We present the results of the interferometric observations of the circumstellar disk surrounding MWC 297 in the continuum at 230 GHz ( 1.3 mm ) and in the ( J=2-1 ) rotational transitions of ^ { 12 } CO , ^ { 13 } CO and C ^ { 18 } O using the Submillimeter Array .
At a distance of 250 pc , MWC 297 is one of the closest , young massive stars ( M _ { \star } \sim 10 M _ { \odot } ) to us .
Compact continuum emission is detected towards MWC 297 from which we estimate a disk mass ( gas+dust ) of 0.07 M _ { \odot } and a disk radius of \leq 80 AU .
Our result demonstrates that circumstellar disks can survive around massive stars well into their main sequence phase even after they have become optically visible .
Complementing our observations with the data compiled from the literature , we find the submm dust opacity index \beta to be between 0.1 and 0.3 .
If the emission is optically thin , the low value of \beta indicates the presence of relatively large grains in the disk , possibly because of grain growth .
We do not detect any CO emission associated with the continuum source .
We argue that the ^ { 13 } CO emission from the disk is likely optically thin , in which case , we derive an upper limit to the gas mass which implies significant depletion of molecular gas in the disk .
The mass of this disk and the evolutionary trends observed are similar to those found for intermediate mass Herbig Ae stars and low mass T Tauri stars .