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

MPG-Autoren
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Andrae,  Ellen
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Tuffs,  Richard J.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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1209.0259.pdf
(Preprint), 3MB

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Zitation

Driver, S. P., Robotham, A. S. G., Kelvin, L., Alpaslan, M., Baldry, I. K., Bamford, S. P., et al. (2012). Galaxy And Mass Assembly (GAMA): The 0.013 < z < 0.1 cosmic spectral energy distribution from 0.1 micron to 1mm. Monthly Notices of the Royal Astronomical Society, 427(4), 3244-3264. Retrieved from http://arxiv.org/abs/1209.0259.


Zitierlink: http://hdl.handle.net/11858/00-001M-0000-0015-1297-C
Zusammenfassung
We use the GAMA I dataset combined with GALEX, SDSS and 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 x 10^5 (Mpc/h)^{3}. The derived luminosity distributions are normalised to the SDSS 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 \mum 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. (2008) 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) x 10^{35} h W Mpc^{-3} of which (1.2 +/- 0.1) x 10^{35} h W Mpc^{-3} is directly released into the inter-galactic medium and (0.6 +/- 0.1) x 10^{35} 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 0.1micron to 0.6mm. 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.