**Table 2:** Main characteristics of the datasets in HDFN. Column (1): observing band. Column (2): effective wavelength of the filter calculated by convolving the Vega spectrum (Colina & Bohlin 1994) with the transmission curve of the filter + detector. Column (3): limiting AB magnitude. Column (4): source from where the data were obtained.
Band	$\lambda_{\rm eff}(\mu {\rm m})$	$m_{\lim}$	Source
(1)	(2)	(3)	(4)
IRAC-3.6..	3.561	21.6	Spitzer GTO
IRAC-4.5..	4.510	21.8	Spitzer GTO
IRAC-5.8..	5.689	21.8	Spitzer GTO
IRAC-8.0..	7.958	21.7	Spitzer GTO
U.........	0.358	25.2	Subaru deep imaging^a
B.........	0.442	25.2	Subaru deep imaging^a
V.........	0.546	24.9	Subaru deep imaging^a
R.........	0.652	24.4	Subaru deep imaging^a
I.........	0.795	23.9	Subaru deep imaging^a
z.........	0.909	23.6	Subaru deep imaging^a
b.........	0.430	25.7	GOODS^b
v.........	0.592	24.9	GOODS^b
i.........	0.770	24.3	GOODS^b
z.........	0.906	23.9	GOODS^b
$HK_{\rm s}$ ..	2.127	21.3	QUIRC deep imaging^a
b, spectra..	0.430	24.4	TKRS^c

^a Publicly available ultra-deep optical and NIR data from Capak et al. (2004); ^b the Great Observatories Origins Deep Survey (GOODS; Giavalisco et al. (2004); ^c team Keck Treasury Redshift Survey (TKRS; Wirth et al. 2004) and Cowie et al. (2004).

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