The Cosmic Flows project : voyage to the Great Attractor - LUTH

The Cosmic Flows project : voyage to the Great Attractor
Hélėne Courtois
Ass. Prof University of Lyon, France
Research associate, Institute for Astronomy, Hawaii, USA
Worshop Structure of the Universe, Obs Paris Nov 28, 2012

2D 3D 4D
Cosmography : mapping with dynamics.
Cosmology question : what is the cause of the CMB motion at 630 km/s?

The large scale cosmic flows constraints on neutrinos
V expansion = H 0 * distance + V peculiar
Peculiar velocities are only due to gravitational interactions.
Our Galaxy has high deviant motion of 630 km/s w.r.t. the CMB dipole (Fixsen et al. 1996)
Decomposition into components:
- Infall towards Virgo cluster at 16 Mpc: ~ 140 km/s (Karachentsev et al. 2010)
- Motion away from a large Local Void (Tully, Courtois et al. 2008)
- Great Attractor at ~ 50 Mpc (Lilje et al. 1986; Lynden-Bell et al. 1988)
- Perseus/Pisces cluster at the opposite side (Hanski et al. 2001)
- Shapley concentration at ~ 150 Mpc ?(Pike & Hudson 2005; Erdoğdu et al. 2006; Bilicki et
al. 2011)
Observed components cannot explain the flow? (Lavaux et al. 2010; Nusser & Davis 2011;
Courtois et al. 2012)

SFI++
Masters, Springob, Haynes, Giovanelli,
2006 ApJ 653, 861
Kraan-Korteweg, 2011, arXiv1107.1069
We are traveling with the Local Sheet as a unit
The Local Sheet is a wall bounding the Local Void which is pushing us away
Edge-on to Supergalactic plane
Tully, Courtois et al. 2008 ApJ 676, 184

2004 : Advent of the new giant radiotelescopes : GBT, Arecibo refurbished, Parkes mulGbeam
2006-­‐2008 : catalog of 1,800 accurate galaxy distances: cosmicflows-­‐1
median error on the peculiar velociGes 13%
2012 : cosmicflows-­‐2 with 7,000 distances up to 80 Mpc
(more than 1,000 hrs at GBT and 200 hrs at Parkes, 30 nights at UH2.2m, 1,800 poinGngs with Spitzer)
Radioastronomy : D. Makarov, I. Karachentsev, S. Mitronova, B. Koribalski, R. Kraan-­‐Korteweg
Photometry ground + Spitzer + WISE : E. Shaya, T. Jarre^, M. Seibert, W. Freedman, B. Madore, E. Persson, K. Sheth
Analysis : S. Go^loeber, Y. Hoffman, G. Yepes, D. Pomarede
PhD Students B. Jacobs, M. Zagurski (USA), B. Depardon, N. Bonhomme, T. Doumler, J. Sorce (Lyon)

Observational methods :
Distances = Peculiar velociGes
V CMB = H 0 * d + V pec
expansion gravitation
V CMB : redshift surveys : only luminous matter, short range correlations
V pec : peculiar velocities : trace full gravitational field : luminous + dark matter, no bias,
long-range correlated fields
Nearby 10 Mpc : Cepheids, Tip red giant branch (TRGB), Surface Brightness Fluctuations (SBF)
Further up to 200 Mpc :
- SNIa : current data too sparse, few hundreds in 8,000 km/s radius
- Fundamental Plane: early types galaxies, in high density regions, not suitable for tracing the
flows, current data quite unreliable (6DF), half-sky
- Tully-Fisher : inclined spiral galaxies, tracing the field where the eddy currents are displayed,
high data number (several 10,000), distance accuracy < 15% and improving, all sky
Very difficult to obtain : 2 accurate deep observations : photometry + radioastronomy

2008 : Cosmicflows-­‐1
2012 : Cosmicflows-­‐2
Courtois et al. AJ, 2009, 138, 1938
Courtois et al. 2011 MNRAS 415,1935
Sorce et al. arXiv:1208.3311 , arXiv:1208.3309
Status of Current observaGonal surveys
Data expands :
Deep I band exposures (UH 2.2m) + HST + Spitzer
Deep HI exposures, NRAO large program
(+1,000 hrs GBT, Parkes, 200 nights/yr )

Simulated Universe CLUES
Full 3D velocity
Full 3D density
TesGng the Wiener Filter reconstrucGon method
Zaroubi et al. 1999 ApJ 520,413
Courtois et al. 2012 ApJ 744,43
Doumler et al. accepted MNRAS 2012
Smoothed at 10 Mpc
Mock catalog : 1,800 radial velocities
5-25% error, median 15%
within 3,000 km/s
…
WF reconstruction:
--> 3D vectors
--> Full density

