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A survey of HC3N in extragalactic sources. Is HC3N a tracer of activity in ULIRGs?

Johan Lindberg ; Susanne Aalto (Institutionen för rymd- och geovetenskap, Radioastronomi och astrofysik) ; Francesco Costagliola (Institutionen för rymd- och geovetenskap, Radioastronomi och astrofysik) ; J. P. Perez-Beaupuits ; R. Monje ; Sebastien Muller (Institutionen för rymd- och geovetenskap, Onsala rymdobservatorium)
Astronomy and Astrophysics (0004-6361). Vol. 527 (2011),
[Artikel, refereegranskad vetenskaplig]

Context. HC3N is a molecule that is mainly associated with Galactic star-forming regions, but it has also been detected in extragalactic environments. Aims. To present the first extragalactic survey of HC3N, when combining earlier data from the literature with six new single-dish detections, and to compare HC3N with other molecular tracers (HCN, HNC), as well as other properties (silicate absorption strength, IR flux density ratios, C II flux, and megamaser activity). Methods. We present mm IRAM 30 m, OSO 20 m, and SEST observations of HC3N rotational lines (mainly the J = 10-9 transition) and of the J = 1-0 transitions of HCN and HNC. Our combined HC3N data account for 13 galaxies (excluding the upper limits reported for the non-detections), while we have HCN and HNC data for more than 20 galaxies. Results. A preliminary definition "HC3N-luminous galaxy" is made based upon the HC3N/HCN ratio. Most (similar to 80%) HC3N-luminous galaxies seem to be deeply obscured galaxies and (U) LIRGs. A majority (similar to 60% or more) of the HC3N-luminous galaxies in the sample present OH mega- or strong kilomaser activity. A possible explanation is that both HC3N and OH megamasers need warm dust for their excitation. Alternatively, the dust that excites the OH megamaser offers protection against UV destruction of HC3N. A high silicate absorption strength is also found in several of the HC3N-luminous objects, which may help the HC3N to survive. Finally, we find that a high HC3N/HCN ratio is related to a high dust temperature and a low C II flux.

Nyckelord: galaxies: ISM, galaxies: starburst, galaxies: active, radio lines:, galaxies, radio lines: ISM, ISM: molecules, dense molecular gas, ultraluminous infrared galaxies, nearby galaxies, star-formation, seyfert-galaxies, interstellar clouds, physical, conditions, starburst galaxies, spiral galaxies, galactic nuclei



Denna post skapades 2011-04-14. Senast ändrad 2016-04-11.
CPL Pubid: 139053

 

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