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dc.contributor.authorGarel, Thibaulten
dc.contributor.authorBlaizot, Jérémyen
dc.contributor.authorRosdahl, Joakimen
dc.contributor.authorMichel-Dansac, Léoen
dc.contributor.authorHaehnelt, Martinen
dc.contributor.authorKatz, Harleyen
dc.contributor.authorKimm, Taysunen
dc.contributor.authorVerhamme, Anneen
dc.date.accessioned2021-04-19T23:31:49Z
dc.date.available2021-04-19T23:31:49Z
dc.identifier.issn0035-8711
dc.identifier.urihttps://www.repository.cam.ac.uk/handle/1810/321315
dc.description.abstractThe Ly$\alpha$ emission line is one of the most promising probes of cosmic reionisation but isolating the signature of a change in the ionisation state of the IGM is challenging because of intrinsic evolution and internal radiation transfer effects. We present the first study of the evolution of Ly$\alpha$ emitters (LAE) during the epoch of reionisation based on a full radiation-hydrodynamics cosmological simulation that is able to capture both the large-scale process of reionisation and the small-scale properties of galaxies. We predict the Ly$\alpha$ emission of galaxies in the $10^3$ cMpc$^3$ SPHINX simulation at $6\leq z\leq9$ by computing the full Ly$\alpha$ radiation transfer from ISM to IGM scales. SPHINX is able to reproduce many observational constraints such as the UV/Ly$\alpha$ luminosity functions and stellar mass functions at z $\geq$ 6 for the dynamical range probed by our simulation ($M_{\rm 1500}\gtrsim-18$, $L_{\rm Ly\alpha}\lesssim10^{42}$ erg/s, $M_{\star}\lesssim10^9$ M$_{\odot}$). As intrinsic Ly$\alpha$ emission and internal Ly$\alpha$ escape fractions barely evolve from $z=6$ to 9, the observed suppression of Ly$\alpha$ luminosities with increasing redshift is fully attributed to IGM absorption. For most observable galaxies ($M_{\rm 1500}\lesssim-16$), the Ly$\alpha$ line profiles are slightly shifted to the red due to internal radiative transfer effects which mitigates the effect of IGM absorption. Overall, the enhanced Ly$\alpha$ suppression during reionisation traces the IGM neutral fraction $x_{\rm HI}$ well but the predicted amplitude of this reduction is a strong function of the Ly$\alpha$ peak shift, which is set at ISM/CGM scales. We find that a large number of LAEs could be detectable in very deep surveys during reionisation when $x_{\rm HI}$ is still $\approx 50\%$.
dc.publisherRoyal Astronomical Society
dc.rightsAll rights reserved
dc.titleLy $α$ as a tracer of cosmic reionization in the SPHINX radiation-hydrodynamics cosmological simulationen
dc.typeArticle
prism.endingPage1926
prism.issueIdentifier2en
prism.publicationNameMonthly Notices of the Royal Astronomical Societyen
prism.startingPage1902
prism.volume504en
dc.identifier.doi10.17863/CAM.68439
dcterms.dateAccepted2021-04-07en
rioxxterms.versionofrecord10.1093/mnras/stab990en
rioxxterms.versionVoR
rioxxterms.licenseref.urihttp://www.rioxx.net/licenses/all-rights-reserveden
rioxxterms.licenseref.startdate2021-04-07en
dc.contributor.orcidHaehnelt, Martin [0000-0001-8443-2393]
dc.identifier.eissn1365-2966
rioxxterms.typeJournal Article/Reviewen
pubs.funder-project-idSTFC (ST/S000623/1)
pubs.funder-project-idSCIENCE & TECHNOLOGY FACILITIES COUNCIL (ST/N000927/1)
cam.issuedOnline2021-04-14en
cam.orpheus.successMon Jun 14 07:30:46 BST 2021 - The item has an open VoR version.*
cam.orpheus.counter7*
rioxxterms.freetoread.startdate2100-01-01


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