Fig. 2 from The GALEX‐VVDS Measurement of the Evolution of the Far‐Ultraviolet Luminosity Density and the Cosmic Star Formation Rate

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The GALEX‐VVDS Measurement of the Evolution of the Far‐Ultraviolet Luminosity Density and the Cosmic Star Formation Rate

Authors: D. Schiminovich, O. Ilbert, S. Arnouts, B. Milliard, L. Tresse, O. Le Fèvre, M. Treyer, T. K. Wyder, T. Budavári, E. Zucca, G. Zamorani, D. C. Martin, C. Adami, M. Arnaboldi, S. Bardelli, T. Barlow, L. Bianchi, M. Bolzonella, D. Bottini, Y.-I. Byun, A. Cappi, T. Contini, S. Charlot, J. Donas, K. Forster, S. Foucaud, P. Franzetti, P. G. Friedman, B. Garilli, I. Gavignaud, L. Guzzo, T. M. Heckman, C. Hoopes, A. Iovino, P. Jelinsky, V. Le Brun, Y.-W. Lee, D. Maccagni, B. F. Madore, R. Malina, B. Marano, C. Marinoni, H. J. McCracken, A. Mazure, B. Meneux, P. Morrissey, S. Neff, S. Paltani, R. Pellò, J. P. Picat, A. Pollo, L. Pozzetti, M. Radovich, R. M. Rich, R. Scaramella, M. Scodeggio, M. Seibert, O. Siegmund, T. Small, A. S. Szalay, G. Vettolani, B. Welsh, C. K. Xu, and A. Zanichelli

Schiminovich et al. 2005 The Astrophysical Journal Letters 619 L47.

Provider: AAS Journals

Caption: Fig. 2.

FUV LD of UVLGs vs. redshift and comparison with QSO LD. Filled circles from ρ_1500, UVLG integrated from ∞ down to ﹩0.2L_{\star ,\, z=3}﹩ or M_FUV − 19.32. Colors same as in Fig. 1. Vertical hatched bars indicate fraction of luminosity emitted by galaxies brighter than 0.2﹩L_{\star ,\, z=3}﹩. Red dashed line shows QSO FUV LD using values from Boyle et al. (2000) and Madau et al. (1999). Solid line is the same as in Fig. 1.

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