Fig. 9 from Faint Galaxies in Deep Advanced Camera for Surveys Observations

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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. 9.

Aperture corrections, defined as the difference between the total "intrinsic" magnitudes and the SExtractor MAG_AUTO magnitude. The thick line corresponds to the central part of the VV 29 field (see Table 1), and the thin line to the combination of the outer VV 29 field and the NGC 4676 field. Note that the behavior is similar in the relatively high signal‐to‐noise regime but quickly differs at faint magnitudes.

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