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    Rights statement: This is a pre-copy-editing, author-produced PDF of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The definitive publisher-authenticated version A. Pallottini, A. Ferrara, F. Pacucci, S. Gallerani, S. Salvadori, R. Schneider, D. Schaerer, D. Sobral, and J. Matthee The brightest Ly α emitter: Pop III or black hole? MNRAS 2015 453: 2465-2470 is available online at: http://mnras.oxfordjournals.org/content/453/3/2465

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The brightest Ly alpha emitter: Pop III or black hole?

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The brightest Ly alpha emitter: Pop III or black hole? / Pallottini, A.; Ferrara, A.; Pacucci, F. et al.
In: Monthly Notices of the Royal Astronomical Society, Vol. 453, No. 3, 01.11.2015, p. 2465-2470.

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Harvard

Pallottini, A, Ferrara, A, Pacucci, F, Gallerani, S, Salvadori, S, Schneider, R, Schaerer, D, Sobral, D & Matthee, J 2015, 'The brightest Ly alpha emitter: Pop III or black hole?', Monthly Notices of the Royal Astronomical Society, vol. 453, no. 3, pp. 2465-2470. https://doi.org/10.1093/mnras/stv1795

APA

Pallottini, A., Ferrara, A., Pacucci, F., Gallerani, S., Salvadori, S., Schneider, R., Schaerer, D., Sobral, D., & Matthee, J. (2015). The brightest Ly alpha emitter: Pop III or black hole? Monthly Notices of the Royal Astronomical Society, 453(3), 2465-2470. https://doi.org/10.1093/mnras/stv1795

Vancouver

Pallottini A, Ferrara A, Pacucci F, Gallerani S, Salvadori S, Schneider R et al. The brightest Ly alpha emitter: Pop III or black hole? Monthly Notices of the Royal Astronomical Society. 2015 Nov 1;453(3):2465-2470. Epub 2015 Aug 31. doi: 10.1093/mnras/stv1795

Author

Pallottini, A. ; Ferrara, A. ; Pacucci, F. et al. / The brightest Ly alpha emitter : Pop III or black hole?. In: Monthly Notices of the Royal Astronomical Society. 2015 ; Vol. 453, No. 3. pp. 2465-2470.

Bibtex

@article{9b3dac0e39ce4cb9b6dc80446057a90f,
title = "The brightest Ly alpha emitter: Pop III or black hole?",
abstract = "CR7 is the brightest z = 6.6 Ly alpha emitter (LAE) known to date, and spectroscopic follow-up by Sobral et al. suggests that CR7 might host Population (Pop) III stars. We examine this interpretation using cosmological hydrodynamical simulations. Several simulated galaxies show the same 'Pop III wave' pattern observed in CR7. However, to reproduce the extreme CR7 Ly alpha/He II1640 line luminosities (L-alpha/He II) a top-heavy initial mass function and a massive (greater than or similar to 10(7)M(circle dot)) Pop III burst with age less than or similar to 2 Myr are required. Assuming that the observed properties of Ly alpha and He II emission are typical for Pop III, we predict that in the COSMOS/UDS/SA22 fields, 14 out of the 30 LAEs at z = 6.6 with L-alpha > 10(43.3) erg s(-1) should also host Pop III stars producing an observable L-He II greater than or similar to 10(42.7) erg s(-1). As an alternate explanation, we explore the possibility that CR7 is instead powered by accretion on to a direct collapse black hole. Our model predicts L-alpha, L-He II, and X-ray luminosities that are in agreement with the observations. In any case, the observed properties of CR7 indicate that this galaxy is most likely powered by sources formed from pristine gas. We propose that further X-ray observations can distinguish between the two above scenarios.",
keywords = "black hole physics, stars: Population III, galaxies: high-redshift, HIGH-REDSHIFT GALAXIES, POPULATION-III, STAR-FORMATION, DIRECT COLLAPSE, STELLAR POPULATIONS, PHYSICAL CONDITIONS, METAL ENRICHMENT, 1ST GALAXIES, REIONIZATION, EVOLUTION",
author = "A. Pallottini and A. Ferrara and F. Pacucci and S. Gallerani and S. Salvadori and R. Schneider and D. Schaerer and D. Sobral and J. Matthee",
note = "This is a pre-copy-editing, author-produced PDF of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The definitive publisher-authenticated version A. Pallottini, A. Ferrara, F. Pacucci, S. Gallerani, S. Salvadori, R. Schneider, D. Schaerer, D. Sobral, and J. Matthee The brightest Ly α emitter: Pop III or black hole? MNRAS 2015 453: 2465-2470 is available online at: http://mnras.oxfordjournals.org/content/453/3/2465 ",
year = "2015",
month = nov,
day = "1",
doi = "10.1093/mnras/stv1795",
language = "English",
volume = "453",
pages = "2465--2470",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "OXFORD UNIV PRESS",
number = "3",

}

RIS

TY - JOUR

T1 - The brightest Ly alpha emitter

T2 - Pop III or black hole?

