Stellar angular momentum of intermediate redshift galaxies in MUSE surveys

We quantify the stellar rotation of galaxies by computing the ₑ 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 10^7. 5 to 10^11. 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 2R₄ 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 ₑ- diagram, we notice that the fraction of round and massive galaxies increases with redshift. We lack galaxies with ₑ < 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 ₑ 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 ₑ values. For the remaining galaxies the classification is uncertain. As we lack galaxies with ₑ< 0. 1, we are not able to identify when galaxies become slow rotators within the surveyed environments, area and redshift range.