Clusters of galaxies and large scale structures

1
Clusters of galaxiesand large scale
structures Activity main results in the period
2004-2007
Staff Bardelli, Cappi, Ettori, Meneghetti,
Zucca Post-docs Gastaldello (2007-), Gitti
(2006-), Rasia (2006) PhD Giacintucci (2007),
Roncarelli (2007), Morandi (2008), Donnarumma
(2010)
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Activity main results (from local to z1
Universe)

• (Super-)cavities, radio halos merging in nearby
  systems
• Metal abundance at intermediate high z
• X-SZ scaling relations gas entropy profiles at
  zgt0.1
• Strong weak lensing techniques
• Simulations of galaxy clusters (X-ray/lensing)

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X-ray supercavities in clusters

• most Cool-Core clusters contain powerful
  central radio sources (AGNs)

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X-ray supercavities in clusters

• most Cool-Core clusters contain powerful
  central radio sources (AGNs)
• central ICM shows holes often coincident with
  radio lobes

? the radio bubbles displace the ICM, creating
X-ray cavities
Supercavities (100s kpc) and weak shocks found
in MS07357421 the most powerful AGN outburst
AGN injects gt1061 erg into the ICM
? Heating of the gas up to
1/2 keV per particle on cluster-wide scale
(McNamara et al. 2005 Gitti et al. 2007)
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X-ray supercavities in clusters
? Effects not strong on T Z profiles
possible on LX fgas

• Clusters with supercavities 3/30 (Rafferty et
  al. 2006) age 108 yr
• ? large outbursts occur 10 of the time in CC
  clusters

L-T relation
MS0735
(Markevitch 1998)
Gitti, McNamara, Nulsen Wise 2007
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RXJ1347 the most X-ray luminous cluster
XMM-Newton data normal X-ray properties of a
relaxed, CC cluster if the disturbed SE
quadrant is excluded detailed mass
determination comparison with
lensing Mlensgt2MX
New VLA data discovery of diffuse,
extended radio emission most distant (z0.45)
radio mini-halo Electron reacceleration
triggered by turbulence in the CC (Gitti et al.
2002) submerger ?
Gitti et al. 2007, AA, 472, 383
Gitti et al. 2007, AA, 470, L25
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Merging clusters

• MUSIC (MUltiwavelength Sample of Interacting
  Clusters)
• Ferrari, Arnaud, Ettori et al. 2006
  Maurogordato, Cappi et al. 2007
• (Observatoire de la Côte dAzur, Sap/CEA Saclay,
  INAF-OA
• Bologna, IOA/NOA Athens, Innsbruck University
  
• PI S. Maurogordato, OCA)
• -- Systematic study of merging processes in
  clusters
• -- Relation between star formation and cluster
  merging
• Based on observations at CFHT (CFH12k, MOS), ESO
• (VIMOS/VLT, EFOSC2/3.6m, WFI/2.2), XMM- Newton,
• Chandra VLA
• CFHTLS Cluster Survey
• Olsen, Benoist, Cappi et al. 2007
• (Observatoire de la Côte dAzur, INAF-OA
  Bologna,
• Sap/CEA, OAMP, OMP, IAP PI C.Benoist, OCA)
• -- Cosmology abundance cluster mass
  function N(z,m)
• -- Cluster evolution galaxy populations in
  clusters

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Cluster scale radio sources halos relics
Double relic in Abell 3376
Radio Halo in A2218
Giant radio Halo in A2163
Very extended radio sources observed in a number
of massive and X-ray luminous clusters ( LX
1044 45 erg/s, Mtot 1015 Mo)

• Radio halos cluster centre, regular
  morphology, unpolarized
• GIANT if 700 kpc
  (Cassano Brunetti, 2005)
• Radio relics cluster outskirts, elongated
  morphology, highly polarized

Are the mergers in massive objects responsible
for the (re-)acceleration of relativistic
particles ?
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Cluster scale radio sources two approaches
1-Statistical GMRT survey at 610 MHz (100
hrs) Final sample of 50 35 new observations 3
new halos 3 new relics
Clusters _at_z0.2-0.4 selected From eBCSREFLEX
surveys
2-Single obj Multiwavelength studies -RADIO
relativistic electrons -XRAY thermal e- merging
on the plane of sky, shocks -OPTICAL 2-d
distribution of galaxies (non-collisional), -SPECT
ROSCOPY merging along the plane of the
sky, kinetic energy of subclumps
S.Gacintucci (PhD), S.Bardelli, E.Zucca
(INAF-OaBo) T.Venturi , G.Brunetti, R.Cassano
(PI) (INAF-IRA Bo) D.Dallacasa, G.Setti (Univ.
Bo), P.Mazzotta (Univ. Rome)
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A case study RXJ1314
LX1.1 1045 erg/s z0.244 The only case known to
date hosting both a double Relic a radio
Halo Relic A distance from the center of 500
kpc and linear dimension of 900 kpc Relic B
distance of 1 Mpc and dimension of 900
kpc Halo linear size of 460 kpc (Giacintucci
et al., in prep)
B
A
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ICM metallicity at high redshift
Radial distribution abundance as function of
cosmic time of the metals observed in the ICM
shed light on the star formation in clusters SN
feedback on the hot phase of the cluster baryons

