The eROSITA Final Equatorial-Depth Survey (eFEDS) -- Splashback radius of X-ray galaxy clusters using galaxies from HSC survey

We present the splashback radius measurements around the SRG/eROSITA eFEDS X-ray selected galaxy clusters by cross-correlating them with HSC S19A photometric galaxies. The X-ray selection is expected to be less affected by systematics related to projection that affects optical cluster finder algorithms. We use a nearly volume-limited sample of 109 galaxy clusters selected in 0.5-2.0 keV band having luminosity $L_X>{10}^{43.5}\mathrm{e}\mathrm{r}\mathrm{g}{\mathrm{s}}^{-1}{\mathrm{h}}^{-2}$ within the redshift $z<0.75$ and obtain measurements of the projected cross-correlation with a signal-to-noise of $17.43$. We model our measurements to infer a three-dimensional profile and find that the steepest slope is sharper than $-3$ and associate the location with the splashback radius. We infer the value of the 3D splashback radius $r_{\mathrm{s}\mathrm{p}}=1.45_{-0.26}^{+0.30}{\mathrm{h}}^{-1}\mathrm{M}\mathrm{p}\mathrm{c}$. We also measure the weak lensing signal of the galaxy clusters and obtain halo mass $\log [M_{200\mathrm{m}}\mathrm{/}{\mathrm{h}}^{-1}{\mathrm{M}}_{\odot }]=14.52\pm 0.06$ using the HSC-S16A shape catalogue data at the median redshift $z=0.46$ of our cluster sample. We compare our $r_{\mathrm{s}\mathrm{p}}$ values with the spherical overdensity boundary $r_{200\mathrm{m}}=1.75\pm 0.08{\mathrm{h}}^{-1}\mathrm{M}\mathrm{p}\mathrm{c}$ based on the halo mass which is consistent within $1.2\sigma$ with the $\mathrm{\Lambda }$CDM predictions. Our constraints on the splashback radius, although broad, are the best measurements thus far obtained for an X-ray selected galaxy cluster sample.