To investigate what drives the reversal of the morphology–density relation at intermediate/high redshift , we present a multi-wavelength analysis of 27 dusty starburst galaxies in the massive cluster Cl 0024+17 at z = 0.4 .
We combine H \alpha dynamical maps from the VLT / FLAMES multi-IFU system with far-infrared imaging using Herschel / SPIRE and millimeter 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 rotational support to line-of-sight velocity dispersion v / \sigma \sim 5 \pm 2 , and specific angular momentum \lambda _ { R } = 0.83 \pm 0.06 – comparable to field spirals of a similar mass at this redshift .
The star formation rates of 3–26 M _ { \odot } yr ^ { -1 } and average ^ { 12 } CO-derived gas mass of \sim 1 \times 10 ^ { 10 } M _ { \odot } suggest gas depletion timescales of \sim 1 Gyr ( \sim 0.25 of the cluster crossing time ) .
We derive characteristic dust temperatures ( mean T _ { d } = 26 \pm 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 \sim 40 % of their specific angular momentum .
We suggest this must occur \geq 1 Gyr later , after the molecular gas has been depleted and/or stripped , via multiple tidal interactions with other cluster members .