Trigger Mechanisms and Time Evolution of Local QSOs and ULIRGs: The Dynamical Point of View.

Details Trigger Mechanisms and Time Evolution of Local QSOs and ULIRGs: The Dynamical Point of View. Trigger Mechanisms and Time Evolution of Local QSOs and ULIRGs: The Dynamical Point of View.

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.3202d&link_type=abstract

American Astronomical Society Meeting 210, #32.02; Bulletin of the American Astronomical Society, Vol. 39, p.144

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We conducted a large program (called QUEST) to study the time evolution of local gas-rich galaxy mergers through near-infrared (NIR) and mid-infrared (MIR) spectroscopy and imaging of local Ultraluminous Infrared Galaxies (ULIRGs) and Quasi-Stellar Objects (QSOs). I will summarize results of the NIR spectroscopic program, which was carried out using the ISAAC and NIRSPEC spectrographs mounted on the VLT and Keck telescopes respectively. We find that local ULIRGs are typically triggered by mergers of equal-mass, sub-m*, gas-rich galaxies and lead to the formation of moderate-mass ellipticals (Es). The velocity dispersion distribution of the ULIRG remnants peaks at a value similar to that of a large number of local Es from the Sloan Digital Sky Survey. The position of ULIRG remnants on the fundamental plane of early-type galaxies is well constrained in comparison with that of remnants of other interaction/merger categories (e.g. Luminous Infrared Galaxies; LIRGs). These results imply that, unlike local LIRGs (or high-z ULIRGs), local ULIRGs have a specific merger input and output. A similar analysis performed for local Palomar-Green (PG) QSOs indicates that PG QSOs have larger velocity dispersions than ULIRGs and that their position on the fundamental-plane of early-type galaxies is between moderate-mass and giant Es. Therefore, only a subsample of the local ULIRGs and PG QSOs have an identical origin. The measurement of the host velocity dispersion in QSO hosts also enables us to place, for the first time, QSOs on the AGN black hole mass-velocity dispersion diagram, populating the high-mass end of that relation.

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