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Kinematics of ionized gas outflows caused by star formation

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Presentation on theme: "Kinematics of ionized gas outflows caused by star formation"— Presentation transcript:

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

2 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.

3 Veilleux et al., 2005

4 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

5 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

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

7 Galactic wind modeling
Oparin, Moiseev 2015

8 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

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

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

11 FPI maps Lopez-Coba et al. 2016

12 BPT diagrams Lopez-Coba et al. 2016

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

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

15 FPI maps

16

17 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.


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