We found a very likely counterpart to the recently discovered hard X-ray source IGR J2018+4043 in the multi-wavelength observations of the source field .
The source , originally discovered in the 20-40 keV band , is now confidently detected also in the 40-80 keV band , with a flux of ( 1.4 \pm 0.4 ) \times 10 ^ { -11 } ~ { } ergs~ { } cm ^ { -2 } ~ { } s ^ { -1 } .
A 5 ks Swift observation of the IGR J2018+4043 field revealed a hard point-like source with the observed 0.5–10 keV flux of 3.4 ^ { +0.7 } _ { -0.8 } \times 10 ^ { -12 } erg cm ^ { -2 } s ^ { -1 } ( 90 % confidence level ) at \alpha = 20 ^ { h } 18 ^ { m } 38 \fs 55 , \delta = +40 ^ { \circ } 41 ^ { \prime } 00 \farcs 4 ( with a 4 \farcs 2 uncertainty ) .
The combined Swift - Integral spectrum can be described by an absorbed power-law model with photon index \Gamma = 1.3 \pm 0.2 and N _ { H } = 6.1 ^ { +3.2 } _ { -2.2 } \times 10 ^ { 22 } cm ^ { -2 } .
In archival optical and infrared data we found a slightly extended and highly absorbed object at the Swift source position .
There is also an extended VLA 1.4 GHz source peaked at a beam-width distance from the optical and X-ray positions .
The observed morphology and multiwavelength spectra of IGR J2018+4043 are consistent with those expected for an obscured accreting object , i.e .
an AGN or a Galactic X-ray binary .
The identification suggests possible connection of IGR J2018+4043 to the bright \gamma -ray source GEV J2020+4023 detected by COS B and CGRO EGRET .