  We present chemodynamical links between the present-day Milky Way halo field
star population and Galactic globular clusters (GCs) using a dataset that
combines information from the $\rm{\it Gaia}$ space mission and the Sloan
Digital Sky Survey (SDSS-IV, DR14). Moreover, we incorporated a sample of halo
giant stars with a distinct chemical signature (strong CN bandheads) that
resembles the light-elements anomaly otherwise only seen in the second
generation of GC stellar populations. Using three different tagging techniques,
we could successfully establish unique associations between 151 extratidal
stars in the neighborhood of eight GCs. In addition, we traced the possible
origin of about $62\%$ of the sample of CN-strong giants to their potential
host clusters. Several of the involved GCs have been brought into connection
with the Gaia-Enceladus and Sequoia merger events. By establishing kinematic
and chemical connections between 17 CN-strong stars and their surrounding
fields, we could identify co-moving groups of stars at the same [Fe/H] with a
possible cluster origin. We found strong evidence that four CN-strong stars and
their associates are connected to the Sagittarius stream whilst their tightly
confined [Fe/H] may hint to a birth site in M 54. Finally, we provide tentative
estimates for the fraction of first-generation cluster stars among all stars
lost to the halo. In the immediate cluster vicinity, this value amounts to
$50.0\pm16.7\%$ while the associations in the halo field rather imply
$80.2_{-5.2}^{+4.9}\%$. We speculate that -- if proven real by spectroscopic
follow-up -- the disparity between these numbers could indicate a major
contribution of low-mass clusters to the overall number of stars escaped to the
halo or, alternatively, point toward a strong mass loss from the first
generation during early cluster dissolution. [abridged]
