Technical Aspects Of How The James Webb Space Telescope Can Measure First Light, Reionization, And Galaxy Assembly.

Biology – Quantitative Biology – Quantitative Methods

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Scientific paper

We review the technical aspects of how the 6.5 meter James Webb Space Telescope (JWST) can measure First Light, Reionization, Galaxy Assembly, building on lessons learned from the Hubble Space Telescope (HST). We show what combination of area, depth, and wavelength coverage are needed for JWST to detect a sufficient number of First Light objects, and to measure their evolving luminosity function (LF). In detail, JWST will map the epoch of First light through Pop III star dominated objects at redshifts z=8--20, and its transition to the first Pop II stars in dwarf galaxies.
We discuss: 1) what deep JWST images will look like compared to the Hubble UltraDeep Field (HUDF), given JWST's expected PSF performance; (2) simulations of what nearby galaxies observed in their restframe UV--optical light by HST would look like to JWST at very high redshifts; (3) quantitative methods to determine structural parameters of faint galaxies in deep JWST images as a function of cosmic epoch to delineate the progress of galaxy assembly; (4) to what extent JWST's short-wavelength performance --- which needed to be relaxed in the 2005 redefinition of the telescope --- will affect JWST's ability to accurately determine faint galaxy parameters; and (5) if ultradeep JWST images will run into the instrumental and natural confusion limits.
We demonstrate an interactive web-tool on a laptop that lets the user pan and zoom 3-D through the HUDF data-base from redshifts z=0 to z=6, with all galaxy images sorted versus spectro-photometric redshift, and visualize what JWST will
add from AB=29.5--32.0 mag and between redshifts z=7--20. This work was funded by NASA JWST grant NAG5-12460 from GSFC, and grant HST/ED14-975 from STScI.

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