<?xml version="1.0" encoding="UTF-8"?><xml><records><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Dasyra, K. M.</style></author><author><style face="normal" font="default" size="100%">Combes, F.</style></author><author><style face="normal" font="default" size="100%">Oosterloo, T.</style></author><author><style face="normal" font="default" size="100%">Oonk, J. B. R.</style></author><author><style face="normal" font="default" size="100%">Morganti, R.</style></author><author><style face="normal" font="default" size="100%">Salomé, P.</style></author><author><style face="normal" font="default" size="100%">Vlahakis, N.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">ALMA reveals optically thin, highly excited CO gas in the jet-driven winds of the galaxy IC 5063</style></title><short-title><style face="normal" font="default" size="100%">Astronomy and Astrophysics</style></short-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">Astrophysics - Astrophysics of Galaxies</style></keyword><keyword><style  face="normal" font="default" size="100%">galaxies: active</style></keyword><keyword><style  face="normal" font="default" size="100%">galaxies: nuclei</style></keyword><keyword><style  face="normal" font="default" size="100%">ISM: jets and outflows</style></keyword><keyword><style  face="normal" font="default" size="100%">ISM: kinematics and dynamics</style></keyword><keyword><style  face="normal" font="default" size="100%">ISM: molecules</style></keyword><keyword><style  face="normal" font="default" size="100%">submillimeter: ISM</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2016</style></year><pub-dates><date><style  face="normal" font="default" size="100%">2016/11/1</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">https://ui.adsabs.harvard.edu/abs/2016A&amp;A...595L...7D</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">595</style></volume><pages><style face="normal" font="default" size="100%">L7</style></pages><isbn><style face="normal" font="default" size="100%">0004-6361</style></isbn><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">Using CO (4-3) and (2-1) Atacama Large Millimeter Array (ALMA) data, we prove that the molecular gas in the jet-driven winds of the galaxy IC 5063 is more highly excited than the rest of the molecular gas in the disk of the same galaxy. On average, the CO(4 - 3) /CO(2 - 1) flux ratio is 1 for the disk and 5 for the jet accelerated or impacted gas. Spatially-resolved maps reveal that in regions associated with winds, the CO(4 - 3) /CO(2 - 1) flux ratio significantly exceeds the upper limit of 4 for optically thick gas. It frequently takes values between 5 and 11, and it occasionally further approaches the upper limit of 16 for optically thin gas. Excitation temperatures of 30-100 K are common for the molecules in these regions. If all of the outflowing molecular gas is optically thin, at 30-50 K, then its mass is 2 × 10&lt;SUP&gt;6&lt;/SUP&gt; M&lt;SUB&gt;⊙&lt;/SUB&gt;. This lower mass limit is an order of magnitude below the mass derived from the CO(2 - 1) flux in the case of optically thick gas. Molecular winds can thus be less massive, but more easily detectable at high z than they were previously thought to be.</style></abstract></record></records></xml>