Imaging Spectroscopy of NGC 4151

Details Imaging Spectroscopy of NGC 4151 Imaging Spectroscopy of NGC 4151

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997hst..prop.7121h&link_type=abstract

HST Proposal ID #7121

Computer Science

Hst Proposal Id #7121

Scientific paper

NGC 4151 is the brightest Seyfert 1 galaxy and thus a perfect target to demonstrate the imaging spectroscopy capabilities of STIS. Slitless spectra in the H-beta and [OIII] 4959,5007 region and CIV 1550 will be compared to optical direct images of the emission line region. The region of interest is about 3 x 6 arcsec and contains many emission-line clouds. The data will consist of images of the cloud line-emission that will reveal their ionisation structure and velocities, together with the nuclear broad-line emission. The line emission flux is much greater than the local continuum flux, so there will be no continuum contamination. The orientation is chosen to avoid overlap between the nuclear and cloud spectra. The images will show the cloud structure in [O II] and [O III]. Parallel WFPC2 exposures will obtain 3 colour images of the outer stellar populations of NGC 4151.

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