Corentin Cadiou
SNO Kickoff

19/12/23

Unravelling the causal origin of galaxy scaling relations, from cosmological scale to ISM scales

Cadiou, Pontzen & Peiris 21 · Cadiou, Pontzen +21 · Kocjan, Cadiou, Agertz, Pontzen 23 · Cadiou, Pichon-Pharabod+23

Corentin Cadiou
SNO Kickoff

19/12/23

Unravelling the causal origin of galaxy scaling relations, from cosmological scale to ISM scales

Playing with RAMSES at too many scales

Cadiou, Pontzen & Peiris 21 · Cadiou, Pontzen +21 · Kocjan, Cadiou, Agertz, Pontzen 23 · Cadiou, Pichon-Pharabod+23

Slide with CW -> Galaxies -> ISM

Plan:

The large scales
From LSS to halo formation → splicing + GM AM
genetIC
The intermediate scales
From CW to gal. form → Zuzanna's work
tracer particles
The small scales
MEGATRON
high-cadence outputs

Galaxies in cosmological env: origin of AM?

Full hydro simulations
(10Mh @ DiRAC):

Resolve disk height
$\Delta x_\mathrm{min} = 35\ \mathrm{pc}$
$M_\mathrm{200c} = 10^{12}\ \mathrm{M}_\odot$ @ $z=2$
SF + AGN & SN feedback
3 galaxies, 5× scenario each

$ j_0 \times 0.66$

$ j_0 \times 0.8$

$ j_0 \times 1.2$

$ j_0 \times 1.5$

Galaxies in cosmological env: origin of AM?

Cadiou, Pontzen & Peiris+21

Low tides

High tides

$\mathcal{B}\searrow R_\mathrm{eff} ,v/\sigma\nearrow$

INPUT: Changes to tides $z=\infty$

OUTPUT: Ang. mom
$z=2$

$ j_0 \times 0.66$

$ j_0 \times 0.8$

$ j_0 \times 1.2$

$ j_0 \times 1.5$

$ j_0 \times 0.66$

$ j_0 \times 0.8$

$ j_0 \times 1.2$

$ j_0 \times 1.5$

See Cadiou, Pontzen & Peiris+21

$ j_0 \times 0.66$

$ j_0 \times 0.8$

$ j_0 \times 1.2$

$ j_0 \times 1.5$

$ j_0 \times 0.66$

$ j_0 \times 0.8$

$ j_0 \times 1.2$

$ j_0 \times 1.5$

See Cadiou, Pontzen & Peiris+21

INPUT: Changes to tides $z=\infty$

OUTPUT: Ang. mom
$z=2$

Stellar disk angular momentum responds ~linearly to large-scale tides

See Cadiou, Pontzen & Peiris+21

INPUT: Changes to tides $z=\infty$

OUTPUT: Ang. mom
$z=2$

Gas + stars spAM

Stars spAM

Halo spAM

See Cadiou, Pontzen & Peiris+21

Halo and disk evolve separately,

but $\lambda_\mathrm{baryon} \propto \lambda_\mathrm{DM}$

Gas + stars spAM

Stars spAM

Halo spAM

See Cadiou, Pontzen & Peiris+21

$z=0$

$ z = 100$

[Genetic modifications: Roth+16, see also Rey&Pontzen 18, Stopyra+20]

Tide $\nearrow$ delay merger

Tide $\searrow$ hasten merger

Corentin Cadiou

This suggests a way to predict ab initio merger orbital parameters (e.g. spin)

See Cadiou, Pichon-Pharabod+23

Corentin Cadiou

So far, I've shown effect of linear perturbations on galaxy formation.

How to probe non-linear couplings?

Corentin Cadiou

What if the galaxy had formed here instead?

Corentin Cadiou

What if the galaxy had formed here instead?

or here?

