Details

Autor(en) / Beteiligte

• Zanchettin, M. V.
• Feruglio, C.
• Bischetti, M.
• Malizia, A.
• Molina, M.
• Bongiorno, A.
• Dadina, M.
• Gruppioni, C.
• Piconcelli, E.
• Tombesi, F.
• Travascio, A.
• Fiore, F.

Titel

The IBISCO survey: I. Multiphase discs and winds in the Seyfert galaxy Markarian 509

Ist Teil von

• Astronomy and astrophysics (Berlin), 2021-11, Vol.655, p.A25

Erscheinungsjahr

2021

Link zum Volltext

Quelle

Electronic Journals Library

Beschreibungen/Notizen

• We present the analysis of the ALMA CO(2−1) emission line and the underlying 1.2 mm continuum of Mrk 509 with spatial resolution of ∼270 pc. This local Seyfert 1.5 galaxy, optically classified as a spheroid, is known to host an ionised disc, a starburst ring, and ionised gas winds on both nuclear (ultra-fast outflows) and galactic scales. From CO(2−1) we estimate a molecular gas reservoir of M H 2  = 1.7 × 10 9   M ⊙ , located within a disc of size ∼5.2 kpc, with M dyn = (2.0 ± 1.1) × 10 10 M ⊙ inclined at 44 ± 10 deg. The molecular gas fraction within the disc is μ gas  = 5%, consistent with that of local star-forming galaxies with similar stellar mass. The gas kinematics in the nuclear region within r  ∼ 700 pc, that is only marginally resolved at the current angular resolution, suggests the presence of a warped nuclear disc. Both the presence of a molecular disc with ongoing star formation in a starburst ring, and the signatures of a minor merger, are in agreement with the scenario where galaxy mergers produce gas destabilisation, feeding both star formation and AGN activity. The spatially resolved Toomre Q-parameter across the molecular disc is in the range Q gas  = 0.5 − 10, and shows that the disc is marginally unstable across the starburst ring, and stable against fragmentation at nucleus and in a lopsided ring-like structure located inside of the starburst ring. We find complex molecular gas kinematics and significant kinematics perturbations at two locations, one within 300 pc of the nucleus and one 1.4 kpc away close to the region with high Q gas , that we interpret as molecular winds with velocity v 98  = 200 − 250 km s −1 . The total molecular outflow rate is in the range 6.4−17.0 M ⊙ yr −1 for the optically thin and thick cases, respectively. The molecular wind total kinetic energy is consistent with a multiphase momentum-conserving wind driven by the AGN with Ṗ of / Ṗ rad in the range 0.06−0.5. The spatial overlap of the inner molecular wind with the ionised wind, and their similar velocity suggest a cooling sequence within a multiphase wind driven by the AGN. The second outer molecular wind component overlaps with the starburst ring, and its energy is consistent with a supernova-driven wind arising from the starburst ring.