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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



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ID: 660693.0, MPI für Astronomie / Publikationen_mpia
Physical properties of dense molecular gas in centres of Seyfert galaxies
Authors:Sani, E.; Davies, R. I.; Sternberg, A.; Graciá-Carpio, J.; Hicks, E. K. S.; Krips, M.; Tacconi, L. J.; Genzel, R.; Vollmer, B.; Schinnerer, E.; García-Burillo, S.; Usero, A.; Orban de Xivry, G.
Date of Publication (YYYY-MM-DD):2012
Title of Journal:Monthly Notices of the Royal Astronomical Society
Journal Abbrev.:MNRAS
Volume:424
Issue / Number:3
Start Page:1963
End Page:1976
Review Status:not specified
Audience:Not Specified
Abstract / Description:We present new ˜1 arcsec resolution data of the dense molecular gas in the central 50-100 pc of four nearby Seyfert galaxies. Plateau de Bure Interferometer (PdBI) observations of HCN and, in two of the four sources, simultaneously HCO+ allow us to carefully constrain the dynamical state of the dense gas surrounding the active galactic nuclei (AGN). The analysis of the kinematics shows large line widths of 100-200 km s-1 full width at half-maximum (FWHM) that can only partially arise from beam smearing of the velocity gradient. The observed morphological and kinematic parameters (dimensions, major axis position angle, red and blue channel separation, and integrated line width) are well reproduced by a thick disc, where the emitting dense gas has a large intrinsic dispersion (20-40 km s-1), implying that it exists at significant scale heights (25-30 per cent of the disc radius). To put the observed kinematics in the context of the starburst and AGN evolution, we estimate the Toomre Q parameter. We find this is always greater than the critical value, i.e. Q is above the limit such that the gas is stable against rapid star formation. This is supported by the lack of direct evidence, in these four Seyfert galaxies, for on-going star formation close around the AGN. Instead, any current star formation tends to be located in a circumnuclear ring. We conclude that the physical conditions are indeed not suited to star formation within the central ˜100 pc.
Free Keywords:galaxies: individual: NGC 2273; galaxies: individual: NGC 3227; galaxies: individual: NGC 4051; galaxies: individual: NGC 6951; galaxies: kinematics and dynamics; galaxies: Seyfert
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:URL:http://cdsads.u-strasbg.fr/abs/2012MNRAS.424.1963S [ID No:1]
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