J/A+A/640/A104ivo://CDS.VizieR/J/A+A/640/A104doi:10.26093/cds/vizier.36400104CDSAalto S.Falstad N.Muller S.Wada K.Gallagher J.S.Koenig S.,Sakamoto K.Vlemmings W.Ceccobello C.Dasyra K.Combes F.,Garcia-Burillo S.Oya Y.Martin S.van der Werf P.Evans A.S.,Kotilainen J.2020-11-26T11:24:02Z2020-08-21T07:36:08ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.fractive-galactic-nucleiradio-astronomySubmillimetre and millimetre line and continuum observations are important in probing the morphology, column density, and dynamics of the molecular gas and dust around obscured active galactic nuclei (AGNs) and their mechanical feedback. With very high resolution (0.02"x0.03" (2x3pc)) ALMA 345GHz observations of CO 3-2, HCO^+^ 4-3, vibrationally excited HCN 4-3 {nu}_2_=1f , and continuum we have studied the remarkable, extremely radio-quiet, molecular jet and wind of the lenticular galaxy NGC 1377. The outflow structure is resolved, revealing a 150pc long, clumpy, high-velocity (600km/s), collimated molecular jet where the molecular emission is emerging from the spine of the jet with an average diameter of 3-7pc. The jet widens to 10-15pc about 25pc from the centre, which is possibly due to jet-wind interactions. A narrow-angle (50-70), misaligned and rotating molecular wind surrounds the jet, and both are enveloped by a larger-scale CO-emitting structure at near-systemic velocity. The jet and narrow wind have steep radial gas excitation gradients and appear turbulent with high gas dispersion (>40km/s). The jet shows velocity reversals that we propose are caused by precession, or more episodic directional changes. We discuss the mechanisms powering the outflow, and we find that an important process for the molecular jet and narrow wind is likely magneto-centrifugal driving. In contrast, the large-scale CO-envelope may be a slow wind, or cocoon that stems from jet-wind interactions. An asymmetric, nuclear r~2pc dust structure with a high inferred molecular column density N(H_2_)=1.8x10^24^cm^-2^ is detected in continuum and also shows compact emission from vibrationally excited HCN. The nuclear dust emission is hot (Td>180K) and its luminosity is likely powered by a buried AGN. The lopsided structure appears to be a warped disk, which is responsible for a significant part of the nuclear obscuration and possibly formed as a result of uneven gas inflows. The dynamical mass inside r=1.4pc is estimated to 9^+2^_3_x10^6^M_{sun}_, implying that the supermassive black hole (SMBH) has a high mass with respect to the stellar velocity dispersion of NGC 1377. We suggest that the SMBH of NGC 1377 is currently in a state of moderate growth, at the end of a more intense phase of accretion and also evolving from a state of more extreme nuclear obscuration. The nuclear growth may be fuelled by low-angular momentum gas inflowing from the gas ejected in the molecular jet and wind. Such a feedback-loop of cyclic outflows and central accretion could explain why there is still a significant reservoir of molecular gas in this ageing, lenticular galaxy. A feedback-loop would be an effective process in growing the nuclear SMBH and thus would constitute an important phase in the evolution of NGC 1377. 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