Spectroscopy of IR Galaxies Over The Merger Sequence

Details Spectroscopy of IR Galaxies Over The Merger Sequence Spectroscopy of IR Galaxies Over The Merger Sequence

Mar 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008sptz.prop50172b&link_type=abstract

Spitzer Proposal ID #50172

Computer Science

Scientific paper

Locally, ~50% of LIRGs and 95% of ULIRGs are driven by galaxy mergers, which provide the primary means of triggering star formation and AGN activity. However, at z>0.7 the dominate mechanisms responsible for the IR emission in LIRG galaxies may be different from those locally, as only 30% of z=0.7 LIRGs exhibit merger signatures and the remaining 70% appear to be undisturbed spiral galaxies. Although the merger process itself is the same at both high and low redshift, the galaxies involved in the mergers are not. At higher redshift, galaxies have higher gas mass fractions, meaning more fuel for star formation and AGN, can have smaller bulges, and are less likely to have bar structures. These differences can affect the onset, strength and relative contribution to their IR luminosity from starbursts and AGN. Using the CFHTLS-Deep Catalog of Interacting Galaxies we have identified 24 (>1mJy at 24um) early to late stage IR bright mergers, between 0.45

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