Fig. 5 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. 5.

Number of expected spurious detections, caused by noise caused by noise fluctuations, as a function of magnitude (see text). The thin solid line corresponds to the central part of the VV 29 field (see Table 1), the dashed line to the outer VV 29 field and the NGC 4676 field, and the thick solid line to the whole field.

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