The CaT strength in Seyfert nuclei revisited: analysing young stars and non-stellar light contributions to the spectra

Details The CaT strength in Seyfert nuclei revisited: analysing young stars and non-stellar light contributions to the spectra The CaT strength in Seyfert nuclei revisited: analysing young stars and non-stellar light contributions to the spectra

Mar 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009mnras.393..846v&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 393, Issue 3, pp. 846-857.

Astronomy and Astrophysics

Astronomy

4

Galaxies: Kinematics And Dynamics, Galaxies: Nuclei, Galaxies: Seyfert, Galaxies: Stellar Content

Scientific paper

In a former paper, we have presented spectra of 64 active, nine normal and five starburst galaxies in the region around the near-infrared calcium triplet (CaT) absorption lines and the [SIII]λ9069 line. In the present paper, we analyse the CaT strength (WCaT) and kinematical products derived in that study, namely stellar (σ*) and ionized gas (σgas) velocity dispersions. Our main results may be summarized as follows. (1) Type 2 Seyfert galaxies show no sign of dilution in WCaT with respect to the values spanned by normal galaxies, even when optical absorption lines such as the CaII K band at 3933 Å are much weaker than in old, bulge-like stellar populations. (2) The location of type 2 Seyfert galaxies in the WCaT-WCaK plane is consistent with evolutionary synthesis models. The implication is that the source responsible for the dilution of optical lines in these active galactic nuclei (AGN) is a young stellar population, rather than an AGN featureless continuum, confirming the conclusion of the pioneer study of Terlevich, Díaz & Terlevich. (3) In type 1 Seyfert galaxies, both W[SIII] and WCaT tend to be diluted due to the presence of a non-stellar component, in agreement with the unification paradigm. (4) A comparison of σ* with σgas (obtained from the core of the [SIII] emitting line) confirms the existence of a correlation between the typical velocities of stars and clouds of the narrow line region. The strength and scatter around this correlation are similar to those previously obtained from the [OIII]λ5007 linewidth.

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