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Title: First Light II: Emission Line Extinction, Population III Stars, and X-ray Binaries

Abstract

Here, we produce synthetic spectra and observations for metal-free stellar populations and high-mass X-ray binaries in the Renaissance Simulations at a redshift of 15. We extend our methodology from the first paper in the series by modelling the production and extinction of emission lines throughout a dusty and metal-enriched interstellar and circum-galactic media extracted from the simulation, using a Monte Carlo calculation. To capture the impact of high-energy photons, we include all frequencies from hard X-ray to far-infrared with enough frequency resolution to discern line emission and absorption profiles. The most common lines in our sample in order of their rate of occurrence are Ly α, the C iv λλ1548, 1551 doublet, H α, and the Ca ii λλλ8498, 8542, 8662 triplet. The best scenario for a direct observation of a metal-free stellar population is a merger between two Population III Galaxies. In mergers between metal-enriched and metal-free stellar populations, some characteristics may be inferred indirectly. Single Population III galaxies are too dim to be observed photometrically at z = 15. Ly α emission is discernible by JWST as an increase in J200w – J277w colour off the intrinsic stellar tracks. Observations of metal-free stars will be difficult, though notmore » impossible, with the next generation of space telescopes.« less

Authors:
 [1];  [2];  [3];  [4];  [5];  [6]
  1. Georgia Inst. of Technology, Atlanta, GA (United States); National Aeronautics and Space Administration, Pasadena, CA (United States)
  2. Georgia Inst. of Technology, Atlanta, GA (United States)
  3. Georgia Inst. of Technology, Atlanta, GA (United States); Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
  4. Michigan State Univ., East Lansing, MI (United States)
  5. Univ. of California, San Diego, La Jolla, CA (United States)
  6. Univ. of California, San Diego, La Jolla, CA (United States); IBM, Armonk, NY (United States)
Publication Date:
Research Org.:
Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
Sponsoring Org.:
USDOE Laboratory Directed Research and Development (LDRD) Program
OSTI Identifier:
1417168
Report Number(s):
LA-UR-17-28139
Journal ID: ISSN 0035-8711; TRN: US1800999
Grant/Contract Number:  
AC52-06NA25396
Resource Type:
Journal Article: Accepted Manuscript
Journal Name:
Monthly Notices of the Royal Astronomical Society
Additional Journal Information:
Journal Volume: 474; Journal Issue: 2; Journal ID: ISSN 0035-8711
Publisher:
Royal Astronomical Society
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; Population III stars, Xray binaries, Observational diagnostics

Citation Formats

Barrow, Kirk S. S., Wise, John H., Aykutalp, Aycin, O’Shea, Brian W., Norman, Michael L., and Xu, Hao. First Light II: Emission Line Extinction, Population III Stars, and X-ray Binaries. United States: N. p., 2017. Web. doi:10.1093/mnras/stx2973.
Barrow, Kirk S. S., Wise, John H., Aykutalp, Aycin, O’Shea, Brian W., Norman, Michael L., & Xu, Hao. First Light II: Emission Line Extinction, Population III Stars, and X-ray Binaries. United States. doi:10.1093/mnras/stx2973.
Barrow, Kirk S. S., Wise, John H., Aykutalp, Aycin, O’Shea, Brian W., Norman, Michael L., and Xu, Hao. Fri . "First Light II: Emission Line Extinction, Population III Stars, and X-ray Binaries". United States. doi:10.1093/mnras/stx2973.
@article{osti_1417168,
title = {First Light II: Emission Line Extinction, Population III Stars, and X-ray Binaries},
author = {Barrow, Kirk S. S. and Wise, John H. and Aykutalp, Aycin and O’Shea, Brian W. and Norman, Michael L. and Xu, Hao},
abstractNote = {Here, we produce synthetic spectra and observations for metal-free stellar populations and high-mass X-ray binaries in the Renaissance Simulations at a redshift of 15. We extend our methodology from the first paper in the series by modelling the production and extinction of emission lines throughout a dusty and metal-enriched interstellar and circum-galactic media extracted from the simulation, using a Monte Carlo calculation. To capture the impact of high-energy photons, we include all frequencies from hard X-ray to far-infrared with enough frequency resolution to discern line emission and absorption profiles. The most common lines in our sample in order of their rate of occurrence are Ly α, the C iv λλ1548, 1551 doublet, H α, and the Ca ii λλλ8498, 8542, 8662 triplet. The best scenario for a direct observation of a metal-free stellar population is a merger between two Population III Galaxies. In mergers between metal-enriched and metal-free stellar populations, some characteristics may be inferred indirectly. Single Population III galaxies are too dim to be observed photometrically at z = 15. Ly α emission is discernible by JWST as an increase in J200w – J277w colour off the intrinsic stellar tracks. Observations of metal-free stars will be difficult, though not impossible, with the next generation of space telescopes.},
doi = {10.1093/mnras/stx2973},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 2,
volume = 474,
place = {United States},
year = {Fri Nov 17 00:00:00 EST 2017},
month = {Fri Nov 17 00:00:00 EST 2017}
}

Journal Article:
Free Publicly Available Full Text
This content will become publicly available on November 17, 2018
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Cited by: 1 work
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