  We present space-based thermal infrared observations of the presumably
Geminid-associated asteroids: (3200)Phaethon, 2005 UD and 1999 YC using
WISE/NEOWISE. The images were taken at the four wavelength bands
3.4$\mu$m(W1),4.6$\mu$m(W2),12$\mu$m(W3),and 22$\mu$m(W4). We find no evidence
of lasting mass-loss in the asteroids over the decadal multi-epoch datasets. We
set an upper limit to the mass-loss rate in dust of Q<2kg s$^{-1}$ for Phaethon
and <0.1kg s$^{-1}$ for both 2005 UD and 1999 YC, respectively, with little
dependency over the observed heliocentric distances of R=1.0$-$2.3au. For
Phaethon, even if the maximum mass-loss was sustained over the 1000(s)yr
dynamical age of the Geminid stream, it is more than two orders of magnitude
too small to supply the reported stream mass (1e13$-$14kg). The
Phaethon-associated dust trail (Geminid stream) is not detected at R=2.3au,
corresponding an upper limit on the optical depth of $\tau$<7e-9. Additionally,
no co-moving asteroids with radii r<650m were found. The DESTINY+ dust analyzer
would be capable of detecting several of the 10$\mu$m-sized interplanetary dust
particles when at far distances(>50,000km) from Phaethon. From 2005 UD, if the
mass-loss rate lasted over the 10,000yr dynamical age of the Daytime Sextantid
meteoroid stream, the mass of the stream would be ~1e10kg. The 1999 YC images
showed neither the related dust trail ($\tau$<2e-8) nor co-moving objects with
radii r<170m at R=1.6au. Estimated physical parameters from these limits do not
explain the production mechanism of the Geminid meteoroid stream. Lastly, to
explore the origin of the Geminids, we discuss the implications for our data in
relation to the possibly sodium (Na)-driven perihelion activity of Phaethon.
