English
 
User Manual Privacy Policy Disclaimer Contact us
  Advanced SearchBrowse

Item

ITEM ACTIONSEXPORT

Released

Journal Article

μ⋆ masses: weak-lensing calibration of the Dark Energy Survey Year 1 redMaPPer clusters using stellar masses

MPS-Authors
/persons/resource/persons221802

Varga,  T. N.
Optical and Interpretative Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

/persons/resource/persons226789

Hoyle,  B.
Optical and Interpretative Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

External Ressource
No external resources are shared
Fulltext (public)
There are no public fulltexts stored in PuRe
Supplementary Material (public)
There is no public supplementary material available
Citation

Pereira, M. E. S., Palmese, A., Varga, T. N., McClintock, T., Soares-Santos, M., Burgad, J., et al. (2020). μ⋆ masses: weak-lensing calibration of the Dark Energy Survey Year 1 redMaPPer clusters using stellar masses. Monthly Notices of the Royal Astronomical Society, 498(4), 5450-5467. doi:10.1093/mnras/staa2687.


Cite as: http://hdl.handle.net/21.11116/0000-0007-FCE4-C
Abstract
We present the weak-lensing mass calibration of the stellar-mass-based μ⋆ mass proxy for redMaPPer galaxy clusters in the Dark Energy Survey Year 1. For the first time, we are able to perform a calibration of μ⋆ at high redshifts, z > 0.33. In a blinded analysis, we use ∼6000 clusters split into 12 subsets spanning the ranges 0.1 ≤ z < 0.65 and μ⋆ up to ∼5.5×1013M⁠, and infer the average masses of these subsets through modelling of their stacked weak-lensing signal. In our model, we account for the following sources of systematic uncertainty: shear measurement and photometric redshift errors, miscentring, cluster-member contamination of the source sample, deviations from the Navarro–Frenk–White halo profile, halo triaxiality, and projection effects. We use the inferred masses to estimate the joint mass–μ⋆–z scaling relation given by ⟨M200c|μ⋆,z⟩=M0(μ⋆/5.16×1012M)Fμ⋆((1+z)/1.35)Gz⁠. We find M0=(1.14±0.07)×1014M with Fμ⋆=0.76±0.06 and Gz = −1.14 ± 0.37. We discuss the use of μ⋆ as a complementary mass proxy to the well-studied richness λ for: (i) exploring the regimes of low z, λ < 20 and high λ, z ∼ 1; and (ii) testing systematics such as projection effects for applications in cluster cosmology.