Metal transport and chemical heterogeneity in early star forming systems

Ritter, Jeremy S.; Sluder, Alan; Safranek-Shrader, Chalence; Milosavljević, Miloš

doi:10.1093/mnras/stv982

Cited by 84 publications

(117 citation statements)

References 95 publications

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“…However, it is expected that enrichment of the primordial gas in the vicinity of early star-forming galaxies is heterogeneous (e.g. Ritter et al 2015) and that for the densest gas in cosmological halos, it involves a complex interplay of physical processes (e.g. Chen et al 2016;Cen & Riquelme 2008;Smith et al 2015).…”

Section: Conclusion and Discussionmentioning

confidence: 99%

Metallicity evolution of direct collapse black hole hosts: CR7 as a case study

Agarwal

Johnson

Khochfar

et al. 2017

Monthly Notices of the Royal Astronomical Society

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In this study we focus on the z ∼ 6.6 Lyman-α CR7 consisting of clump A that is host to a potential direct collapse black hole (DCBH), and two metal enriched star forming clumps B and C. In contrast to claims that signatures of metals rule out the existence of DCBHs, we show that metal pollution of A from star forming clumps clumps B and C is inevitable, and that A can form a DCBH well before its metallicity exceeds the critical threshold of 10 −5 − 10 −6 Z ⊙ . Assuming metal mixing happens instantaneously, we derive the metallicity of A based on the star formation history of B and C. We find that treating a final accreting black hole of 10 6 − 10 7 M ⊙ in A for nebular emission already pushes its H 160 -[3.6] and [3.6]-[4.5] colours into the 3σ limit of observations. Hence, we show that the presence of metals in DCBH hosts is inevitable, and that it is the coevolution of the LW radiation field and metals originating from neighbouring galaxies that governs DCBH formation in a neighbouring initially pristine atomic cooling haloes.

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Section: Conclusion and Discussionmentioning

confidence: 99%

Metallicity evolution of direct collapse black hole hosts: CR7 as a case study

Agarwal

Johnson

Khochfar

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…Ji et al (2016a) also estimated the yield of the r-process event (M Eu ∼ 10 −4.5±1 M e ) by considering typical metal dilution gas masses in UFDs in conjunction with the observed [Eu/H] ratios. More sophisticated hydrodynamic simulations of these dilution masses in the aftermath of a supernova explosion or neutron star merger (e.g., Bland-Hawthorn et al 2015;Ritter et al 2015;Montes et al 2016) may be able to further constrain the dilution mass and thus the yield of the event.…”

Section: Site Of the R-processmentioning

confidence: 99%

COMPLETE ELEMENT ABUNDANCES OF NINE STARS IN THE r-PROCESS GALAXY RETICULUM II*

Frebel

Simon

et al. 2016

ApJ

185

175

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We present chemical abundances derived from high-resolution Magellan/Magellan Inamori Kyocera Echelle spectra of the nine brightest known red giant members of the ultra-faint dwarf galaxy ReticulumII (Ret II). These stars span the full metallicity range of RetII (−3.5 < [Fe/H] < −2). Seven of the nine stars have extremely high levels of r-process material ([Eu/Fe] ∼ 1.7), in contrast to the extremely low neutron-capture element abundances found in every other ultra-faint dwarf galaxy studied to date. The other two stars are the most metal-poor stars in the system ([Fe/H] < −3), and they have neutron-capture element abundance limits similar to those in other ultrafaint dwarf galaxies. We confirm that the relative abundances of Sr, Y, and Zr in these stars are similar to those found in r-process halo stars, but they are ∼0.5 dex lower than the solar r-process pattern. If the universal r-process pattern extends to those elements, the stars in RetII display the least contaminated known r-process pattern. The abundances of lighter elements up to the iron peak are otherwise similar to abundances of stars in the halo and in other ultra-faint dwarf galaxies. However, the scatter in abundance ratios is large enough to suggest that inhomogeneous metal mixing is required to explain the chemical evolution of this galaxy. The presence of low amounts of neutron-capture elements in other ultra-faint dwarf galaxies may imply the existence of additional rprocess sites besides the source of r-process elements in RetII. Galaxies like RetII may be the original birth sites of r-process enhanced stars now found in the halo.

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“…Mixing on small scales in the explosion must also be understood to predict the metallicities of the stars that form in the debris of the SN because it sets the initial conditions for mixing, cooling and collapse of gas on larger scales in the intergalactic medium (IGM). Mixing in Pop III CC and PI SNe has previously been studied by Joggerst et al (2009);Joggerst & Whalen (2011);Chen et al (2011Chen et al ( , 2014 and on larger, cosmological scales by Wise & Abel (2008); Greif et al (2010); Jeon et al (2014); Chiaki et al (2015); Chen et al (2015); Ritter et al (2015); Sluder et al (2015).…”

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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Metal transport and chemical heterogeneity in early star forming systems

Cited by 84 publications

References 95 publications

Metallicity evolution of direct collapse black hole hosts: CR7 as a case study

Metallicity evolution of direct collapse black hole hosts: CR7 as a case study

COMPLETE ELEMENT ABUNDANCES OF NINE STARS IN THE r-PROCESS GALAXY RETICULUM II*

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

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