Volume 597, January 2017
|Number of page(s)||14|
|Published online||11 January 2017|
Inflowing gas onto a compact obscured nucleus in Arp 299A⋆
Herschel spectroscopic studies of H2O and OH
1 Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, 439 92 Onsala, Sweden
2 Universidad de Alcalá de Henares, Departamento de Física, Campus Universitario, 28871 Alcalá de Henares, Madrid, Spain
3 Naval Research Laboratory, Remote Sensing Division, 4555 Overlook Ave SW, Washington, DC 20375, USA
Received: 3 June 2016
Accepted: 2 November 2016
Aims. We probe the physical conditions in the core of Arp 299A and try to put constraints on the nature of its nuclear power source.
Methods. We used Herschel Space Observatory far-infrared and submillimeter observations of H2O and OH rotational lines in Arp 299A to create a multi-component model of the galaxy. In doing this, we employed a spherically symmetric radiative transfer code.
Results. Nine H2O lines in absorption and eight in emission, as well as four OH doublets in absorption and one in emission, are detected in Arp 299A. No lines of the 18O isotopologues, which have been seen in compact obscured nuclei of other galaxies, are detected. The absorption in the ground state OH 2Π3/2-2Π3/2(5/2)+-(3/2)- doublet at 119 μm is found redshifted by ~ 175 km s-1 compared with other OH and H2O lines, suggesting a low excitation inflow. We find that at least two components are required in order to account for the excited molecular line spectrum. The inner component has a radius of 20−25 pc, a very high infrared surface brightness (≳3 × 1013L⊙kpc-2), warm dust (Td > 90 K), and a large H2 column density (NH2 > 1024 cm-2). The modeling also indicates high nuclear H2O (1−5 × 10-6) and OH (0.5−5 × 10-5) abundances relative to H nuclei. The outer component is larger (50−100 pc) with slightly cooler dust (70−90 K) and molecular abundances that are approximately one order of magnitude lower. In addition to the two components that account for the excited OH and H2O lines, we require a much more extended inflowing component to account for the OH 2Π3/2-2Π3/2(5/2)+-(3/2)- doublet at 119 μm.
Conclusions. The Compton-thick nature of the core makes it difficult to determine the nature of the buried power source, but the high surface brightness indicates that it is an active galactic nucleus and/or a dense nuclear starburst. Our results are consistent with a composite source. The high OH/H2O ratio in the nucleus indicates that ion-neutral chemistry induced by X-rays or cosmic-rays is important. Finally we find a lower limit to the 16O/18O ratio of 400 in the nuclear region, possibly indicating that the nuclear starburst is in an early evolutionary stage, or that it is fed through a molecular inflow of, at most, solar metallicity.
Key words: ISM: molecules / galaxies: ISM / galaxies: individual: Arp 299 / line: formation / infrared: galaxies / submillimeter: galaxies
© ESO, 2017
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