Exploiting the slitless spectroscopy taken as part of the Grism Lens-Amplified Survey from Space ( GLASS ) , we present an extended analysis of the spatial distribution of star formation in 76 galaxies in 10 clusters at 0.3 < z < 0.7 .
We use 85 foreground and background galaxies in the same redshift range as a field sample .
The samples are well matched in stellar mass ( 10 ^ { 8 } -10 ^ { 11 } M _ { \odot } ) and star formation rate ( 0.5-50 M _ { \odot } yr ^ { -1 } ) .
We visually classify galaxies in terms of broad-band morphology , H \alpha morphology and likely physical process acting on the galaxy .
Most H \alpha emitters have a spiral morphology ( 41 \pm 8 % in clusters , 51 \pm 8 % in the field ) , followed by mergers/interactions ( 28 \pm 8 % , 31 \pm 7 % , respectively ) and early-type galaxies ( remarkably as high as 29 \pm 8 in clusters and 15 \pm 6 % in the field ) .
A diversity of H \alpha morphologies is detected , suggesting a diversity of physical processes .
In clusters , 30 \pm 8 % of the galaxies present a regular morphology , mostly consistent with star formation diffused uniformly across the stellar population ( mostly in the disk component , when present ) .
The second most common morphology ( 28 \pm 8 % ) is asymmetric/jellyfish , consistent with ram pressure stripping or other non-gravitational processes in 18 \pm 8 % of the cases .
Ram pressure stripping appears significantly less prominent in the field ( 2 \pm 2 % ) , where the most common morphology/mechanism appears to be consistent with minor gas rich mergers or clump accretion .
This work demonstrates that while environment specific mechanisms affect galaxy evolution at this redshift , they are diverse and their effects subtle .
A full understanding of this complexity requires larger samples and detailed and spatially resolved physical models .