1 / 56

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. ...

flora
Download Presentation

Galaxies Emission in the Mid-InfraRed MIR: 5

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript


    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:

More Related