Following the Cosmic Evolution of Pristine Gas. III. The Observational Consequences of the Unknown Properties of Population III Stars

Sarmento, Richard; Scannapieco, Evan; Côté, Benoît

doi:10.3847/1538-4357/aafa1a

Cited by 35 publications

(35 citation statements)

References 113 publications

(146 reference statements)

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“…However, metal (and dust) enrichment is known to be a highly inhomogeneous process, particularly at high redshift. Cosmological hydrodynamic simulations (Tornatore et al 2007;Maio et al 2011;Wise et al 2012;Johnson et al 2013;Muratov et al 2013;Pallottini et al 2015;Xu et al 2016;Jaacks et al 2018;Sarmento et al 2019;Graziani et al 2019) supported by observations (Robert et al 2019;Vanzella et al 2020) show that metals ejected in the ISM by SNe and AGB stars propagate from higher density peaks to lower density regions, allowing the co-existence of pristine and metal enriched objects in the pre-reionization epoch.…”

Section: Inhomogeneous Feedbackmentioning

confidence: 93%

Light, medium-weight, or heavy? The nature of the first supermassive black hole seeds

Sassano

Schneider

Valiante

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Observations of hyper-luminous quasars at z > 6 reveal the rapid growth of supermassive black holes (SMBHs $>10^9 \rm M_{\odot }$) whose origin is still difficult to explain. Their progenitors may have formed as remnants of massive, metal free stars (light seeds), via stellar collisions (medium-weight seeds) and/or massive gas clouds direct collapse (heavy seeds). In this work we investigate for the first time the relative role of these three seed populations in the formation of z > 6 SMBHs within an Eddington-limited gas accretion scenario. To this aim, we implement in our semi-analytical data-constrained model a statistical description of the spatial fluctuations of Lyman-Werner (LW) photo-dissociating radiation and of metal/dust enrichment. This allows us to set the physical conditions for BH seeds formation, exploring their relative birth rate in a highly biased region of the Universe at z > 6. We find that the inclusion of medium-weight seeds does not qualitatively change the growth history of the first SMBHs: although less massive seeds ($<10^3 \rm M_\odot$) form at a higher rate, the mass growth of a $\sim 10^9 \rm M_\odot$ SMBH at z < 15 is driven by efficient gas accretion (at a sub-Eddington rate) on to its heavy progenitors ($10^5 \rm M_\odot$). This conclusion holds independently of the critical level of LW radiation and even when medium-weight seeds are allowed to form in higher metallicity galaxies, via the so-called super-competitive accretion scenario. Our study suggests that the genealogy of z ∼ 6 SMBHs is characterized by a rich variety of BH progenitors, which represent only a small fraction ($< 10 - 20{{\ \rm per\ cent}}$) of all the BHs that seed galaxies at z > 15.

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Section: Inhomogeneous Feedbackmentioning

confidence: 93%

Light, medium-weight, or heavy? The nature of the first supermassive black hole seeds

Sassano

Schneider

Valiante

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…To address under what conditions JWST could detect the UV accretion disks of Pop III stellar-mass BHs lensed individually through cluster caustic transits at very high magnification, we first need to discuss their plausible range in physical properties, and under what conditions these may be fed from early massive stellar binaries for the expected range in IMF-slope (Fig. 2) and metallicity evolution (Sarmento et al 2019). For the Pop III ZAMS mass range in our MESA models, we adopt similar end-products as in Woosley et al (2002).…”

Section: A Parameters Adopted For Pop III Star Black Hole Accretionmentioning

confidence: 99%

On the Observability of Individual Population III Stars and Their Stellar-mass Black Hole Accretion Disks through Cluster Caustic Transits

