3D Spectroscopic Study of the Line Emitting Regions of Mrk 493

Details 3D Spectroscopic Study of the Line Emitting Regions of Mrk 493 3D Spectroscopic Study of the Line Emitting Regions of Mrk 493

2008-12-28

arxiv.org/abs/0812.4817v1

Astronomy and Astrophysics

Astrophysics

accepted in AJ

Scientific paper

10.1088/0004-6256/137/3/3548

We report the results of 3D spectroscopic observations of Mrk 493 (NLS1 galaxy) with the integral-field spectrograph MPFS of the SAO RAS 6-m telescope. The difference in the slope of the optical continuum emission intensity across the nucleus part and an extensive continuum emission region} is detected. The emission in lines (H$\alpha$, H$\beta$, [OIII], etc.) coincides with a composite nuclear region: an AGN plus a circum-nuclear star-forming ring observed in the HST UV/optical images. The [SII] emission region tends to be up to 1kpc around the center. The H$\alpha$ and H$\beta$ could be decomposed into three components (broad $\sim$ 2000 km/s. intermediate $\sim$ 700 km/s and narrow $\sim$ 250 km/s). We found that width ($\sim$ 750 km/s) of the Fe II lines correspond to the intermediate component, that may indicate a non-BLR origin of the Fe II lines, or that a large fraction of the Fe II emission arise in the outher parts of the BLR. The weak broad component detected in the H$\alpha$, H$\beta$ and He$\lambda$4686 may come from the unresolved central BLR, but also partly produced by violent starburst in the circum-nuclear ring. Moreover, diagnostic diagrams clearly show presence of the HII regions (not a Sy 1 nucleus) in the NLR of Mrk 493.

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