deletions | additions       diff --git a/h2o_megamasers.tex b/h2o_megamasers.tex  index 2c82f14..dba532d 100644  --- a/h2o_megamasers.tex  +++ b/h2o_megamasers.tex 
...
\subsection{Extragalactic versus Galactic Properties}  \label{sub:h2o_props}  Galactic  \begin{itemize}  \item   \end{itemize}  Extragalactic  \begin{itemize}  \item sales+15, wagner+13,mccallum+05,  raluy+1998 \item circumnuclear and nuclear jet driven masers and outflow  \item Detection rates: 150/3000 searched galaxies show H2O MM (tarchi+2012)  \item majority are Seyfert 2 or LINERs (z<0.05)  \item much higher detection rates simply among these 2 classes (~25\%, tarchi+12)  \item AGN w/ H2O MM show high N_H > 10^23 cm^-2, some are compton-thick (>10^24)  \item rough correlation w/ unabsorbed X-ray luminosities (kondratko+06) -- uncertain due to poor X-ray data for 1/2 of MM detections  \item Properties of AGN w/ MM: primarily in X-ray absorbed source (zhang+10, ramolla+11, zhu+11); have larger radio luminosities (zhang+12), sample based on extinction-corrected [OIII]5007 flux (zhu+11)  \item highest occurence in Seyfert 2 galaxies -- not suprising since Unified model as it predicts an edge-on disk or torus (ie giving longest path length), tarchi+12  \item Some Seyfert 1 detections have occurred -- more unclear since Unified model predicts these should be face-on  \item Only 1/150 searches of pure Sy1 have given detection, but seem to occure more often with narrow line Sy1's (narrowst balmer lines, strongest FeII emission, exteme X-ray properties (komossa 08))  \item 5/71 detections in this subclass (tarchi+11b) (~7\% rate), sample is volume-limited (those within 1e4 km/s boost rate to ~24\%, highest rate of any AGN class)  \item many proposed reasons: intermediate viewing angles, accretion rates near eddington, strong outflows (tarchi+12)  \item No detections in elliptical or radio-loud galaxies -- several surveys conducted (see refs in Tarchi+12); seems regardless of the AGN type  \item however, there are 4 unclassified H2O MM galaxies which show unique properties (5 including NGC 1052)  \item Could be due to: lack of molecular gas (henkel+98); instability from tidal disruption in clouds orbiting particularly massive SMBHs (tarchi+07b); insufficient sensitivity of completed surveys  \end{itemize}  \subsection{AGN: Disks \& SMBH masses} 
...
\item   \end{itemize}  \subsection{Outflow Masers}  \label{sub:h2o_outflows}  \begin{itemize}  \item tarchi+12, greeenhill+03, mccallum+05  \item Only detected in Circinus -- seyfert 2   \item 0.2 pc radius disk where masers located (tristram+07), also a thick torus out to pc scales, slightly cooler than disk, show a clumpy distribution in torus  \item evidence for collimated AGN outflow w/ maser position  \item mccallum+03 confirm scintillation of H2O mm, rapid variability linked to interstellar scintillation seen in many flat spectrum AGN  \item orginal variation obersved by greenhill+97  \item can test for annual cycles in scintillation, constraining the peculiar velocity of the scattering materialm estimate anisotropies in the medium -- create model of the source  \item can also lead to direct measurement of ISM velocity -- important for constraining any model of anisotropic structure  \item weak scintillation model explains observed variability assuming a local screen; distant, strongly scattering screen model fits observations, shows unseen anti-correlation b/w modulation index and timescale  \end{itemize}  \subsection{Cosmology: Distance Determination}  \label{sub:h2o_cosmo} 
...
\begin{itemize}  \item wiggins+15, tarchi+12  \item OH megamaser seem to be uniquely associated with LIRGs and ULIRGs (L_IR>10^11 L_sol) -- ideal for IR radiative pumping   \item Darling Paper III IR OH correlation  \item  \end{itemize}