Enhanced UV radiation and dense clumps in the molecular outflow of Mrk 231
Journal article, 2020

We present interferometric observations of the CN(1-0) line emission in Mrk 231 and combine them with previous observations of CO and other H-2 gas tracers to study the physical properties of the massive molecular outflow. We find a strong boost of the CN/CO(1-0) line luminosity ratio in the outflow of Mrk 231, which is unprecedented compared to any other known Galactic or extragalactic astronomical source. For the dense gas phase in the outflow traced by the HCN and CN emissions, we infer X-CN equivalent to [CN]/[H-2]> X-HCN by at least a factor of three, with H-2 gas densities of n(H2) similar to 10(5-6)& x2006;cm(-3). In addition, we resolve for the first time narrow spectral features in the HCN(1-0) and HCO+(1-0) high-velocity line wings tracing the dense phase of the outflow. The velocity dispersions of these spectral features, sigma(v) similar to 7-20 km s(-1), are consistent with those of massive extragalactic giant molecular clouds detected in nearby starburst nuclei. The H-2 gas masses inferred from the HCN data are quite high, M-mol similar to 0.3-5 x 10(8) M-circle dot. Our results suggest that massive complexes of denser molecular gas survive embedded into the more diffuse H-2 phase of the outflow, and that the chemistry of these outflowing dense clouds is strongly affected by UV radiation.

galaxies: evolution

galaxies: individual: Mrk 231

galaxies: interactions

submillimeter: galaxies

galaxies: ISM

galaxies: active


Claudia Cicone

University of Oslo

Osservatorio Astronomico di Brera

Roberto Maiolino

University of Cambridge

Susanne Aalto

Chalmers, Space, Earth and Environment, Astronomy and Plasmaphysics

Sebastien Muller

Chalmers, Space, Earth and Environment, Onsala Space Observatory, Observation Support

Chiara Feruglio

INAF Osservatorio Astron Trieste

Astronomy and Astrophysics

0004-6361 (ISSN) 1432-0746 (eISSN)

Vol. 633 A163

Subject Categories

Astronomy, Astrophysics and Cosmology



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