Using the Mopra telescope , we have targeted 61 regions in the Carina Nebula , covering an area of 1.5 square degrees , of bright and compact 870 \mu m dust continuum emission for molecular line emission from a host of 16 spectral lines at 3mm , including several dense gas tracers .
We found that the clumps detected in Carina in general have in average higher temperatures ( 27 K compared to 21 K ) , and lower masses ( 214 M _ { \odot } compared to 508 M _ { \odot } ) than clumps located at a similar distance to us in the Galactic Plane .
We compare the properties of the molecular line emission of these clumps with the MALT90 survey , finding that the detection rates of the molecular lines are similar to MALT90 clumps that are classified as PDRs .
However , most of the clumps located within 10 \arcmin of \eta Carina have little molecular line emission detected in our observations .
Given the lack of maser detection in the Carina region , we also compared the properties the clumps in Carina to those of Galactic clumps associated with 6.7-GHz methanol masers .
We found that the clumps in Carina are warmer , less massive , and show less emission from the four most commonly detected molecules , HCO ^ { + } , N _ { 2 } H ^ { + } , HCN , and HNC , compared to clumps associated with masers in the Galactic Plane .
Overall our results are consistent with the scenario in which the high radiation field of \eta Carina is dramatically affecting its local environment , and therefore the chemical composition of the dense clumps .