High energy radiation from a planet host star can have strong influence on the final habitability of a system through several mechanisms .
In this context we have constructed a catalogue containing the X-ray luminosities , as well as basic stellar and planetary properties of all known stars hosting giant planets ( > 0.1 ~ { } M _ { \mathrm { J } } ) that have been observed by the Chandra X-ray Observatory , XMM-Newton and/or ROSAT .
Specifically in this paper we present a first application of this catalogue to search for a possible imprint of X-ray photoevaporation of planet-forming discs on the present-day orbital distribution of the observed giant planets .
We found a suggestive void in the semi-major axis , a , versus X-ray luminosity , L _ { \mathrm { x } } , plane , roughly located between a \sim 0.05 – 1 ~ { } \mathrm { au } and L _ { \mathrm { x } } \sim 10 ^ { 27 } – 10 ^ { 29 } ~ { } \mathrm { erg s ^ { -1 } } , which would be expected if photoevaporation played a dominant role in the migration history of these systems .
However , due to the small observational sample size , the statistical significance of this feature can not be proven at this point .