# H0LiCOW III. Quantifying the effect of mass along the line of sight to the gravitational lens HE0435−1223 through weighted galaxy counts.

In our quest to measure the Hubble Constant H_{0} from the lensed quasar HE0435-1223 via the time delay method (Refsdal 1964), a major bias is potentially introduced by ignoring the effect of mass in galaxies surrounding the main lens, and along the line-of-sight to it. With reduced uncertainties on the other components of the time delay distance measurement, provided by state-of-the-art time-delay measurements and modeling techniques of strong lenses from high-resolution imaging, the line-of-sight/enveronmental effect remains an important source of uncertainty, contributing up to ∼ 5% to the error budget on H_{0} (Suyu et al. 2010, 2013). While in H0LICOW IV we explicitely model the nearest, most massive 1-5 galaxies, the net effect of the other galaxies, which act as weak perturbers, can be approximated with a constant external convergence term κ_{ext} (Suyu et al. 2010). Due to the well-known 'mass-sheet degeneracy' (Falco, Gorenstein, & Shapiro 1985; Schneider & Sluse 2013) this term cannot be inferred from the observed strongly lensed image properties, and instead requires a dedicated study based on wide-field, multi-band images, as well as spectroscopy.

In this paper, we have estimated a probability distribution function for κ_{ext}, from imaging data obtained with CFHT, Subaru, Gemini, and the Spitzer telescope, as well as from spectroscopy (see H0LICOW II). Our main approach was to measure the number of galaxies in a given aperture, and down to a given flux threshold, around HE0435-1223. Then, to measure in the same way the number of galaxies in a large sky survey, the CFHTLenS (Heymans et al. 2012). By doing so, we determined how over/under-dense the field around HE0435-1223 is, compared to a typical field on the sky. Next, we counted the galaxies across simulated fields from a large-scale cosmological simulation: the Millennium Simulation (Springel et al. 2005). Each field of the Millennium Simulation has a corresponding κ_{ext} value at its center, calculated via ray-tracing (Hilbert et al. 2009). By picking up only the fields from the simulation which have the same over/under-density as the HE0435-1223 field, we were able to build a histogram of the associated κ_{ext} values, hence estimate the probability distribution of the external convergence.

We have been particularly careful in the implementation of the technique above, taking into account the quality of both the HE0435-1223 field data and the CFHTLenS data, and adding similar relative uncertainties to the Millennium Simulation catalogues. We have also considered multiple choices of apertures (45" and 120"), as well as depth (i < 23 and i < 24 mag). More importantly, as suggested by Greene et al. 2013, we measured not only over/under-densities in terms of galaxy numbers, but we also weighted those numbers by quantities more physically relevant to gravitational lensing. These include: the distance of each galaxy to HE0435-1223 (or to the center of their apertures), their stellar masses, and their redshifts. Corresponding to the weight that we use, the over/under-density we measure is different, because distinct galaxies have different contributions (figure 1).

*Figure 1. When weighted by different, physically relevant quantities, individual galaxies have different contributions to the over/under-density of HE0435-1223. The relative contributions are represented by circles of different radii. The 45" and 120" radial apertures are marked by black circles, and the i < 23 mag, i > 23 mag galaxies are marked by blue and red, respectively.*

By selecting from the Millennium Simulation only fields which have similar over/under-density to HE0435-1223 when more than just a single weight is considered, we aimed to bring the inferred probability distribution for κ_{ext} closer to its actual, unknown value. Figure 2 shows how selected weight combinations translate into probability distributions for κ_{ext}.

*Figure 2. Various selected weight combinations translate into probability distributions for κ*

_{ext}.Our typical distribution for κ_{ext} has a median of ~0, and a spread of ~0.025, corresponding to an uncertainty of ~2.5% on H_{0}. We have found that the choice of weights, as well as aperture radius and flux limit, affect the median κ_{ext} by only ~0.005 or less (figure 3), as long as we consider only fields from the Millennium Simulation with the same external shear as HE0435-1223.

*Figure 3. The median and standard deviation of κ*

_{ext}, for various weight combinations, aperture radii and limiting fluxes.