The First Gamma-Ray Bursts in the Universe

Mesler, Robert A.; Whalen, Daniel J.; Smidt, Joseph; Fryer, Chris L.; Lloyd-Ronning, Nicole M.; Pihlström, Y. M.

doi:10.1088/0004-637x/787/1/91

Cited by 45 publications

(43 citation statements)

References 128 publications

(126 reference statements)

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“…Although X-rays from these events may be detected by Swift or its successors such as the Joint Astrophysics Nascent Universe Satellite (JANUS; Mészáros & Rees 2010;Roming 2008;Burrows et al 2010), their afterglows ) might also be detected in all-sky radio surveys by the Extended Very Large Array (eVLA), eMERLIN, and the Square Kilometer Array (SKA; de Souza et al 2011). We are now studying detection limits for Pop III GRBs in a variety of circumstellar environments (Mesler et al 2012(Mesler et al , 2013.…”

Section: Resultsmentioning

confidence: 99%

Finding the First Cosmic Explosions. Ii. Core-Collapse Supernovae

Whalen

Joggerst

Fryer

et al. 2013

ApJ

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Understanding the properties of Population III (Pop III) stars is prerequisite to elucidating the nature of primeval galaxies, the chemical enrichment and reionization of the early intergalactic medium, and the origin of supermassive black holes. While the primordial initial mass function (IMF) remains unknown, recent evidence from numerical simulations and stellar archaeology suggests that some Pop III stars may have had lower masses than previously thought, 15-50 M in addition to 50-500 M . The detection of Pop III supernovae (SNe) by JWST, WFIRST, or the TMT could directly probe the primordial IMF for the first time. We present numerical simulations of 15-40 M Pop III core-collapse SNe performed with the Los Alamos radiation hydrodynamics code RAGE. We find that they will be visible in the earliest galaxies out to z ∼ 10-15, tracing their star formation rates and in some cases revealing their positions on the sky. Since the central engines of Pop III and solar-metallicity core-collapse SNe are quite similar, future detection of any Type II SNe by next-generation NIR instruments will in general be limited to this epoch.

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Section: Resultsmentioning

confidence: 99%

Finding the First Cosmic Explosions. Ii. Core-Collapse Supernovae

Whalen

Joggerst

Fryer

et al. 2013

ApJ

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“…Mesler et al 2014). We assume an explosion energy of ESN = 1.2 × 10 51 erg for all SNe, use the ejecta masses by Heger & Woosley (2002), and the individual metal yields by Heger & Woosley (2010).…”

Section: Chemical Feedbackmentioning

confidence: 99%

Constraining the primordial initial mass function with stellar archaeology

Hartwig

Bromm

Klessen

et al. 2015

Monthly Notices of the Royal Astronomical Society

107

103

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We present a new near-field cosmological probe of the initial mass function (IMF) of the first stars. Specifically, we constrain the lower-mass limit of the Population III (Pop III) IMF with the total number of stars in large, unbiased surveys of the Milky Way. We model the early star formation history in a Milky Way-like halo with a semi-analytic approach, based on Monte-Carlo sampling of dark matter merger trees, combined with a treatment of the most important feedback mechanisms. Assuming a logarithmically flat Pop III IMF and varying its low mass limit, we derive the number of expected survivors of these first stars, using them to estimate the probability to detect any such Pop III fossil in stellar archaeological surveys. Following our analysis, the most promising region to find possible Pop III survivors is the stellar halo of the Milky Way, which is the best target for future surveys. We find that if no genuine Pop III survivor is detected in a sample size of 4 × 10 6 (2 × 10 7 ) halo stars with wellcontrolled selection effects, then we can exclude the hypothesis that the primordial IMF extended down below 0.8M ⊙ at a confidence level of 68% (99%). With the sample size of the Hamburg/ESO survey, we can tentatively exclude Pop III stars with masses below 0.65M ⊙ with a confidence level of 95%, although this is subject to significant uncertainties. To fully harness the potential of our approach, future large surveys are needed that employ uniform, unbiased selection strategies for high-resolution spectroscopic follow-up.

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“…Non-rotating Pop III stars from 10 -40 M die as core-collapse supernovae (CC SNe) and 90 -260 M stars can explode as pair-instability (PI) SNe (Barkat et al 1967;Glatzel et al 1985;Heger & Woosley 2002Chatzopoulos & Wheeler 2012;Chatzopoulos et al 2013Chatzopoulos et al , 2015Chen et al 2014). A recent arc of radiation hydrodynamical simulations has shown that PI SNe will be visible in the near infrared (NIR) at z ∼ 15 -20 to the James Webb Space Telescope (JWST), the Wide-Field Infrared Survey Telescope (WFIRST) and the Thirty-Meter Telescope (Kasen et al 2011;Cooke et al 2012;Hummel et al 2012;Pan et al 2012;Whalen et al 2013a,c,d,f;de Souza et al 2013de Souza et al , 2014Smidt et al 2014a) and that CC SNe and gamma-ray bursts (GRBs) will be visible out to z ∼ 10 -15 (e.g., Whalen et al 2008a;Moriya et al 2010;Tanaka et al 2012;Whalen et al 2013b,e;Tanaka et al 2013;Mesler et al 2014;Smidt et al 2014b;de Souza et al 2014;Magg et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Low-energy Population III supernovae and the origin of extremely metal-poor stars

Chen

Heger

Whalen

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Some ancient, dim, metal-poor stars may have formed in the ashes of the first supernovae. If their chemical abundances can be reconciled with the elemental yields of specific Pop III explosions, they could reveal the properties of primordial stars. But multidimensional simulations of such explosions are required to predict their yields because dynamical instabilities can dredge material up from deep in the ejecta that would otherwise be predicted to fall back onto the central remnant and be lost in one-dimensional (1D) models. We have performed two-dimensional (2D) numerical simulations of two low-energy Pop III supernovae, a 12.4 M explosion and a 60 M explosion, and find that they produce elemental yields that are a good fit to those measured in the most iron-poor star discovered to date, SMSS J031300.36-670839.3 (J031300). Fallback onto the compact remnant in these weak explosions accounts for the lack of measurable iron in J031300 and its low iron-group abundances in general. Our 2D explosions produce higher abundances of heavy elements (atomic number Z > 20) than their 1D counterparts due to dredge-up by fluid instabilities. Since almost no 56 Ni is ejected by these weak SNe, their low luminosities will prevent their detection in the near infrared with the James Webb Space Telescope and future 30-meter telescopes on the ground. The only evidence that they ever occurred will be in the fossil abundance record.

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The First Gamma-Ray Bursts in the Universe

Cited by 45 publications

References 128 publications

Finding the First Cosmic Explosions. Ii. Core-Collapse Supernovae

Finding the First Cosmic Explosions. Ii. Core-Collapse Supernovae

Constraining the primordial initial mass function with stellar archaeology

Low-energy Population III supernovae and the origin of extremely metal-poor stars

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