# The SAMI Galaxy Survey: The cluster redshift survey, target selection and cluster properties

Owers, MS and Allen, JT and Baldry, IK and Bryant, JJ and Cecil, GN and Cortese, L and Croom, SM and Driver, SP and Fogarty, LMR and Green, AW and Helmich, E and Jong, JTAD and Kuijken, K and Mahajan, S and McFarland, J and Pracy, MB and Robotham, AGS and Sikkema, G and Sweet, S and Taylor, EN and Kleijn, GV and Bauer, AE and Bland-Hawthorn, J and Brough, S and Colless, M and Couch, WJ and Davies, RL and Drinkwater, MJ and Goodwin, M and Hopkins, AM and Konstantopoulos, IS and Foster, C and Lawrence, JS and Lorente, NPF and Medling, AM and Metcalfe, N and Richards, SN and Sande, JVD and Scott, N and Shanks, T and Sharp, R and Thomas, AD and Tonini, C (2017) The SAMI Galaxy Survey: The cluster redshift survey, target selection and cluster properties. Monthly Notices of the Royal Astronomical Society, 468 (2). pp. 1824-1849. ISSN 0035-8711

We describe the selection of galaxies targeted in eight low redshift clusters (APMCC0917, A168, A4038, EDCC442, A3880, A2399, A119 and A85; $0.029 < z < 0.058$) as part of the Sydney-AAO Multi-Object integral field Spectrograph Galaxy Survey (SAMI-GS). We have conducted a redshift survey of these clusters using the AAOmega multi-object spectrograph on the 3.9m Anglo-Australian Telescope. The redshift survey is used to determine cluster membership and to characterise the dynamical properties of the clusters. In combination with existing data, the survey resulted in 21,257 reliable redshift measurements and 2899 confirmed cluster member galaxies. Our redshift catalogue has a high spectroscopic completeness ($\sim 94\%$) for $r_{\rm petro} \leq 19.4$ and clustercentric distances $R< 2\rm{R}_{200}$. We use the confirmed cluster member positions and redshifts to determine cluster velocity dispersion, $\rm{R}_{200}$, virial and caustic masses, as well as cluster structure. The clusters have virial masses $14.25 \leq {\rm log }({\rm M}_{200}/\rm{M}_{\odot}) \leq 15.19$. The cluster sample exhibits a range of dynamical states, from relatively relaxed-appearing systems, to clusters with strong indications of merger-related substructure. Aperture- and PSF-matched photometry are derived from SDSS and VST/ATLAS imaging and used to estimate stellar masses. These estimates, in combination with the redshifts, are used to define the input target catalogue for the cluster portion of the SAMI-GS. The primary SAMI-GS cluster targets have $R< \rm{R}_{200}$, velocities $|v_{\rm pec}| < 3.5\sigma_{200}$ and stellar masses $9.5 \leq {\rm log(M}^*_{approx}/\rm{M}_{\odot}) \leq 12$. Finally, we give an update on the SAMI-GS progress for the cluster regions.