far-IR bands stemming from the dust attenuation correction and its currently poorly constrained dependence on environment, stellar mass and morphology.
Original languageEnglish
Pages (from-to)3244-3264
JournalMonthly Notices of the Royal Astronomical Society
Volume427
Issue number4
DOIs
Publication statusPublished - 2012

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