Narrow-band surveys for very high redshift Lyman-alpha emitters

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dc.contributor.authorNilsson, K. K.
dc.contributor.authorOrsi, A.
dc.contributor.authorLacey, C. G.
dc.contributor.authorBaugh, C. M.
dc.contributor.authorThommes, E.
dc.date.accessioned2024-01-10T13:15:22Z
dc.date.available2024-01-10T13:15:22Z
dc.date.issued2007
dc.description.abstractContext. Many current and future surveys aim to detect the highest redshift ( z greater than or similar to 7) sources through their Lyman-alpha (Ly alpha) emission, using the narrow- band imaging method. However, to date the surveys have only yielded non- detections and upper limits as no survey has reached the necessary combination of depth and area to detect these very young star forming galaxies.
dc.description.abstractAims. We aim to calculate model luminosity functions and mock surveys of Ly alpha emitters at z greater than or similar to 7 based on a variety of approaches calibrated and tested on observational data at lower redshifts.
dc.description.abstractMethods. We calculate model luminosity functions at different redshifts based on three different approaches: a semi-analytical model based on CDM, a simple phenomenological model, and an extrapolation of observed Schechter functions at lower redshifts. The results of the first two models are compared with observations made at redshifts z similar to 5.7 and z similar to 6.5, and they are then extrapolated to higher redshift.
dc.description.abstractResults. We present model luminosity functions for redshifts between z = 7-12.5 and give specific number predictions for future planned or possible narrow- band surveys for Ly alpha emitters. We also investigate what constraints future observations will be able to place on the Ly alpha luminosity function at very high redshift.
dc.description.abstractConclusions. It should be possible to observe z = 7- 10 Ly alpha emitters with present or near-future instruments if enough observing time is allocated. In particular, large area surveys such as ELVIS ( Emission Line galaxies with VISTA Survey) will be useful in collecting a large sample. However, to get a large enough sample to constrain well the z greater than or similar to 10 Ly alpha luminosity function, instruments further in the future, such as an ELT, will be necessary.
dc.fechaingreso.objetodigital2024-05-07
dc.format.extent8 páginas
dc.fuente.origenWOS
dc.identifier.doi10.1051/0004-6361:20077913
dc.identifier.issn1432-0746
dc.identifier.urihttps://doi.org/10.1051/0004-6361:20077913
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/78495
dc.identifier.wosidWOS:000250106100011
dc.information.autorucBachillerato;Orsi A;S/I;127321
dc.issue.numero2
dc.language.isoen
dc.nota.accesocontenido parcial
dc.pagina.final392
dc.pagina.inicio385
dc.publisherEDP SCIENCES S A
dc.revistaASTRONOMY & ASTROPHYSICS
dc.rightsacceso restringido
dc.subjectcosmology : theory
dc.subjectcosmology : early Universe
dc.subjectgalaxies : high-redshift
dc.subjectsurveys
dc.subjectSUBARU DEEP FIELD
dc.subjectGUNN-PETERSON TROUGH
dc.subjectLY-ALPHA
dc.subjectEMISSION-LINES
dc.subjectLUMINOSITY FUNCTION
dc.subjectEMITTING GALAXIES
dc.subjectCOSMOLOGICAL SIMULATIONS
dc.subjectCOSMIC REIONIZATION
dc.subjectPOPULATION-III
dc.subjectSEARCH
dc.titleNarrow-band surveys for very high redshift Lyman-alpha emitters
dc.typeartículo
dc.volumen474
sipa.codpersvinculados127321
sipa.indexWOS
sipa.indexScopus
sipa.trazabilidadCarga SIPA;09-01-2024
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