Fig. 3 from New Constraints on ΩM, ΩΛ, and w from an Independent Set of 11 High‐Redshift Supernovae Observed with the Hubble Space Telescope

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New Constraints on Ω_M, Ω_Λ, and w from an Independent Set of 11 High‐Redshift Supernovae Observed with the Hubble Space Telescope

Authors: R. A. Knop, G. Aldering, R. Amanullah, P. Astier, G. Blanc, M. S. Burns, A. Conley, S. E. Deustua, M. Doi, R. Ellis, S. Fabbro, G. Folatelli, A. S. Fruchter, G. Garavini, S. Garmond, K. Garton, R. Gibbons, G. Goldhaber, A. Goobar, D. E. Groom, D. Hardin, I. Hook, D. A. Howell, A. G. Kim, B. C. Lee, C. Lidman, J. Mendez, S. Nobili, P. E. Nugent, R. Pain, N. Panagia, C. R. Pennypacker, S. Perlmutter, R. Quimby, J. Raux, N. Regnault, P. Ruiz-Lapuente, G. Sainton, B. Schaefer, K. Schahmaneche, E. Smith, A. L. Spadafora, V. Stanishev, M. Sullivan, N. A. Walton, L. Wang, W. M. Wood-Vasey, N. Yasuda, and (The Supernova Cosmology Project)

Knop et al. 2003 The Astrophysical Journal 598 102.

Provider: AAS Journals

Caption: Fig. 3.

Plot of E(B−V) as a function of redshift for the 11 HST‐observed SNe of this paper, showing that the blue edge of the distribution shows no significant evolution with redshift. (The larger dispersion at lower redshifts is expected for a flux‐limited sample.) Error bars include only measurement errors and no assumed intrinsic color dispersion. Filled circles are those SNe in the low‐extinction subset (subset 2).

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