Context : Bubble N107 was discovered in the infrared emission of dust in the Galactic Plane observed by the Spitzer Space Telescope ( GLIMPSE survey : l \approx 51 \aas@@fstack { \circ } 0 , b \approx 0 \aas@@fstack { \circ } 1 ) .
The bubble represents an example of shell-like structures found all over the Milky Way Galaxy .

Aims : We aim to analyse the atomic and molecular components of N107 , as well as its radio continuum emission .
With the help of numerical simulations , we aim to estimate the bubble age and other parameters which can not be derived directly from observations .

Methods : From the observations of the H i ( I-GALFA ) and \@element [ ] [ 13 ] [ ] [ ] { \mathrm { CO } } ( GRS ) lines we derive the bubble ’ s kinematical distance and masses of the atomic and molecular components .
With the algorithm DENDROFIND , we decompose molecular material into individual clumps .
From the continuum observations at 1420 \mathrm { MHz } ( VGPS ) and 327 \mathrm { MHz } ( WSRT ) , we derive the radio flux density and the spectral index .
With the numerical code ring , we simulate the evolution of stellar-blown bubbles similar to N107 .

Results : The total H i mass associated with N107 is 5.4 \times 10 ^ { 3 } M _ { \odot } .
The total mass of the molecular component ( a mixture of cold gasses of H _ { 2 } , CO , He and heavier elements ) is 1.3 \times 10 ^ { 5 } M _ { \odot } , from which 4.0 \times 10 ^ { 4 } M _ { \odot } is found along the bubble border .
We identified 49 molecular clumps distributed along the bubble border , with the slope of the clump mass function of -1.1 .
The spectral index of -0.30 of a strong radio source located apparently within the bubble indicates nonthermal emission , hence part of the flux likely originates in a supernova remnant , not yet catalogued .
The numerical simulations suggest N107 is likely less than 2.25 \mathrm { Myr } old .
Since first supernovae explode only after 3 \mathrm { Myr } or later , no supernova remnant should be present within the bubble .
It may be explained if there is a supernova remnant in the direction towards the bubble , however not associated with it .

Conclusions :