Corentin Cadiou

Splicing technique Cadiou, Pontzen & Peiris 21

Extended by A. Storck

Galaxies haloes in cosmological env

Splicing technique Cadiou, Pontzen & Peiris 21

Extended by A. Storck

Galaxies haloes in cosmological env

Splicing technique Cadiou, Pontzen & Peiris 21

Extended by A. Storck

Galaxies haloes in cosmological env

Far

Halo (mis-)aligns itself to filament

Tracer particles to investigate high-$z$ inflows

CC+19

Evolution of angular momentum

CC+21

Realignment between…

…$3R_\mathrm{vir}$ and $R_\mathrm{vir}$

…$R_\mathrm{vir}$ and $R_\mathrm{vir}/3$

…$R_\mathrm{vir}$ and $R_\mathrm{vir}/10$

✅ Most of realignment happens in “CGM” ($\leq R_\mathrm{vir}/3$)

Mostly due to grav. torques (consistent with e.g. Danovich+15)

[CC+21]

$t_{1/3}$

$t_{\star}$

$T_\mathrm{max}$ between $2 R_\mathrm{vir}$ and $R_\mathrm{vir}/3$?

$\leq 3\times10^4\,\mathrm{K}$

Cold accretion

$\geq 5\times10^5\,\mathrm{K}$

Hot accretion

What happens in the CGM?

✅ Cold accretion is slow to form stars

Quick depletion right after merger

How long to form stars after accretion?

Kocjan, CC+23 (submitted)

Dwarfs may contribute to IGM enrichment... But how much?

EDGE2 collaboration (Read, Pontzen, Agertz, Rey, Cadiou, …)

Angular momentum: bridging galaxy formation to cosmology

2 Spin $\leftrightarrow$ morphology

Romanowsky&Fall 12

Harrison+17

Hasan+23 (TNG)

3 Cosmic web $\leftrightarrow$ SFR

Kraljic+CC+19 (HAGN)

1 Cosmic web $\leftrightarrow$ spin

Ganeshaiah Veena+21

Corentin Cadiou

Angular momentum: bridging galaxy formation to cosmology

2 Spin $\leftrightarrow$ morphology

Romanowsky&Fall 12

Harrison+17

Hasan+23 (TNG)

3 Cosmic web $\leftrightarrow$ SFR

Kraljic+CC+19 (HAGN)

1 Cosmic web $\leftrightarrow$ spin

Ganeshaiah Veena+21

Corentin Cadiou

Why is the effect of the cosmic web at % level?
What's the arrow of causality?
CW ⇒ spin ⇒ morphology?
How stochastic is galaxy formation?

MEGATRON (w/ Harley Katz & Martin Rey)

Vintergatan rerun: $M_\mathrm{DM} = 10^{12}\,M_\odot$ at $z=0$ (Rey+23a)
2 runs: constant physical + constant comoving $25\mathrm{pc}$ at $z=2$
- $\Delta M_\star = 500\,M_\odot$
- $M_\mathrm{DM} = 1.6\times 10^4\,M_\odot$
Out of equilibrium chemistry + RT (PRISM model; Katz 23)
- 8 bands (IR to EUV)
- H I-II, He I-III, 𝑒−, C I-VI, N I-VII, O I-VIII, Ne I-X, Mg I-X, Si I-XI, S I-XI, & Fe I-XI, H2 & CO
  (110 variables!)
Tracer particles + on-the-fly-dump (Cadiou+19, 24 in prep)
- $M_\mathrm{tracer} = 7\times 10^4 \,M_\odot$
- $\Delta t = 0.8\,\mathrm{Myr}$
Restarts with refinement on cooling-length (Rey+23b)
Dust: broken power law for dust-to-metal ratio

Purple: density, white: H$\beta$, yellow: OIII

tides ×0.5 ⇒ merger @ $z=0.7$

tides ×1.1 ⇒ merger @ $z=0.55$

tides ×1.2 ⇒ merger @ $z=0.5$

tides ×2 ⇒ merger @ $z=0.2$

Changes to tides at $z=100$, effect at $z<1$

import yt

ds = yt.load("NewHorizon/OUTPUT_DIR/output_01026")
center = ds.arr([0.49929798, 0.49699318, 0.49730742], "code_length")
radius = (200, "kpc")

# Create a sphere of 1 Rvir
sp = ds.sphere(center, radius)

# Read density
p = yt.ProjectionPlot(
	ds, "z", "density", center=center, width=radius, weight_field="density", data_source=sp
)
p.set_axes_unit("kpc")
p.save("frames/")

# Read particles
sp["io", "particle_position"]

1,400,000 hydro cells

2,500,000 particles read

in 53 domains (out of 4800)

Now runs in ~10s 🎉!

