The spatially resolved dynamics of dusty starburst galaxies in a z ∼ 0.4 cluster: beginning the transition from spirals to S0s

To investigate what drives the reversal of the morphology–density relation at intermediate/high redshift, we present a multiwavelength analysis of 27 dusty starburst galaxies in the massive clusterCl 0024+17 at z= 0.4.We combineHα dynamicalmaps from theVLT/FLAMESmultiIFU systemwith far-infrared imaging usingHerschel/SPIRE andmillimetre spectroscopy from IRAM/NOEMA, in order to measure the dynamics, star formation rates and gas masses of this sample. Most galaxies appear to be rotationally supported, with a median ratio of rotationalsupport to line-of-sight velocity dispersion v/σ ∼ 5 ± 2, and specific angular momentum λR = 0.83 ± 0.06 – comparable to field spirals of a similar mass at this redshift. The star formation rates of 3–26 M yr−1 and average 12CO-derived gas mass of ∼ 1 × 1010 M suggest gas depletion time-scales of ∼1 Gyr (∼0.25 of the cluster crossing time). We derive characteristic dust temperatures (mean Td = 26 ± 1 K) consistent with local galaxies of similar far-infrared luminosity, suggesting that the low-density gas is yet to be stripped. Taken together, these results suggest that these starbursts have only recently accreted from the field, with star formation rates likely enhanced due to the effects of ram pressure. In order to make the transition to cluster S0s these galaxies must lose ∼40 per cent of their specific angular momentum.We suggest this must occur≥1Gyr later, after themolecular gas has been depleted and/or stripped, via multiple tidal interactions with other cluster members.