Tracing the Evolution of High Redshift Galaxies Using Stellar Abundances

Crosby, Brian D.; O’Shea, Brian W.; Tumlinson, Jason

doi:10.48550/arxiv.1312.0606

Cited by 4 publications

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“…Zahn et al 2011;Alvarez et al 2012), (iii) subgrid models of unresolved star formation (Trenti & Stiavelli 2007), and (iv) chemical evolution models (e.g. Salvadori et al 2007;Tumlinson 2010;Crosby et al 2013). For instance, including halos that host low levels of star formation into a reionization calculation would produce a more extended reionization history, better matching constraints provided by the cosmic microwave background (Zahn et al 2012;Planck Collaboration et al 2013) and the z ∼ 6 Gunn-Peterson troughs (Fan et al 2006).…”

Section: Discussionmentioning

confidence: 99%

Scaling Relations for Galaxies Prior to Reionization

Chen

Wise

Norman

et al. 2014

ApJ

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The first galaxies in the Universe are the building blocks of all observed galaxies. We present scaling relations for galaxies forming at redshifts z ≥ 15 when reionization is just beginning. We utilize the "Rarepeak" cosmological radiation hydrodynamics simulation that captures the complete star formation history in over 3,300 galaxies, starting with massive Population III stars that form in dark matter halos as small as ∼10 6 M . We make various correlations between the bulk halo quantities, such as virial, gas, and stellar masses and metallicities and their respective accretion rates, quantifying a variety of properties of the first galaxies up to halo masses of 10 9 M . Galaxy formation is not solely relegated to atomic cooling halos with virial temperatures greater than 10 4 K, where we find a dichotomy in galaxy properties between halos above and below this critical mass scale. Halos below the atomic cooling limit have a stellar mass -halo mass relationship log M 3.5 + 1.3 log(M vir /10 7 M ). We find a non-monotonic relationship between metallicity and halo mass for the smallest galaxies. Their initial star formation events enrich the interstellar medium and subsequent star formation to a median of 10 −2 Z and 10 −1.5 Z , respectively, in halos of total mass 10 7 M that is then diluted by metal-poor inflows, well beyond Population III pre-enrichment levels of 10 −3.5 Z . The scaling relations presented here can be employed in models of reionization, galaxy formation and chemical evolution in order to consider these galaxies forming prior to reionization.

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Section: Discussionmentioning

confidence: 99%

Scaling Relations for Galaxies Prior to Reionization

Chen

Wise

Norman

et al. 2014

ApJ

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“…The ISM was treated as a multiphase gas with a central region of dense, cold gas that is capable of forming stars and a hot, diffuse region exterior to the star-forming central region that is incapable of forming stars. For more details see the work of Crosby et al (2013b); Crosby et al (2013a).…”

Section: Lw Feedbackmentioning

confidence: 99%

Tracing the first stars and galaxies of the Milky Way

Griffen

Dooley

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We use 30 high-resolution dark matter halos of the Caterpillar simulation suite to probe the first stars and galaxies of Milky Way-mass systems. We quantify the environment of the high-z progenitors of the Milky Way and connect them to the properties of the host and satellites today. We identify the formation sites of the first generation of Population III (Pop III) stars (z ∼ 25) and first galaxies (z ∼ 22) with several different models based on a minimum halo mass including a simple model for Lyman-Werner feedback. Through this method we find approximately 23,000 ± 5,000 Pop III potentially star-forming sites per Milky Way-mass host, though this number is drastically reduced to ∼550 star-forming sites when Lyman-Werner feedback is included, as it has critical effects at these length scales. The majority of these halos identified form in isolation (96% at z = 15) and are not subject to external enrichment by neighboring halos (median separation ∼1 pkpc at z = 15), though half merge with a system larger than themselves within 1.5 Gyrs. Approximately 55% of the entire population has merged into the host halo by z = 0. Using particle tagging, we additionally trace the Pop III remnant population to z = 0 and find an order of magnitude scatter in their number density at small (i.e. r < 5 kpc) and large (i.e. r > 50 kpc) galactocentric radii at z = 0. Using our large number of realizations, we provide fitting functions for determining the number of progenitor minihalo and atomic cooling halo systems that present-day dwarf galaxies and the Magellanic cloud system might have accreted since their formation. We demonstrate that observed dwarf galaxies with stellar masses below 10 4.6 M are unlikely to have merged with any other star-forming systems.

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“…Metal enrichment involves complex interactions between SNe blastwaves, the IGM, halo mergers, and cosmological accretion. This topic has been extensively studied with semi-analytic models (Scannapieco et al 2003;Yoshida et al 2004;Tumlinson 2006;Salvadori et al 2007;Komiya et al 2010;Gómez et al 2012;Crosby et al 2013a), postprocessing of numerical simulations (Karlsson et al 2008;Trenti et al 2009), and direct numerical simulations (Tornatore et al 2007;Ricotti et al 2008;Maio et al 2010;Wise et al 2012b;Muratov et al 2013b;Xu et al 2013). Studies have suggested that Pop III stars may continue to form at low redshifts to the end of reionization.…”

Section: Introductionmentioning

confidence: 99%

Heating the Intergalactic Medium by X-Rays From Population Iii Binaries in High-Redshift Galaxies

Ahn

Wise

et al. 2014

ApJ

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Due to their long mean free path, X-rays are expected to have an important impact on cosmic reionization by heating and ionizing the intergalactic medium (IGM) on large scales, especially after simulations have suggested that Population III (Pop III) stars may form in pairs at redshifts as high as 20 -30. We use the Pop III distribution and evolution from a self-consistent cosmological radiation hydrodynamic simulation of the formation of the first galaxies and a simple Pop III X-ray binary model to estimate their X-ray output in a high-density region larger than 100 comoving (Mpc) 3 . We then combine three different methods -ray tracing, a one-zone model, and X-ray background modeling -to investigate the X-ray propagation, intensity distribution, and long-term effects on the IGM thermal and ionization state. The efficiency and morphology of photoheating and photoionization are dependent on the photon energies. The sub-keV X-rays only impact the IGM near the sources, while the keV photons contribute significantly to the X-ray background and heat and ionize the IGM smoothly. The X-rays just below 1 keV are most efficient in heating and ionizing the IGM. We find that the IGM might be heated to over 100 K by z = 10 and the high-density source region might reach 10 4 K, limited by atomic hydrogen cooling. This may be important for predicting the 21 cm neutral hydrogen signals. On the other hand, the free electrons from X-ray ionizations are not enough to contribute significantly to the optical depth of the cosmic microwave background to the Thomson scattering.

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Tracing the Evolution of High Redshift Galaxies Using Stellar Abundances

Cited by 4 publications

References 0 publications

Scaling Relations for Galaxies Prior to Reionization

Scaling Relations for Galaxies Prior to Reionization

Tracing the first stars and galaxies of the Milky Way

Heating the Intergalactic Medium by X-Rays From Population Iii Binaries in High-Redshift Galaxies

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