Results from cosmicflows-­‐1 in 2012: Expulsion from the Local Void.
SGY-SGZ plane
Courtois et al, in prep

The Great A^ractor in the XY plane
Results from cosmicflows-­‐1 in 2012:
Reconstructed ma^er density (luminous + dark ma^er) versus galaxy catalog

Results from cosmicflows-­‐1 in 2012:
Reconstructed ma^er density (luminous + dark ma^er) versus galaxy catalog

Results from cosmicflows-­‐1 in 2012: Pushing the limits: outside the data-­‐zone
Full Matter
Div Tidal
Courtois et al. 2012 ApJ 744,43
• Great Attractor : direction
outside the zone of
avoidance
• Some remaining tidal longrange
velocity field ~ 90
km/s

Results from cosmicflows-­‐1 in 2012: MRI or tomography of the Universe

Status of constrained simulaGons: http://www.clues-project.org/
2009 : CLUES-­‐1 using MARKIII+SBF+Karachentsev peculiar velociGes
2012 : CLUES-­‐2 using cosmicflows-­‐1 : 2,000 (20+%) all-­‐sky 40 Mpc
2014 : CLUES-­‐3 using cosmicflows-­‐2 : 7,000 (10%) all-­‐sky 100 Mpc
improvements on how to implement the constraints in the IniGal condiGons : RZA
SimulaGons will contain Shapley, Peculiar Velocity Data will predict Shapley super-­‐cluster
Do we reach the end of the cosmic flow mo2on towards the CMB?
Great
Attractor
CLUES-1 : 180 Mpc box
Virgo
Perseus

Constraint simulations using peculiar
velocities in the Initial Conditions:
WF + the back in time machine RZA

SGY [Mpc/h]
160
140
120
100
80
60
40
20
0
GA
Test re-­‐simulaGons at z=0, box 160 Mpc/h Doumler et al. Accepted MNRAS 2012
COMA
LSC
30
60
0 20 40 60 80 100 120 140 160
SGX [Mpc/h]
Original simulation full box
PP
log(δ+1)
BOX160 2.5
Y [Mpc/h]
Y [Mpc/h]
100
90
80
70
60
50
40
30
100
90
80
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60
50
40
30
2
1.5
1
0.5
0
40 50 60 70 80 90 100 110
C30_10_II_A -0.5 (with RZA)
Original simulation
X [Mpc/h]
40 50 60 70 80 90 100 110
X [Mpc/h]
Y [Mpc/h]
Y [Mpc/h]
100
90
80
70
60
50
40
30
100
90
80
70
60
50
40
30
C30_10_I_A (without RZA)
40 50 60 70 80 90 100 110
Re-simulation X [Mpc/h] no RZA
E60_10_II_A (with RZA)
Re-simulation with a CF1 mock Re-simulation with a CF2 mock
40 50 60 70 80 90 100 110
X [Mpc/h]
2
1.5
1
0.5
0
2
1.5
1
0.5
0

CLUES 2
A simulation of the Local Universe using cosmicflows-1 peculiar velocities as initial
conditions (+WMAP7) with direct comparison to the observed galaxy distribution (black
dots) : only CDM.
Preliminary results (last week) Sorce, Courtois and CLUES collab
nd generation
What happens if we add a « pinch » of HDM
or even if we try to revisit some WDM models ?
Tikhonov et al. 2009, MNRAS 399, 1611
WDM 1keV

CLUES 2 nd generation, some preliminary validity tests
- Virgo Mass : 8 out on 10 simulations gives us a good Virgo at ~7-9.10^14 Msol in accordance with
observational measurements of the Virgo Mass ~ 8.10^14 Msol
- Peculiar velocities looks in accordance with the observations: amplitude and gaussianity
these tests are not final , run higher resolution simulations in order to check the halo numbers, masses etc ..
Preliminary results , Sorce, Courtois and CLUES collab
Valageas arxiv1206.0554

Preliminary results (yesterday)
Comparison between the average on 10 simulations and the observations: offset on the
Virgo cluster position : X+1, Y+1.5, Z+2.8 Mpc/h
could be due to the Non-Linear part of the peculiar motions : this is a well-known
limitation of our WF+RZA code, that could be covered by a coupling with a Lagrangian
perturbation theory method
we also need to check for the effect of shear and tidal field on the IC

CLUES 2 nd generation
A simulation of the Local Universe using cosmicflows-1 peculiar velocities as initial
conditions (+WMAP7) with direct comparison to the observed galaxy distribution (white
dots) : only CDM.
Preliminary results (yesterday) Sorce, Courtois and CLUES collab

