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Since the launch of the Herschel Space Observatory, our understanding aboutthe photo-dissociation regions (PDR) has taken a step forward. In the bandwidthof the Fourier Transform Spectrometer (FTS) of the Spectral and PhotometricImaging REceiver (SPIRE) on board Herschel, ten CO rotational transitions,including J=4-3 to J=13-12, and three fine structure lines, including [CI] 609,[CI] 370, and [NII] 250 micron, are covered. In this paper, we present ourfindings from the FTS observations at the nuclear region of M83, based on thespatially resolved physical parameters derived from the CO spectral line energydistribution (SLED) map and the comparisons with the dust properties andstar-formation tracers. We discuss (1) the potential of using [NII] 250 and[CI] 370 micron as star-formation tracers; (2) the reliability of tracingmolecular gas with CO; (3) the excitation mechanisms of warm CO; (4) thepossibility of studying stellar feedback by tracing the thermal pressure ofmolecular gas in the nuclear region of M83.

Spatially resolved physical conditions of molecular gas and potential star formation tracers in M83, revealed by the Herschel SPIRE FTS