The stellar populations of low-luminosity active galactic nuclei - III. Spatially resolved spectral properties

Abstract

In a recently completed survey of the stellar population properties of low‐ionization nuclear emission‐line regions (LINERs) and LINER/H ii transition objects (TOs), we have identified a numerous class of galactic nuclei which stand out because of their conspicuous 108−9 yr populations, traced by high‐order Balmer absorption lines and other stellar indices. These objects are called ‘young‐TOs’, because they all have TO‐like emission‐line ratios. In this paper we extend this previous work, which concentrated on the nuclear properties, by investigating the radial variations of spectral properties in low‐luminosity active galactic nuclei (LLAGNs). Our analysis is based on high signal‐to‐noise ratio (S/N) long‐slit spectra in the 3500–5500 Å interval for a sample of 47 galaxies. The data probe distances of typically up to 850 pc from the nucleus with a resolution of ∼100 pc (∼1 arcsec) and S/N ∼ 30. Stellar population gradients are mapped by the radial profiles of absorption‐line equivalent widths and continuum colours along the slit. These variations are further analysed by means of a decomposition of each spectrum in terms of template galaxies representative of very young (≤107 yr), intermediate age (108–9 yr) and old (1010 yr) stellar populations. This study reveals that young‐TOs also differ from old‐TOs and old‐LINERs in terms of the spatial distributions of their stellar populations and dust. Specifically, our main findings are as follows. (i) Significant stellar population gradients are found almost exclusively in young‐TOs. (ii) The intermediate age population of young‐TOs, although heavily concentrated in the nucleus, reaches distances of up to a few hundred pc from the nucleus. Nevertheless, the half width at half‐maximum of its brightness profile is more typically 100 pc or less. (iii) Objects with predominantly old stellar populations present spatially homogeneous spectra, be they LINERs or TOs. (iv) Young‐TOs have much more dust in their central regions than other LLAGNs. (v) The B‐band luminosities of the central ≲1 Gyr population in young‐TOs are within an order of magnitude of MB=−15, implying masses of the order of ∼107–108 M⊙. This population was 10–100 times more luminous in its formation epoch, at which time young massive stars would have completely outshone any active nucleus, unless the AGN too was brighter in the past.

Nearby early-type galaxies with ionized gas

“…The first result agrees with previous findings that LINERs are older than Seyferts (e.g., Kewley et al 2006), and supports the idea that the star formation and the AGN phenomena coexist (Terlevich et al 1990;Cid Fernandes & Terlevich 1995;Heckman et al 1997;González Delgado et al 2001;Kauffmann et al 2003;Cid Fernandes et al 2005;Davies et al 2007;Riffel et al 2009). The young luminosity-weighted ages in the Seyferts of our sample are probably caused by recent star formation episodes superimposed on a several Gyr old stellar population (see Paper III).…”

Stellar population properties for a sample of hard X-ray AGNs

“…Their percentage, which is higher than what we found, could be ascribed in that we were observing a larger region of the galaxy compared to what had been performed. For this reason, we were less sensitive to the young stellar populations that are possibly increasing towards the nucleus of the galaxy (Cid Fernandes et al 2005). This could be the reason for the young component detected in PBC J0919.9+3712 and PBC J1345.4+4141.…”

Activity of the Seyfert galaxy neighbours

“…Spectra processing and fits were carried in the same fashion as described in Sect. Asari et al 2007;Cid-Fernandes et al 2005. We only note that we have calculated the 1σ standard deviation of the flux as follows (Tresse et al 1999):…”