2016
DOI: 10.1093/mnras/stw788
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Physical conditions in three high-zH2-bearing DLAs: implications for grain size

Abstract: We present results of our numerical simulation of three H2-bearing damped Lyman α absorbers (DLAs) in the redshift interval ~ 2-3. The systems we have modelled are the DLAs at zabs = 2.3377 towards the quasar LBQS 1232+0815, at zabs = 2.41837 towards SDSS J143912.04+111740.5 and at zabs = 2.6265 towards FBQS J081240.6+320808. We have used the spectral synthesis code CLOUDY to simulate the physical environment of these DLAs, and constrain the density, radiation field, geometry and dust-grain properties of the D… Show more

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Cited by 23 publications
(27 citation statements)
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References 79 publications
(135 reference statements)
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“…The chosen radiation field has three components: a meta-galactic radiation at appropriate redshift (Haardt & Madau 2012), a synchrotron radiation (power-law continuum) arising from GRB afterglow and a blackbody radiation from in situ star formation. Our GRB-DLA models are similar to our previous QSO-DLA models (Srianand et al 2005a;Shaw et al 2016;Rawlins et al 2018) except that here we have an additional synchrotron radiation arising from GRB afterglows. While the gas is exposed to UV radiation from everywhere it is exposed to GRB afterglow only from one side.…”
Section: Modellingsupporting
confidence: 84%
“…The chosen radiation field has three components: a meta-galactic radiation at appropriate redshift (Haardt & Madau 2012), a synchrotron radiation (power-law continuum) arising from GRB afterglow and a blackbody radiation from in situ star formation. Our GRB-DLA models are similar to our previous QSO-DLA models (Srianand et al 2005a;Shaw et al 2016;Rawlins et al 2018) except that here we have an additional synchrotron radiation arising from GRB afterglows. While the gas is exposed to UV radiation from everywhere it is exposed to GRB afterglow only from one side.…”
Section: Modellingsupporting
confidence: 84%
“…The dust-to-gas ratio in this system could be higher than that observed in the SMC, i.e. κ could be greater than unity, as is possible in high-z absorbers due to different grain chemistry or size (see Shaw et al 2016;Noterdaeme et al 2017;Dutta et al 2017b;Rawlins et al 2018). This is similar to what is inferred from the lack of H i 21-cm absorption towards the red quasar J0956+4046 (see Section 2.1.1 and Gupta et al 2012).…”
Section: H I 21-cm Absorption Towards J1521+5508supporting
confidence: 75%
“…In other words, a higher total surface of grains favours CO production without going too deep into the cloud. Shaw et al (2016) also highlight the need of increased grain surface area to reproduce the CO column density towards SDSS J1439+1117 .…”
Section: Model With Small Dust Grainsmentioning
confidence: 88%