The Metallicity of Gas in the Local Universe: Beyond the Milky Way

Details The Metallicity of Gas in the Local Universe: Beyond the Milky Way The Metallicity of Gas in the Local Universe: Beyond the Milky Way

Jul 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000hst..prop.8625b&link_type=abstract

HST Proposal ID #8625

Computer Science

Hst Proposal Id #8625 Quasar Absorption Lines And Igm

Scientific paper

We wish to obtain STIS spectra of three QSO/AGN which lie behind nearby galaxies, to measure the metallicity of the interstellar gas at the present epoch beyond the local group. We aim to provide the first steps in establishing a low- redshift anchor to the ever burgeoning abundance measurements of gas at high redshift, to quantify the range of abundances seen in the galaxies today, and thereby examine whether our galaxy might simply be metal rich in comparison. Our data will also provide valuable information for discriminating between competing models of galaxy evolution. The three probes are the best available for obtaining UV data with sufficient quality to reliably measure column densities and Doppler parameters; Q1219+047 passes 21 h through the outer H I disk of M61, where there are no sites of current star formation; Mrk 205 shines through the inter-arm region of NGC 4319, and can be used to construct the first UV absorption-line atlas of a galaxy beyond the Magellanic Clouds; and Q1543+489 directly intercepts an intergalactic H I cloud associated with two nearby galaxies. In this latter case, direct measurement of the cloud's metallicity and hydrogen column density will also enable us to constrain the ionization parameter of the UV background radiation field.

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