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Faint Galaxies in Deep Advanced Camera for Surveys Observations

  • Authors: N. Benítez, H. Ford, R. Bouwens, F. Menanteau, J. Blakeslee, C. Gronwall, G. Illingworth, G. Meurer, T. J. Broadhurst, M. Clampin, M. Franx, G. F. Hartig, D. Magee, M. Sirianni, D. R. Ardila, F. Bartko, R. A. Brown, C. J. Burrows, E. S. Cheng, N. J. G. Cross, P. D. Feldman, D. A. Golimowski, L. Infante, R. A. Kimble, J. E. Krist, M. P. Lesser, Z. Levay, A. R. Martel, G. K. Miley, M. Postman, P. Rosati, W. B. Sparks, H. D. Tran, Z. I. Tsvetanov, R. L. White, and W. Zheng

Benítez et al. 2004 The Astrophysical Journal Supplement Series 150 1.

  • Provider: AAS Journals

Caption: Fig. 19.

Comparison with number count models. The points correspond to our final corrected number counts (same as the open squares in the previous plot). The thick solid line represents a no‐evolution model and the dashed line a passive luminosity evolution (PLE) model. The dotted and dot‐dashed line represent PLE models including merger of galaxies following, respectively, the Guiderdoni & Rocca‐Volmerange (1990) and the Broadhurst et al. (1992) prescriptions. The thin solid line represents the LCDM predictions of Nagashima et al. (2002). See the text for details about the model generation and comments.

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