Central kiloparsec of NGC 1326 observed with SINFONI

• Published in: Astronomy and astrophysics (Berlin) Vol. 638
• Main Authors: Fazeli, Nastaran, Busch, Gerold, Eckart, Andreas, Combes, Françoise, Misquitta, Persis, Straubmeier, Christian
• Format: Journal Article
• Language: English
• Published: Heidelberg EDP Sciences 01.06.2020
• Subjects: Elongated structure; Emission analysis; Field of view; Galactic evolution; Galactic nuclei; Galactic rotation; Galaxies; Molecular gases; Morphology; Radio telescopes; Star formation; Stellar rotation; Supermassive black holes; Toruses; Velocity distribution; Very Large Telescope
• ISSN: 0004-6361; 1432-0746
• DOI: 10.1051/0004-6361/201936451

Gas inflow processes in the vicinity of galactic nuclei play a crucial role in galaxy evolution and supermassive black hole growth. Exploring the central kiloparsec of galaxies is essential to shed more light on this subject. We present near-infrared H- and K-band results of the nuclear region of the nearby galaxy NGC 1326, observed with the integral-field spectrograph SINFONI mounted on the Very Large Telescope. The field of view covers 9″ × 9″ (650 × 650 pc2). Our work is concentrated on excitation conditions, morphology, and stellar content. The nucleus of NGC 1326 was classified as a LINER, however in our data we observed an absence of ionised gas emission in the central r ∼ 3″. We studied the morphology by analysing the distribution of ionised and molecular gas, and thereby detected an elliptically shaped, circum-nuclear star-forming ring at a mean radius of 300 pc. We estimate the starburst regions in the ring to be young with dominating ages of < 10 Myr. The molecular gas distribution also reveals an elongated east to west central structure about 3″ in radius, where gas is excited by slow or mild shock mechanisms. We calculate the ionised gas mass of 8 × 105 M⊙ completely concentrated in the nuclear ring and the warm molecular gas mass of 187 M⊙, from which half is concentrated in the ring and the other half in the elongated central structure. The stellar velocity fields show pure rotation in the plane of the galaxy. The gas velocity fields show similar rotation in the ring, but in the central elongated H2 structure they show much higher amplitudes and indications of further deviation from the stellar rotation in the central 1″ aperture. We suggest that the central 6″ elongated H2 structure might be a fast-rotating central disc. The CO(3–2) emission observations with the Atacama Large Millimeter/submillimeter Array reveal a central 1″ torus. In the central 1″ of the H2 velocity field and residual maps, we find indications for a further decoupled structure closer to a nuclear disc, which could be identified with the torus surrounding the supermassive black hole.