FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W2979474331> ?p ?o ?g. }

• W2979474331 endingPage "11" @default.
• W2979474331 startingPage "11" @default.
• W2979474331 abstract "This is the second in a series of papers devoted to exploring a set of six dusty models of active galactic nuclei (AGN) with available spectral energy distributions. These models are the smooth torus by Fritz et al., the clumpy torus by Nenkova et al., the clumpy torus by Hönig & Kishimoto, the two-phase torus by Siebenmorgen et al., the two-phase torus by Stalevski et al., and the wind model by Hönig & Kishimoto. The first paper explores discrimination among models and the parameter restriction using synthetic spectra. Here we perform spectral fitting of a sample of 110 AGN drawn from the Swift/BAT survey with Spitzer/IRS spectroscopic data. The aim is to explore which is the model that describes better the data and the resulting parameters. The clumpy wind–disk model by Hönig & Kishimoto provides good fits for ∼50% of the sample, and the clumpy torus model by Nenkova et al. is good at describing ∼30% of the objects. The wind–disk model by Hönig & Kishimoto is better for reproducing the mid-infrared spectra of type 1 Seyferts (with 60% of the type 1 Seyferts well reproduced by this model compared to the 10% well represented by the clumpy torus model by Nenkova et al.), while type 2 Seyferts are equally fitted by both models (roughly 40% of the type 2 Seyferts). Large residuals are found irrespective of the model used, indicating that the AGN dust continuum emission is more complex than predicted by the models or that the parameter space is not well sampled. We found that all the resulting parameters for our AGN sample are roughly constrained to 10%–20% of the parameter space. Contrary to what is generally assumed, the derived outer radius of the torus is smaller (reaching up to a factor of ∼5 smaller for 10 pc tori) for the smooth torus by Fritz et al. and the two-phase torus by Stalevski et al. than the one derived from the clumpy torus by Nenkova et al. Covering factors and line-of-sight viewing angles strongly depend on the model used. The total dust mass is the most robust derived quantity, giving equivalent results for four of these models." @default.
• W2979474331 created "2019-10-18" @default.
• W2979474331 creator A5015399991 @default.
• W2979474331 creator A5017557147 @default.
• W2979474331 creator A5019361950 @default.
• W2979474331 creator A5022527645 @default.
• W2979474331 creator A5026042385 @default.
• W2979474331 creator A5040803702 @default.
• W2979474331 creator A5048608289 @default.
• W2979474331 creator A5060303861 @default.
• W2979474331 creator A5061277127 @default.
• W2979474331 creator A5068379591 @default.
• W2979474331 creator A5076930537 @default.
• W2979474331 creator A5090307711 @default.
• W2979474331 date "2019-10-08" @default.
• W2979474331 modified "2023-10-08" @default.
• W2979474331 title "Exploring the Mid-infrared SEDs of Six AGN Dusty Torus Models. II. The Data" @default.
• W2979474331 cites W1492972489 @default.
• W2979474331 cites W1894812898 @default.
• W2979474331 cites W1968549171 @default.
• W2979474331 cites W1975582108 @default.
• W2979474331 cites W1978188520 @default.
• W2979474331 cites W1986399271 @default.
• W2979474331 cites W1994671833 @default.
• W2979474331 cites W1995204235 @default.
• W2979474331 cites W1998392974 @default.
• W2979474331 cites W2003637061 @default.
• W2979474331 cites W2012096146 @default.
• W2979474331 cites W2024235708 @default.
• W2979474331 cites W2025474131 @default.
• W2979474331 cites W2033756463 @default.
• W2979474331 cites W2048316219 @default.
• W2979474331 cites W2086105458 @default.
• W2979474331 cites W2089167229 @default.
• W2979474331 cites W2117914127 @default.
• W2979474331 cites W2121569158 @default.
• W2979474331 cites W2125383073 @default.
• W2979474331 cites W2150973413 @default.
• W2979474331 cites W2153714254 @default.
• W2979474331 cites W2153931839 @default.
• W2979474331 cites W2244839445 @default.
• W2979474331 cites W2285880218 @default.
• W2979474331 cites W2500423254 @default.
• W2979474331 cites W2505344592 @default.
• W2979474331 cites W2525022873 @default.
• W2979474331 cites W2561172536 @default.
• W2979474331 cites W2586892223 @default.
• W2979474331 cites W2621385311 @default.
• W2979474331 cites W2758268742 @default.
• W2979474331 cites W2891633603 @default.
• W2979474331 cites W2908920652 @default.
• W2979474331 cites W2935486123 @default.
• W2979474331 cites W2949364460 @default.
• W2979474331 cites W2964087321 @default.
• W2979474331 cites W2979944347 @default.
• W2979474331 cites W3033697379 @default.
• W2979474331 cites W3098198236 @default.
• W2979474331 cites W3099428329 @default.
• W2979474331 cites W3099432868 @default.
• W2979474331 cites W3099533589 @default.
• W2979474331 cites W3099541415 @default.
• W2979474331 cites W3099723478 @default.
• W2979474331 cites W3101365736 @default.
• W2979474331 cites W3102993162 @default.
• W2979474331 cites W3104045735 @default.
• W2979474331 cites W3104964765 @default.
• W2979474331 cites W3105249828 @default.
• W2979474331 cites W3105302391 @default.
• W2979474331 cites W3105466767 @default.
• W2979474331 cites W3106161605 @default.
• W2979474331 cites W3106453265 @default.
• W2979474331 cites W3106461171 @default.
• W2979474331 cites W3106525495 @default.
• W2979474331 cites W3121670601 @default.
• W2979474331 cites W3124137174 @default.
• W2979474331 cites W3124194601 @default.
• W2979474331 cites W3124221423 @default.
• W2979474331 cites W3125598333 @default.
• W2979474331 cites W4294950512 @default.
• W2979474331 cites W4295695032 @default.
• W2979474331 cites W4300793255 @default.
• W2979474331 cites W4301261148 @default.
• W2979474331 doi "https://doi.org/10.3847/1538-4357/ab3e4f" @default.
• W2979474331 hasPublicationYear "2019" @default.
• W2979474331 type Work @default.
• W2979474331 sameAs 2979474331 @default.
• W2979474331 citedByCount "27" @default.
• W2979474331 countsByYear W29794743312019 @default.
• W2979474331 countsByYear W29794743312020 @default.
• W2979474331 countsByYear W29794743312021 @default.
• W2979474331 countsByYear W29794743312022 @default.
• W2979474331 countsByYear W29794743312023 @default.
• W2979474331 crossrefType "journal-article" @default.
• W2979474331 hasAuthorship W2979474331A5015399991 @default.
• W2979474331 hasAuthorship W2979474331A5017557147 @default.
• W2979474331 hasAuthorship W2979474331A5019361950 @default.
• W2979474331 hasAuthorship W2979474331A5022527645 @default.
• W2979474331 hasAuthorship W2979474331A5026042385 @default.

• next