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Eric W. Koch edited Hydroxyl_OH_produces_maser_emission__.tex
over 8 years ago
Commit id: e0edd52871c01e6b47e9ca28085da5ad489cb6bb
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\item robishaw+08 measure splitting at 1667 in 5 ULIRGS w/ Arecibo+GBT (8 in survey)
\item B_LOS ~ .5 - 18 mG -- similar to galactic ones, suggesting local massive star formation is similar in starbursts
\item similar to B measured from synch radiation -- fields pervade multiple ISM phases
\item
Equation 2 in robishaw+08 for B_LOS -- adapted Equation 1 in mcbride heiles 13
\item Some profiles show multiple components -- total of 14 individual components (spatial)
\item 1667 dominates over 1665, despite measuring similar B values to galactic -- maybe due to wider extragalactic maser lines
\item in Arp 220 - 4 spots - 2 w/ fields toward us and 2 w/ fields away
\item VLBI follow-up would give high-resolution field maps of B about the nucleus - robishaw heiles 09
\item additional 11 confident detections - mcbride heiles 13, 6.1-27.6 mG
\item new detections suggest larger than typical galactic B-fields -- median of 12 mG, ~2 larger than the Fish et al 2005
\item used all confirmed targets from Darling paper III and Willett 2012
\item Some non-detections may be due to much larger B, where the narrow line width approx doesn't hold
\item Can constrain some dynamics -- spherical cloud stability inferred suggests B plays a significant role in region dynamics, lws of ~20 km/s from Parra et al 05 in III Zw35 suggest non-gravitationally bound clouds. Magnetic support may keep confinement (not unlike some proposed schemes for cloud substructure)
\item McBride+14 include other B estimates from other methods, determine that ISM B-fields are greater in ULIRGs
\item dependent on minimum energy argument holding in the center of starburst galaxies
\item u_B > u_photon -- synchrotron cooling dominates over inverse Compton cooling -- CR electrons radiate energy via synchroton before leaving galaxy
\end{itemize}
\subsection{Cosmology}