(soon to be released)

Also happy to talk about pynbody & tangos!

SNO wishlist

Ensure stability / backward compatibility of outputs and
auto-document them (à la part_file_descriptor.txt)

Library of on-the-fly analysis tools

movie routine is a mess and can't be extended
power-spectrum? Flux through $R_\mathrm{vir}$?

Decouple different parts of the code (e.g., gradually remove global variables)

Fully ported to GPU, bug free

Conclusions

Corentin Cadiou

Tides drive stellar angular momentum, which drives scaling relations
AM causes bulge to reduce, radius and $v/\sigma$ to increase
Explains $j_\star-M_\star-\mathcal{B}$ relation (and Tully-Fisher?)
$j_\mathrm{gal}$ retain memory of the cosmic web
Galaxies are less stochastic than expected
Galactic spin & DM spins are partially independent at the level of individual galaxies
Non-linear effects are important to understand the origin of spin fully (so disk!)
At MW mass, the closer to a filament, the more $\perp$ the halo spin
Galaxy simulations are in the pipes

Conclusions

Corentin Cadiou

What's the effect of anisotropic env DM/gal formation?

Study same object, different environment.

CC+21, arXiv: 2107.03407

Cosmic web drives AM acquisition... what scales? what's affected?

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

The causal origin of DM halo concentration

$M^{(1)}_{200\mathrm{c}}, c^{(1)}_\mathrm{NFW}, \dots$

$M^{(2)}_{200\mathrm{c}}, c^{(2)}_\mathrm{NFW}, \dots$

$M^{(\dots)}_{200\mathrm{c}}, c^{(\dots)}_\mathrm{NFW}, \dots$

$M^{(10)}_{200\mathrm{c}}, c^{(10)}_\mathrm{NFW}, \dots$

Same halo in 10× different environments

Repeat experiment for 7 halos (70 realisations in total)

Same halo in 10× different environments

Repeat experiment for 7 halos (70 realisations in total)

$M^{(1)}_{200\mathrm{c}}, c^{(1)}_\mathrm{NFW}, \dots$

$M^{(2)}_{200\mathrm{c}}, c^{(2)}_\mathrm{NFW}, \dots$

$M^{(\dots)}_{200\mathrm{c}}, c^{(\dots)}_\mathrm{NFW}, \dots$

$M^{(10)}_{200\mathrm{c}}, c^{(10)}_\mathrm{NFW}, \dots$

The causal origin of DM halo concentration

Same halo in 10× different environments

Repeat experiment for 7 halos (70 realisations in total)

$M^{(1)}_{200\mathrm{c}}, c^{(1)}_\mathrm{NFW}, \dots$

$M^{(2)}_{200\mathrm{c}}, c^{(2)}_\mathrm{NFW}, \dots$

$M^{(\dots)}_{200\mathrm{c}}, c^{(\dots)}_\mathrm{NFW}, \dots$

$M^{(10)}_{200\mathrm{c}}, c^{(10)}_\mathrm{NFW}, \dots$

The causal origin of DM halo concentration

50% of population

Harrison+17 (KMOS, $z=1$)

Spiral galaxies $\leftrightarrow$ high $J_\star$

What's the arrow of causality?

Rodriguez-Gomez+22 (TNG)

Angular momentum: controls disk formation?

Tillson+15

Dekel&Birnboim 06

High-z:
most of mass + AM flow along filaments

How do we study these effects?

