THE SPECTRAL EVOLUTION OF THE FIRST GALAXIES. I. JAMES WEBB SPACE TELESCOPE DETECTION LIMITS AND COLOR CRITERIA FOR POPULATION III GALAXIES

被引:250
作者
Zackrisson, Erik [1 ,2 ]
Rydberg, Claes-Erik [1 ,2 ]
Schaerer, Daniel [3 ,4 ]
Ostlin, Goran [1 ,2 ]
Tuli, Manan [1 ,2 ]
机构
[1] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden
[2] AlbaNova Univ Ctr, Oskar Klein Ctr Cosmoparticle Phys, S-10691 Stockholm, Sweden
[3] IRAP, CNRS, F-31400 Toulouse, France
[4] Univ Geneva, Observ Geneva, CH-1290 Versoix, Switzerland
基金
瑞典研究理事会; 瑞士国家科学基金会;
关键词
dark ages; reionization; first stars; galaxies: high-redshift; stars: Population III; INITIAL MASS FUNCTION; EXTREMELY METAL-POOR; LYMAN BUMP GALAXIES; LY-ALPHA; STAR-FORMATION; STELLAR POPULATIONS; MILKY-WAY; CHEMICAL ENRICHMENT; IONIZING-RADIATION; NEBULAR EMISSION;
D O I
10.1088/0004-637X/740/1/13
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
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 similar to 10(5) M-circle dot at z approximate to 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 approximate to 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.
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页数:15
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