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Detection of HCN, H...
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Aalto, Susanne,1964Chalmers tekniska högskola,Chalmers University of Technology
(author)
Detection of HCN, HCO+, and HNC in the Mrk 231 molecular outflow. Dense molecular gas in the AGN wind
- Article/chapterEnglish2012
Publisher, publication year, extent ...
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2012-01-06
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EDP Sciences,2012
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electronicrdacarrier
Numbers
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LIBRIS-ID:oai:research.chalmers.se:b81d3ce0-904f-4e7a-9686-38765f432621
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https://research.chalmers.se/publication/156376URI
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https://doi.org/10.1051/0004-6361/201117919DOI
Supplementary language notes
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Language:English
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Summary in:English
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Subject category:art swepub-publicationtype
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Subject category:ref swepub-contenttype
Notes
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We obtained high-resolution (1.''55 × 1.''28) observations of HCN, HCO+, HNC 1-0 and HC3N 10-9 of the ultraluminous galaxy (ULIRG) Mrk 231 with the IRAM Plateau de Bure Interferometer.Results: We detect luminous emission from HCN, HCO+ and HNC 1-0 in the QSO ULIRG Mrk 231. All three lines show broad line wings - which are particularly prominent for HCN. Velocities are found to be similar ( ≈ ± 750 km s-1) to those found for CO 1-0. This is the first time bright HCN, HCO+ and HNC emission has been detected in a large-scale galactic outflow. We find that both the blue- and red-shifted line wings are spatially extended by at least 0.''75 (>700 pc) in a north-south direction. The line wings are brighter (relative to the line center intensity) in HCN than in CO 1-0 and line ratios suggest that the molecular outflow consists of dense (n > 104 cm-3) and clumpy gas with a high HCN abundance X(HCN) > 10-8. These properties are consistent with the molecular gas being compressed and fragmented by shocks in the outflow. Alternatively, HCN is instead pumped by mid-IR continuum, but we propose that this effect is not strong for the spatially extended outflowing gas. In addition, we find that the rotation of the main disk, in east-west direction, is also evident in the HCN, HCO+ and HNC line emission. An unexpectedly bright HC3N 10-9 line is detected inside the central 400 pc of Mrk 231. This HC3N emission may emerge from a shielded, dust-enshrouded region within the inner 40-50 pc where the gas is heated to high temperatures (200-300 K) by the AGN.
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Burillo, S. G.Observatorio Astronómico Nacional (OAN),Spanish National Observatory (OAN)
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Muller, Sebastien,1976Chalmers tekniska högskola,Chalmers University of Technology(Swepub:cth)mullers
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Winters, J.M.Institut de Radioastronomie Millimétrique (IRAM)
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van der Werf, P.Universiteit Leiden (UL),Leiden University (UL)
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Henkel, C.Max Planck Gesellschaft zur Förderung der Wissenschaften e.V. (MPG),Max Planck Society for the Advancement of Science (MPG),King Abdulaziz University
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Costagliola, Francesco,1981Chalmers tekniska högskola,Chalmers University of Technology(Swepub:cth)costagli
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Neri, R.Institut de Radioastronomie Millimétrique (IRAM)
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Chalmers tekniska högskolaObservatorio Astronómico Nacional (OAN)
(creator_code:org_t)
Related titles
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In:Astronomy and Astrophysics: EDP Sciences537, s. 44-510004-63611432-0746
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