Stellar angular momentum of intermediate redshift galaxies in MUSE surveys

We quantify the stellar rotation of galaxies by computing the λR parameter, a proxy for the stellar angular momentum in a sample of 106 galaxies with redshift 0.1 $<$ z $<$ 0.8 and stellar masses from ~107.5 to 1011.8 M_. The sample is located in the CANDELS/GOODS-S and COSMOS fields, and it was observed by various MUSE surveys. We create stellar velocity and velocity dispersion maps using a full-spectrum fitting technique, covering spatially ~2Rₑ for the galaxies. We study the impact of the atmospheric seeing on the spin parameter and apply corrections when pertinent. Through the analysis of the λR-ε diagram, we notice that the fraction of round and massive galaxies increases with redshift. We lack galaxies with λR < 0.1 in the sample and we find only one potential, but uncertain, low-mass slow rotator at z ~0.3. Moreover, we do not see an evident evolution or trend in the stellar angular momentum with redshift. We characterize the sample environment using two indicators: a local estimator based on the Voronoi tesselation method, and a global estimator derived by the use of the Friends-of-Friends algorithm. We find no correlation between the environment and λR given that we are not probing dense regions or massive galaxy structures. We also analyze the kinematic maps of the sample finding that about 40$%$ of galaxies are consistent with being regular rotators, having rotating stellar discs with flat velocity dispersion maps, while ~20% of galaxies have complex velocity maps and can be identified as non-regular rotators in spite of their λR values. For the remaining galaxies the classification is uncertain. As we lack galaxies with λR< 0.1, we are not able to identify when galaxies become slow rotators within the surveyed environments, area and redshift range.