Kinematics of ionized gas outflows caused by star formation

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Presentation transcript:

Kinematics of ionized gas outflows caused by star formation D. Oparin, A. Moiseev. SAO RAS, Russia

Galactic outflows A commonplace phenomenon Widely variable in scale Caused by different processes related to stellar wind from massive stars, supernovae explosions, AGN activity etc. Play important role in galactic evolution: shaking ISM, transmitting energy, heating the gas... M82, Veilleux et al.

Veilleux et al., 2005

Fabri-Perot interferometer 3D-spectroscopy method Has a spatial resolution ~10pc for close galaxies. Has a wide field. Allows detailed study of wind structures. IFP

NGC 4460 Isolated dwarf lenticular galaxy Has a cone-like structure outside the galaxy plane, produced by galactic wind (Kaisin, Karachencev, 2008; Mioseev, Kaisin, Karachencev, 2010) Oparin, Moiseev 2015

FPI maps Oparin, Moiseev 2015 r-SDSS map Hα image Velocity map Velocity dispersion map Oparin, Moiseev 2015

Galactic wind modeling Oparin, Moiseev 2015

Galactic wind modeling Map of residual velocities along the cone walls (S-E cone is closest) Model of rotation of galaxy disc and swept-out matter Map of residual velocities Map of residual velocities along the cone walls (N-W cone is closest) Oparin, Moiseev 2015

NGC 4460 galactic wind typical Vout~30. 80 км/с, σ~50 км/с, Ewind~0. 3 NGC 4460 galactic wind typical Vout~30..80 км/с, σ~50 км/с, Ewind~0.3...2.2*10e52 erg The ejected matter will fall back to the galaxy Oparin, Moiseev 2015

UGC 10043 Spiral edge-on galaxy Galactic wind, Vout<250 км/с, σ<300 км/с Lopez-Coba et al. 2016

FPI maps Lopez-Coba et al. 2016

BPT diagrams Lopez-Coba et al. 2016

Line ratio and velocity dispersion corellation Lopez-Coba et al. 2016

NGC 3077 A dwarf galaxy,M81 group member Has several outflow structures

FPI maps

Summary Studying of gas outflows phenomenon requires spatial resolved spectroscopy. Thus combining of LS and 3D-spectroscopy (including FPI) methods is neсessary. FPI velocity dispersion maps in addition to BPT diagrams allow to determine the source of ionization of the gas forming the wind structure.