  Using observations carried out with the GMRT, we performed high-quality
full-synthesis imaging at 610 MHz of the source G29.37+0.1, which is an
as-yet-unclassified object linked to the TeV source HESS J1844-030. These data,
combined with observations at 1400 MHz from MAGPIS were used to investigate the
properties of its radio emission. Additionally, we reprocessed XMM-Newton and
Chandra archival data. G29.37+0.1 mainly consists of a bright twisted
structure, named the S-shaped feature. The high sensitivity of the new GMRT
observations allowed the identification of potential lobes, jets, and a nuclear
central region in the S-shaped morphology of G29.37+0.1. We also highlight the
detection of diffuse and low surface brightness emission enveloping the
brightest emitting regions. The brightest emission in G29.37+0.1 has a radio
synchrotron spectral index 0.59+/-0.09. Variations in the spectral behavior are
observed across the whole radio source with the flattest spectral features in
the central nuclear and jets components (alpha~0.3). These results lead us to
conclude that the brightest radio emission from G29.37+0.1 likely represents a
newly recognized radio galaxy. The identification of optical and infrared
counterparts to the emission from the core of G29.37+0.1 strengthens our
interpretation of an extragalactic origin of the radio emission. Our spectral
analysis demonstrated that a non-thermal origin for the X-ray emission
compatible with a pulsar wind nebula is quite possible. The analysis of the
spatial distribution of the CO gas revealed the presence of a complex of
molecular clouds located in projection adjacent to the radio halo emission and
probably interacting with it. We propose that the faint halo represents a
composite supernova remnant with a pulsar powered component given by the
diffuse X-ray emission superimposed along the line of sight to the radio
galaxy.
