Physics
Scientific paper
Nov 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aipc.1294..259f&link_type=abstract
THE FIRST STARS AND GALAXIES: CHALLENGES FOR THE NEXT DECADE. AIP Conference Proceedings, Volume 1294, pp. 259-260 (2010).
Physics
Clusters Of Galaxies, Stellar Mass, Redshift, Star Formation, Origin, Formation, Evolution, Age, And Star Formation, Masses, Distances, Redshifts, Radial Velocities, Spatial Distribution Of Galaxies, Star Formation
Scientific paper
Understanding the escape fraction fesc from early galaxies gives an important constraint on the sources that reionize the universe. Previous studies of fesc have found a wide range of values, varying from less than 0.01 to nearly 1. Rather than try to find an exact value of fesc, we seek to understand how internal properties of the galaxy affect fesc. Two are: 1) the density and distribution of neutral hydrogen within the galaxy and 2) the number of ionizing photons produced. How the neutral medium is clumped significantly affects fesc. If there are some paths that photons follow out of the galaxy that do not intercept a clump, fesc is greater than the case with no clumps, with clumps of higher density causing a greater fesc. If all paths intersect at least one clump, fesc will drop below the no-clump case, and increasing the density of the clump will decrease fesc. Populations of stars with larger numbers of ionizing photons, such as metal-free or more massive stars, or disks with a high star formation efficiency increase fesc because the angle from which photons can escape the disk is increased, allowing more to escape. fesc also decreases for halos formed at higher redshifts because they are more dense, if there is no change in stellar population over redshift. We also find that the mass of the galaxy does not affect fesc, as long as the star formation efficiency is constant.
Fernandez Elizabeth R.
Shull Michael J.
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