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We investigate the effects of Active Galactic Nuclei (AGN) on the gas kinematics of their host galaxies, using MaNGA data for a sample of 62 AGN hosts and 109 control galaxies (inactive galaxies). We compare orientation of the line of nodes (kinematic Position Angle - PA) measured from the gas and stellar velocity fields for the two samples. We found that AGN hosts and control galaxies display similar kinematic PA offsets between gas and stars. However, we note that AGN have larger fractional velocity dispersion $sigma$ differences between gas and stars [$sigma_{frac}=(sigma_{rm gas}-sigma_{stars})/sigma_{rm stars}$] when compared to their controls, as obtained from the velocity dispersion values of the central (nuclear) pixel (2.5 diameter). The AGN have a median value of $sigma_{rm frac}$ of $<sigma_{frac}>_{rm AGN}=0.04$, while the the median value for the control galaxies is $<sigma_{frac}>_{rm CTR}=-0.23$. 75% of the AGN show $sigma_{frac}>-0.13$, while 75% of the normal galaxies show $sigma_{rm frac}<-0.04$, thus we suggest that the parameter $sigma_{rm frac}$ can be used as an indicative of AGN activity. We find a correlation between the [OIII]$lambda$5007 luminosity and $sigma_{frac}$ for our sample. Our main conclusion is that the AGN already observed with MaNGA are not powerful enough to produce important outflows at galactic scales, but at 1-2 kpc scales, AGN feedback signatures are always present on their host galaxies.
We report the characterization of the first $62$ MaNGA Active Galactic Nuclei (AGN) hosts in the Fifth Product Launch (MPL-5) and the definition of a control sample of non-active galaxies. This control sample - comprising two galaxies for each AGN -
We present the first asymmetric drift (AD) measurements for unresolved stellar populations of different characteristic ages above and below 1.5 Gyr. These measurements sample the age-velocity relation (AVR) in galaxy disks. In this first paper we dev
Based on MaNGA integral field unit (IFU) spectroscopy we search 60 AGN candidates, which have stellar masses $M_{star}leqslant5times10^{9}$$M_{odot}$ and show AGN ionization signatures in the BPT diagram. For these AGN candidates, we derive the spati
Bars in galaxies are thought to stimulate both inflow of material and radial mixing along them. Observational evidence for this mixing has been inconclusive so far however, limiting the evaluation of the impact of bars on galaxy evolution. We now use
We study the properties of 66 galaxies with kinematically misaligned gas and stars from MaNGA survey. The fraction of kinematically misaligned galaxies varies with galaxy physical parameters, i.e. M*, SFR and sSFR. According to their sSFR, we further