Context :

Aims : We conducted the first X-ray observations of the newly erupting FU Ori-type outburst in HBC 722 ( V2493 Cyg ) with the aim to characterize its X-ray behavior and near-stellar environment during early outburst .

Methods : We used data from the XMM-Newton and Chandra X-ray observatories to measure X-ray source temperatures and luminosities as well as the gas column densities along the line of sight toward the source .

Results : We report a Chandra X-ray detection of HBC 722 with an X-ray luminosity of L _ { X } \approx 4 \times 10 ^ { 30 } ~ { } \mathrm { ergs~ { } s } ^ { -1 } .
The gas column density exceeds values expected from optical extinction and standard gas-to-dust ratios .
We conclude that dust-free gas masses are present around the star , such as strong winds launched from the inner disk , or massive accretion columns .
A tentative detection obtained by XMM-Newton two years earlier after an initial optical peak revealed a fainter X-ray source with only weak absorption .

Conclusions :