Evolution of the observed Ly α luminosity function from z = 6.5 to z = 7.7: Evidence for the epoch of reionization?

dc.contributor.authorClément, B.en
dc.contributor.authorCuby, J. G.en
dc.contributor.authorCourbin, F.en
dc.contributor.authorFontana, A.en
dc.contributor.authorFreudling, W.en
dc.contributor.authorFynbo, J.en
dc.contributor.authorGallego, J.en
dc.contributor.authorHibon, P.en
dc.contributor.authorKneib, J. P.en
dc.contributor.authorLe Fèvre, O.en
dc.contributor.authorLidman, C.en
dc.contributor.authorMcMahon, R.en
dc.contributor.authorMilvang-Jensen, B.en
dc.contributor.authorMoller, P.en
dc.contributor.authorMoorwood, A.en
dc.contributor.authorNilsson, K. K.en
dc.contributor.authorPentericci, L.en
dc.contributor.authorVenemans, B.en
dc.contributor.authorVillar, V.en
dc.contributor.authorWillis, J.en
dc.date.accessioned2026-01-01T13:41:22Z
dc.date.available2026-01-01T13:41:22Z
dc.date.issued2012en
dc.description.abstractAims. Lyα emitters (LAEs) can be detected out to very high redshifts during the epoch of reionization. The evolution of the LAE luminosity function with redshift is a direct probe of the Lyα transmission of the intergalactic medium (IGM), and therefore of the IGM neutral-hydrogen fraction. Measuring the Lyα luminosity function (LF) of Lyα emitters at redshift z = 7.7 therefore allows us to constrain the ionizing state of the Universe at this redshift. Methods. We observed three 7′.5 × 7′.5 fields with the HAWK-I instrument at the VLT with a narrow band filter centred at 1.06 μm and targeting Lyα emitters at redshift z ∼ 7.7. The fields were chosen for the availability of multiwavelength data. One field is a galaxy cluster, the Bullet Cluster, which allowed us to use gravitational amplification to probe luminosities that are fainter than in the field. The two other fields are subareas of the GOODS Chandra Deep Field South and CFHTLS-D4 deep field. We selected z = 7.7 LAE candidates from a variety of colour criteria, in particular from the absence of detection in the optical bands. Results. We do not find any LAE candidates at z = 7.7 in ∼2.4 × 10 4 Mpc 3 down to a narrow band AB magnitude of ∼26, which allows us to infer robust constraints on the Lyα LAE luminosity function at this redshift. Conclusions. The predicted mean number of objects at z = 6.5, derived from somewhat different luminosity functions of Hu et al. (2010, ApJ, 725, 394), Ouchi et al. (2010, ApJ, 723, 869), and Kashikawa et al. (2011, ApJ, 734, 119) are 2.5, 13.7, and 11.6, respectively. Depending on which of these luminosity functions we refer to, we exclude a scenario with no evolution from z = 6.5 to z = 7.7 at 85% confidence without requiring a strong change in the IGM Lyα transmission, or at 99% confidence with a significant quenching of the IGM Lyα transmission, possibly from a strong increase in the high neutral-hydrogen fraction between these two redshifts.en
dc.description.sponsorshipWe acknowledge financial support from Agence Nationale de la Recherche (grant ANR-09-BLAN-0234-01). F.C. is supported by the Swiss National Science Foundation (SNSF). The Dark Cosmology Centre is funded by the Danish National Research Foundation.en
dc.description.statusPeer-revieweden
dc.identifier.issn0004-6361en
dc.identifier.scopus84856754670en
dc.identifier.urihttps://hdl.handle.net/1885/733800674
dc.language.isoenen
dc.sourceAstronomy and Astrophysicsen
dc.subjectdark ages, reionization, first starsen
dc.subjectearly Universeen
dc.subjectgalaxies: high-redshiften
dc.subjectgalaxies: luminosity function, mass functionen
dc.subjectmethods: observationalen
dc.subjecttechniques: image processingen
dc.titleEvolution of the observed Ly α luminosity function from z = 6.5 to z = 7.7: Evidence for the epoch of reionization?en
dc.typeJournal articleen
dspace.entity.typePublicationen
local.contributor.affiliationClément, B.; Aix Marseille Universitéen
local.contributor.affiliationCuby, J. G.; Aix Marseille Universitéen
local.contributor.affiliationCourbin, F.; Swiss Federal Institute of Technology Lausanneen
local.contributor.affiliationFontana, A.; Osservatorio Astronomico Romaen
local.contributor.affiliationFreudling, W.; European Southern Observatoryen
local.contributor.affiliationFynbo, J.; University of Copenhagenen
local.contributor.affiliationGallego, J.; Complutense Universityen
local.contributor.affiliationHibon, P.; Arizona State Universityen
local.contributor.affiliationKneib, J. P.; Aix Marseille Universitéen
local.contributor.affiliationLe Fèvre, O.; Aix Marseille Universitéen
local.contributor.affiliationLidman, C.; Australian Astronomical Observatoryen
local.contributor.affiliationMcMahon, R.; University of Cambridgeen
local.contributor.affiliationMilvang-Jensen, B.; University of Copenhagenen
local.contributor.affiliationMoller, P.; European Southern Observatoryen
local.contributor.affiliationMoorwood, A.; European Southern Observatoryen
local.contributor.affiliationNilsson, K. K.; European Southern Observatoryen
local.contributor.affiliationPentericci, L.; Osservatorio Astronomico Romaen
local.contributor.affiliationVenemans, B.; European Southern Observatoryen
local.contributor.affiliationVillar, V.; Complutense Universityen
local.contributor.affiliationWillis, J.; University of Victoria BCen
local.identifier.citationvolume538en
local.identifier.doi10.1051/0004-6361/201117312en
local.identifier.pure04ed4686-6998-47f5-886d-1cf3ee5a622een
local.identifier.urlhttps://www.scopus.com/pages/publications/84856754670en
local.type.statusPublisheden

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