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Galaxies Emission in the Mid-InfraRed MIR: 5

Why InfraRed and Radio? With MIR/FIR/radio we can approach the history of galaxy ... Radio observations are tracers of very recent star formation in galaxies. ...

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Galaxies Emission in the Mid-InfraRed MIR: 5

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    Slide 1:. 18/12/2010i. 18/12/2010i

    Slide 4:. 18/12/2010i. 18/12/2010i

    Slide 5:. 18/12/2010i. 18/12/2010i

    Slide 7:Galaxy Emission in the Far-InfraRed (FIR): 40-500 µm

    Slide 11:The radio-FIR correlation is locally well assessed, over a wide range of luminosities, from normal spirals to ULIGs:

    Slide 16:Comparison between different SFR indicators

    Slide 23:Cosmic Evolution

    Slide 28:

    Slide 46:Does IR Reveal Hidden AGN Activity?(see Houck et al. 2004; 2005; Higdon et al. 2004; etc…) Obscured AGN are needed: - to reproduce the X-ray background peak (Setti & Woltjer 1989, Comastri et al. 1995 etc. ) - Unified Models: dusty torus around AGN responsible for absorption of X-ray to NIR nuclear radiation - models predict that AGN activity in the past take place in “dusty” environments/systems Need to separate AGN from stellar activity to: - Have a complete picture of galaxy(-AGN) formation and (co)evolution, since ? Luminous Infrared Galaxies (LIGs) represent an active phase of star-formation and/or AGN activity and dominate the luminosity density at z>1 Main weakness of actual data : galaxy/AGN separation

    Slide 48:IR colour selection AGN (unobs and obs) are expected to have warm power-law SEDs at >1 µm (? from elliptical/starburst)

    Slide 49:Type 2 AGN Optical emission from Type 2 AGN can be diluted by the host galaxy difficult to classify as AGN from optical line diagnostics. Crucial range: near-/mid-infrared (NIR/MIR) where galaxy SEDs have a dip (2-5 ?m) and the hot dust heated by the AGN start contributing, filling up the dip.

    Slide 52:STRONG IMPACT ON EVOLUTIONARY MODELS?

    Slide 53:YES: STRONG IMPACT ON EVOLUTIONARY MODELS!

    Slide 54:MAIN MODEL CHANGES:

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