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Title:
Spectroscopy and photometric flux correlations for a sample of AGNs in the range of 4 ×10^3-25 ×10^4Å
Authors:
Higuera G., M. A.; Rodríguez-Ardila, A.; Tejeiro, J. M.
Affiliation:
AA(Observatorio Astronómico Nacional, Universidad Nacional, Bogotá, Colombia (mahiguerag@unal.edu.co).)
Publication:
XI IAU Regional Latin American Meeting of Astronomy (Eds. L. Infante & M. Rubio) Revista Mexicana de Astronomía y Astrofísica (Serie de Conferencias) Vol. 26, pp. 203 (RMxAC Homepage)
Publication Date:
06/2006
Origin:
RMXAA
Abstract Copyright:
(C) 2006; Instituto de Astronomía, Universidad Nacional Autónoma de México
Bibliographic Code:
2006RMxAC..26..203H

Abstract

The Active Galactic Nuclei (AGN) unified theory says that the primary role of a dusty torus around a central AGN is to hide the central engine. Nowdays based on near-infrared spectroscopy L-band spectroscopy and data collected from ground and space-based observatories is possible to explore the occurrence of starbursts in the dusty torus (Imanishi et al. 2004). Because the torus is rich in dust and molecular gas, it is a natural place to the ocurrence of starburts activity. The detection of PAH emission from the inner tens of parsecs in several Seyfert sources (Imanishi 2003; Rodríguez-Ardila et al. 2004; Peeters et al. 2004), suggest that the PAH detected emission can be directly associated to star formation episodes in the torus structure. The main goal of this work is to test the above hypothesis by means of flux correlations between the PAHs emission lines and the optical-infrared continuum using the data available in the literature. For a subset of galaxies from the CfA sample we choose continuum flux measurements at the wavelengths 0.6μm, 1.6μm, 2.1μm, 3.5μm (Alonso-Herrero et al. 2003), and 12μm, 25μm (Imanishi 2003, 2004). For our analysis, we selected the ratios F1.6/F3.3, F2.1/F3.3, F12/F3.3 and F25/F3.3 as a function of FOpt/F3.3, and F3.5/F3.3. We found a good correlation between F1.6/F.3.3 vs. FOpt/F3.3 and F2.1/F3.3 vs F3.5/F3.3, however in the other cases the correlations are not so good. The values observed show the presence of dust emission and reddening. In order to refine our study, new relationships need to be established, for example, between the 3.3μm and the other PAH emission lines with: radio emission (1.49); emission from molecular hydrogen H_2 (2.121μm), Brγ (2.165μm) and emissions in the range of soft and hard X-rays.
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