Windhorst

Alpaslan

Andrews

et al. 2018

ApJS

112

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Recent near-infrared power-spectra and panchromatic Extragalactic Background Light (EBL) measurements provide upper limits on the integrated near-infrared surface brightness (SB > ∼ 31mag arcsec −2 at 2µm) that may come from Population III (Pop III) stars and possible accretion disks around resulting stellar-mass black holes (BHs) in the epoch of First Light, broadly taken from z 7-17. Physical parameters for zero metallicity Pop III stars at z > ∼ 7 can be estimated from MESA stellar evolution models through helium-depletion, and for BH accretion disks from quasar microlensing results and multicolor accretion models. Second-generation non-zero metallicity stars can form at higher multiplicity, so that BH accretion disks may be fed by Roche-lobe overflow from lower-mass companions in their AGB stage. The near-infrared SB constraints can be used to calculate the number of caustic transits behind lensing clusters that the James Webb Space Telescope (JWST) and the next generation 25-39 m ground-based telescopes may detect for both Pop III stars and stellar mass BH accretion disks. Because Pop III stars and stellar mass BH accretion disks have sizes of a few×10 −11 arcsec at z > ∼ 7, typical caustic magnifications can be µ 10 4 -10 5 , with rise times of hours and decline times of < ∼ 1 year for cluster transverse velocities of v T < ∼ 1000 km s −1 . Microlensing by intracluster medium objects can modify transit magnifications, and lengthen visibility times. Depending on BH masses, accretion-disk radii and feeding efficiencies, stellar-mass BH accretion-disk caustic transits could outnumber those from Pop III stars. To observe Pop III caustic transits directly may require monitoring 3-30 lensing clusters to AB < ∼ 29 mag over a decade or more. Such a program must be started with JWST at the start of Cycle 1, and -depending on the role of microlensing in the Intra Cluster Light (ICL) -should be continued for decades with the next generation 25-39 m ground-based telescopes, where both JWST and the ground-based facilities each will play a unique and strongly complementary role.

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“…III and Pop. II stars (e.g., Salvadori et al 2015;de Bennassuti et al 2017;Sarmento et al 2017;Chiaki et al 2018;Sarmento et al 2019).…”

Section: The Impact Of Host Galaxy Environment On Cemp-no Group Morphmentioning

confidence: 99%

Origin of the CEMP-no Group Morphology in the Milky Way

Yoon

Tian

Whitten

2019

ApJ

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The elemental-abundance signatures of the very first stars are imprinted on the atmospheres of CEMP-no stars, as various evidence suggests they are bona-fide second-generation stars. It has recently been recognized that the CEMP-no stars can be sub-divided into at least two groups, based on their distinct morphology in the A(C)-[Fe/H] space, indicating the likely existence of multiple pathways for their formation. In this work, we compare the halo CEMP-no group morphology with that of stars found in satellite dwarf galaxies of the Milky Way -a very similar A(C)-[Fe/H] pattern is found, providing clear evidence that halo CEMP-no stars were indeed accreted from their host mini-halos, similar in nature to those that formed in presently observed ultra faint dwarfs (UFDs) and dwarf spheroidal (dSph) galaxies. We also infer that the previously noted "anomalous" CEMP-no halo stars (with high A(C) and low [Ba/Fe] ratios) that otherwise would be associated with Group I may have the same origin as the Group III CEMP-no halo stars, by analogy with the location of several Group III CEMP-no stars in the UFDs and dSphs and their distinct separation from that of the CEMP-s stars in the A(Ba)-A(C) space. Interestingly, CEMP-no stars associated with UFDs include both Group II and Group III stars, while the more massive dSphs appear to have only Group II stars. We conclude that understanding the origin of the CEMP-no halo stars requires knowledge of the masses of their parent mini-halos, which is related to the amount of carbon dilution prior to star formation, in addition to the nature of their nucleosynthetic origin.

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Following the Cosmic Evolution of Pristine Gas. III. The Observational Consequences of the Unknown Properties of Population III Stars

Cited by 35 publications

References 113 publications

Light, medium-weight, or heavy? The nature of the first supermassive black hole seeds

Light, medium-weight, or heavy? The nature of the first supermassive black hole seeds

On the Observability of Individual Population III Stars and Their Stellar-mass Black Hole Accretion Disks through Cluster Caustic Transits

Origin of the CEMP-no Group Morphology in the Milky Way

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