Large volumes

sample $p(M_\star, M_\mathrm{DM},\mathbf{J}, d_\mathrm{fil}, \dots)$

This talk

sample $p(\mathbf{J}|M_\star, M_\mathrm{DM}, d_\mathrm{fil}, \dots)$

Angular momentum: bridging galaxy to cosmology

Lower-zs:
intrinsic alignment problem

Angular momentum: where are we?

Porciani+02

Rodriguez-Gomez+22

Predictions for $j_\mathrm{DM}$ remain qualitative

$j_\mathrm{DM}-j_\mathrm{\star}$
weak correlation
(statistically strong)

Is $j_\mathrm{DM}$ chaotic or our theory poor?
Do $j_\mathrm{gal}$ retain memory of their environment?
How is AM transported to the disk?

1. Is $j_\mathrm{DM}$ chaotic or our theory poor?

First controlled experiment of testing tidal torque theory for individual halos

CC+21a, arXiv: 2012.02201

2. Do $j_\mathrm{gal}$ retain memory
of the environment?

3. How is AM transported
to the disk?

Predicting angular momentum

$z=0$

$ z = 100$

Predicting angular momentum

$z=0$

$ z = 100$

[White 84]

Predicting angular momentum

$z=0$

$ z = 100$

[Genetic modifications: Roth+16, see also Rey&Pontzen 18, Stopyra+20]

Predicting angular momentum

Time

Sampling $p(\mathbf{J}|M_\mathrm{DM}, d_\mathrm{fil}, \dots)$

Predicting angular momentum

Time

Predicting angular momentum

✅ AM of fixed DM regions responds ~linearly (so is not chaotic!)

Improve theory?

Go to non-linear order (non-linear TTT)
Accurate prediction of Lagrangian patch boundaries (see Musso&Sheth 23)

1. Is $j_\mathrm{DM}$ chaotic or our theory poor?

2. Do $j_\mathrm{gal}$ retain memory
of the environment?

First controlled experiment of angular momentum accretion on individual galaxies

CC+22, arXiv: 2206.11913

Main idea: stars are deeper in potential well so less sensitive to what happens at large scales

⇒ stellar Lagrangian patch should be more stable to perturbations

3. How is AM transported
to the disk?

1. Is $j_\mathrm{DM}$ chaotic or our theory poor?

2. Do $j_\mathrm{gal}$ retain memory
of the environment?

3. How is AM transported
to the disk?

CC+Pichon+Dubois, 21, arXiv: 2110.05384

Kocjan, CC in prep.

The effects of environment on halo properties

Kraljic+18 [see also Laigle15, Song+21,…]

$ M_\mathrm{DM}(\text{node}) $ > $M_\mathrm{DM}(\text{fil}) $ >$M_\mathrm{DM}(\text{void})$, higher clustering
spins align with cosmic web ⇒ issue for weak lensing
$v/\sigma(\mathrm{fil})>v/\sigma(\mathrm{void})$ ⇒ bias in galaxy formation
….

The effects of environment on halo properties

Isotropic effects

Kaiser bias, cluster vs. groups, ...

From theory: $M\propto \int\mathrm{d}^3R\rho$

Mass regulated

An-isotropic effects

Intrinsic alignment, formation of disks?

From theory: $J \propto \int\mathrm{d}^3R \nabla \phi$

Angular momentum regulated?

Predicting angular momentum

$z=0$

$ z = 100$

\[\mathbf{L}_\mathrm{lin.} \propto \int\mathrm{d}^3q(\mathbf{q}-\bar{\mathbf{q}})\times \nabla\phi\]

Position w.r.t. center

Velocity

[White 84]

Note: vanishes at 1st order in a sphere

\[ \int_\Gamma \mathrm{d}^3{q}(\mathbf{q}-\mathbf{\bar{q}}) \times\nabla\phi = \int_{\partial\Gamma}\phi(q)(\mathbf{q}-\mathbf{\bar{q}})\times\mathrm{d}\mathbf{S}\]

Note: the following is a (poor) approximation:

\[ \mathbf{L} \propto \epsilon_{ijk} T_{jl}I_{lk},\quad\text{with \textbf{T} the tidal tensor and \textbf{I} the inertia tensor}\]

