NGC 2992: The interplay between the multiphase disk, wind and radio bubbles

Maria Vittoria Zanchettin; Chiara Feruglio; Marcella Massardi; Andrea Lapi; Manuela Bischetti; Sebastiano Cantalupo; Fabrizio Fiore; Angela Bongiorno; Angela Malizia; Andrea Marinucci; Manuela Molina; Enrico Piconcelli; Francesco Tombesi; Andrea Travascio; Giulia Tozzi; Roberta Tripodi

doi:10.1051/0004-6361/202245729

paper

NGC 2992: The interplay between the multiphase disk, wind and radio bubbles

arXiv:2308.04108 · doi:10.1051/0004-6361/202245729

Abstract

We present an analysis of the gas kinematics in NGC 2992, based on VLT/MUSE, ALMA and VLA data, aimed at characterising the disk, the wind and their interplay in the cold molecular and warm ionised phases. CO(2-1) and H $α$ arise from a multiphase disk with inclination 80 deg and radii 1.5 and 1.8 kpc, respectively. We find that the velocity dispersion of the cold molecular phase is consistent with that of star forming galaxies at the same redshift, except in the inner 600 pc region, and in the region between the cone walls and the disk. This suggests that a disk-wind interaction locally boosts the gas turbulence. We detect a clumpy ionised wind distributed in two wide opening angle ionisation cones reaching scales of 7 kpc. The [O III] wind expands with velocity exceeding -1000 km/s in the inner 600 pc, a factor of 5 larger than the previously reported wind velocity. Based on spatially resolved electron density and ionisation parameter maps, we infer an ionised outflow mass of $M_{of, ion} = (3.2 \pm 0.3) \times 1 0^{7} M_{⊙}$ , and a total ionised outflow rate of $M ˙_{of, ion} = 13.5 \pm 1$ \sfr. We detected clumps of cold molecular gas located above and below the disk reaching maximum projected distances and velocities of 1.7 kpc and 200 km/s, respectively. On these scales, the wind is multiphase, with a fast ionised component and a slower molecular one, and a total mass of $M_{of, ion + mol} = 5.8 \times 1 0^{7} M_{⊙}$ , of which the molecular component carries the bulk of the mass. The dusty molecular outflowing clumps and the turbulent ionised gas are located at the edges of the radio bubbles, suggesting that the bubbles interact with the surrounding medium through shocks. We detect a dust reservoir co-spatial with the molecular disk, with a cold dust mass $M_{dust} = (4.04 \pm 0.03) \times 1 0^{6} M_{⊙}$ .

arXiv comment19 pages, 17 figures, 6 tables; Accepted by A&A

NGC 2992: The interplay between the multiphase disk, wind and radio bubbles

Abstract

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