We present results based on the systematic analysis of currently available Chandra archive data on the brightest galaxy in the Draco constellation NGC 6338 , in order to investigate the properties of the X-ray cavities .
In the central \sim 6 kpc , at least a two and possibly three , X-ray cavities are evident .
All these cavities are roughly of ellipsoidal shapes and show a decrement in the surface brightness of several tens of percent .
In addition to these cavities , a set of X-ray bright filaments are also noticed which are spatially coincident with the H \alpha filaments over an extent of 15 kpc .
The H \alpha emission line filaments are perpendicular to the X-ray cavities .
Spectroscopic analysis of the hot gas in the filaments and cavities reveal that the X-ray filaments are cooler than the gas contained in the cavities .
The emission line ratios and the extended , asymmetric nature of the H \alpha emission line filaments seen in this system require a harder ionizing source than that produced by star formation and/or young , massive stars .
Radio emission maps derived from the analysis of 1.4 GHz VLA FIRST survey data failed to show any association of these X-ray cavities with radio jets , however , the cavities are filled by radio emission .
The total power of the cavities is 17 \times 10 ^ { 42 } erg s ^ { -1 } and the ratio of the radio luminosity to cavity power is \sim 10 ^ { -4 } , implying that most of the jet power is mechanical .