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Title:
Detecting primordial stars
Authors:
Scannapieco, Evan; Ferrara, Andrea; Heger, Alexander; Madau, Piero; Schneider, Raffaella; Woosley, Stan
Affiliation:
AA(Kavli Institute for Theoretical Physics, UC Santa Barbara, CA 93106, United States), AB(SISSA/Int. School for Advanced Studies, Via Beirut 4, 34014 Trieste, Italy), AC(Theoretical Astrophysics Group, T6, MS B227, Los Alamos National Laboratory, Los Alamos, NM 87545, United States), AD(Department of Astronomy and Astrophysics, UC Santa Cruz, Santa Cruz, CA 95064, United States), AE(Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy), AF(Department of Astronomy and Astrophysics, UC Santa Cruz, Santa Cruz, CA 95064, United States)
Publication:
New Astronomy Reviews, Volume 50, Issue 1-3, p. 89-93. (NewAR Homepage)
Publication Date:
03/2006
Origin:
ELSEVIER
DOI:
10.1016/j.newar.2005.11.009
Bibliographic Code:
2006NewAR..50...89S

Abstract

We study the detectability of primordial metal-free stars, both through direct searches for their emission, as well as searches for the resulting supernovae. We show that enrichment is a local process that takes place over an extended redshift range. While the duration of the transition from a metal-free to an enriched universe depends on several unknown factors, in all models late-forming metal-free stars are found in 107.5 108.0Mȯ objects, which are just large enough to cool, but small enough to not be clustered near areas of previous star formation. We discuss the observational properties of these objects, some of which may have already been detected in ongoing surveys of high-redshift Lyman-α emitters. If metal-free stars have masses 140Mȯ ≲ M* ≲ 260Mȯ, they are expected to end their lives as pair-production supernovae (PPSNe), in which an electron positron pair-production instability triggers explosive nuclear burning. Using the implicit hydrodynamics code KEPLER, we calculate a set of PPSNe light curves that allows us to assess observational strategies for finding these objects. The peak luminosities of typical PPSNe are only slightly greater than those of Type Ia supernovae, but they remain bright much longer (˜1 year) and have hydrogen lines. Ongoing supernova searches may soon be able to place stringent limits on the fraction of very massive stars out to z ≈ 2. The planned Joint Dark Energy Mission satellite will be able to extend these limits out to z ≈ 6.
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