The Star Formation Rate in the Reionization Era as Indicated by Gamma-Ray Bursts

Kistler, Matthew D.; Yüksel, Hasan; Beacom, J. F.; Hopkins, A. M.; Wyithe, J. Stuart B.

doi:10.1088/0004-637x/705/2/l104

Cited by 296 publications

(420 citation statements)

References 46 publications

(65 reference statements)

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“…Some examples of CSFR measurements which differ substantially from the trend shown by the data collected by MD14 can be found in, e.g., Faucher-Giguére et al (2008) and Kistler et al (2009).…”

Section: Csfr: Cosmic Star Formation Ratementioning

confidence: 86%

The cosmic dust rate across the Universe

Gioannini¹,

Matteuccí

Calura

2017

Monthly Notices of the Royal Astronomical Society

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We investigate the evolution of interstellar dust in the Universe by means of chemical evolution models of galaxies of different morphological types, reproducing the main observed features of present day galaxies. We adopt the most updated prescriptions for dust production from supernovae and asymptotic giant branch (AGB) stars as well as for dust accretion and destruction processes. Then, we study the cosmic dust rate in the framework of three different cosmological scenarios for galaxy formation: i) a pure luminosity scenario (PLE), ii) a number density evolution scenario (DE), as suggested by the classical hierarchical clustering scenario and iii) an alternative scenario, in which both spirals and ellipticals are allowed to evolve in number on an observationally motivated basis. Our results give predictions about the evolution of the dust content in different galaxies as well as the cosmic dust rate as a function of redshift. Concerning the cosmic dust rate, the best scenario is the alternative one, which predicts a peak at 2 < z < 3 and reproduces the cosmic star formation rate. We compute the evolution of the comoving dust density parameter Ω dust and find agreement with data for z < 0.5 in the framework of DE and alternative scenarios. Finally, the evolution of the average cosmic metallicity is presented and it shows a quite fast increase in each scenario, reaching the solar value at the present time, although most of the heavy elements are incorporated into solid grains, and therefore not observable in the gas phase.

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Section: Csfr: Cosmic Star Formation Ratementioning

confidence: 86%

The cosmic dust rate across the Universe

Gioannini¹,

Matteuccí

Calura

2017

Monthly Notices of the Royal Astronomical Society

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“…The first results obtained on host galaxy samples showed that they were primarily blue with lowmass, and low-metallicity (e.g., Fruchter et al 1999;Le Floc'h et al 2003;Berger et al 2003;Christensen, Hjorth & Gorosabel 2004;Tanvir et al 2004;Savaglio, Glazebrook & Le Borgne 2009) and suggested that the metallicity of the host could be a proxy for the progenitor. Such proxies exerted a strict metallicity-cut (e.g., Langer & Norman 2006;Salvaterra & Chincarini 2007;Butler, Bloom & Poznanski 2010;Elliott et al 2012), such that only host galaxies below a given value could host a LGRB, which lead to predictions that the CSFH flattens at higher redshifts (e.g., Kistler et al 2009;Salvaterra et al 2012). However, these host galaxy studies were optically biased, which when accounted for, systematically more massive galaxies were found (e.g., Krühler et al 2011;Rossi et al 2012).…”

Section: Manymentioning

confidence: 99%

“…1. We compare it to several values obtained from the literature, de- termined from star-forming galaxies (Mannucci et al 2007;Bouwens et al 2008;Li 2008), Lyman-break galaxies (Laporte et al 2012;Zheng et al 2012), Lyman-α emitters (Ota et al 2008), and LGRBs (Kistler et al 2009;Ishida, de Souza & Ferrara 2011) that reach a redshift of z ∼ 10. Both the CSFH of the FiBY simulation and the measured distribution are seen to be consistent throughout redshift.…”

