deletions | additions       diff --git a/section_OH_Megamasers_label_sec__.tex b/section_OH_Megamasers_label_sec__.tex  index 89cc458..5cbbb34 100644  --- a/section_OH_Megamasers_label_sec__.tex  +++ b/section_OH_Megamasers_label_sec__.tex 
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\item time variability constraints - Darling paper IV  \end{itemize}  \subsection{Probing Distant Galaxies}  \label{sub:oh_distance}  \subsection{Galaxy Mergers}  \label{sub:oh_mergers}  The evolution of galaxies remains a substantial question in astrophysics. Observationally, it has long been established that major galaxies will undergo interactions and mergers, and many systems have been observed in this process. The massive tidal disruptions give rise to near global instability in the molecular (and maybe atomic) ISM, leading to extreme outbursts. In fact, the LIRGs and ULIRGs hosting OH mega-maser emission are nearly all in a system undergoing a major merger.   This raises the obvious question put forward by \citet{lo2005}: what properties of these galaxy mergers give rise of OH mega-maser emission?  The clear relation between OH mega-masers and major galaxy mergers leads to another potential application: understanding the formation of super-massive black holes (SMBHs).  \begin{itemize}  \item LIRGS w/ and w/o mm emission (Lo); BGC 6240 examples if ULIRG w/o mm emission (Tacconi 1999)  \item role of IR radiation  \item Arecibo survey (Darling papers)  \item galactic weak anomalous OH maser emission (Mirable, Rodriquez, Ruiz 1989)  \item relation to H2CO emission - all non-masing merges show 6cm H2CO absorption, all masing show emission (Mangum+08)  \item ~100 pc extents from intense starbursts w/ high concentrations of molecular gas  \item always near to nucleus regions 
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\item dust temp and optical depth significantly different b/w mm merger galaxies and those w/o - (Willett+11b)  \end{itemize}  \subsection{Luminosity function}  FIGURE 4 from Darling+ 02  \begin{itemize} 
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\item extinction free redshift determination from sub-mm galaxies  \end{itemize}  \subsection{Zeeman Effect} \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.  \begin{itemize}  \item McBride+14, mcbride heiles 13, robishaw heiles 09, robishaw+08  \item robishaw+08 measure splitting at 1667 in 5 ULIRGS w/ Arecibo+GBT (8 in survey)