Computer Science
Scientific paper
Jan 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995phdt........35s&link_type=abstract
Thesis (PH.D.)--THE UNIVERSITY OF ROCHESTER, 1995.Source: Dissertation Abstracts International, Volume: 57-02, Section: B, page:
Computer Science
2
Scientific paper
Near-infrared spectroscopy combined with high spatial resolution imaging are used in this thesis to probe the dust enshrouded nuclei of two starburst galaxies. A starburst model is constructed and compared to observations to infer the properties of the starburst episodes, such as the age and initial mass function (IMF) of the stellar population. One of the main goals of this work is to conduct a thorough investigation of the prototypical starburst galaxy, M82. Study of this galaxy provides insight into a phenomenon that appears to be occurring in many more distant galaxies. A similar study of one example, the interacting system Arp 299 (NGC 3690 and IC 694), is also carried out in this thesis. Our analysis implies that the starburst in both galaxies is approximately 10^7 years old. This is a typical age derived for starburst galaxies; examination of the evolution of our model quantities reveals the inherent selection effect that is taking place. In addition, our high spatial resolution observations of M81 indicate that there is an age dispersion within the M82 starburst complex that is correlated with the projected radius from the center of the galaxy. This suggests that the starburst in M82 is propagating outwards from the nucleus. The inferred age dispersion is ~6 times 10^6 years, corresponding to a velocity of propagation of ~50 km s^{-1}. Our high spatial resolution recombination-line data have allowed us to obtain the most accurate extinction -corrected colors and luminosities to date toward the starburst region in M82. Our extinction-corrected K magnitude, the most stringent constraint on the IMF of the starburst population in M82, is -22.0, substantially fainter than previous values adopted. This difference substantially weakens the arguments made previously for a low mass-deficient IMF for the starburst region in M82. A quantitative analysis reveals that the observed properties of M82 can be accommodated by a solar-neighborhood IMF if we assume that 30% of the total dynamical mass within the central 450 pc is in the burst population, leaving more than 60% of the mass for a pre-existing population.
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