Star formation at low and high IR luminosity in high-z interacting ...
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Star formation at low and high IR luminosity in high-z interacting galaxies G. Drouart (Chalmers), Marstrand, 4 June 2015 C. De Breuck (ESO), J. Vernet (ESO), N. Seymour (Curtin Uni.), M. Lehnert (IAP), B. Rocca-Volmerange (IAP), D. Stern (JPL), B. Emonts (CSIC-INTA), B. Gullberg (ESO->Durham), T. Nilsson (ESO/IAP), K. Knudsen (Chalmers), J. Fogasy (Chalmers), L. Lindroos (Chalmers), J. Richard (Lyon U.), J.P. Kneib (EPFL), A. Romeo (Chalmers) Collaborators
Transcript of Star formation at low and high IR luminosity in high-z interacting ...
Star formation at low and high IR luminosity in high-z interacting galaxies
G. Drouart (Chalmers), Marstrand, 4 June 2015
C. De Breuck (ESO), J. Vernet (ESO), N. Seymour (Curtin Uni.), M. Lehnert (IAP),
B. Rocca-Volmerange (IAP), D. Stern (JPL), B. Emonts (CSIC-INTA), B. Gullberg (ESO->Durham),
T. Nilsson (ESO/IAP),
K. Knudsen (Chalmers), J. Fogasy (Chalmers),
L. Lindroos (Chalmers), J. Richard (Lyon U.), J.P. Kneib (EPFL),
A. Romeo (Chalmers)
Collaborators
The high IR luminosity:
HzRGs/HeRGE
HeRGE sample - HzRGs
Sample of 71 HzRGsz>1 and L3GHz>1026 W/Hz
entire sample: Spitzer, Herschel, submm, radio
+ subsamples: mm, optical/NIR
Drouart et al. 2014
Pre-ALMA era - the dragonfly galaxy
Emonts et al. 2011
Drouart et al. 2014
Herschel SED ~3000 M⊙/yrno evidence of merger
HST images reveal a perturbed system
The dragonfly galaxyMajor Merger at z~2
Emonts et al., arxiv
MRC 0943-242, z=2.9
2 arc seconds
Dust continuum Ly� emission HeII emission 4.5!m emission CO(8-7) line emission Radio lobes
A Glimpse of Valhalla
2 arc seconds
Dust continuum Ly� emission HeII emission 4.5!m emission CO(8-7) line emission Radio lobes
Yggdrasil
Thor
Bifrost
Loke
BifrostOdin
Freja
Ly�
IRAC 4.5!m
Dust continuum
Synergy of MUSE and ALMA
Before and After ALMA
SFR ~ 2000 M�/yr
The “low” IR luminosity:
Lensed sources
MS0451.6-0305: LIRG interacting system at z~2.9
• Amplified by foreground galaxy cluster
• Large differential magnification (!~3-45)
• Extremely rare case of alignment
• 70h PdBI programme, 2003-2005
• centred on CO(3-2) emission at z~2.91
Lensing amplification
Mac Kenzie et al. 2014
Lensing amplification
Mac Kenzie et al. 2014Berciano Alba et al. 2010
Lensing amplification
Mac Kenzie et al. 2014
Lensing amplification
Mac Kenzie et al. 2014
?Stephen Quintet
Drouart et al, in prep
L’CO vs far-IR properties
if only z>2 sources, only a few
below the ULIRG regime
CO emission onto the critical line, so most probably ten time intrinsically
fainter
Villar-Martin et al. 2013
Thank you!
Taken Monday, by the Nautic Hotel around 22h
Disentangle AGN and Star formation
• SED fitting UV to FIR (restframe)• 3 components: AGN+PEGASE.3• 𝝌2-‐minimization, grid-method• 10 free parameters• 11 HzRGs (1<z<4 and L3GHz>1026 W/Hz)
PKS 1138-262, z=2.1
4C 28.58, z=2.9
MRC 0406-244, z=2.4
4C 41.17, z=3.8
Physical properties of star formation
Disentangling AGN and Star formation
Specific growth rates
Host galaxies Black holes
HzRGs above the average objects in both cases
Time delay in relative SMBH-host growth
