  Over the past few years, chemical studies have revealed multiple structures
in the vicinity of young stellar objects (YSOs). It has become evident that
specific physical conditions are associated with the emission of particular
molecular lines, allowing us to use molecular probes of the YSO physics.
Consequently, chemical surveys are now necessary to fully constrain the origin
of the observed structures. Several surveys have been conducted to explore the
chemistry of YSOs, focusing on Class 0 and Class II objects. However, our
knowledge of intermediate objects, that are Class I objects, remains limited.
To bridge the gap and establish the relationship between observed structures
and molecular line emission at the Class I evolutionary stage, we investigate
the spatial distribution of key molecular gas species in the low-mass Class I
protostar L1489 IRS (IRAS 04016+2610), a source part of the ChemYSO survey. We
performed a 3mm line survey at high spatial and high spectral resolution using
the NOEMA interferometer and the IRAM-30m telescope. We present here the ten
brightest lines of our survey, in which we identified a new ~ 3 000 au long
streamer in HC3N, C2H, and c-C3H2 emission, likely associated with more
localized accretion shocks probed in SO. In addition, two ~ 10 000 au bubbles
are seen with the dense molecular tracers HCO+, CS, and HCN around the YSO.
Additionally, potential indicators of a second outflow appear in CS and HCN
emission, but its nature remains to be confirmed. The late infall identified at
large scales may originate from the nearby prestellar core L1489 and is likely
responsible for the formation of an external warped disk in this system. The
detection of a potential second outflow could be the direct evidence of a
binary system. Finally, we hypothesize that the bubbles may result from the
magnetic pressure as observed in numerical simulations.
