Abstract
Over the last decade, the quantity of scientific results brought by the observations of very faint objects has been quite spectacular. In particular, they concern the photometry of faint galaxies up to B = 27 (Tyson 1988) or K = 22 (Cowie et al. 1994). The consequences of these observations are the detection of a large population of faint galaxies more numerous than any prediction given by standard galaxy evolution and probably a new vision of the distant universe. For faint object spectroscopy, the most recent surveys of field galaxies reach a magnitude range of 23–24 (Colless et al. 1990, 1993, Lilly and Cowie 1993, Tresse et al. 1993) with a reasonable S/N ratio that allows a redshift measurement from absorption-line identification. But in this magnitude range, the sky background flux is dominant with respect to the source, being at least 10 times brighter. It is well known that in that case, with a low readout noise detector and a “perfect” spectrograph, the S/N ratio scales as:
Access this chapter
Tax calculation will be finalised at checkout
Purchases are for personal use only
Preview
Unable to display preview. Download preview PDF.
References
Boksenberg, A. 1975 in Image Processing Techniques in Astronomy, C. de Jager and H. Nieuwenhuizen, eds., Reidel, Dordrecht, p. 59
Colless, M. M., Ellis, R. S., Taylor, K. and Hook, R. N. 1990 MNRAS 244, 408
Colless, M. M., Ellis, R. S., Broadhurst, T. J., Taylor, K. and Peterson, B. A. 1993 MNRAS 261, 19
Cowie, L. L. and Lilly, S. J. 1989 ApJ 336, L41
Cowie, L. L., Gardner, J., Wainscoat, R. J. and Hoddap, K. W. 1994, preprint
Cuillandre, J. C., Fort, B., Picat, J. P., Soucail, G., Altieri, B., Beigbeder, F., Dupin, J. P., Pourthié T. and Ratier, G. 1994 A&A 281, 603
Lilly, S. J., Cowie, L. L. and Gardner, J. P. 1991 ApJ 369, 79
McLean, I. S., Cormack, W. A., Herd, J. T. and Aspin, C. 1981 Proc. SPIE 290, p. 155
Picat, J. P., Cuillandre, J. C., Fort, B. and Soucail, G. 1994 Proc. SPIE 2198, AstronomicalTelescopes and Instrumentation for the 21st Century, D. L. Crawford, ed., p. 1274
Shectman, S. A. and Hiltner, W. 1976 PASP 88, 960
Soucail, G., Mellier, Y., Fort, B., Cailloux, M. and Mathez, G. 1988 A&A 191, L19
Tresse, L., Hammer, F., Le Fèvre, O. and Proust, D. 1993 A&A 277, 53
Tyson, J. A. 1988 AJ 96, 1
Author information
Authors and Affiliations
Editor information
Editors and Affiliations
Rights and permissions
Copyright information
© 1995 Springer Science+Business Media Dordrecht
About this paper
Cite this paper
Soucail, G., Cuillandre, J.C., Picat, J.P., Fort, B. (1995). “Va-et-Vient” (“Back-and-Forth”) CCD Spectroscopy: A New Way to Increase the Limiting Magnitude of Very Large Telescopes. In: Philip, A.G.D., Janes, K.A., Upgren, A.R. (eds) New Developments in Array Technology and Applications. International Astronomical Union / Union Astronomique Internationale, vol 167. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-0383-1_32
Download citation
DOI: https://doi.org/10.1007/978-94-011-0383-1_32
Publisher Name: Springer, Dordrecht
Print ISBN: 978-0-7923-3640-2
Online ISBN: 978-94-011-0383-1
eBook Packages: Springer Book Archive