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We exploit the synergy between low-resolution spectroscopy and photometricredshifts to study environmental effects on galaxy evolution in slitlessspectroscopic surveys from space. As a test case, we consider the future EuclidDeep survey (~40deg$^2$), which combines a slitless spectroscopic surveylimited at H$\alpha$ flux $\geq5\times 10^{-17}$ erg cm$^{-2}$ s$^{-1}$ and aphotometric survey limited in H-band ($H\leq26$). We use Euclid-like galaxymock catalogues, in which we anchor the photometric redshifts to the 3D galaxydistribution of the available spectroscopic redshifts. We then estimate thelocal density contrast by counting objects in cylindrical cells with radiusfrom 1 to 10 h$^{-1}$Mpc over the redshift range 0.9<z<1.8. We compare thisdensity field with the one computed in a mock catalogue with the same depth asthe Euclid Deep survey (H=26) but without redshift measurement errors. We findthat our method successfully separates high from low density environments (thelast from the first quintile of the density distribution), with higherefficiency at low redshift and large cell: the fraction of low density regionsmistaken by high density peaks is <1% for all scales and redshifts explored,but for scales of 1 h$^{-1}$Mpc for which is a few percent. These results showthat we can efficiently study environment in photometric samples ifspectroscopic information is available for a smaller sample of objects thatsparsely samples the same volume. We demonstrate that these studies arepossible in the Euclid Deep survey, i.e. in a redshift range in whichenvironmental effects are different from those observed in the local universe,hence providing new constraints for galaxy evolution models.

Measuring galaxy environment with the synergy of future photometric and spectroscopic surveys