Dust grain growth in the interstellar medium of 5 &lt; z &lt; 6.5 quasars

Michałowski, M. J.; Murphy, E. J.; Hjorth, J.; Watson, Derrick G.; Gall, C.; Dunlop, James

doi:10.1051/0004-6361/201014902

Cited by 99 publications

(110 citation statements)

References 91 publications

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“…This process is simply referred to as accretion in this paper. Including accretion into dust evolution models is motivated not only to explain the dust abundance in nearby galaxies (Hirashita 1999;Inoue 2011;Zhukovska & Henning 2013;de Bennassuti et al 2014;Schneider et al 2014), but also to explain the observations of huge amounts of dust (∼ 10 8 M⊙) in high-z quasars and starbursts (Michałowski et al 2010;Mattsson 2011;Valiante et al 2011;Kuo & Hirashita 2012;Rowlands et al 2014;Nozawa et al 2015). Grain growth by accretion occurs efficiently only after the ISM is significantly enriched with dust and metals, since the grain growth rate is proportional to the collision rate between these two components.…”

Section: Review Of the Processesmentioning

confidence: 99%

Two-size approximation: a simple way of treating the evolution of grain size distribution in galaxies

Hirashita

2015

Monthly Notices of the Royal Astronomical Society

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Full calculations of the evolution of grain size distribution in galaxies are in general computationally heavy. In this paper, we propose a simple model of dust enrichment in a galaxy with a simplified treatment of grain size distribution by imposing a 'two-size approximation'; that is, all the grain population is represented by small (grain radius a < 0.03 µm) and large (a > 0.03 µm) grains. We include in the model dust supply from stellar ejecta, destruction in supernova shocks, dust growth by accretion, grain growth by coagulation and grain disruption by shattering, considering how these processes work on the small and large grains. We show that this simple framework reproduces the main features found in full calculations of grain size distributions as follows. The dust enrichment starts with the supply of large grains from stars. At a metallicity level referred to as the critical metallicity of accretion, the abundance of the small grains formed by shattering becomes large enough to rapidly increase the grain abundance by accretion. Associated with this epoch, the mass ratio of the small grains to the large grains reaches the maximum. After that, this ratio converges to the value determined by the balance between shattering and coagulation, and the dust-to-metal ratio is determined by the balance between accretion and shock destruction. With a Monte Carlo simulation, we demonstrate that the simplicity of our model has an advantage in predicting statistical properties. We also show some applications for predicting observational dust properties such as extinction curves.

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Section: Review Of the Processesmentioning

confidence: 99%

Two-size approximation: a simple way of treating the evolution of grain size distribution in galaxies

Hirashita

2015

Monthly Notices of the Royal Astronomical Society

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“…6), and inferred observationally (Dunne et al , 2009bMorgan et al 2003;Gomez et al 2009;Green et al 2004;Ercolano et al 2007;Meikle et al 2007;Lee et al 2009;Sibthorpe et al 2010;Barlow et al 2010). Given the possibility of rapid (∼10 Myr) dust grain growth in the ISM (Draine & Salpeter 1979;Draine 1990Draine , 2009Hirashita 2000;Zhukovska et al 2008;Michałowski et al 2010b), which would lower the required dust yield per star, it is not unreasonable to assume that the dust present in the WR region could have been formed during a short (∼10 Myr) recent period of star formation, even if it had contained no pre-existing dust formed by AGB stars. Moreover, these massive stars would alone produce enough metals necessary for this dust production (not counting metals produced by older AGB stars).…”

Section: Dust and Star Formation In The Wr Region: High Densitymentioning

confidence: 99%

Spatially-resolved dust properties of the GRB 980425 host galaxy

Michałowski

Hunt

Palazzi

et al. 2014

A&A

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Gamma-ray bursts (GRBs) have been proposed as a tool for studying star formation in the Universe, so it is crucial to investigate whether their host galaxies and immediate environments are in any way special compared with other star-forming galaxies. Here we present spatially resolved maps of dust emission of the host galaxy of the closest known GRB 980425 at z = 0.0085 using our new high-resolution observations from Herschel, Atacama Pathfinder Experiment (APEX), Atacama Large Millimeter Array (ALMA) and Australia Telescope Compact Array (ATCA). We modelled the spectral energy distributions of the host and of the star-forming region displaying the Wolf-Rayet signatures in the spectrum (WR region), located 800 pc from the GRB position. The host is characterised by low dust content and a high fraction of UV-visible star formation, similar to other dwarf galaxies. These galaxies are abundant in the local universe, so it is not surprising to find a GRB in one of them, assuming the correspondence between the GRB rate and star formation. The WR region contributes substantially to the host emission at the far-infrared, millimetre, and radio wavelengths and we propose that this is a consequence of its high gas density. If dense environments are also found close to the positions of other GRBs, then the ISM density should also be considered, along with metallicity, an important factor influencing whether a given stellar population can produce a GRB.

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“…Despite the included detailed treatment of the dust contribution from stellar sources in the developed model, the poorly understood dust production by SNe, but also dust destruction by SN shock interactions, very likely constitute the largest uncertainties in the evolution of dust. Although not included in the model, alternative dust sources such as dust grain growth in the ISM might be relevant (e.g., Dwek et al 2007;Draine 2009;Michałowski et al 2010b). …”

Section: Caveats In Our Approachmentioning

confidence: 99%

Genesis and evolution of dust in galaxies in the early Universe

Gall

Andersen

Hjorth

2011

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Aims. The aim is to elucidate the astrophysical conditions required for generating large amounts of dust in massive starburst galaxies at high redshift. Methods. We have developed a numerical galactic chemical evolution model. The model is constructed such that the effect of a wide range of parameters can be investigated. It takes into account results from stellar evolution models, a differentiation between diverse types of core collapse supernovae (CCSN), and the contribution of asymptotic giant branch (AGB) stars in the mass range 3-8 M . We consider the lifetime-dependent yield injection into the interstellar medium (ISM) by all sources, and dust destruction due to supernova (SN) shocks in the ISM. We ascertain the temporal progression of the dust mass and the dust-to-gas and dust-to-metal mass ratios, as well as other physical properties of a galaxy, and study their dependence on the mass of the galaxy, the initial mass function (IMF), dust production efficiencies, and dust destruction in the ISM. Results. The amount of dust and the physical properties of a galaxy strongly depend on the initial gas mass available. Overall, while the total amount of dust produced increases with galaxy mass, the detailed outcome depends on the SN dust production efficiency, the IMF, and the strength of dust destruction in the ISM. Dust masses are higher for IMFs biased towards higher stellar masses, even though these IMFs are more strongly affected by dust destruction in the ISM. The sensitivity to the IMF increases as the mass of the galaxy decreases. SNe are primarily responsible for a significant enrichment with dust at early epochs (<200 Myr). Dust production with a dominant contribution by AGB stars is found to be insufficient to account for dust masses in excess of 10 8 M within 400 Myr after starburst. Conclusions. We find that galaxies with initial gas masses between 1-5 × 10 11 M are massive enough to enable production of dust masses >10 8 M . Our preferred scenario is dominated by SN dust production in combination with top-heavy IMFs and moderate dust destruction in the ISM.

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Dust grain growth in the interstellar medium of 5 < z < 6.5 quasars

Cited by 99 publications

References 91 publications

Two-size approximation: a simple way of treating the evolution of grain size distribution in galaxies

Two-size approximation: a simple way of treating the evolution of grain size distribution in galaxies

Spatially-resolved dust properties of the GRB 980425 host galaxy

Genesis and evolution of dust in galaxies in the early Universe

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