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We measure the gravitational lensing signal around satellite galaxies in asample of galaxy clusters at $z<0.15$ by combining high-quality imaging datafrom the Canada-France-Hawaii Telescope with a large sample ofspectroscopically-confirmed cluster members. We use extensive image simulationsto assess the accuracy of shape measurements of faint, background sources inthe vicinity of bright satellite galaxies. We find a small but significantbias, as light from the lenses makes the shapes of background galaxies appearradially aligned with the lens. We account for this bias by applying acorrection that depends on both lens size and magnitude. We also correct forcontamination of the source sample by cluster members. We use aphysically-motivated definition of subhalo mass, namely the mass bound to thesubhalo, $m_\mathrm{bg}$, similar to definitions used by common subhalo findersin numerical simulations. Binning the satellites by stellar mass we provide adirect measurement of the subhalo-to-stellar-mass relation, $\logm_\mathrm{bg}/\mathrm{M}_\odot = (11.54\pm0.05) +(0.95\pm0.10)\log[m_\star/(2\times10^{10}\mathrm{M}_\odot)]$. This best-fittingrelation implies that, at a stellar mass$m_\star\sim3\times10^{10}\,\mathrm{M}_\odot$, subhalo masses are roughly 50per cent of those of central galaxies, and this fraction decreases at higherstellar masses. We find some evidence for a sharp change in thetotal-to-stellar mass ratio around the clusters' scale radius, which could beinterpreted as galaxies within the scale radius having suffered more stronglyfrom tidal stripping, but remain cautious regarding this interpretation.

The galaxy-subhalo connection in low-redshift galaxy clusters from weak gravitational lensing