Submillimetre and millimetre observations are important in probing theproperties of the molecular gas and dust around obscured active galactic nuclei(AGNs) and their feedback. With very high-resolution (0."02x0."03 (2x3 pc))ALMA 345 GHz observations of CO 3-2, HCO$^+$ 4-3, HCN 4-3 $\nu_2$=1$f$, andcontinuum we have studied the molecular outflow and nucleus of the extremelyradio-quiet lenticular galaxy NGC1377. The outflow is resolved, revealing a 150pc long, clumpy, high-velocity, collimated molecular jet. The molecularemission is emerging from the spine of the jet with an average diameter of 3-7pc. A narrow-angle, rotating molecular wind surrounds the jet and is envelopedby a larger-scale, slower CO-emitting structure. The jet and narrow wind areturbulent ($\sigma>$40 kms$^{-1}$) and have steep radial gas excitationgradients. The jet shows velocity reversals that we propose are caused byprecession, or episodic directional changes. We suggest that an importantprocess powering the outflow is magneto-centrifugal driving. In contrast, thelarge-scale CO-envelope may be a slow wind, or cocoon that stems from jet-windinteractions. An asymmetric, nuclear r$\sim$2 pc and hot (>180 K) duststructure with a high molecular column density, N(H$_2$)$\sim1.8 \times10^{24}$ cm$^{-2}$, is detected in continuum and vibrationally excited HCN. Itsluminosity is likely powered by a buried AGN. The mass of the supermassiveblack hole (SMBH) is estimated to $\sim9\times10^6$ M$_\odot$ and the SMBH ofNGC1377 appears to be at the end of an intense phase of accretion. The nucleargrowth may be fuelled by low-angular momentum gas inflowing from gas ejected inthe molecular jet and wind. Such a feedback-loop of cyclic accretion andoutflows would be an effective process in growing the nuclear SMBH. This resultinvites new questions as to SMBH growth processes in obscured, dusty galaxies.

The majority of galaxies with current star-formation rates (SFRs), SFRo >=10^-3 Msun/yr, in the Local Cosmological Volume where observations should bereliable, have the property that their observed SFRo is larger than theiraverage star formation rate. This is in tension with the evolution of galaxiesdescribed by delayed-tau models, according to which the opposite would beexpected. The tension is apparent in that local galaxies imply the starformation timescale tau approx 6.7 Gyr, much longer than the 3.5-4.5 Gyrobtained using an empirically determined main sequence at several redshifts.Using models where the SFR is a power law in time of the form propto (t -t1)^eta for t1 = 1.8 Gyr (with no stars forming prior to t1) implies that eta =0.18 +- 0.03. This suggested near-constancy of a galaxy's SFR over time raisesnon-trivial problems for the evolution and formation time of galaxies, but isbroadly consistent with the observed decreasing main sequence with increasingage of the Universe.