dc.contributor.author | Thean, Andy | en_US |
dc.contributor.author | Pedlar, Alan | en_US |
dc.contributor.author | Kukula, Marek | en_US |
dc.contributor.author | Baum, Stefi | en_US |
dc.contributor.author | O'Dea, Christopher | en_US |
dc.date.accessioned | 2006-05-08T22:00:26Z | en_US |
dc.date.available | 2006-05-08T22:00:26Z | en_US |
dc.date.issued | 2001-08 | en_US |
dc.identifier.citation | Monthly Notices of the Royal Astronomical Society 325 (2001) 737 | en_US |
dc.identifier.issn | 1365-2966 | en_US |
dc.identifier.uri | http://hdl.handle.net/1850/1759 | en_US |
dc.description | RIT community members may access full-text via RIT Libraries licensed databases: http://library.rit.edu/databases/ | |
dc.description.abstract | We discuss the properties of compact nuclear radio components in Seyfert galaxies from the extended 12 µm AGN sample of Rush et al. (1993). Our main results can be summarised as follows.
Type 1 and type 2 Seyferts produce compact radio components which are indistinguishable in strength and aspect, indicating that their central engines are alike as proposed by the unification model. Infrared IRAS fluxes are more closely correlated with low–resolution radio fluxes than high–resolution radio fluxes, suggesting that they are dominated by kiloparsec–scale, extra–nuclear emission regions; extra–nuclear emission may be stronger in type 2 Seyferts. Early–type Seyfert galaxies tend to have stronger nuclear radio emission than late–type Seyfert galaxies. V–shaped extended emission–line regions, indicative of ‘ionisation cones’, are usually found in sources with large, collimated radio outflows. Hidden broad lines are most likely to be found in sources with powerful nuclear radio sources. Type 1 and type 2 Seyferts selected by their IRAS 12 µm flux densities have well matched properties. | en_US |
dc.description.sponsorship | AHCT would like to acknowledge the receipt of a studentship from the Particle Physics and Astronomy Re-search Council and a visit funded by the STScI visitor program. Part of this research was supported by the European Commission, TMR Programme, Research Network Contract ERBFMRXCT96-0034 “CERES”. We have made use of NASA’s Astrophysics Data System Abstract Service,
the NASA/IPAC Extragalactic database (NED), which is operated by the Jet Propulsion Laboratory, and ASURV Rev 1.1 (Lavalley, Isobe & Feigelson 1992), which implements
the methods presented in Feigelson & Nelson (1985) and Isobe, Feigelson & Nelson (1986). We thank the referee, R. Antonucci, for helpful comments. | en_US |
dc.format.extent | 757132 bytes | en_US |
dc.format.mimetype | application/pdf | en_US |
dc.language.iso | en_US | en_US |
dc.publisher | Blackwell Publishing | en_US |
dc.relation.ispartofseries | vol. 325 | en_US |
dc.relation.ispartofseries | no. 2 | en_US |
dc.relation.ispartofseries | p. 737 | en_US |
dc.subject | Galaxies-active | en_US |
dc.subject | Galaxies-Seyfert | en_US |
dc.subject | Galaxies-statistics | en_US |
dc.subject | Infrared-galaxies | en_US |
dc.subject | Radio continuum-galaxies | en_US |
dc.title | High-resolution radio observations of Seyfert galaxies in the extended 12-micron sample - II. The Properties of compact radio components | en_US |
dc.type | Article | en_US |
dc.identifier.url | http://dx.doi.org/10.1046/j.1365-8711.2001.04485.x | |