Measures of star formation rates from infrared (Herschel) and UV (GALEX) emissions of galaxies in the HerMES fields
dc.contributor.author | Buat, V. | |
dc.contributor.author | Giovannoli, E. | |
dc.contributor.author | Burgarella, D. | |
dc.contributor.author | Altieri, B. | |
dc.contributor.author | Amblard, A. | |
dc.contributor.author | Arumugam, V. | |
dc.contributor.author | Aussel, H. | |
dc.contributor.author | Babbedge, T. | |
dc.contributor.author | Blain, A.W. | |
dc.contributor.author | Bock, J. | |
dc.contributor.author | Boselli, A. | |
dc.contributor.author | Castro-Rodriguez, N. | |
dc.contributor.author | Cava, A. | |
dc.contributor.author | Chanial, P. | |
dc.contributor.author | Clements, D. | |
dc.contributor.author | Conley, A. | |
dc.contributor.author | Conversi, L. | |
dc.contributor.author | Cooray, A. | |
dc.contributor.author | Dowell, C.D. | |
dc.contributor.author | Dwek, E. | |
dc.contributor.author | Eales, S. | |
dc.contributor.author | Elbaz, D. | |
dc.contributor.author | Fox, M. | |
dc.contributor.author | Franceschini, A. | |
dc.contributor.author | Gear, W.K. | |
dc.contributor.author | Glenn, J. | |
dc.contributor.author | Griffin, M. | |
dc.contributor.author | Halpern, M. | |
dc.contributor.author | Hatziminaoglou, E. | |
dc.contributor.author | Heinis, S. | |
dc.contributor.author | Ibar, E. | |
dc.contributor.author | Isaak, K.G. | |
dc.contributor.author | Ivison, R.J. | |
dc.contributor.author | Lagache, G. | |
dc.contributor.author | Levenson, L. | |
dc.contributor.author | Lonsdale, C.J. | |
dc.contributor.author | Lu, N. | |
dc.contributor.author | Madden, S. | |
dc.contributor.author | Maffei, B. | |
dc.contributor.author | Magdis, G. | |
dc.contributor.author | Mainetti, G. | |
dc.contributor.author | Marchetti, L. | |
dc.contributor.author | Morrison, G.E. | |
dc.contributor.author | Nguyen, H.T. | |
dc.contributor.author | O'Halloran, B. | |
dc.contributor.author | Oliver, S. | |
dc.contributor.author | Omont, A. | |
dc.contributor.author | Owen, F. | |
dc.contributor.author | Page, M.J. | |
dc.contributor.author | Pannella, M. | |
dc.contributor.author | Papageorgiou, A. | |
dc.contributor.author | Pearson, C. | |
dc.contributor.author | Perez-Fournon, I. | |
dc.contributor.author | Pohlen, M. | |
dc.contributor.author | Rigopoulou, D. | |
dc.contributor.author | Rizzo, D. | |
dc.contributor.author | Roseboom, I.G. | |
dc.contributor.author | Rowan-Robinson, M. | |
dc.contributor.author | Portal, M.S. | |
dc.contributor.author | Schulz, B. | |
dc.contributor.author | Seymour, N. | |
dc.contributor.author | Shupe, D. | |
dc.contributor.author | Smith, A.J. | |
dc.contributor.author | Stevens, J. A. | |
dc.contributor.author | Strazzullo, V. | |
dc.contributor.author | Symeonidis, M. | |
dc.contributor.author | Trichas, M. | |
dc.contributor.author | Tugwell, K.E. | |
dc.contributor.author | Vaccari, M. | |
dc.contributor.author | Valiante, E. | |
dc.contributor.author | Valtchanov, I. | |
dc.contributor.author | Vigroux, L. | |
dc.contributor.author | Wang, L. | |
dc.contributor.author | Ward, R. | |
dc.contributor.author | Wright, G. | |
dc.contributor.author | Xu, C.K. | |
dc.contributor.author | Zemcov, M. | |
dc.date.accessioned | 2011-05-10T10:05:42Z | |
dc.date.available | 2011-05-10T10:05:42Z | |
dc.date.issued | 2010 | |
dc.identifier.citation | Buat , V , Giovannoli , E , Burgarella , D , Altieri , B , Amblard , A , Arumugam , V , Aussel , H , Babbedge , T , Blain , A W , Bock , J , Boselli , A , Castro-Rodriguez , N , Cava , A , Chanial , P , Clements , D , Conley , A , Conversi , L , Cooray , A , Dowell , C D , Dwek , E , Eales , S , Elbaz , D , Fox , M , Franceschini , A , Gear , W K , Glenn , J , Griffin , M , Halpern , M , Hatziminaoglou , E , Heinis , S , Ibar , E , Isaak , K G , Ivison , R J , Lagache , G , Levenson , L , Lonsdale , C J , Lu , N , Madden , S , Maffei , B , Magdis , G , Mainetti , G , Marchetti , L , Morrison , G E , Nguyen , H T , O'Halloran , B , Oliver , S , Omont , A , Owen , F , Page , M J , Pannella , M , Papageorgiou , A , Pearson , C , Perez-Fournon , I , Pohlen , M , Rigopoulou , D , Rizzo , D , Roseboom , I G , Rowan-Robinson , M , Portal , M S , Schulz , B , Seymour , N , Shupe , D , Smith , A J , Stevens , J A , Strazzullo , V , Symeonidis , M , Trichas , M , Tugwell , K E , Vaccari , M , Valiante , E , Valtchanov , I , Vigroux , L , Wang , L , Ward , R , Wright , G , Xu , C K & Zemcov , M 2010 , ' Measures of star formation rates from infrared (Herschel) and UV (GALEX) emissions of galaxies in the HerMES fields ' , Monthly Notices of the Royal Astronomical Society , vol. 409 , no. 1 , pp. L1-L6 . https://doi.org/10.1111/j.1745-3933.2010.00916.x | |
dc.identifier.issn | 0035-8711 | |
dc.identifier.other | dspace: 2299/5779 | |
dc.identifier.other | ORCID: /0000-0002-4010-8310/work/62747655 | |
dc.identifier.uri | http://hdl.handle.net/2299/5779 | |
dc.description | The definitive version can be found at : http://onlinelibrary.wiley.com/ Copyright Royal Astronomical Society | |
dc.description.abstract | The reliability of infrared (IR) and ultraviolet (UV) emissions to measure star formation rates (SFRs) in galaxies is investigated for a large sample of galaxies observed with the Spectral and Photometric Imaging Receiver (SPIRE) and the Photodetector ArrayCamera and Spectrometer (PACS) instruments on Herschel as part of the Herschel Multi-Tiered Extragalactic Survey (HerMES) project. We build flux-limited 250-mu m samples of sources at redshift z < 1, cross-matched with the Spitzer/MIPS and GALEX catalogues. About 60 per cent of the Herschel sources are detected in UV. The total IR luminosities, L-IR, of the sources are estimated using a spectral energy distribution (SED) fitting code that fits to fluxes between 24 and 500 mu m. Dust attenuation is discussed on the basis of commonly used diagnostics: the L-IR/L-UV ratio and the slope, beta, of the UV continuum. A mean dust attenuation A(UV) of similar or equal to 3 mag is measured in the samples. L-IR/L-UV is found to correlate with L-IR. Galaxies with L-IR > 10(11) L-circle dot and 0.5 < z < 1 exhibit a mean dust attenuation A(UV) of about 0.7 mag lower than that found for their local counterparts, although with a large dispersion. Our galaxy samples span a large range of beta and L-IR/L-UV values which, for the most part, are distributed between the ranges defined by the relations found locally for starburst and normal star-forming galaxies. As a consequence the recipe commonly applied to local starbursts is found to overestimate the dust attenuation correction in our galaxy sample by a factor of similar to 2-3. The SFRs deduced from L-IR are found to account for about 90 per cent of the total SFR; this percentage drops to 71 per cent for galaxies with SFR < 1M(circle dot) yr(-1) (or L-IR < 10(10) L-circle dot). For these faint objects, one needs to combine UV and IR emissions to obtain an accurate measure of the SFR. | en |
dc.format.extent | 1004475 | |
dc.language.iso | eng | |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society | |
dc.subject | galaxies : evolution | |
dc.subject | galaxies : stellar content | |
dc.subject | infrared : galaxies | |
dc.subject | ultraviolet : galaxies | |
dc.title | Measures of star formation rates from infrared (Herschel) and UV (GALEX) emissions of galaxies in the HerMES fields | en |
dc.contributor.institution | School of Physics, Astronomy and Mathematics | |
dc.contributor.institution | Department of Allied Health Professions and Midwifery | |
dc.contributor.institution | Health & Human Sciences Research Institute | |
dc.contributor.institution | Science & Technology Research Institute | |
dc.contributor.institution | Centre for Astrophysics Research (CAR) | |
dc.contributor.institution | Social Sciences, Arts & Humanities Research Institute | |
dc.contributor.institution | School of Education | |
dc.description.status | Peer reviewed | |
rioxxterms.versionofrecord | 10.1111/j.1745-3933.2010.00916.x | |
rioxxterms.type | Journal Article/Review | |
herts.preservation.rarelyaccessed | true |