  Age and mass determinations for isolated stellar objects remain
model-dependent. While stellar interior and atmospheric theoretical models are
rapidly evolving, we need a powerful tool to test them. Open clusters are good
candidates for this role. We complement previous studies on the Hyades
multiplicity by Lucky Imaging observations with the AstraLux Norte camera. This
allows us to exclude possible binary and multiple systems with companions
outside 2--7 AU separation and to create a "single-star sequence" for the
Hyades. The sequence encompasses 250 main-sequence stars ranging from A5V to
M6V. Using the "Tool for Astrophysical Data Analysis" (TA-DA), we create
various theoretical isochrones applying different combinations of interior and
atmospheric models. We compare the isochrones with the observed Hyades
single-star sequence on J vs. J - K_s, J vs. J - H and K_s vs. H - K_s
color-magnitude diagrams. As a reference we also compute absolute fluxes and
magnitudes for all stars from X-ray to mid-infrared based on photometric
measurements available in the literature(ROSAT X-ray, GALEX UV, APASS gri,
2MASS JHK_s, and WISE W1 to W).We find that combinations of both PISA and
DARTMOUTH stellar interior models with BT-Settl 2010 atmospheric models
describe the observed sequence well. The full sequence covers the mass range
0.13 to 2.3 Msun, and effective temperatures between 3060 K and 8200 K. Within
the measurement uncertainties, the current generation of models agree well with
the single-star sequence. The primary limitations are the uncertainties in the
measurement of the distance to individual Hyades members, and uncertainties in
the photometry. Additionally, a small (~0.05 mag) systematic offset can be
noted on J vs. J - K and K vs. H - K diagrams - the observed sequence is
shifted to redder colors from the theoretical predictions.
