Laurence Tresse

More documents

Recommendations

Info

The detailed NNG population at z < 1.5 Best fit Pegase templates on U, B, V, R, I data Courtesy Ilbert Lauger et al. AA '05 submitted I AB = 23 Rest-(B-I) AB Type 1 CWW-Ell 9% 1.58 Type 2 CWW-Sbc 17% 1.11 Type 3 CWW-Scd 34% 0.79 Type 4 CWW-Irr+SB 40% 0.57 Late types have the strongest EL, and bluest continuum Early types exhibit star formation D4000, H δ and [OII] Strong correlation between the bimodality and A-C morphology Zucca et al. astro-ph/0506393 The spectro-photometric-morphological properties are well correlated at z < 1.5 L. <strong>Tresse</strong> NNG Conference, Santa Cruz 10/08/2005 8
Suite Early Franzetti et al. in prep Bimodality clearly present up to z=1.5 Fraction M B < -20 Zucca et al. astro-ph/0506393 Fraction of bright late types decreases by a factor 7 Fraction of bright early types increases by a factor 11 Bright late types dominate at z>1.1 0.6 0.8 1.0 1.2 1.4 1.6 L. <strong>Tresse</strong> NNG Conference, Santa Cruz 10/08/2005 9 redshift Late δ gal = b(z,δ,R)δ Marinoni et al. AA '05 Bright types are not formed below a mass overdensity whose threshold amplitude decreases with z
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: Multi-wavelength emissivities LD α
Page 11 and 12: FUV from UBVRI mag FUV LFs at z < 2
Page 13 and 14: Luminosities Densities at 1500Å an
Page 15: The VVDS Core Team PI/Co-PI : Le F

Laurence Tresse

Create successful ePaper yourself

Delete template?

Save as template?