  We report the first direct measurement of the helium isotope ratio, 3He/4He,
outside of the Local Interstellar Cloud, as part of science verification
observations with the upgraded CRyogenic InfraRed Echelle Spectrograph
(CRIRES). Our determination of 3He/4He is based on metastable HeI* absorption
along the line-of-sight towards Tet02 Ori A in the Orion Nebula. We measure a
value 3He/4He=(1.77+/-0.13)x10^{-4}, which is just ~40 per cent above the
primordial relative abundance of these isotopes, assuming the Standard Model of
particle physics and cosmology, (3He/4He)_p = (1.257+/-0.017)x10^-4. We
calculate a suite of galactic chemical evolution simulations to study the
Galactic build up of these isotopes, using the yields from Limongi & Chieffi
(2018) for stars in the mass range M=8-100 M_sun and Lagarde (2011,2012) for
M=0.8-8 M_sun. We find that these simulations simultaneously reproduce the
Orion and protosolar 3He/4He values if the calculations are initialized with a
primordial ratio (3He/4He)_p=(1.043+/-0.089)x10^-4. Even though the quoted
error does not include the model uncertainty, this determination agrees with
the Standard Model value to within ~2sigma. We also use the present-day
Galactic abundance of deuterium (D/H), helium (He/H), and 3He/4He to infer an
empirical limit on the primordial 3He abundance, (3He/H)_p <
(1.09+/-0.18)x10^-5, which also agrees with the Standard Model value. We point
out that it is becoming increasingly difficult to explain the discrepant
primordial 7Li/H abundance with non-standard physics, without breaking the
remarkable simultaneous agreement of three primordial element ratios (D/H,
4He/H, and 3He/4He) with the Standard Model values.
