# Radio and X-ray properties of the source G29.37+0.1 linked to HESS J1844-030

## TL;DR

This study combines radio and X-ray observations to analyze the complex structure of G29.37+0.1, revealing it as a likely radio galaxy with possible supernova remnant features and interactions with nearby molecular clouds.

## Contribution

It provides the first detailed multi-wavelength analysis of G29.37+0.1, identifying its radio galaxy nature and potential supernova remnant characteristics.

## Key findings

- G29.37+0.1 is likely a radio galaxy with a twisted S-shaped morphology.
- The source exhibits a spectral index of 0.59, with flatter spectra in the core and jets.
- Possible supernova remnant with a pulsar wind nebula component is suggested.

## Abstract

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.