[See also Danovich+15, Prieto+17]

✅ Most of re-alignment happens in the CGM $0.1\leq \displaystyle\frac{r}{R_\mathrm{vir}}\leq 0.3$

The longer gas remains in CGM, the more it realigns with disk

[See also Danovich+15, Prieto+17]

Ongoing work by Z. Kocjan

[Kocjan, CC+ in prep]

Filamentary accretion ~ Cold flow = $T \leq 10^5\mathrm{K}$ for $0.3R_\mathrm{vir} < r < 2R_\mathrm{vir}$

Not necessarily fast-track to star formation ⇒ lose connection to CW?

[Kocjan, CC+ in prep]

$M_\mathrm{DM}(z=2)\approx 10^{11}-10^{12} \mathrm{M_\odot}$

Ongoing work by Z. Kocjan

Ex Uno Plures: direct measure of the impact of the cosmic web on individual objects to shed light on their population statistics

Corentin Cadiou
The Co-evolution of the CW and Galaxies across Cosmic Time

The causal origin of DM halo concentration

$$\rho_\mathrm{DM}(r) = \frac{\rho_0}{\frac{r}{R_\mathrm{vir}/c} \left(1 + \frac{r}{R_\mathrm{vir}/c}\right)^2}$$

Wechsler+02

Origin of scatter at fixed $M_\mathrm{vir}$?

Predicting angular momentum

Angular momentum of individual regions can be predicted accurately.
AM of halos ⇒ requires boundaries of patch

\[\mathbf{L}_\mathrm{lin.} \propto \int\mathrm{d}^3q(\mathbf{q}-\bar{\mathbf{q}})\times \nabla\phi\]

[On patch boundaries: see Lucie-Smith+18]

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 $\Gamma$

minimizes $\mathcal{Q} = (b-f)^\dagger\mathbf{C}^{-1}(b-f) $ outside $\Gamma$

Can we control baryonic
angular momentum?

Wechsler & Tinker 18

${\color{red}M_\star} / M_\mathrm{h} \ll \Omega_b / \Omega_m $
⇒ baryons & DM stem from different regions

Baryons more strongly bound
⇒ less prone to being ejected

Verify that

\[\xi_\mathrm{lin}(r) \sim \left\langle {\color{green}\underbrace{\delta(x=d)}_\mathrm{in}} {\color{purple} \underbrace{\delta(x=d+r)}_\mathrm{out}}\right\rangle \]

is the same in spliced / ref simulation.

Verify that

\[\xi_\mathrm{lin}(r) \sim \left\langle {\color{green}\underbrace{\delta(x=d)}_\mathrm{in}} {\color{purple} \underbrace{\delta(x=d+r)}_\mathrm{out}}\right\rangle \]

is the same in spliced / ref simulation.

Verify that

\[\xi_\mathrm{lin}(r) \sim \left\langle {\color{green}\underbrace{\delta(x=d)}_\mathrm{in}} {\color{purple} \underbrace{\delta(x=d+r)}_\mathrm{out}}\right\rangle \]

is the same in spliced / ref simulation.

Temporary conclusions

angular momentum is predictable
boundary of halos in the ICs is a hard problem
⇒ limits practicality of predictions (for now)
baryons appear to be simpler!
⇒ good news for weak lensing predictions
⇒ key to understand morphology

Galaxy formation in cosmology: the role of the environment

Environmental effects:

source of “pollution” in weak lensing surveys
⇒ intrinsic alignment
extra parameters in semi-analytical models
⇒ galaxy-halo correlation

$ R_{1/2} $

$ l_0 \times 1.2$

$ l_0 \times 1.5$

$ l_0 \times 0.66$

$ l_0 \times 0.8$

$ l_0 \times 0.66$

$ l_0 \times 0.8$

$ l_0 \times 1.2$

$ l_0 \times 1.5$

$ l_0 \times 1.2$

$ l_0 \times 1.5$

$ l_0 \times 0.66$

$ l_0 \times 0.8$

$ l_0 \times 1.2$

$ l_0 \times 1.5$

$ l_0 \times 0.66$

$ l_0 \times 0.8$

AM of baryons originates from initial conditions…
can be controlled…
and regulate galaxy morphology
Negligible AGN/SN global self-regulation

Galaxy formation

[L. Cortese; SDSS.]

