  The development of techniques to measure accurately black hole spins is
crucial to study the physics and astrophysics of these objects. X-ray
reflection spectroscopy is currently the most popular method to estimate the
spins of accreting black holes; so far it has provided a spin measurement of
about 40 stellar-mass black holes in X-ray binaries and 40 supermassive black
holes in active galactic nuclei. The relativistic precession model (RPM) is
another method to measure the spins of stellar-mass black holes: it requires
the measurement of the frequencies of three simultaneous quasi-periodic
oscillations and can potentially provide precise estimates of the black hole
mass and spin. However, the two methods do not seem to provide consistent
results when applied to the same sources, which questions the reliability and
accuracy of these measurements. Recently, the RPM has been applied to infer the
spin of the black hole in XTE J1859+226. The authors found $a_* = 0.149 \pm
0.005$ (68% CL). There are no other spin measurements of this source. We looked
for archived RXTE observations of XTE J1859+226 with blurred reflection
features and found 23 spectra suitable for measuring the spin. We employed two
different models with relxill and relxillD and obtained a higher spin value
from all these fits. From simultaneous fitting of 7 spectra of higher quality,
we found $a_* = 0.986^{+0.001}_{-0.004}$ and $a_* =0.987 \pm 0.003$ (90% CL,
statistical) with relxill and relxillD, respectively. Our results confirm the
discrepancy between the spin measurements inferred from the two techniques.
