Far-infrared properties of UV selected galaxies from z=4 to z=1.5: unveiling obscured star formation Véronique Buat & Sebastien Heinis With the contribution of Laure Ciesla Based on HerMES/SPIRE data in the COSMOS field Heinis, Buat et al. 2013 From Exoplanets to Distant Galaxies: SPICA’s New Window on the Cool Universe 18-21 june 2013-University of Tokyo, Japan
19
Embed
Véronique Buat & Sebastien Heinis With the contribution of Laure Ciesla
Far-infrared properties of UV selected galaxies from z=4 to z=1.5: unveiling obscured star formation. Véronique Buat & Sebastien Heinis With the contribution of Laure Ciesla Based on HerMES /SPIRE data in the COSMOS field Heinis , Buat et al. 2013. - PowerPoint PPT Presentation
Welcome message from author
This document is posted to help you gain knowledge. Please leave a comment to let me know what you think about it! Share it to your friends and learn new things together.
Transcript
Far-infrared properties of UV selected galaxies from z=4 to z=1.5: unveiling obscured star
formationVéronique Buat & Sebastien Heinis
With the contribution of Laure Ciesla
Based on HerMES/SPIRE data in the COSMOS fieldHeinis, Buat et al. 2013
From Exoplanets to Distant Galaxies: SPICA’s New Window on the Cool Universe18-21 june 2013-University of Tokyo, Japan
Elbaz’s lectures (david.elbaz3.free.fr/coursJ1.html), adapted from Devriendt+99
Visible
Infrared mm
UV
wavelength
inte
nsit
y
dust
Both UV and IR are related to recent star formationThey are anti-correlated because of dust attenuation
IR selected objects are usually obscured with a low residual emission in UV
Conversely: we expect a UV selection to be dominated by IR faint sources
Only few words about the physical link between UV and IR emissions
We perform a UV rest-frame selection in the COSMOS field @ z=1.5, 3 & 4
Based on photometric redshifts (Ilbert+13)Down to u, r, i ≈ 26 ABmag
What do we find within HerMES/ SPIRE images?
Almost nothing…….
Z = 1.5
Stacking per bin of LFUV
LIR measured by fitting Dale & Helou (2002) templates on SPIRE data
AFUV = f(LIR/LFUV) (Buat+05) LIRGs and sub-LIRGs
Stacking per bin of M*(again on the UV selection)
Z=1.5Z=3Z=4
Stacking per bin of (LFUV,M*)
Dust attenuation increases with M* for a given LFUV
Dust attenuation decreases with LFUV for a given M*
The dispersion in dust attenuation decreases with LFUV
See also Burgarella+06, Buat+09,12
A recipe to derive LIR/LFUV=IRXHeinis+13, very close to be submitted