I chose to focus on spectral classifications B, A, and F. I made this decision because B spectral type stars are too hot to have substantial convective envelopes, while F classification stars have well developed convective envelopes that can cause magnetic braking, and A-type stars provide an intermediate comparison between these two cases. I chose not to focus on O type stars due to the lack of absorption lines in the range of Rice University's spectrograph. Stars later than F-type were also excluded because their rotational velocities tend to be below our spectrograph's resolution limit of around 20 km/s, making it difficult to get accurate measurements on rotational broadening.

These are the steps I took in performing my data reduction using my data collected from Rice University's Lhires III Shelyak Spectrograph on a 23 micron setting:

1. Trim, dark subtract, and flat field correct my science frames
2. Wavelength calibration
3. 1D Spectrum Extraction
4. Normalization of data
5. Gaussian Fitting
6. Correction for instrumental broadening
7. Calculation of v sin i and associated error propagation