SIMBAD references

2011ApJ...740...13Z - Astrophys. J., 740, 13 (2011/October-2)

The spectral evolution of the first galaxies. I. James webb space telescope detection limits and color criteria for population III galaxies.

ZACKRISSON E., RYDBERG C.-E., SCHAERER D., OSTLIN G. and TULI M.

Abstract (from CDS):

The James Webb Space Telescope (JWST) is expected to revolutionize our understanding of the high-redshift universe, and may be able to test the prediction that the first, chemically pristine (Population III) stars are formed with very high characteristic masses. Since isolated Population III stars are likely to be beyond the reach of JWST, small Population III galaxies may offer the best prospects of directly probing the properties of metal-free stars. Here, we present Yggdrasil, a new spectral synthesis code geared toward the first galaxies. Using this model, we explore the JWST imaging detection limits for Population III galaxies and investigate to what extent such objects may be identified based on their JWST colors. We predict that JWST should be able to detect Population III galaxies with stellar population masses as low as ∼105 M at z ~ 10 in ultra deep exposures. Over limited redshift intervals, it may also be possible to use color criteria to select Population III galaxy candidates for follow-up spectroscopy. The colors of young Population III galaxies dominated by direct starlight can be used to probe the stellar initial mass function (IMF), but this requires almost complete leakage of ionizing photons into the intergalactic medium. The colors of objects dominated by nebular emission show no corresponding IMF sensitivity. We also note that a clean selection of Population III galaxies at z ~ 7-8 can be achieved by adding two JWST/MIRI filters to the JWST/NIRCam filter sets usually discussed in the context of JWST ultra deep fields.

Abstract Copyright:

Journal keyword(s): dark ages, reionization, first stars - galaxies: high-redshift - stars: Population III

Status at CDS:  

Simbad objects: 5

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2020.04.06-11:35:11

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