Fe II emission lines as a chronometer for high-redshift quasars

Details Fe II emission lines as a chronometer for high-redshift quasars Fe II emission lines as a chronometer for high-redshift quasars

Jul 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999hst..prop.8098k&link_type=abstract

HST Proposal ID #8098

Physics

Hst Proposal Id #8098 Agn Physics

Scientific paper

We request STIS observations of the symbiotic nova RR-TEL to give complete coverage of FeII emission lines in the 1150- 9800 Angstrom wavelength range. We have embarked on a long- term program to fully simulate the physical conditions within FeII-emitting gas, and predict the resulting spectrum. The first steps of generating the initial atomic database and incorporating it into the photoionization code Cloudy, are complete. Analysis of the FeII lines from RR-TEL using Cloudy will allow us to check the r eliability and completeness of the atomic data and processes considered, to investigate the sensitivity of emission to temperature and density variations, and to assess the importance of blending. Although emission lines from FeII are observed from a wide variety of astronomical objects, including protostellar disks, novae, supernovae, and quasars, these lines have been notoriously difficult to interpret because of the great complexity of the FeII energy level structure. We no w have the tools to quantify the abundances in these objects and, once calibrated against the RR-TEL data, we will apply the same technique to deduce iron abundances from FeII emission in high-redshift quasars. This, in conjunction with predictions of ste llar evolution and galactic nucleosynthesis, will result in a chronometer measuring the redshift when the universe passed through an age of 1 Gyr, thus constraining several cosmological parameters.

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