[Dubois+16]

AGN no AGN

Origin of morphological diversity at fixed mass?

[L. Cortese; SDSS.]

[Dubois+16]

AGN no AGN

Origin of morphological diversity at fixed mass?

How to explain environmental effects?

[Kraljic+ in prep]

Galaxy formation

[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

[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?

Unravelling the causal origin of galaxy scaling relations, from cosmological scale to ISM scales | SNO Kickoff

By Corentin Cadiou

Unravelling the causal origin of galaxy scaling relations, from cosmological scale to ISM scales | SNO Kickoff

Presentation at IAP symposium

Unravelling the causal origin of galaxy scaling relations, from cosmological scale to ISM scales

Unravelling the causal origin of galaxy scaling relations, from cosmological scale to ISM scales

Playing with RAMSES at too many scales

Galaxies in cosmological env: origin of AM?

Galaxies in cosmological env: origin of AM?

Galaxies haloes in cosmological env

Galaxies haloes in cosmological env

Galaxies haloes in cosmological env

Tracer particles to investigate high-\(z\) inflows

Evolution of angular momentum

What happens in the CGM?

How long to form stars after accretion?

Angular momentum: bridging galaxy formation to cosmology

Angular momentum: bridging galaxy formation to cosmology

SNO wishlist

Conclusions

Conclusions

What's the effect of anisotropic env DM/gal formation?

The “splicing” technique

The causal origin of DM halo concentration

The causal origin of DM halo concentration

The causal origin of DM halo concentration

Angular momentum: controls disk formation?

Angular momentum: bridging galaxy to cosmology

Angular momentum: where are we?

1. Is \(j_\mathrm{DM}\) chaotic or our theory poor?

2. Do \(j_\mathrm{gal}\) retain memory of the environment?

3. How is AM transported to the disk?

Predicting angular momentum

Predicting angular momentum

Predicting angular momentum

Predicting angular momentum

Predicting angular momentum

Predicting angular momentum

1. Is \(j_\mathrm{DM}\) chaotic or our theory poor?

2. Do \(j_\mathrm{gal}\) retain memory of the environment?

3. How is AM transported to the disk?

1. Is \(j_\mathrm{DM}\) chaotic or our theory poor?

2. Do \(j_\mathrm{gal}\) retain memory of the environment?

3. How is AM transported to the disk?

The effects of environment on halo properties

The effects of environment on halo properties

Isotropic effects

An-isotropic effects

Predicting angular momentum

Ex Uno Plures: direct measure of the impact of the cosmic web on individual objects to shed light on their population statistics

The causal origin of DM halo concentration

Predicting angular momentum

Splicing in 1D

Splicing in 1D

Can we control baryonic angular momentum?

Temporary conclusions

Galaxy formation in cosmology: the role of the environment

Galaxy formation

Galaxy formation

The origin of high \(z\) angular momentum

The origin of high \(z\) angular momentum

The origin of high \(z\) angular momentum

The origin of high \(z\) angular momentum

The origin of high \(z\) angular momentum

The origin of high \(z\) angular momentum

The origin of high \(z\) angular momentum

The origin of high \(z\) angular momentum

Unravelling the causal origin of galaxy scaling relations, from cosmological scale to ISM scales | SNO Kickoff

More from Corentin Cadiou

2. Do \(j_\mathrm{gal}\) retain memory
of the environment?

3. How is AM transported
to the disk?

2. Do \(j_\mathrm{gal}\) retain memory
of the environment?

3. How is AM transported
to the disk?

2. Do \(j_\mathrm{gal}\) retain memory
of the environment?

3. How is AM transported
to the disk?

Can we control baryonic
angular momentum?