# Presentation: 721095

## XMM-Newton -Project

**	****	****	****	****J.P. Bernard**
**	****	****	****	****A. Blanchard**
**	****	****	****	****M. Boer**
**	****	****	****	****D.J. Burke**
**	****	****	****	****C.A. Collins**
**	****	****	****	****M. Giard**
**	****	****	****	****D.H. Lumb **
**	****	****	****	****P. Marty**
**	****	****	****	****J. Nevalainen **
**	****	****	****	****R.C. Nichol**
**	****	****	****	****A.K. Romer**
**	****	****	****	****R. Sadat**

**+ BAX : X-ray cluster data base**
- _[http://webast.ast.obs-mip.fr/bax](http://webast.ast.obs-mip.fr/bax)_
**See the Poster by R. Sadat et al.**

**Sébastien C. VAUCLAIR**

- XMM-Newton -Project

## XMM-Newton -Project

- =>	D. Lumb et al., astro-ph/0311344
- =>	S.C.Vauclair et al., A&A 412, L37-L41 (2003)

** ****8 clusters with accurate  Lx, Tx, Rc, ********, z...**
** ****A significant fraction of the high-z SHARC clusters at z > 0.45**
** ****Goals : **
**   **** ****I-**** L-T relation at high-z **
**	****=> key ingredient in the number counts calculation**
**    ****II-**** ********matter**** from the evolution of cluster population at high-z**
**	****	****	****	****	****	****	****(z > 0.3)**

- Sébastien C. Vauclair, Greenbelt 2004

## XMM-Newton  -Project I : Observations

** ****Z ******** 0.6**
** ****T****x****=5.45 ******** 0.3 keV L****bol****=14.4 10****44**** erg s****-1**** **

**RXJ1120, M. Arnaud et al, 2002**** **

**D. Lumb et al., astroph/0311344**

**XMM-Newton**  -Project I : Observations

- Sébastien C. Vauclair, Greenbelt 2004

## Evolution of L-T confirmed 

**+ **local
****XMM
- * Chandra

-   **Lx/Tx)****z**** = Lx/Tx)****z = 0****(1+z)******** with**** ******** = 0.65 ******** 0.28**
- 	in agreement with Chandra (Vikhlinin et al, 2002),
- 	and ASCA (Sadat et al., 1998; Novicki et al., 2003....)
- and with Lumb et al. after cooling flow corrections  (****** = 0.6 ******** 0.3**)

- Sébastien C. Vauclair, Greenbelt 2004

##  Number counts :

- models predictions VS observations

**=> L****x****-T****x**** relation**

**=> M-T****x**** relation         **

**=> mass function**

**XMM-Newton** -Project II : Cosmological interpretation

- Sébastien C. Vauclair, Greenbelt 2004

## Surveys used: 

**6 different flux limited X-Ray surveys: **
**EMSS, RDCS, B-SHARC, 160 deg****2****, NEP and MACS**
**~****300 clusters with z > 0.3**
**Modelling with **
**a)**** ****high ******** no free parameters **
**b) Concordance model (************=0.7, ********m****=0.3, ********8****~1, ********=0.2****)**
**[models normalized to local counts] **

**MACS : 119 clusters at z>0.3 ****	****	****        **(Ebeling et al.)

- (NEP,       Mullis)

- Sébastien C. Vauclair, Greenbelt 2004

## Local Normalization

**Local Normalization**

- => **Need redshift evolution study to break the degeneracy between ********m**** and ********8**

**TDF**

**Local degeneracy between ********m**** and ********8**

**50-60 ROSAT clusters  **
- Agreement with previous works:
- Markevitch (1998), Blanchard et al. (2000), Pierpaoli al (2001, 2002),
- Ikebe et al (2002), Novicki et al (2002)

- Sébastien C. Vauclair, Greenbelt 2004

## Local Normalization :

**Local Normalization :**
**The X-ray Luminosity Function**

**Observed TDF**
**+**
**Observed L-T**
**=> Observed XLF !**

******=1**

******m=0.3**

- Sébastien C. Vauclair, Greenbelt 2004

## m from TDF evolution

**Using Henri****’s**** sample **
**from EMSS ****(1997)**

**=>**

** ********m****= 0.86**
**Update : ********m****=[0.85-1] depending on M-T**

**Blanchard et al., 2000 **
**Oukbir & Blanchard, 1992**

******m**** from TDF evolution**

**Maximum Likelihood**

**Agreement with:**
**Reichart et al., 1999 **
**Borgani et al., 1999**

- Sébastien C. Vauclair, Greenbelt 2004

## RDCS: 50 deg2

- fx  3. 10-14 erg/s/cm2

- MACS: 22 000 deg2
- fx  10-12 erg/s/cm2

- Sébastien C. Vauclair, Greenbelt 2004

## CDM model with low 8

- =0.65, m=0.35, 8=0.66, =0.2

- Sébastien C. Vauclair, Greenbelt 2004

## Local XLF with

** ************=0.65, ********m****=0.35, ********8****=0.66, ********=0.2**

**BUT...**

- ~4 keV

- Sébastien C. Vauclair, Greenbelt 2004

## 160deg2 with fx > 2.10-13 erg.cm-2.s-1

**S.C.Vauclair et al., A&A 412, L37-L41 (2003)**

- Sébastien C. Vauclair, Greenbelt 2004

## Conclusions:  

** ****L-T**** evolution with redshift**** ****confirmed by XMM**** **
** ****S****trong**** E****volution in the abundance of x-ray clusters appears from all existing surveys in a  fully ****consistent**** way ****	**
** ****I****nsensitive**** ****to systematics (L-T, M-T, mass function...)**
** ****T****his provides a strong argument in favor of a high matter density universe ****within the standard modelling of clusters**
** ****O****ne way out : major revision of standard scaling of ****M-T (z)**** for instance i.e. ****Tx ******** GM/r  **
**=>** **new degeneracy...? (break with SZ counts)**

- Sébastien C. Vauclair, Greenbelt 2004

## Compatible with CMB

***Compatible with CMB***