Using infrared , radio continuum and spectral observations , we performed a detailed investigation of the H ii region RCW175 .
We determined that RCW175 , which actually consists of two separate H ii regions , G29.1-0.7 and G29.0-0.6 , is located at a distance of 3.2 \pm 0.2 kpc .
Based on the observations we infer that the more compact G29.0-0.6 is less evolved than G29.1-0.7 and was possibly produced as a result of the expansion of G29.1-0.7 into the surrounding interstellar medium .
We compute a star formation rate for RCW175 of ( 12.6 \pm 1.9 ) \times 10 ^ { -5 } M _ { \sun } yr ^ { -1 } , and identified 6 possible young stellar object candidates within its vicinity .
Additionally , we estimate that RCW175 contains a total dust mass of 215 \pm 53 M _ { \sun } .

RCW175 has previously been identified as a source of anomalous microwave emission ( AME ) , an excess of emission at cm wavelengths often attributed to electric dipole radiation from the smallest dust grains .
We find that the AME previously detected in RCW175 is not correlated with the smallest dust grains ( polycyclic aromatic hydrocarbons or small carbonaceous dust grains ) , but rather with the exciting radiation field within the region .
This is a similar result to that found in the Perseus molecular cloud , another region which harbors AME , suggesting that the radiation field may play a pivotal role in the production of this new Galactic emission mechanism .
Finally , we suggest that these observations may hint at the importance of understanding the role played by the major gas ions in spinning dust models .