Context : The Core Mass Functions of low-mass star-forming regions are found to resemble the shape of the Initial Mass Function ( IMF ) .
A similar result is observed for the dust clumps in high-mass star forming regions , although at spatial scales of clusters that do not resolve the substructure that is found in these massive clumps .
The region IRAS 19410+2336 is one exception , having been observed at spatial scales on the order of \sim 2500 AU , sufficient to resolve the clump substructure into individual cores .

Aims : We investigate the protostellar content of IRAS 19410+2336 at high spatial resolution at 1.4 mm , determining the temperature structure of the region and deriving its Core Mass Function .

Methods : The massive star-forming region IRAS 19410+2336 was mapped with the PdBI ( BCD configurations ) at 1.4 mm and 3 mm in the continuum and several transitions of formaldehyde ( H _ { 2 } CO ) and methyl cyanide ( CH _ { 3 } CN ) .
The H _ { 2 } CO transitions were also observed with the IRAM 30 m Telescope .

Results : We detected 26 continuum sources at 1.4 mm with a spatial resolution down to \sim 2200 AU , several of them with counterparts at NIR and MIR wavelengths , distributed in two ( proto ) clusters .
With the PdBI CH _ { 3 } CN and PdBI/IRAM 30 m H _ { 2 } CO emission we derived the temperature structure of the region , ranging from 35 to 90 K. Using these temperatures we calculated the core masses of the detected sources , ranging from \sim 0.7 to \sim 8 M _ { \odot } .
These masses were strongly affected by the spatial filtering of the interferometer , filtering out a common envelope with \sim 90 \% of the single-dish flux .
Considering only the detected dense cores , and accounting for binning effects as well as cumulative distributions , we derived a Core Mass Function , with a power-law index \beta = -2.3 \pm 0.2 .
We resolve the Jeans length of the ( proto ) clusters by one order of magnitude , and only find little velocity dispersion between the different subsources .

Conclusions : Since we can not unambiguously differentiate protostellar and prestellar cores , the derived CMF is not prestellar .
Furthermore , because of the large fraction of missing flux , we can not establish a firm link between the CMF and the IMF .
This implies that future high-mass CMF studies will require to complement the interferometer continuum data with the short spacing information , a task suitable for ALMA .
We note that the method of extracting temperatures using H _ { 2 } CO lines becomes less applicable when reaching the dense core scales of the interferometric observations because most of the H _ { 2 } CO appears to originate in the envelope structure .