Image Details

Choose export citation format:

Ultraviolet Luminosity Functions from 132 z ∼ 7 and z ∼ 8 Lyman-break Galaxies in the Ultra-deep HUDF09 and Wide-area Early Release Science WFC3/IR Observations

  • Authors: R. J. Bouwens, G. D. Illingworth, P. A. Oesch, I. Labbé, M. Trenti, P. van Dokkum, M. Franx, M. Stiavelli, C. M. Carollo, D. Magee, and V. Gonzalez

Bouwens et al. 2011 The Astrophysical Journal 737 90.

  • Provider: AAS Journals

Caption: Figure 15.

68% and 95% likelihood contours on the model Schechter parameters M* and ϕ* for our LF determination at z ~ 7 (magenta lines) and z ~ 8 (dotted red lines). For comparison, we also show the constraints on the UV LF at z ~ 4 (blue lines), z ~ 5 (green lines), and z ~ 6 (cyan lines) from Bouwens et al. (2007). This figure is the same as the left panel to Figure 13, but now fixing the faint-end slope α to −1.7. A faint-end slope α of −1.7 is similar to the values found at z ~ 1–6 (Yoshida et al. 2006; Bouwens et al. 2007; Oesch et al. 2007, 2010c; McLure et al. 2009; Reddy & Steidel 2009; Arnouts et al. 2005; see Figure 14). No constraint on the faint-end slope at z ~ 4–6 is imposed, and therefore the error contours there are somewhat larger than at z ~ 7.

Other Images in This Article

Show More

Copyright and Terms & Conditions