TY - JOUR
T1 - The impact of AGN on stellar kinematics and orbits in simulated massive galaxies
AU - Frigo, Matteo
AU - Naab, Thorsten
AU - Hirschmann, Michaela
AU - Choi, Ena
AU - Somerville, Rachel S.
AU - Krajnovic, Davor
AU - Dave, Romeel
AU - Cappellari, Michele
N1 - Publisher Copyright:
© 2019 The Author(s).
PY - 2019/10/21
Y1 - 2019/10/21
N2 - We present a series of 10 × 2 cosmological zoom simulations of the formation of massive galaxies with and without a model for active galactic nucleus (AGN) feedback. Differences in stellar population and kinematic properties are evaluated by constructing mock integral field unit maps. The impact of the AGN is weak at high redshift when all systems are mostly fast rotating and disc-like. After z ∼ 1 the AGN simulations result in lower mass, older, less metal rich, and slower rotating systems with less discy isophotes - in general agreement with observations. 2D kinematic maps of in situ and accreted stars show that these differences result from reduced in-situ star formation due to AGN feedback. A full analysis of stellar orbits indicates that galaxies simulated with AGN are typically more triaxial and have higher fractions of x-tubes and box orbits and lower fractions of z-tubes. This trend can also be explained by reduced late in-situ star formation. We introduce a global parameter, ξ 3, to characterize the anticorrelation between the third-order kinematic moment h3 and the lineof- sight velocity (Vavg/σ), and compare to ATLAS3D observations. The kinematic correlation parameter ξ 3 might be a useful diagnostic for large integral field surveys as it is a kinematic indicator for intrinsic shape and orbital content.
AB - We present a series of 10 × 2 cosmological zoom simulations of the formation of massive galaxies with and without a model for active galactic nucleus (AGN) feedback. Differences in stellar population and kinematic properties are evaluated by constructing mock integral field unit maps. The impact of the AGN is weak at high redshift when all systems are mostly fast rotating and disc-like. After z ∼ 1 the AGN simulations result in lower mass, older, less metal rich, and slower rotating systems with less discy isophotes - in general agreement with observations. 2D kinematic maps of in situ and accreted stars show that these differences result from reduced in-situ star formation due to AGN feedback. A full analysis of stellar orbits indicates that galaxies simulated with AGN are typically more triaxial and have higher fractions of x-tubes and box orbits and lower fractions of z-tubes. This trend can also be explained by reduced late in-situ star formation. We introduce a global parameter, ξ 3, to characterize the anticorrelation between the third-order kinematic moment h3 and the lineof- sight velocity (Vavg/σ), and compare to ATLAS3D observations. The kinematic correlation parameter ξ 3 might be a useful diagnostic for large integral field surveys as it is a kinematic indicator for intrinsic shape and orbital content.
KW - Galaxies: Evolution
KW - Galaxies: Formation
KW - Galaxies: Kinematics and dynamics
KW - Methods: numerical
UR - http://www.scopus.com/inward/record.url?scp=85075164960&partnerID=8YFLogxK
U2 - 10.1093/mnras/stz2318
DO - 10.1093/mnras/stz2318
M3 - Article
AN - SCOPUS:85075164960
SN - 0035-8711
VL - 489
SP - 2702
EP - 2722
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 2
ER -