Feedback: in the form of outflow. AGN driven outflow.

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  • Feedback:in the form of outflow

  • AGN driven outflow

  • M82Blue: ChandraRed: SpitzerCyan: Optical

  • Star formation driven outflow

  • Two categories of the gas in a SF/SB galaxy wind Ambient interstellar medium

    Energetic fluid created by thermalization of the SBs stellar eject or AGN

    The hydrodynamical interaction between these two generates the multiphase starburst-driven galactic wind.

  • Observations of multiphase wind (cold, warm, hot gas & dust) X-ray

    Morphology and kinematics of interstellar emission lines (e.g. Ha)

    Outflow kinematics in the interstellar absorption lines (e.g. MgII, NaD)

  • From X-ray: Hot Gas Escapes from Dwarf StarburstsMartin 1999, Heckman et al 2000, Martin 2004Tremonti et al. 2004Vc= 130 km/s

  • From optical absorption lines--NaD(5890,5896A)Low- ionization potential 5.1eV(Martin et al. 2005, 2006)

  • Circular velocityStar formation rateOutflow velocityisothermal escape speedFrom optical absorption lines (Rupke et al. 2005a,b,c)Murray et al. 2004, Martin 2005

  • Stack spectrum and stellar continuumMg IHe INa I

  • Two-component fit of ISM Na D Line center shift: outflow velocity Voff

    Line strength (EW): covering factor Cf Line width b

    Line ratio 0

  • Two-component fit of ISM Na D Line center shift: outflow velocity Voff

    Line strength (EW): covering factor Cf Line width b

    Line ratio 0

  • Inclination effectface onedge on

  • Isolate the main driver of the observedcorrelation: Disk-like components

  • Isolate the main driver of the observedcorrelation: outflow components

  • Outflow velocity vs. SFRVoff ~ SFR0.3

  • Martin et al. 2009

    Spectra from LRIS on Keck I

    Using multi-components to fit each absorption line

  • Through the fitting in last slides, they find that components with different velocity have different covering factoroutflow is accelerating

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