Spectroscopy in the Inner Region of the 3C 48 Host Galaxy

Details Spectroscopy in the Inner Region of the 3C 48 Host Galaxy Spectroscopy in the Inner Region of the 3C 48 Host Galaxy

Jul 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002hst..prop.9365s&link_type=abstract

HST Proposal ID #9365

Computer Science

Hst Proposal Id #9365

Scientific paper

As far as we are aware, there is only one host galaxy continuum feature in a luminous QSO that is bright enough for practical STIS spectroscopy: this is the bright peak 1" NE of the well-known quasar 3C 48. This feature {3C 48A} is enigmatic, with an apparently distorted morphology. It may be the distended nuclear region of one of the galaxies in this major merger. It might, instead, possibly be the result of interaction of the compact-steep spectrum radio jet with ambient material; but this seems unlikely because the correspondence between the radio and optical morphologies is not very good. We also know from ground-based and HST imaging that 3C 48A is overwhelmingly dominated by continuum radiation, not line emission, and the colors seem to be inconsistent with stars as young as the probable age of the radio jet. Our previous high S/N ground-based spectroscopy of 3C 48 covered most regions of host galaxy beyond 2" from the QSO. From this spectroscopy and spectral synthesis models, we have been able to determine mean ages for recent starbursts in various parts of the host galaxy as well as the velocity field of the stars. By tying the proposed STIS spectroscopy of 3C 48A to our existing spectroscopy of the host galaxy, together with archival PC images, we expect to be able to determine the nature of this unusual inner structure and its role in the evolutionary history of 3C 48.

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