Weak lensing magnification of SpARCS galaxy clusters

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dc.contributor.authorTudorica, A.
dc.contributor.authorHildebrandt, H.
dc.contributor.authorTewes, M.
dc.contributor.authorHoekstra, H.
dc.contributor.authorMorrison, C.B.
dc.contributor.authorMuzzin, A.
dc.contributor.authorWilson, G.
dc.contributor.authorYee, H.K.C.
dc.contributor.authorLidman, C.
dc.contributor.authorHicks, A.
dc.contributor.authorNantais, J.
dc.contributor.authorErben, T.
dc.contributor.authorVan Der Burg, R.F.J.
dc.contributor.authorDemarco, R.
dc.date.accessioned2018-06-26T20:22:07Z
dc.date.available2018-06-26T20:22:07Z
dc.date.issued2017
dc.descriptionIndexación: Scopus.es_ES
dc.description.abstractContext. Measuring and calibrating relations between cluster observables is critical for resource-limited studies. The mass-richness relation of clusters offers an observationally inexpensive way of estimating masses. Its calibration is essential for cluster and cosmological studies, especially for high-redshift clusters. Weak gravitational lensing magnification is a promising and complementary method to shear studies, that can be applied at higher redshifts. Aims. We aim to employ the weak lensing magnification method to calibrate the mass-richness relation up to a redshift of 1.4. We used the Spitzer Adaptation of the Red-Sequence Cluster Survey (SpARCS) galaxy cluster candidates (0.2 < z < 1.4) and optical data from the Canada France Hawaii Telescope (CFHT) to test whether magnification can be effectively used to constrain the mass of high-redshift clusters. Methods. Lyman-break galaxies (LBGs) selected using the u-band dropout technique and their colours were used as a background sample of sources. LBG positions were cross-correlated with the centres of the sample of SpARCS clusters to estimate the magnification signal, which was optimally-weighted using an externally-calibrated LBG luminosity function. The signal was measured for cluster sub-samples, binned in both redshift and richness. Results. We measured the cross-correlation between the positions of galaxy cluster candidates and LBGs and detected a weak lensing magnification signal for all bins at a detection significance of 2.6-5.5σ. In particular, the significance of the measurement for clusters with z> 1.0 is 4.1σ; for the entire cluster sample we obtained an average M200 of 1.28 -0.21 +0.23 × 1014 M⊙. Conclusions. Our measurements demonstrated the feasibility of using weak lensing magnification as a viable tool for determining the average halo masses for samples of high redshift galaxy clusters. The results also established the success of using galaxy over-densities to select massive clusters at z > 1. Additional studies are necessary for further modelling of the various systematic effects we discussed.es_ES
dc.description.urihttps://www.aanda.org/articles/aa/pdf/2017/12/aa31267-17.pdf
dc.description.urihttps://www.aanda.org/articles/aa/abs/2017/12/aa31267-17/aa31267-17.html
dc.identifier.citationAstronomy and Astrophysics, 608, art. no. A141.es_ES
dc.identifier.issn0004-6361
dc.identifier.otherDOI: 10.1051/0004-6361/201731267
dc.identifier.urihttp://repositorio.unab.cl/xmlui/handle/ria/6203
dc.language.isoenes_ES
dc.publisherEDP Scienceses_ES
dc.subjectGalaxies: clusters: generales_ES
dc.subjectGalaxies: clusters: individual: SpARCSes_ES
dc.subjectGravitational lensing: weakes_ES
dc.titleWeak lensing magnification of SpARCS galaxy clusterses_ES
dc.typeArtículoes_ES
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