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The nature of LINER galaxies: Ubiquitous hot old stars and rare accreting black holes



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Marino, Raffaella Anna and otros, ... (2013) The nature of LINER galaxies: Ubiquitous hot old stars and rare accreting black holes. Astronomy & Astrophysics, 558 . ISSN 0004-6361


Official URL: http://dx.doi.org/10.1051/0004-6361/201322062



Context. Galaxies, which often contain ionised gas, sometimes also exhibit a so-called low-ionisation nuclear emission line region (LINER). For 30 years, this was attributed to a central mass-accreting supermassive black hole (more commonly known as active galactic nucleus, AGN) of low luminosity, making LINER galaxies the largest AGN sub-population, which dominate in numbers over higher luminosity Seyfert galaxies and quasars. This, however, poses a serious problem. While the inferred energy balance is plausible, many LINERs clearly do not contain any other independent signatures of an AGN. Aims. Using integral field spectroscopic data from the CALIFA survey, we compare the observed radial surface brightness profiles with what is expected from illumination by an AGN. Methods. Essential for this analysis is a proper extraction of emission lines, especially weak lines, such as Balmer H beta lines, which are superposed on an absorption trough. To accomplish this, we use the GANDALF code, which simultaneously fits the underlying stellar continuum and emission lines. Results. For 48 galaxies with LINER-like emission, we show that the radial emission-line surface brightness profiles are inconsistent with ionisation by a central point-source and hence cannot be due to an AGN alone. Conclusions. The most probable explanation for the excess LINER-like emission is ionisation by evolved stars during the short but very hot and energetic phase known as post-AGB. This leads us to an entirely new interpretation. Post-AGB stars are ubiquitous and their ionising effect should be potentially observable in every galaxy with the gas present and with stars older than ~1 Gyr unless a stronger radiation field from young hot stars or an AGN outshines them. This means that galaxies with LINER-like emission are not a class defined by a property but rather by the absence of a property. It also explains why LINER emission is observed mostly in massive galaxies with old stars and little star formation.

Item Type:Article
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© ESO, 2013.
Artículo firmado por 21 autores.
The authors would like to thank all of the CALIFA collaboration for their input, Brent Groves for very useful discussions on ionisation properties, and Remco van den Bosch for his technical and scientific advises. R. S. acknowledges support by the IMPRS for Astronomy & Cosmic Physics at the University of Heidelberg. K. J. is supported by the Emmy NoetherProgramme of the German Science Foundation DFG under grant Ja 1114/3-2 and the German Space Agency DLR. G. v. d. V. and J. F.-B. acknowledge the DAGAL network from the People Programme (Marie Curie Actions) of the European Union's Seventh Framework Programme FP7/2007-2013/under REA grant agreement number PITN-GA-2011-289313. J. F.-B. further acknowledges financial support from the Ramón y Cajal Program and grant AYA2010-21322-C03-02 from the Spanish Ministry of Economy and Competitiveness (MINECO). V. W. acknowledges support from the ERC Starting Grant SEDmorph. R. A. Marino was also funded by the spanish programme of International Campus of Excellence Moncloa (CEI). This study makes uses of the data provided by the Calar Alto Legacy Integral Field Area (CALIFA) survey (http://califa.caha.es/) and is based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max-Planck-Institut fur Astronomie and the Instituto de Astrofísica de Andalucía (CSIC).

Uncontrolled Keywords:Active galactic nuclei; Dogota sky survey; Field area survey; Lenticular galaxies; Elliptic galaxies; Sauron Project; Host galaxies; Califa; Emission; Classification
Subjects:Sciences > Physics > Astrophysics
Sciences > Physics > Astronomy
ID Code:37549
Deposited On:09 May 2016 13:52
Last Modified:10 Dec 2018 15:05

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