Corentin Cadiou
Santa Cruz Galaxy Workshop

8 August 2023

The causal origin of high-\(z\) galactic angular momentum: replacing galaxies in their cosmological context

Corentin Cadiou
Santa Cruz Galaxy Workshop

8 August 2023

The causal origin of high-\(z\) galactic angular momentum: replacing galaxies in their cosmological context

low \(z\sim 2\)

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?

Angular momentum: bridging galaxy to cosmology

Tillson+15

[AM: Dekel & Birboim 06; Stewart+11; Kim+11; Pichon+11; Codis+12; Danovich+12,15; Stewart+13; Codis+15; Prieto+15; Tillson+15; Stewart+17, Cadiou+21,…]

Dekel&Birnboim 06

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

Lower-zs:
intrinsic alignment problem

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)

  1. Is \(j_\mathrm{DM}\) chaotic or our theory poor?
  2. Do \(j_\mathrm{gal}\) retain memory of their environment?

  3. 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?

  1. Go to non-linear order (non-linear TTT)
  2. 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?

Baryon angular momentum

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

\( j_0 \times 0.66\)

\( j_0 \times 0.8\)

\( j_0 \times 1.2\)

\( j_0 \times 1.5\)

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

Baryon angular momentum

\( j_0 \times 0.66\)

\( j_0 \times 0.8\)

\( j_0 \times 1.2\)

\( j_0 \times 1.5\)

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

… by delaying/hastening time of last major merger

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

INPUT  \(z=\infty\)

OUTPUT
\(z=2\)

\( j_0 \times 0.66\)

\( j_0 \times 0.8\)

\( j_0 \times 1.2\)

\( j_0 \times 1.5\)

\( j_0 \times 0.66\)

\( j_0 \times 0.8\)

\( j_0 \times 1.2\)

\( j_0 \times 1.5\)

✅ Stellar AM driven by (past) tides with the cosmic web (which can be predicted)

✅ Useful to make sense out of e.g. JWST data

✅ Changes in baryon spAM \(\propto\) changes in Halo spAM

\({\color{#808080}{\lambda_\mathrm{DM}}} \underset{f_j}{\Longrightarrow} \lambda_\mathrm{\color{#0000ff}{bar}\color{#daa520}{yon}} \underset{\text{SF+fb}}{\Longrightarrow} \color{#daa520}\lambda_\star\)

❗Per-galaxy fluctuation of \(\lambda_\star/\lambda_\mathrm{DM} \)

\(\Rightarrow\) cannot be captured with HOD modelling

Gas + stars spAM

Stars spAM

Halo spAM

Halo spAM

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.

Dynamics of angular momentum

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

[Kocjan, CC+ in prep]

What happens in the CGM?

Ongoing work by Z. Kocjan

✅ Cold accretion is slow to form stars

Quick depletion right after merger

[Kocjan, CC+ in prep]

Take home messages

  1. \(j_\mathrm{DM}\) responds linearly to tides
    Good accuracy (few ~10%) achievable for individual halos in principle iff correct growth rate+boundary
     
  2. \(j_\mathrm{gal}\) retain memory of the cosmic web
    Galaxies may be less stochastic than expected
    Galactic spin & DM spins are (partially) independent at level of individual galaxies
     
  3. Boundary CW \(\rightarrow\) galaxy formation: CGM
    Buffer zone: transition from gravity-dominated to baryon-dominated regime
    Delay in star formation for cold-accreted gas in CGM: what's the physics?

Take home messages

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 \(0.3R_\mathrm{vir} < r < 2R_\mathrm{vir}\)

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

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?

What if the galaxy had formed here instead?

What if the galaxy had formed here instead?

or here?

The “splicing” technique

  1. Generate ICs
  2. Integrate (\(N\)-nody)
  3. Select region of interest
  4. Trace back to ICs
  5. “Splice”
  6. 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

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

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

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?

The causal origin of high-z galactic angular momentum: replacing galaxies in their cosmological context | Santa Cruz Galaxy Workshop

By Corentin Cadiou

The causal origin of high-z galactic angular momentum: replacing galaxies in their cosmological context | Santa Cruz Galaxy Workshop

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