Corentin Cadiou
Interview for postdoc @ LASTRO/EPFL
16-19 PhD at Institut d'Astrophysique de Paris
“The impact of the large-scale structures of the Universe on dark matter halo and galaxy formation”. Supervisors: C. Pichon and Y. Dubois.
19-now Postdoc on ERC at University College London
Working with A. Pontzen and H. V. Peiris
(ERC: “Tracing galaxy evolution in the early universe”).
6 authored or co-authored papers
+ 8 contributed articles
(simulation, theory)
PI of a 10 Mcpuhr-allocation
co-I in EDGE2.0 & Vintergatan 2 (40 Mcpuhr each)
Short curriculum
Research project
The origin of galaxy properties
[L. Cortese; SDSS.]
[Dubois+16]
AGN no AGN
How to explain morphological diversity at fixed mass?
- Feedback processes (AGN & SN)
- Different assembly (my project)
[L. Cortese; SDSS.]
[Dubois+16]
AGN no AGN
How to explain morphological diversity at fixed mass?
How to explain environmental effects?
- spin alignment to be mitigated in Euclid
- extra parameter in models?
The origin of galaxy properties
The origin of angular momentum
Past research
z=0
z=100
Genetically modified angular momentum
Genetically modified angular momentum
z=0
z=100
[Genetic modifications: Roth+16, see also Rey&Pontzen 18, Stopyra+20]
[AM prediction: described by tidal torque theory, White 84]
z=0
z=100
[Genetic modifications: Roth+16, see also Rey&Pontzen 18, Stopyra+20]
Genetically modified angular momentum
Further described in Cadiou+21a
[AM prediction: described by tidal torque theory, White 84]
The origin of angular momentum
Current & proposed work
Baryon angular momentum
Simulations (10Mh @ DiRAC):
- Resolve disk height
Δx=35 pc - M200c(z=2)=1012 M⊙
- RAMSES
SF + AGN & SN feedback (à la New-Horizon) - Modify l(z=2)
- Tracer particles
Cadiou+19
l0×0.66
l0×0.8
l0×1.2
l0×1.5
PRELIMINARY
Total of ~ 50 simulations
l0×1.2
l0×1.5
l0×0.66
l0×0.8
+
A.M. of the baryons in Rvir
PRELIMINARY
Mock edge-on star maps
Same M200c,M⋆ & early assembly history
Proposed work
- Lower-AM ⇒ bulge ⇒ higher SMBH accretion?
Morphology-AGN relation - ≠scenarios ⇒ relate SMHR to assembly
COSMOS-Webb JWST survey - Can a high-z galaxy be turned quiescent?
Rarity of massive quiescents, simulate them
l0×1.2
l0×1.5
l0×0.66
l0×0.8
The effect of environment on halo properties
Past research
What if the galaxy had formed here instead?
What if the galaxy had formed here instead?
or here?
The “splicing” technique
- Generate ICs
- Integrate (N-nody)
- Select region of interest
- Trace back to ICs
- “Splice”
- Integrate again
t
Splicing: equivalent of constraining field at all points in spliced region
Further described in Cadiou+21b
The effect of environment on halo properties
Proposed work
The effect of environment on halo properties
Proposed work
[Sphinx project]
[Sphinx project]
Proposed work
- Role of environment in setting spin
Contrib. to Euclid weak-lensing mocks - Environmental quenching
effects beyond mere density? - Different effect on DM vs baryons
source of scatter in SMHR?
The effect of environment on halo properties
Summary
Summary
My research
Crosstalk theory ↔ simulations
Testbench of galactic angular momentum & environment
- AM ⇒ interpret IFU/spectro
WEAVE, NIRSpec / MOONS, 4MOST - assembly ⇒ kinematics ⇒ observables
morphology, disk size, spin, BH mass - origin of intrinsic alignment
lensing surveys Euclid
This postdoc
Interpret observations (NirSPEC):
- Morphology-AGN relation
- SMHR relation COSMOS-Webb survey
- Origin of high-z quiescent galaxies
- etc.
Contribute to new models of BH/AGN:
BH seeding, early SMBH growth
The effect of environment on halo properties
Distance to filament
Kraljic+18 [see also Laigle15, Song+21,…]
The causal origin of DM halo concentration
ρDM(r)=Rvir/cr(1+Rvir/cr)2ρ0
Wechsler+02
Origin of scatter at fixed Mvir?
Splicing in 1D
Splicing in 1D
Most likely* field f with
- same value in spliced region (a),
- as close as possible outside (b)
Mathematically f is solution of:
f=a in Γ
minimizes Q=(b−f)†C−1(b−f) outside Γ
Verify that
ξlin(r)∼⟨inδ(x=d)outδ(x=d+r)⟩
is the same in spliced / ref simulation.
Verify that
ξlin(r)∼⟨inδ(x=d)outδ(x=d+r)⟩
is the same in spliced / ref simulation.
Verify that
ξlin(r)∼⟨inδ(x=d)outδ(x=d+r)⟩
is the same in spliced / ref simulation.
[Danovich+15]
The origin of high z angular momentum
[Danovich+15]
I. Torque with cosmic web
The origin of high z angular momentum
[Danovich+15]
I. Torque with cosmic web
II. Transport at constant AM
The origin of high z angular momentum
[Danovich+15]
I. Torque with cosmic web
II. Transport at constant AM
III. Torque down in inner halo
The origin of high z angular momentum
[Danovich+15]
I. Torque with cosmic web
II. Transport at constant AM
III. Torque down in inner halo
IV. Mixing in inner disk & bulge
The origin of high z angular momentum
The origin of high z angular momentum
[Danovich+15]
IV. Mixing in inner disk & bulge
Fraction that ends up in disk vs. IGM?
Influence of galactic physics?
III. Torque down in inner halo
Origin of torque down (pressure or gravity)?
Loss of link with cosmic AM?
II. Transport at constant AM
Same evolution in cold/hot accretion modes?
I. Torque with cosmic web
Predict pre-accretion AM?
Alignment with environment?
The origin of high z angular momentum
[Danovich+15]
IV. Mixing in inner disk & bulge
Fraction that ends up in disk vs. IGM?
Influence of galactic physics?
III. Torque down in inner halo
Origin of torque down (pressure or gravity)?
Loss of link with cosmic AM?
See Cadiou+21c
II. Transport at constant AM
Same evolution in cold/hot accretion modes?
I. Torque with cosmic web
Predict pre-accretion AM?
Alignment with environment?
The origin of high z angular momentum
[Danovich+15]
IV. Mixing in inner disk & bulge
Fraction that ends up in disk vs. IGM?
Influence of galactic physics?
III. Torque down in inner halo
Origin of torque down (pressure or gravity)?
Loss of link with cosmic AM?
II. Transport at constant AM
Same evolution in cold/hot accretion modes?
I. Torque with cosmic web
Predict pre-accretion AM?
Alignment with environment?