AU - Pallottini, A.

AU - Ferrara, A.

AU - Pacucci, F.

AU - Gallerani, S.

AU - Salvadori, S.

AU - Schneider, R.

AU - Schaerer, D.

AU - Sobral, D.

AU - Matthee, J.

N1 - This is a pre-copy-editing, author-produced PDF of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The definitive publisher-authenticated version A. Pallottini, A. Ferrara, F. Pacucci, S. Gallerani, S. Salvadori, R. Schneider, D. Schaerer, D. Sobral, and J. Matthee The brightest Ly α emitter: Pop III or black hole? MNRAS 2015 453: 2465-2470 is available online at: http://mnras.oxfordjournals.org/content/453/3/2465

PY - 2015/11/1

Y1 - 2015/11/1

N2 - CR7 is the brightest z = 6.6 Ly alpha emitter (LAE) known to date, and spectroscopic follow-up by Sobral et al. suggests that CR7 might host Population (Pop) III stars. We examine this interpretation using cosmological hydrodynamical simulations. Several simulated galaxies show the same 'Pop III wave' pattern observed in CR7. However, to reproduce the extreme CR7 Ly alpha/He II1640 line luminosities (L-alpha/He II) a top-heavy initial mass function and a massive (greater than or similar to 10(7)M(circle dot)) Pop III burst with age less than or similar to 2 Myr are required. Assuming that the observed properties of Ly alpha and He II emission are typical for Pop III, we predict that in the COSMOS/UDS/SA22 fields, 14 out of the 30 LAEs at z = 6.6 with L-alpha > 10(43.3) erg s(-1) should also host Pop III stars producing an observable L-He II greater than or similar to 10(42.7) erg s(-1). As an alternate explanation, we explore the possibility that CR7 is instead powered by accretion on to a direct collapse black hole. Our model predicts L-alpha, L-He II, and X-ray luminosities that are in agreement with the observations. In any case, the observed properties of CR7 indicate that this galaxy is most likely powered by sources formed from pristine gas. We propose that further X-ray observations can distinguish between the two above scenarios.

AB - CR7 is the brightest z = 6.6 Ly alpha emitter (LAE) known to date, and spectroscopic follow-up by Sobral et al. suggests that CR7 might host Population (Pop) III stars. We examine this interpretation using cosmological hydrodynamical simulations. Several simulated galaxies show the same 'Pop III wave' pattern observed in CR7. However, to reproduce the extreme CR7 Ly alpha/He II1640 line luminosities (L-alpha/He II) a top-heavy initial mass function and a massive (greater than or similar to 10(7)M(circle dot)) Pop III burst with age less than or similar to 2 Myr are required. Assuming that the observed properties of Ly alpha and He II emission are typical for Pop III, we predict that in the COSMOS/UDS/SA22 fields, 14 out of the 30 LAEs at z = 6.6 with L-alpha > 10(43.3) erg s(-1) should also host Pop III stars producing an observable L-He II greater than or similar to 10(42.7) erg s(-1). As an alternate explanation, we explore the possibility that CR7 is instead powered by accretion on to a direct collapse black hole. Our model predicts L-alpha, L-He II, and X-ray luminosities that are in agreement with the observations. In any case, the observed properties of CR7 indicate that this galaxy is most likely powered by sources formed from pristine gas. We propose that further X-ray observations can distinguish between the two above scenarios.

KW - black hole physics

KW - stars: Population III

KW - galaxies: high-redshift

KW - HIGH-REDSHIFT GALAXIES

KW - POPULATION-III

KW - STAR-FORMATION

KW - DIRECT COLLAPSE

KW - STELLAR POPULATIONS

KW - PHYSICAL CONDITIONS

KW - METAL ENRICHMENT

KW - 1ST GALAXIES

KW - REIONIZATION

KW - EVOLUTION

U2 - 10.1093/mnras/stv1795

DO - 10.1093/mnras/stv1795

M3 - Journal article

VL - 453

SP - 2465

EP - 2470

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 3

ER -