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.
AMICO galaxy clusters in KiDS-DR3: Weak lensing mass calibration / Bellagamba, F.; Sereno, M.; Roncarelli, M.; Maturi, M.; Radovich, M.; Bardelli, S.; Puddu, E.; Moscardini, L.; Getman, F.; Hildebrandt, H.; Napolitano, N.. - In: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY. - ISSN 0035-8711. - 484:2(2019), pp. 1598-1615. [10.1093/mnras/stz090]
AMICO galaxy clusters in KiDS-DR3: Weak lensing mass calibration
Sereno M.;Moscardini L.;Napolitano N.
2019
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.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
