ALMA reveals optically thin, highly excited CO gas in the jet-driven winds of the galaxy IC 5063

¹ Department of Astrophysics, Astronomy & Mechanics, Faculty of Physics, National and Kapodistrian University of Athens, Panepistimiopolis Zografou, 15784, Greece
e-mail: kdasyra@phys.uoa.gr
² LERMA, Observatoire de Paris, CNRS, UPMC, PSL Univ., Sorbonne Univ., 75014 Paris, France
³ Collège de France, 11 place Marcelin Berthelot, 75005 Paris, France
⁴ ASTRON, The Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA Dwingeloo, The Netherlands
⁵ Kapteyn Astronomical Institute, University of Groningen, Postbus 800, 9700 AV Groningen, The Netherlands
⁶ Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands

Received: 12 September 2016
Accepted: 14 October 2016

Abstract

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 × 10⁶ M_⊙. 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.