• Iron abundance profiles
• _at_z0.1-0.3
• from 12 CXO objects
• (Baldi, Ettori et al. 2007)

• Iron abundance evolution
• _at_z0.3-1.3
• from 56 CXO objects
• (Tozzi, Rosati, Ettori et al. 2003
• Balestra, Tozzi, Ettori et al. 2007
• Balestra, Ettori et al. in prep.)

r / R180
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ICM metallicity at high redshift
Maughan et al. (07) 116 clusters at 0.1ltzlt1.3
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Gas entropy profiles at zgt0.1
Morandi Ettori (2007)
Entropy determines the ICM structure records
its thermodynamic history. We need to know how it
evolves with the redshift.
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Lensing _at_INAF-OABo
The INAF-OABo is active in several international
collaborations whose main task is studying
galaxy clusters through lensing

• Strong lensing
• Cluster mass models (mass distribution, density
  profiles)
• Arc statistics (constraints on cosmological
  parameters)
• Weak lensing
• Detection of clusters through weak lensing using
  optimal filtering techniques
• Mass reconstructions
• Cluster mass distributions combining strong and
  weak lensing

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Strong lensing parametric mass model
We have developed a code for doing parametric
mass reconstrictions The code has been used to
reconstruct the inner mass distribution of 11
clusters observed with HST (Comerford,
Meneghetti, Bartelmann Schirmer, 2006)
3c220.1
A370
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Strongweak lensing mass reconstructions

• The method is outlined in Cacciato, Meneghetti,
  Bartelmann Moscardini (2006)
• Uses finite differencing methods for linking the
  observable shear and critical lines to the
  lensing potential
• Produces non-parametric reconstructions of the
  lensing potential maps. Convergence maps are
  obtained from the potential.

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Skylens ( DUNE) (Meneghetti et al. 2007,
arXiv0711.3418)
shapelets
real galaxies
new galaxies
GOODS-ACS archiveCOMBO17
observations
lensing
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Simulated galaxy clusters
To use galaxy clusters as cosmological probes, we
need to know their physical properties (Mtot in
particular) up to R200. X-ray data just cover the
region within 60 of R200.

• First characterization of the physical properties
  at R200
• Systematic studies of the uncertainties on the
  mass and metallicity estimates through X-ray
  analysis (X-ray simulator XMAS2)
• Tackling the X-ray / lensing mass discrepancy
  XMAS2 SkyLens

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Simulated galaxy clusters ICM at Rvir
ngas
Tgas
Roncarelli, Ettori et al 2006
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Simulated galaxy clusters ICM at Rvir
Tgas
ngas
Unresolved CXB w. CXO (Hickox Markevitch 05)
Sb 0.5-2 keV
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Simulated galaxy clusters systematics in Mtot
and metallicity
Rasia, Ettori et al. 06 5 clusters in different
dynamical state have been extracted from a
cosmological hydrodynamical simulation and
processed with X-MAS to obtain mock Chandra
ACIS-S3 1 Ms observations analyze them with
standard procedures
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Simulated galaxy clusters systematics in Mtot
X-ray Mest underestimates Mtrue by 10-45
Ratios btw estimated and true mass profile of the
simulated cluster
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Simulated galaxy clusters Mtot from X-ray and
Optical
MX / X-MAS2 vs Mlensing / SkyLens
from hydrodynamical simulated clusters
(Meneghetti, Ettori, Rasia et al.)
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Simulated galaxy clusters Mtot from X-ray and
Optical
MX / X-MAS2 vs Mlensing / SkyLens
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Activity main results (from local to z1
Universe)

• (Super-)cavities, radio halos merging in nearby
  systems
• Metal abundance at intermediate high z
• X-SZ scaling relations gas entropy profiles at
  zgt0.1
• Strong weak lensing techniques
• Simulations of galaxy clusters (X-ray/lensing)