SDSS-IV MaNGA: Uncovering the Angular Momentum Content of Central and Satellite Early-type Galaxies

Abstract

We study 379 central and 159 satellite early-type galaxies with two-dimensional kinematics from the integral-field survey Mapping Nearby Galaxies at APO (MaNGA) to determine how their angular momentum content depends on stellar and halo mass. Using the Yang et al. group catalog, we identify central and satellite galaxies in groups with halo masses in the range . As in previous work, we see a sharp dependence on stellar mass, in the sense that ∼70% of galaxies with stellar mass * > - M h M 10 11 2 tend to have very little rotation, while nearly all galaxies at lower mass show some net rotation. The ∼30% of high-mass galaxies that have significant rotation do not stand out in other galaxy properties, except for a higher incidence of ionized gas emission. Our data are consistent with recent simulation results suggesting that major merging and gas accretion have more impact on the rotational support of lower-mass galaxies. When carefully matching the stellar mass distributions, we find no residual differences in angular momentum content between satellite and central galaxies at the 20% level. Similarly, at fixed mass, galaxies have consistent rotation properties across a wide range of halo mass. However, we find that errors in classification of central and satellite galaxies with group finders systematically lower differences between satellite and central galaxies at a level that is comparable to current measurement uncertainties. To improve constraints, the impact of group-finding methods will have to be forward-modeled via mock catalogs.

A numerical twist on the spin parameter, λR

“…This is consistent with the uncertainty quoted by van de Sande et al (2017b) in which it was proposed from repeat SAMI observations that adverse seeing conditions could lower measurements of λ R by 0.05 − 0.1; our study shows that this bias could be slightly larger for very disky galaxies. Similarly, we agree with the work of Greene et al (2018) in which two corrections were suggested based on the spin parameter measured. Fig.…”

“…Previous studies have sought to quantify or correct this bias (e.g. D 'Eugenio et al 2013;van de Sande et al 2017a,b;Greene et al 2018;Graham et al 2018), and we investigate how well such corrections perform. In particular, we focus on the recent work Graham et al (2018), who used Jeans Anisotropic Modelling (JAM) to derive a general analytic correction to λ R for regularly rotating galaxies of different types, based on the ratio of the width of the point spread function (σ PSF ) to the effective radius of the galaxy (R eff ); we investigate how well it performs when applied to 3D dynamical galaxy models.…”

Stellar Kinematics and Environment at z ∼ 0.8 in the LEGA-C Survey: Massive Slow Rotators Are Built First in Overdense Environments

“…In the two right-most panels, we show the running average rotational support for each overdensity bin, with a slight offset from the center of the bin for clarity. As shown in Bezanson et al (2018b), the average range in rotational support tends to decrease with increasing stellar mass, which is consistent with studies of massive, quiescent galaxies in the local Universe (Veale et al 2017;Greene et al 2018). We do not see a strong environmental trend at all masses, but we note two statistically significant trends at the massive end of the sample.…”

The SAMI Galaxy Survey: The contribution of different kinematic classes to the stellar mass function of nearby galaxies

“…From Figure 5a, it is clear that the number density of FRs overwhelms SRs for most stellar masses covered by SAMI, with SRs matching the fraction of FRs only at > 2 × 10 11 M (see also Khochfar et al 2011;Emsellem et al 2011;Greene et al 2017Greene et al , 2018van de Sande et al 2017b;Brough et al 2017). We should note that this transition mass looks systematically lower than that found in Graham et al (2018, Figure 13) based on MaNGA galaxies.…”