Contamination by field late-M, L and T dwarfs in deep surveys

Details Contamination by field late-M, L and T dwarfs in deep surveys Contamination by field late-M, L and T dwarfs in deep surveys

2008-05-29

arxiv.org/abs/0805.4480v2

Astronomy and Astrophysics

Astrophysics

A&A, accepted. 11 pages, 4 figures, 4 tables. Version 2: deleted two spurious figures at the end of the file

Scientific paper

10.1051/0004-6361:200809520

Context: Deep photometric surveys for substellar objects in young clusters and for high-redshift quasars are affected by contaminant sources at different heliocentric distances.If not correctly taken into account, the contamination may have a strong effect on the Initial Mass Function determination and on the identification of quasars. Aims: We calculate in detail the back- and foreground contamination by field dwarfs of very late spectral types (intermediate and late M, L and T) in deep surveys and provide the data and tools for the computation. Methods: Up-to-date models and data from the literature have been used: (i) a model of the Galactic thin disc by an exponential law; (ii) the length and height scales for late-type dwarfs; (iii) the local spatial densities, absolute magnitudes and colours of dwarfs for each spectral type. Results: We derive a simplified expression for the spatial density in the thin disc that depends on the heliocentric distance and the galactic coordinates (l, b) and integrate it in the truncated cone screened in the survey. As a practical application, we compute the numbers of L- and T-type field dwarfs in very deep (I = 21-29 mag) surveys in the direction of the young sigma Orionis cluster. The increasing number of contaminants at the faintest magnitudes could inhibit the study of the opacity mass limit at M <~ 0.003 M_sol in the cluster.

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