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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
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dc.contributor.author | Driver, S.P. | |
dc.contributor.author | Robotham, A.S.G. | |
dc.contributor.author | Kelvin, L. | |
dc.contributor.author | Alpaslan, M. | |
dc.contributor.author | Baldry, I.K. | |
dc.contributor.author | Bamford, S.P. | |
dc.contributor.author | Brough, S. | |
dc.contributor.author | Brown, M. | |
dc.contributor.author | Hopkins, A.M. | |
dc.contributor.author | Liske, J. | |
dc.contributor.author | Loveday, J. | |
dc.contributor.author | Norberg, P. | |
dc.contributor.author | Peacock, J.A. | |
dc.contributor.author | Andrae, E. | |
dc.contributor.author | Bland-Hawthorn, J. | |
dc.contributor.author | Bourne, N. | |
dc.contributor.author | Cameron, E. | |
dc.contributor.author | Colless, M. | |
dc.contributor.author | Conselice, C.J. | |
dc.contributor.author | Croom, S.M. | |
dc.contributor.author | Dunne, L. | |
dc.contributor.author | Frenk, C.S. | |
dc.contributor.author | Graham, A.W. | |
dc.contributor.author | Gunawardhana, M. | |
dc.contributor.author | Hill, D.T. | |
dc.contributor.author | Jones, D.H. | |
dc.contributor.author | Kuijken, K. | |
dc.contributor.author | Madore, B. | |
dc.contributor.author | Nichol, R.C. | |
dc.contributor.author | Parkinson, H.R. | |
dc.contributor.author | Pimbblet, K.A. | |
dc.contributor.author | Phillipps, S. | |
dc.contributor.author | Popescu, C.C. | |
dc.contributor.author | Prescott, M. | |
dc.contributor.author | Seibert, M. | |
dc.contributor.author | Sharp, R.G. | |
dc.contributor.author | Sutherland, W.J. | |
dc.contributor.author | Taylor, E.N. | |
dc.contributor.author | Thomas, D. | |
dc.contributor.author | Tuffs, R.J. | |
dc.contributor.author | van Kampen, E. | |
dc.contributor.author | Wijesinghe, D. | |
dc.contributor.author | Wilkins, S. | |
dc.date.accessioned | 2014-05-12T14:31:04Z | |
dc.date.available | 2014-05-12T14:31:04Z | |
dc.date.issued | 2012-12-21 | |
dc.identifier | 117858864 | |
dc.identifier | 4fb5411b-1021-4938-9392-c5fc0b9b1d35 | |
dc.identifier | 84875043961 | |
dc.identifier.citation | Driver , S P , Robotham , A S G , Kelvin , L , Alpaslan , M , Baldry , I K , Bamford , S P , Brough , S , Brown , M , Hopkins , A M , Liske , J , Loveday , J , Norberg , P , Peacock , J A , Andrae , E , Bland-Hawthorn , J , Bourne , N , Cameron , E , Colless , M , Conselice , C J , Croom , S M , Dunne , L , Frenk , C S , Graham , A W , Gunawardhana , M , Hill , D T , Jones , D H , Kuijken , K , Madore , B , Nichol , R C , Parkinson , H R , Pimbblet , K A , Phillipps , S , Popescu , C C , Prescott , M , Seibert , M , Sharp , R G , Sutherland , W J , Taylor , E N , Thomas , D , Tuffs , R J , van Kampen , E , Wijesinghe , D & Wilkins , S 2012 , ' Galaxy And Mass Assembly (GAMA) : the 0.013 < z < 0.1 cosmic spectral energy distribution from 0.1 μm to 1 mm ' , Monthly Notices of the Royal Astronomical Society , vol. 427 , no. 4 , pp. 3244-3264 . https://doi.org/10.1111/j.1365-2966.2012.22036 | en |
dc.identifier.issn | 0035-8711 | |
dc.identifier.uri | https://hdl.handle.net/10023/4766 | |
dc.description.abstract | 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 × 10 (Mpc h). 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) × 10h W Mpc of which (1.2 ± 0.1) × 10h W Mpc is directly released into the inter-galactic medium and (0.6 ± 0.1) × 10h W Mpc 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 0.1μm 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. | |
dc.format.extent | 21 | |
dc.format.extent | 5091973 | |
dc.language.iso | eng | |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society | en |
dc.subject | QB Astronomy | en |
dc.subject.lcc | QB | en |
dc.title | Galaxy And Mass Assembly (GAMA) : the 0.013 < z < 0.1 cosmic spectral energy distribution from 0.1 μm to 1 mm | en |
dc.type | Journal article | en |
dc.contributor.sponsor | Science & Technology Facilities Council | en |
dc.contributor.institution | University of St Andrews. University of St Andrews | en |
dc.contributor.institution | University of St Andrews. School of Physics and Astronomy | en |
dc.identifier.doi | https://doi.org/10.1111/j.1365-2966.2012.22036 | |
dc.description.status | Peer reviewed | en |
dc.identifier.url | http://www.scopus.com/inward/record.url?eid=2-s2.0-84875043961&partnerID=8YFLogxK | en |
dc.identifier.grantnumber | en |
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