  The region around the H$_2$O ice line, due to its higher surface density,
seems to be the ideal location to form planets. The core of Jupiter, as well as
the cores of close in gas giants are thus thought to form in this region of the
disk. Actually constraining the formation location of individual planets has
proven to be difficult, however. We aim to use the Nitrogen abundance in
Jupiter, which is around 4 times solar, in combination with \textit{Juno}
constraints on the total mass of heavy elements in Jupiter, to narrow down its
formation scenario. Different pathways of enrichment of Jupiter's atmosphere,
such as the accretion of enriched gas, pebbles or planetesimals are considered
and their implications for the oxygen abundance of Jupiter is discussed. The
super solar Nitrogen abundance in Jupiter necessitates the accretion of extra
N$_2$ from the proto-solar nebula. The only location of the disk that this can
happen is outside, or just inside the N$_2$ ice line. These constraints favor a
pebble accretion origin of Jupiter, both from the composition as well as from a
planet formation perspective. We predict that Jupiter's oxygen abundance is
between 3.6 and 4.5 times solar.
