Weak-Lensing Surface Mass Density

Author

NumCosmo developers

Weak-Lensing Surface Mass Density

This page describes the projected surface mass density and the related weak-lensing observables — convergence and tangential shear — implemented by NcWLSurfaceMassDensity. The three-dimensional mass distribution is supplied by a halo density profile NcHaloDensityProfile, and the geometry by NcDistance.

Projected Surface Mass Density

The projected surface mass density is the line-of-sight integral of the three-dimensional density profile \(\rho(r)\), \[ \Sigma(R) = \int \mathrm{d}\chi\,\rho\!\left(\sqrt{R^2 + \chi^2}\right), \] where \(R\) is the projected (two-dimensional) distance from the halo center and \(\chi\) is the distance along the line of sight, so that \(r^2 = R^2 + \chi^2\).

The mean surface mass density within a circular aperture of radius \(R\) is \[ \overline{\Sigma}(<R) = \frac{2}{R^2}\int_0^R \mathrm{d}R^\prime\,R^\prime\,\Sigma(R^\prime). \]

Convergence and Shear

The convergence \(\kappa(R)\) and tangential shear \(\gamma(R)\) are \[ \kappa(R) = \frac{\Sigma(R)}{\Sigma_\mathrm{crit}}, \qquad \gamma(R) = \frac{\Delta\Sigma(R)}{\Sigma_\mathrm{crit}} = \frac{\overline{\Sigma}(<R) - \Sigma(R)}{\Sigma_\mathrm{crit}}, \] where the critical surface density is \[ \Sigma_\mathrm{crit} = \frac{c^2}{4\pi G}\frac{D_s}{D_l D_{ls}}, \] with \(c\) the speed of light, \(G\) the gravitational constant, and \(D_s\), \(D_l\), \(D_{ls}\) the angular diameter distances to the source, to the lens, and between lens and source, respectively.

For background on cluster weak-lensing mass measurements, see Mandelbaum et al. (2006), Umetsu et al. (2012), Applegate et al. (2014), Melchior et al. (2017), and Parroni et al. (2017).

Mandelbaum, R., U. Seljak, R. J. Cool, M. Blanton, C. M. Hirata, and J. Brinkmann. 2006. Density profiles of galaxy groups and clusters from SDSS galaxy-galaxy weak lensing.” MNRAS 372 (October): 758–76. https://doi.org/10.1111/j.1365-2966.2006.10906.x.
Umetsu, K., E. Medezinski, M. Nonino, et al. 2012. CLASH: Mass Distribution in and around MACS J1206.2-0847 from a Full Cluster Lensing Analysis.” ApJ 755 (August): 56. https://doi.org/10.1088/0004-637X/755/1/56.
Applegate, D. E., A. von der Linden, P. L. Kelly, et al. 2014. Weighing the Giants - III. Methods and measurements of accurate galaxy cluster weak-lensing masses.” MNRAS 439 (March): 48–72. https://doi.org/10.1093/mnras/stt2129.
Melchior, P., D. Gruen, T. McClintock, et al. 2017. Weak-lensing mass calibration of redMaPPer galaxy clusters in Dark Energy Survey Science Verification data.” MNRAS 469 (August): 4899–920. https://doi.org/10.1093/mnras/stx1053.
Parroni, C., S. Mei, T. Erben, et al. 2017. Next Generation Virgo Cluster Survey. XXI. The Weak Lensing Masses of the CFHTLS and NGVS RedGOLD Galaxy Clusters and Calibration of the Optical Richness.” ApJ 848 (October): 114. https://doi.org/10.3847/1538-4357/aa8b6c.

API Reference

See NcWLSurfaceMassDensity for the full class reference. The most relevant methods are: