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Kambiz Fathi ; Takuma Izumi ; Alessandro Romeo (Institutionen för rymd- och geovetenskap, Radioastronomi och astrofysik) ; Sergio Martín ; Masatoshi Imanishi ; Evanthia Hatziminaoglou ; Susanne Aalto (Institutionen för rymd- och geovetenskap, Radioastronomi och astrofysik) ; Daniel Espada ; Kotaro Kohno ; Melanie Krips ; Satoki Matsushita ; David S Meier ; Naomasa Nakai ; Yuichi Terashima
Astrophysical Journal (0004-637X). Vol. 806 (2015), 2, p. L34 (6pp).
[Artikel, refereegranskad vetenskaplig]

We present an unprecedented measurement of the disk stability and local instability scales in the luminous infrared Seyfert 1 host, NGC 7469, based on ALMA observations of dense gas tracers and with a synthesized beam of 165 × 132 pc. While we confirm that non-circular motions are not significant in redistributing the dense interstellar gas in this galaxy, we find compelling evidence that the dense gas is a suitable tracer for studying the origin of its intensely high-mass star-forming ringlike structure. Our derived disk stability parameter $\mathcal{Q}$ accounts for a thick disk structure, and its value falls below unity at the radii in which intense star formation is found. Furthermore, we derive the characteristic instability scale ${\lambda }_{c}$ and find a striking agreement between our measured scale of ~180 pc and the typical sizes of individual complexes of young and massive star clusters seen in high-resolution images.

Denna post skapades 2015-07-06. Senast ändrad 2016-01-25.
CPL Pubid: 219485


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