Towards combined analysis of the most distant massive

Towards combined analysis of the most
distant massive galaxy clusters with
XMM and Chandra
Iacopo Bartalucci
CEA SACLAY SERVICE D’ASTROPHYSIQUE
With: Monique Arnaud, Jessica Democles, Gabriel Pratt, Remco van der Burg
XMM-Newton: the next decade
Our sample
Chandra and XMM combination
Results and future prospects
Why this region?
z > 0.9 High z:
comparison
with local
sample
14
MYz
M°]
500 [10
10
High Mass:
- N(M) sensitive
to high mass
objects
- Gravitationally
dominated
clusters
M > 4 x 1014 M¤ ESZ/PSZ1/PSZ2
SPT
1
0.0
-cosmology
-evolution of gravitational
processes
0.2
0.4
0.6
0.8
1.0
1.2
Redshift
XMM LP (PI M. Arnaud) complented with
Chandra LP (PI P. Mazzotta) and archive
Iacopo Bartalucci
1/8
11/05/2016
Our sample
Chandra and XMM combination
Results and future prospects
X-ray observations of high Z clusters suffer from:
Cosmological dimming
Chandra
Chandra
Iacopo Bartalucci
2/8
11/05/2016
Our sample
Chandra and XMM combination
Results and future prospects
X-ray observations of high Z clusters suffer from:
Cosmological dimming
XMM-Newton bigger effective area…
Chandra
XMM-Newton
Chandra
PSF ~ 15’’
...but AGN confusion problem
Iacopo Bartalucci
2/8
11/05/2016
Our sample
Chandra and XMM combination
Results and future prospects
What do we gain for the imaging?
We gain:
-  Information on
large scale
structure
Point source or substructure? -  Presence of
substructures
BCG -  Chracterization
of the core,
choose of the
center
XX ray peak Iacopo Bartalucci
3/8
11/05/2016
Our sample
Chandra and XMM combination
Results and future prospects
What do we gain for the imaging?
XMM-Newton
Iacopo Bartalucci
4/8
Chandra
11/05/2016
Our sample
Chandra and XMM combination
Results and future prospects
What do we gain for the imaging?
XMM-Newton
Chandra
XMM-Newton and Chandra
combination is fundamental to
investigate morphological status
and XMM PSF is sufficient for <w>
Iacopo Bartalucci
4/8
11/05/2016
Our sample
Chandra and XMM combination
With XMM-Newton we probe
the outskrits @ R~R500
With Chandra we probe
the core @ R<0.1R500
Iacopo Bartalucci
Results and future prospects
5/8
11/05/2016
Our sample
Chandra and XMM combination
Results and future prospects
Profiles are consistent! No PSF issues so…
Iacopo Bartalucci
5/8
11/05/2016
Our sample
Chandra and XMM combination
Results and future prospects
We combine the profiles fitting simultaneosuly a parametric profile
Vikhlinin et al 2006
Iacopo Bartalucci
5/8
11/05/2016
Our sample
Chandra and XMM combination
Results and future prospects
We combine the profiles fitting simultaneosuly a parametric profile
Vikhlinin et al 2006
Iacopo Bartalucci
5/8
11/05/2016
Our sample
Chandra and XMM combination
Results and future prospects
Combination of Chandra and
XMM-Newton is fundamental to
efficiently probe the core and
the outskirts
We combine the profiles fitting simultaneosuly a parametric profile
Vikhlinin et al 2006
Iacopo Bartalucci
5/8
11/05/2016
Our sample
Chandra and XMM combination
Results and future prospects
Hints of evolution? Taking as reference the REXCESS sample
(Boehringer et al 2007,Pratt et al 2009, Arnaud et al 2010)
No clear signs of evolution for ne.
Deviations due to dynamical status
Iacopo Bartalucci
6/8
11/05/2016
Our sample
Chandra and XMM combination
Results and future prospects
Hints of evolution? Taking as reference the REXCESS sample
(Boehringer et al 2007, Pratt et al (2009,2010), Arnaud et al 2010)
Individual profiles Entropy profiles are, on average,
lower than local sample at R~R500
Iacopo Bartalucci
Same behavior in the K-­‐M plane at high R 7/8
11/05/2016
We presented a new method to efficiently analyse high redshift clusters.
Science coming in! BUT we need to populate the sample and apply the
same strategy to spectroscopic analysis.
…working on combining also
spectroscopic information,
i.e. temperature profiles!
Combination of XMM-Newton deep
observations and shorter Chandra
brings fundamental information…
Snapshot strategy
Iacopo Bartalucci
Martino et al (2014)
8/8
11/05/2016