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
contributor to EDGE 2 / PRACE Run
[L. Cortese; SDSS.]
[Dubois+16]
AGN no AGN
How to explain morphological diversity at fixed mass?
[L. Cortese; SDSS.]
[Dubois+16]
AGN no AGN
How to explain morphological diversity at fixed mass?
How to explain environmental effects?
Past research
z=0
z=100
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]
Further described in Cadiou+21a
[AM prediction: described by tidal torque theory, White 84]
Current & proposed work
Simulations (10Mh @ DiRAC):
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
l0×1.2
l0×1.5
l0×0.66
l0×0.8
Past research
What if the galaxy had formed here instead?
What if the galaxy had formed here instead?
or here?
t
Splicing: equivalent of constraining field at all points in spliced region
Further described in Cadiou+21b
Proposed work
Proposed work
[Sphinx project]
[Sphinx project]
Crosstalk theory ↔ simulations
Testbench of galactic angular momentum & environment
Understand angular momentum
Happy to contribute expertise of RAMSES!
Distance to filament
Kraljic+18 [see also Laigle15, Song+21,…]
ρDM(r)=Rvir/cr(1+Rvir/cr)2ρ0
Wechsler+02
Origin of scatter at fixed Mvir?
Most likely* field f with
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]
[Danovich+15]
I. Torque with cosmic web
[Danovich+15]
I. Torque with cosmic web
II. Transport at constant AM
[Danovich+15]
I. Torque with cosmic web
II. Transport at constant AM
III. Torque down in inner halo
[Danovich+15]
I. Torque with cosmic web
II. Transport at constant AM
III. Torque down in inner halo
IV. Mixing in inner disk & bulge
[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?
[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?
[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?