CLUES Structure Formation with cold and warm Dark Matter http://www.clues-project.org/
Evolution of the gas density in the Local Group for CDM (left) and WDM (right), 4096^3 resimulation,
from z=41 to z=0. same color table and density scale was used.
Cosmological Parameters
Species WDM, 1 keV
L box 64 Mpc/h
Ω Λ 0.76
Ω m 0.24
Ω bar 0.0418
h 0.73
σ 8 0.75
N 0.95
Iseed 186592
Spectrum EisHu approximation with an
exponential cut-off according to a 1keV WDM
particle

What is causing the tidal flow after 80 Mpc ?
The Local Void in the YZ plane

Status of Current observaGonal surveys :
Cosmicflows-­‐2 : Data ready 11,000 galaxies with accurate HI / 8,000 galaxies with deep I band and NIR Spitzer
+ inclinaGon + pathological cases 5,000 thrown away ….
40 Mpc 100 Mpc
1,800 cosmicflows-­‐1 at 15% ~ 7,000 galaxy distances at < 10% (~ 2000 GBT)
Peculiar Velocity Data include Great A>ractor,
reconstruc2on predicts Shapley?
2008 2012

Cosmicflows-2 : TFR calibration in I band and 3.6 microns “L” band
Tully and Courtois, 2012 ApJ 749, 78
Courtois and Tully, 2012 ApJ, 749, 174
H 0 = 75.9 ± 3.8 km.s −1 Mpc −1
Sorce et al. 2012 AJ 144, 133
Sorce et al. 2012 ApJ 758, 12

Preliminary results from cosmicflows-2 in 2013 : Reconstructed matter density
(luminous + dark matter) versus galaxy catalog
Coma
The Great A^ractor
Perseus-­‐Pisces
The Great A^ractor seems to be part of a complex flow linked to the Great Wall

Preliminary results from cosmicflows-2 in 2013 : Reconstructed matter
density (luminous + dark matter) versus galaxy catalog : Perseus-Pisces
These results are initial conditions for the 2 nd and 3 rd generation of CLUES constrained
cosmological simulations.

Future surveys and simulaGons
2015 : cosmicflows-­‐3
Radio : -­‐ conGnue deep HI GBT + PARKES + Archives (~900 GBT -­‐ 200 Parkes)
-­‐ SKA precursors mulGdish : WALLABY ASKAP, WNSHS AperGf Westerbrok
Photometry : -­‐ near-­‐infrared (SPITZER + WISE) (analysis started)
-­‐ mulGband (Pan-­‐STARRS + SKYMAPPER)
1,800 > 7,000 > 40,000 distances / at 5% / all-­‐sky / 200 Mpc
Peculiar Velocity Data will include Shapley
super-­‐cluster, observe closer to ZOA
Do we reach the end of the cosmic flow
mo2on towards the CMB?
Can we explain it with standard cosmology ?
space
Zone of avoidance
North South

COSFLO team, major results in 2012
• Publication of analysis of cosmicflows-1 catalog (observational data) :
Production of 4D dynamic maps of the dark matter in the Local Universe up to 80 Mpc (z=0.01).
Localisation of the Great Attractor region and of the remaining tidal field of 90km/s wrt CMB dipole.
in collaboration with Hawaii Univ., USA and Special Observatory, Russia
• Publication of a new code (IceCore) to build constrained initial conditions from peculiar velocities.
in collaboration with Hebrew Univ, Israel and Potsdam Univ., Germany
• Preparation of the second generation of catalog of peculiar velocities cosmicflows-2, publication of the
recalibration of the Tully-Fisher relation using more than 200 SNIa, Cepheids and 13 galaxy clusters.
in collaboration with Hawaii Univ.
• Publication of a new accurate Hubble constant (up to z=1) derived from I band ground photometry
and space near-infrared measurements : H0 = 75.9 ± 3.8 km.s−1Mpc−1 140
in collaboration with Carnegie Institute (Hubble key project) and Univ. Maryland, USA
• Start of the science work on Euclid space mission :
Definition of the interface between NISP instrument simulator OU-SIM and the
cosmological numerical simulations CSWG.
Preparing the production of the first simulated images for NISP.
in collaboration with CPPM Marseille and Durham Univ., UK
SGY [Mpc/h]
160
120
100
80
60
40
20
0
GA
COMA
LSC
30
60
Great attractor
0 20 40 60 80 100 120 140 160
SGX [Mpc/h]
PP
log(δ+1)
2.5
2
1.5
1
0.5
0
-0.5

Thank you
hope you will take home some sense
of your cosmography !