Direct measurement of magnetic field strengths is only possible through the so-called Zeeman effect that causes an observable splitting in spectral lines. The star-forming region W3 (OH) contains several water masers, which are used for measuring the Zeeman effect. Matlab routines were created to fit Gaussian profiles in order to determine center velocity, intensity, and line width of each maser. The magnetic field was then determined through another Matlab routine that calculated the Stokes V profile, which was equal to the derivative of the Gaussian profiles.
"Magnetic Field Analysis for Star Forming Region W3 (OH),"
1, Article 3.
Available at: http://via.library.depaul.edu/depaul-disc/vol2/iss1/3