Hatziminaoglou, E.; Fritz, J.; Franceschini, A.; Afonso-Luis, A.; Hernán-Caballero, A.; Pérez-Fournon, I.; Serjeant, Stephen; Lonsdale, C.; Oliver, S.; Rowan-Robinson, M.; Shupe, D.; Smith, H. E. and Surace, J.
PDF (Version of Record)
- Requires a PDF viewer such as GSview, Xpdf or Adobe Acrobat Reader
|DOI (Digital Object Identifier) Link:||http://doi.org/10.1111/j.1365-2966.2008.13119.x|
|Google Scholar:||Look up in Google Scholar|
We derive the properties of dusty tori in active galactic nuclei from the comparison of observed spectral energy distributions (SEDs) of SDSS quasars and a precomputed grid of torus models. The observed SEDs comprise SDSS photometry, Two-Micron All-Sky Survey J, H and K data, whenever available, and mid-infrared (mid-IR) data from the Spitzer Wide-area InfraRed Extragalactic Survey. The adopted model is that of Fritz, Franceschini & Hatziminaoglou. The fit is performed by standard χ2-minimization; the model, however, can be a multicomponent comprising a stellar and a starburst component, whenever necessary. Models with low equatorial optical depth, τ9.7, were allowed as well as ‘traditional’ models with τ9.7≥ 1.0, corresponding to AV≥ 22 and the results were compared. Fits using high optical depth tori models only produced dust more compactly distributed than in the configuration where all τ9.7 models were permitted. Tori with decreasing dust density with the distance from the centre were favoured while there was no clear preference for models with or without angular variation of the dust density. The computed outer radii of the tori are of some tens of parsecs large but can reach, in a few cases, a few hundreds of parsecs. The mass of dust, MDust, and IR luminosity, LIR, integrated in the wavelength range between 1 and 1000 μm, do not show significant variations with redshift, once the observational biases are taken into account. Objects with 70-μm detections, representing 25 per cent of the sample, are studied separately and the starburst contribution (whenever present) to the IR luminosity can reach, in the most extreme but very few cases, 80 per cent.
|Item Type:||Journal Article|
|Copyright Holders:||2008 The Authors, 2008 RAS (journal compilation)|
|Extra Information:||The definitive version is available at www.blackwell-synergy.com|
|Keywords:||galaxies: active; quasars: general; galaxies: starburst; infrared: general|
|Academic Unit/Department:||Science > Physical Sciences
|Interdisciplinary Research Centre:||Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR)|
|Depositing User:||Tracy Bartlett|
|Date Deposited:||15 Dec 2010 12:15|
|Last Modified:||24 Feb 2016 03:00|
|Share this page:|
Download history for this item
These details should be considered as only a guide to the number of downloads performed manually. Algorithmic methods have been applied in an attempt to remove automated downloads from the displayed statistics but no guarantee can be made as to the accuracy of the figures.