the (kinematic) cosmic web: halo alignments and galaxy...

The (kinematic) cosmic web: halo alignments

and galaxy properties

Noam I Libeskind Leibniz Institute for Astrophysics Potsdam

Halo alignments and the cosmic web

Yehuda Hoffman (Jerusalem)

Stefan Gottloeber (Potsdam) Matthias Steinmetz (Potsdam)

Alexander Knebe (Madrid)

Anatoly Klypin (New Mexico)

Galaxy Properties and the cosmic web

Ofer Metuki (Jerusalem)

Rob Crain (Leiden)

Tom Theuns (Durham) Carlos Frenk (Durham)

Motivation: Galaxy alignments

The MW disc - as well as nearby disc galaxies - are perpendicular to the Super Galactic Plane

Navarro, Abadi & Steinmetz 2004

T  

II  Disc is

Motivation: Galaxy alignments

Alignment of a galaxy’s spin axis with the intermediate axes of the local shear tensor from the reconstructed tidal field of 2MASS

Lee & Erdogdu 2007

The MW disc - as well as nearby disc galaxies - are perpendicular to the Super Galactic Plane

Navarro, Abadi & Steinmetz 2004

Angle between galaxy spin and intermediate shear axis

Pawlowski et al 2012

The spatial alignment of satellite galaxies (the “disc of Satellites”) is a thorn in the side of CDM

Occurs either rarely (~10%) or exceedingly rarely (<1%)

Therefore, in order to keep me from becoming conceited, I was given a thorn in my flesh … to torment me. 2 Corinthians 12:7

“classical satellites” Ultra faints Young GC Streams MW disc Zone of obscuration

Motivation: Satellite Galaxy alignments

Proper motions appear to display rotational support – also rare

In the frame defined by the principle axes of the shear , the angular momentum can be written as

where the ‘s are the eigenvalues of

Angular momentum Inertia tensor  

Tidal shear  

Lee & Lee 2006 Lee & Erdogdu 2008 Navarro et al 2004 + others

The alignment of galaxy spins with the intermediate axis of the shear is not unexpected

In the frame defined by the principle axes of the shear , the angular momentum can be written as

where the ‘s are the eigenvalues of

Angular momentum Inertia tensor  

Tidal shear  

Greatest, hence halo spin should align

with the intermediate axis of

the Shear

Lee & Lee 2006 Lee & Erdogdu 2008 Navarro et al 2004 + others

The alignment of galaxy spins with the intermediate axis of the shear is not unexpected

The cosmic web can be classified by looking at the velocity shear tensor (V-web)

We can diagonalize the shear tensor to obtain the eigenvectors êi and eigenvalues λi . (Order them such that λ1>λ2>λ3)

By counting the number of eigenvalues above a given threshold λth we can classify each point (cell) in the simulation as a specific web element.

The cosmic web can be classified by looking at the velocity shear tensor (V-web)

shear eigensystem

Simulation   Grid + CIC of the

velocity  

smoothing  

Web classification Associate haloes

VOID λth >λ1>λ2>λ3 All three eigenvectors of the shear tensor are expanding

SHEET λ1> λth ; λ2,λ3< λth Collapse along one axis (ê1), expansion along the two (ê2, ê3) �

FILAMENT λ1, λ2> λth ; λ3< λth Collapse along two axes (ê1, ê2), expansion along the other (ê3)

KNOT λ1>λ2>λ3 >λth All three eigenvectors of the shear tensor are collapsing ê3  

ê1  

Bolshoi Simulation (Klypin et al 2011)

Lbox=250 h-1 Mpc with 20483 ≈ 8 billion particles mDM∼ 1.3 × 108 h－ 1M⊙ rsoft∼ 1 kpc.

2563 grid cells = ~1 Mpc

h=0.7, ΩΛ =0.73, Ωm =0.27, Ωb =0.046, n= 0.95 σ8 = 0.82.

This is a kinematical classification, not a geometric one – hence it is interesting to compare with kinematic halo properties (spin)

Mass dependent bias – More massive haloes, the greater the eigenvalues

Just as the distribution of haloes is biased towards high density peaks so to is the value of the cosmic shear.

