Laurence Tresse

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The Cosmic SFR History a decade after 4.0±0.2 2.5±0.7 Early type dominated Late type dominated --- Hα, Tresse et al. '02 --- 12μ m, Perez-Gonzalez et al. '05 --- 1.4Ghz, Haarsma et al. '00 The Millennium run, Croton et al. '05 Somerville, Primack, Faber '01 Directly observed ionizing UV flux --- 1500, Schiminovich et al. '05 ● 1500, Tresse et al. in prep. □ 1500, Giavalisco et al. '04 ■ 1700, Steidel et al. '99 Dust attenuation increases up to z~0.4 then it is constant. It is related to the change of the dominant population. L. Tresse NNG Conference, Santa Cruz 10/08/2005 14
The VVDS Core Team PI/Co-PI : Le Fèvre, Vettolani Builders : Bottini, Garilli, Le Brun, Maccagni, Picat, Scaramella, Scodeggio, Tresse, Zanichelli Core-Members : Adami, Arnouts, Bardelli, Bolzonella, Cappi, Charlot, Ciliegi, Contini, Foucaud, Franzetti, Gavignaud, Guzzo, Ilbert, Iovino, McCracken, Marano, Marinoni, Mazure, Meneux, Merighi, Paltani, Pellò, Pollo, Pozzetti, Radovich, Zamorani, Zucca The Institutes France : Marseille LAM, Toulouse OMP, Paris IAP Italy : Milan IASF/OABr, Bologne OABo/IRA, Naples OAC The GALEX team in Marseille and Caltech working with VVDS Martin (PI), Milliard Arnouts, Donas, Schiminovich, Treyer L. Tresse NNG Conference, Santa Cruz 10/08/2005 15
Page 1 and 2: Cosmic Star Formation Rate from the
Page 3 and 4: Recap of the VVDS main features VVD
Page 5 and 6: I-selected VVDS & CFRS 1.5 mag fain
Page 7 and 8: Multi-wavelength emissivities LD α
Page 9 and 10: Suite Early Franzetti et al. in pre
Page 11 and 12: FUV from UBVRI mag FUV LFs at z < 2
Page 13: Luminosities Densities at 1500Å an

Laurence Tresse

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