AX J2049.6+2939 is a compact X-ray source in the vicinity of the southern blow-up region of the Cygnus Loop supernova remnant ( Miyata et al .
1998a ) .
This source was the brightest X-ray source inside the Cygnus Loop observed during the ASCA survey project .
The X-ray spectrum was well fitted by a power-law function with a photon index of -2.1 \pm 0.1 .
Short-term timing analysis was performed and no coherent pulsation was found .
Follow-up observations with ASCA have revealed a large variation in X-ray intensity by a factor of \simeq 50 , whereas the spectral shape did not change within the statistical uncertainties .
In the second ASCA observation , we found another X-ray source , AX J2050.0+2941 , at the north east of AX J2049.6+2939 .
During the three ASCA observations , the X-ray intensity of AX J2050.0+2941 varied by a factor of \simeq 4 .
No coherent pulsations could be found for AX J2050.0+2941 .

We have performed optical photometric and spectroscopic observations in the vicinity of AX J2049.6+2939 at the Kitt Peak National Observatory ( KPNO ) .
As a result , all objects brighter than B -band magnitude of 22 in the error box can be identified with normal stars .
Combined with the X-ray results and the fact that there are no radio counterparts , AX J2049.6+2939 is not likely to be either an ordinary rotation-powered pulsar or an AGN .
The nature of AX J2049.6+2939 is still unclear and further observations over a wide energy band are strongly required .

As to AX J2050.0+2941 , the long-term X-ray variability and the radio counterpart suggests that it is an AGN .