The distribution of measured eigenvalues

How can we quantifying the uniformity of the eigenvalues

1. Triaxiality:

(λ12-λ3

2 )/( λ12-λ2

2) FAILS since the ordering of λ’s is by value not magnitude

How can we quantifying the uniformity of the eigenvalues

1. Triaxiality:

(λ12-λ3

2 )/( λ12-λ2

2) FAILS since the ordering of λ’s is by value not magnitude

2. Eigenvalue ratio

λ1/λ3 or|λ1/λ3| FAILS for the same reason – also sign makes it a problem

How can we quantifying the uniformity of the eigenvalues

1. Triaxiality:

(λ12-λ3

2 )/( λ12-λ2

2) FAILS since the ordering of λ’s is by value not magnitude

2. Eigenvalue ratio

λ1/λ3 or|λ1/λ3| FAILS for the same reason – also sign makes it a problem

3. Bardeen et al 1986, eccentricity

e = (λ1-λ3 )/ 2 | λ1+λ2+λ3|

FAILS when e.g. λ1~ - λ3 and λ2 ~ 0, e infty. Also, unbound

All these measures are WEB TYPE DEPENDENT

“Diffusion Tensor Imaging”

Fractional Anisotropy FA:

P. J. Basser Inferring microstructural features and the physiological state of tissues from diffusion-weighted images. NMR in Biomedical Imaging, 8, 333 (1995)

Quantifying the uniformity of the shear with the Fractional Anisotropy FA:

FA = 1

FA = √(2/5) ~ 0.632

FA = √(1/7) ~ 0.377

FA = 0

FA=0 FA=1 Isotropy low anisotropy high anisotropy

“magnitude” of the shear

“anisotropy” of the shear

FA probes the structure of voids

FA = 1 0 anisotropic isotropic

FA probes the structure of voids

FA = 1 0 anisotropic isotropic

Voids expand anisotropically (idea in progress…)

FA = 1 0 anisotropic isotropic

IDEA IN PROGRESS

Quantifying the uniformity of the shear with the Fractional Anisotropy FA:

No anisotropy A lot of anisotropy

Quantifying the uniformity of the shear with the Fractional Anisotropy FA:

1.  Knots are the most isotropic

2.  Voids are highly anisotropic

3.  Sheets and filaments span many anisotropy types

No anisotropy A lot of anisotropy

Mass of halo is correlated with the FA

Mass is constant with respect to FA until a critical mass after which mass becomes correlated with FA.

Knots ~ 1012.8 Msol Filaments ~ 1012.4 Msol

Sheets ~ 1011.8 Msol Voids ~ 1011.4 Msol

”Low” mass haloes exist in regions of any FA, while high mass haloes tend to prefer low FA

Assign an FA to each halo

(1) Calculate Shear eigenvalues and eigenvectors

(3) How are haloes aligned with the web (eigenvectors) and how does this depend on the FA?

(BOLSHOI)

(2) Looked at their distribution and quantified their isotropy

(4) Does the web affect galaxy properties?

(GIMIC)

Alignment of halo shape – halo is defined by the inertia tensor a, b, c

a

b

c

c

b

a

Alignment of halo shape – halo is defined by the inertia tensor a, b, c

Use the principle axes of the web ê1, ê2, ê3 and construct angular distribution of a . ê3 , b . ê2 , c . ê1

a . ê3  

Web INDEPENDENT (a bit stronger in voids: could be statistical )

Strength is mass DEPENDENT

Statistically significant alignment of a with ê3 at all masses

Knots

Filaments

M < 1011.5 1011.5 < M < 1012.5 1012.5 < M

(… Marius Cautun’s talk)

Halo shapes aligned with local shear

spin alignment

Look at the angle formed between a halo’s spin and ê3

High mass haloes aligned perpendicular to ê3

(… Marius Cautun’s talk)

Spin flip occurs at 1e12 (Codis et al, Aragon-Calvo et al) as a halo’s merger history goes from being accretion dominated to merger dominated

Spin alignment is web independent, but the mass transition is web dependent.  

Alignment of J with e3 following these cuts gives the proper mass of the transition

Knots ~ 1012.8 Msol

Filaments ~ 1012.4 Msol Sheets ~ 1011.8 Msol

Voids ~ 1011.4 Msol

Each web environment has a characteristic mass – determined by the tendency towards isotropy – that designates the spin flip

Apply V-web to the GIMIC simulation

WORK IN PROGRESS

V-web on GIMIC– luminosity function

V-web on GIMIC - satellite luminosity function

V-web on GIMIC - satellite mass function

V-web on GIMIC – baryon fraction

Conclusions

ALIGNMENTS (Bolshoi)

1.  Strong alignment found between a halo’s shape and the cosmic web 2.  An alignment is also found between the Spin and the cosmic web – the sense of

which is mass dependent. 3.  The mass transition at which haloes go from spinning parallel to perpendicular is

web dependent 4.  Used the Fractional Anisotropy to quantify the uniformity of the local velocity

shear – high mass haloes live in regions of less anisotropy. 5.  There’s a mass scale at which the median fractional anisotropy of a given web

element starts to decrease – this scale corresponds to the mass of the J-e3 spin flip

GALAXIES (Gimic) 1.  Web affects (satellite and central) luminosity

function, satellite mass function.

2.  Baryon fraction as a function of mass, not terribly different across the web

Work in progress