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EnglishWe present the mass calibration for galaxy clusters detected with the AMICO code in KiDS DR3 data. The cluster sample comprises 7000 objects and covers the redshift range 0.1 < z < 0.6. We perform a weak lensing stacked analysis by binning the clusters according to redshift and two different mass proxies provided by AMICO, namely the amplitude A (measure of galaxy abundance through an optimal filter) and the richness λ∗ (sum of membership probabilities in a consistent radial and magnitude range across redshift). For each bin, we model the data as a truncated NFW profile plus a two-halo term, taking into account uncertainties related to concentration and miscentring. From the retrieved estimates of the mean halo masses, we construct the A–M200 and the λ∗–M200 relations. The relations extend over more than 1 order of magnitude in mass, down to M200 ∼ 2 (5) × 1013 M⊙ h−1 at z = 0.2 (0.5), with small evolution in redshift. The logarithmic slope is 2.0 for the A–mass relation, and 1.7 for the λ∗–mass relation, consistent with previous estimations on mock catalogues and coherent with the different nature of the two observables.
| Titolo: | AMICO galaxy clusters in KiDS-DR3: weak lensing mass calibration | |
| Autore/i: | Fabio Bellagamba; Mauro Sereno; Mauro Roncarelli; Matteo Maturi; Mario Radovich; Sandro Bardelli; Emanuella Puddu; Lauro Moscardini; Fedor Getman; Hendrik Hildebrandt; Nicola Napolitano | |
| Autore/i Unibo: | ||
| Anno: | 2019 | |
| Rivista: | ||
| Digital Object Identifier (DOI): | http://dx.doi.org/10.1093/mnras/stz090 | |
| Abstract: | We present the mass calibration for galaxy clusters detected with the AMICO code in KiDS DR3 data. The cluster sample comprises 7000 objects and covers the redshift range 0.1 < z < 0.6. We perform a weak lensing stacked analysis by binning the clusters according to redshift and two different mass proxies provided by AMICO, namely the amplitude A (measure of galaxy abundance through an optimal filter) and the richness λ∗ (sum of membership probabilities in a consistent radial and magnitude range across redshift). For each bin, we model the data as a truncated NFW profile plus a two-halo term, taking into account uncertainties related to concentration and miscentring. From the retrieved estimates of the mean halo masses, we construct the A–M200 and the λ∗–M200 relations. The relations extend over more than 1 order of magnitude in mass, down to M200 ∼ 2 (5) × 1013 M⊙ h−1 at z = 0.2 (0.5), with small evolution in redshift. The logarithmic slope is 2.0 for the A–mass relation, and 1.7 for the λ∗–mass relation, consistent with previous estimations on mock catalogues and coherent with the different nature of the two observables. | |
| Data stato definitivo: | 2019-03-29T18:57:40Z | |
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