deletions | additions       diff --git a/section_OH_Megamasers_label_sec__.tex b/section_OH_Megamasers_label_sec__.tex  index 4f98655..b9d9d3f 100644  --- a/section_OH_Megamasers_label_sec__.tex  +++ b/section_OH_Megamasers_label_sec__.tex 
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\subsection{Magnetic fields in Extreme Starbursts}  \label{sub:oh_zeeman}  The star formation process is poorly understood due to the many dynamical components, over a large range of scales, that may play vital roles. One important constraint to understand how star formation occurs in a particular environment is the magnetic field XXX Ostriker \& McKee 07 XXX. Since these regions of extreme star-formation are highly obscured (see above), OH mega-masers offer a unique look into the magnetic field properties through Zeeman splitting. OH is the only observed para-magnetic masing species \citep{Elitzur1992_text}, since the outer electron shell contains an unpaired electron. Galactic OH masers associated with HII regions are typically strongly circularly polarized, as is expected for a para-magnetic species with a fully resolved Zeeman pattern \citep{Elitzur1992_text}. Megamasers are not  \begin{itemize}  \item McBride+14, mcbride heiles 13, robishaw heiles 09, robishaw+08