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Molecular clouds (MCs) in galaxies are complex places with many phases. Itis, therefore, essential to study the physics and kinematics of the MCs usingmultiple emission lines. We probe the physics of the molecular gas and dust inthe nearby spiral galaxy NGC 7331 using multiple emission lines, i.e. carbonmonoxide (CO), 24{\mu}m and far-ultraviolet (FUV) data. 14 positions weretargeted across the gaseous disc of NGC 7331. We found that CO intensities, gasmass, gas surface density, and 24{\mu}m-to-FUV flux ratio (i.e. the extinction)increase up to about 40 arcsec from the centre and then start to decrease.There is a positive correlation between most of the pair of parameters studied(except FUV flux density). The beam-averaged physical parameters on the easternside of the disc show higher median values than those on the western side. Ourresults indicate that the star formation activity, stellar populations andoverall physical properties of the ISM are different on either side of thedisc. Our study provides notable insights into the complex nature of theinterstellar medium (ISM) in galaxies and has the potential to provoke futurehigher-resolution studies yet to come.

Correlations of gas, dust and young stellar populations in the spiral galaxy NGC 7331