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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. 10.

On the left plots, the X‐axis shows the difference between the VI color measured by SExtractor and the intrinsic or "true" colors of the galaxies. The Y‐axis shows the same quantity, but for the ﹩g﹩−V color. The bottom left plot corresponds to isophotal and the top left plot to Kron magnitudes. Only 20% of the points are plotted for clarity. Note that the scatter is considerably smaller for isophotal magnitudes. The right plots display the color distributions as histograms. The top right plot for the VI colors and the bottom right plot for the ﹩g﹩−V ones. The thick line corresponds to the isophotal colors, the thin line to the Kron ones.

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