Probing the structure of the shocks in the narrow line region of M 51

Details Probing the structure of the shocks in the narrow line region of M 51 Probing the structure of the shocks in the narrow line region of M 51

Jul 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001hst..prop.9147f&link_type=abstract

HST Proposal ID #9147

Computer Science

Hst Proposal Id #9147 Agn/Quasars

Scientific paper

Despite many studies, the question of whether nuclear or shock-induced photoionization dominates the gaseous ionization in the narrow-line region {NLR} of LINERs and Seyfert galaxies remains unanswered. One critical issue is the determination of the input of mechanical energy in the NLR through jet/ISM interactions. According to Bicknell et al. {1998}, the latter could actually suffice to power the NLR in most Seyfert galaxies. Previous approaches to this problem have obtained integrated UV/visible line flux ratios, which are sensitive to uncertain reddening. We instead propose to exploit the high spatial resolution of HST/STIS to map several spectral lines across the shock/precursor complex in the spatially extended, jet-driven NLR of the nearby Seyfert 2 galaxy M 51. With spatial resolution of 4-5 pc {unprecedented for a galaxy jet/ISM interaction}, we will map the spatial distribution of kinematic subsystems, the ionization structure, and the gaseous density, across this structure. These HST/STIS observations {probing the shock structure} will be combined with proprietary CHANDRA/ACIS data {probing the hot, shocked gas component}, ground-based 3D spectroscopy {probing the more diffuse, extended structures} and radio maps. The resulting data set will be unique, and will allow us to derive quantitative measurements of the amount of mechanical energy injected in the NLR by the jet/ISM interaction.

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