A mid infrared study of low-luminosity AGNs with WISE

 

R. Coziol,¹ J. P. Torres-Papaqui,¹ I. Plauchu-Frayn,² H. Andernach,¹ D. M. Neri-Larios,³ R. A. Ortega-Minakata,¹ and J. M. Islas-Islas¹

 

¹ Departamento de Astronomía, Universidad de Guanajuato, Apdo. Postal 144, 36000, Guanajuato, Gto, México (heinz, rcoziol, jmislas, rene, papaqui@astro.ugto.mx).

² Instituto de Astronomía, Universidad Nacional Autónoma de México, Campus Ensenada, Apdo. Postal 877, Ensenada, B.C., México (ilse@astrosen.unam.mx).

³ School of Physics, The University of Melbourne, Parkville, Vic. 3010, Australia (danielnl@student.unimelb.edu.au).

 

Received 2014 January 26.
Accepted 2014 May 16.

 

RESUMEN

Utilizando datos en el infrarrojo medio (MIR) del Wide-field Infrared Survey Explorer (WISE), mostramos que las galaxias AGNs de baja luminosidad (LLAGNs) presentan colores en el infrarrojo medio (MIR) significamente diferentes de los de las estrellas post-rama asintótica gigante (PAGBs). Esto se debe a una diferencia en la distribución de energía espectral (SED), pues los LLAGNs muestran una componente plana debida a un AGN. Congruentemente con esta interpretación, mostramos que en un diagrama color-color los LINERs y las Seyfert 2s siguen una ley de potencia con colores específicos que permiten distinguir unas de las otras, y de las galaxias con formación estelar, en base a sus diferentes niveles de formación reciente de estrellas. Basado en estos resultados, presentamos un nuevo diagrama de diagnóstico en el MIR que confirma la clasificación obtenida en el óptico a partir de diagramas de diagnóstico estándar, e identifican claramente los LINERs y LLAGNs como verdaderos AGNs.

 

ABSTRACT

Using data from the Wide-field Infrared Survey Explorer (WISE) we show that the mid infrared (MIR) colors of low-luminosity AGNs (LLAGNs) are significantly different from those of post-asymptotic giant branch stars (PAGBs). This is due to a difference in the spectral energy distribution (SEDs), the LLAGNs showing a flat component due to an AGN. Consistent with this interpretation we show that in a MIR color-color diagram the LINERs and the Seyfert 2s follow a power law with specific colors that allow to distinguish them from each other, and from star forming galaxies, according to their present level of star formation. Based on this result we present a new diagnostic diagram in the MIR that confirms the classification obtained in the optical using standard diagnostic diagrams, clearly identifying LINERs and LLAGNs as genuine AGNs.

Key Words: galaxies: active — infrared: galaxies.

 

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ACKNOWLEDGMENTS

We thank an anonymous referee for making comments and suggestions that helped us to improve the quality of our study and its presentation. J.P. T.-P. acknowledges PROMEP for grant 103.5-10-4684, and DAIP for grant DAIP-Ugto (0432/14). This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France: (http://vizier.u-strasbg.fr/). This publication made use of data products from the Wide-field Infrared Survey Explorer (WISE), which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. The funding for Sloan Digital Sky Survey (SDSS) has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The full acknowledgement can be found here: http://www.sdss3.org/.

 

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