Probing the epoch of reinization with HST and JWST

Details Probing the epoch of reinization with HST and JWST Probing the epoch of reinization with HST and JWST

May 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aas...202.5404s&link_type=abstract

American Astronomical Society Meeting 202, #54.04; Bulletin of the American Astronomical Society, Vol. 35, p.773

Astronomy and Astrophysics

Astronomy

Scientific paper

I will present estimates of the luminosity of the sources of reionization and discuss their observability with HST and JWST. The model used to derive the luminosity of these sources is parametrized by the escape fraction of UV photons, the clumpiness of the IGM and the steepeness of the ionizing continuum. Zero metallicity, population III, sources are the most efficient ionizing sources and - if their UV escape fraction is high - the hardest to detect. Less efficienct producers of ionizing photons are easier to detect longwards of Lyman alpha. The detection limits are discussed in the number density vs luminosity plane and compared to both existing and planned deep surveys with HST: HDF/HDFS, GOODS, and the Ultra Deep Field. I will also discuss the capibilities of JWST in detecting these objects.

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