Context :

Aims : We present a detailed X-ray and radio wavelength study of G308.4–1.4 , a candidate supernova remnant ( SNR ) in the ROSAT All Sky Survey and the MOST supernova remnant catalogue , in order to identify it as a SNR .

Methods : The SNR candidate and its central sources were studied using observations from the Chandra X-ray Observatory , SWIFT , the Australian Telescope Compact Array ( ATCA ) at 1.4 and 2.5 GHz and WISE infrared observation at 24 \mu m .

Results : We conclude that G308.4–1.4 is indeed a supernova remnant by means of its morphology matching at X-ray , radio and infrared wavelength , its spectral energy distribution in the X-ray band and its emission characteristics in the radio band .
G308.4–1.4 is a shell-type SNR .
X-ray , radio and infrared emission is seen only in the eastern part of the remnant .
The X-ray emission can best be described by an absorbed non-equilibrium collisional plasma with a hydrogen density of n _ { \mathrm { H } } = ( 1.02 \pm 0.04 ) \times 10 ^ { 22 } cm ^ { -2 } , a plasma temperature of 6.3 ^ { +1.2 } _ { -0.7 } million Kelvin and an under-abundance of Iron , Neon and Magnesium , as well as an overabundance in Sulfur with respect to the solar values .
The SNR has a spectral index in the radio band of \alpha = -0.7 \pm 0.2 .
A detailed analysis revealed that the remnant is at a distance of 6 to 12 kpc and the progenitor star exploded \sim 5000 to 7500 years ago .
Two faint X-ray point sources located near to the remnant ’ s geometrical center are detected .
Both sources have no counterpart at other wavelengths , leaving them as candidates for the compact remnant of the supernova explosion .

Conclusions :