Section: Cosmic Star Formation Historymentioning

confidence: 99%

The First Billion Years project: gamma-ray bursts at z > 5

Elliott

Khochfar

Greiner

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Long gamma-ray burst's (LGRB's) association to the death of massive stars suggest they could be used to probe the cosmic star formation history (CSFH) with high accuracy, due to their high luminosities. We utilise cosmological simulations from the First Billion Years project to investigate the biases between the CSFH and the LGRB rate at z > 5, assuming various different models and constraints on the progenitors of LGRBs. We populate LGRBs using a selection based on environmental properties and demonstrate that the LGRB rate should trace the CSFH to high redshifts. The measured LGRB rate suggests that LGRBs have opening angles of θ jet = 0.1 • , although the degeneracy with the progenitor model cannot rule out an underlying bias. We demonstrate that proxies that relate the LGRB rate with global LGRB host properties do not reflect the underlying LGRB environment, and are in fact a result of the host galaxy's spatial properties, such that LGRBs can exist in galaxies of solar metallicity. However, we find a class of host galaxies that have low stellar mass and are metal-rich, and that their metallicity dispersions would not allow low-metallicity environments. Detection of hosts with this set of properties would directly reflect the progenitor's environment. We predict that 10% of LGRBs per year are associated with this set of galaxies that would have forbidden line emission that could be detected by instruments on the James Webb Space Telescope. Such a discovery would place strong constraints on the collapsar model and suggest other avenues to be investigated.

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“…Evolution with z of the Star Formation Efficiency (SFE) defined by the ratio between far-infrared luminosity and molecular gas mass (LFIR /M(H2 )), for the sources detected between 0.2 < z < 0.6 (black full dots, and upward-arrows), compared with other detections in the literature (cf Combes et al 2010). The red curve is a schematic line summarizing the cosmic star formation history, from the compilation by Hopkins & Beacom (2006), implemented with the GRB data by Kistler et al (2009), and the optical data from Bouwens et al (2008).…”

Section: F Combesmentioning

confidence: 99%

Molecular Gas in Galaxies at all Redshifts

Combes¹

2010

Proc. IAU

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Abstract. I review some recent results about the molecular content of galaxies, obtained essentially from the CO lines, but also dense tracers, or the dust continuum emission. New results have been obtained on molecular cloud physics, and their efficiency to form stars, shedding light on the Kennicutt-Schmidt law as a function of surface density and galaxy type. Large progress has been made on galaxy at moderate and high redshifts, allowing to interprete the star formation history and star formation efficiency as a function of gas content, or galaxy evolution. In massive galaxies, the gas fraction was higher in the past, and galaxy disks were more unstable and more turbulent. ALMA observations will allow the study of more normal galaxies at high z with higher spatial resolution and sensitivity.Keywords. galaxies: general, galaxies: high-redshift, galaxies: evolution, ISM: molecule, galaxies: ISM, galaxies: spiral, galaxies: starburst, galaxies: structure Nearby galaxiesA new survey (HERACLES) has been completed with the IRAM receiver array in the CO(2-1) line, allowing extended maps of nearby galaxies, at 12" resolution (Leroy et al. 2009). The survey contains an atlas of 18 nearby galaxies, observed at multi-wavelengths, and in particular in the HI line, and in the mid infrared by Spitzer. Among the results, it is interesting to note a very good correlation between CO and HI kinematics. The excitation of the molecular gas, as traced by the first two rotational lines of CO, is usually low in the disk (R = CO(2-1)/CO(1-0) = 0.6) while it is higher in nuclei (R = 1), indicating denser gas. The CO emission is compatible with optically thick clouds at a kinetic temperature of T = 10K.A more refined view of the star formation law in galaxies has been obtained by Bigiel et al. (2008). The Schmidt-Kennicutt law relating star formation and gas density has a different slope n, according to the gas surface density. At high surface density, when the gas is molecular, the gas forms stars at a constant efficiency (n = 1), and the time-scale for star formation is 2 10 9 yrs. While, at low surface density, when the gas is atomic, the slope is much higher n = 2 or more. At sub-kpc scale, the star formation rate is not strongly correlated with HI surface density. The transition between HI and H 2 occurs when the surface density is > 9 M pc −2 .In order to better determine the change across the spiral arms of the molecular gas physical properties, Schinnerer et al. (2010) have mapped at interferometric resolution several lines of CO and its isotopes, together with dense gas tracers, such as HCN and HCO + , in two selected regions across M51 spiral arms. They find no change across the arms, and the GMC population in the spiral arms of M51 is similar to those of the Milky Way, even if the star formation rate is much higher.On the contrary, the low surface brightness dwarf spiral M33 reveals different conditions than in the Milky Way. In the center, the lower metallicity is the cause of a higher conversion factor, as will be describ...

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The Star Formation Rate in the Reionization Era as Indicated by Gamma-Ray Bursts

Cited by 296 publications

References 46 publications

The cosmic dust rate across the Universe

The cosmic dust rate across the Universe

The First Billion Years project: gamma-ray bursts at z > 5

Molecular Gas in Galaxies at all Redshifts

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