1. Deep Chandra observation of WARPJ1415.1+3612 at z=1: an evolved cool-core cluster at high-z (and a bonus…) P. Tozzi, M.Nonino (INAF-TS), P. Rosati (ESO), G. Giovannini (INAF-BO) M. Sanchez-Portal (ESAC) Joana S. Santos (ESAC) Galaxy Clusters as Giant Cosmic Laboratories ESAC –Madrid 21-23 May 2012

2. Joana Santos - ESA2 Cool-core clusters at high-z CCs represent the bulk (50-70%) of the local cluster population (e.g. Hudson et al. 2010) - Central surface brightness excess - Central cooling time << t HUBBLE - Temperature drop: T c ~ 1/3 T tot - Strong Fe peak - Low entropy (< 30 kev cm 2 ) Up to z~1.4: moderate evolution (Santos et al. 2008, 2010) Most high-z clusters are mild CCs - SB concentration cSB: SB(r<40 kpc) / SB(r<400 kpc) - cluster samples: RDCS, WARPS, 400SD  Best target: WARPJ1415, z= 1 (90 ksec Chandra ACIS-I)

3. 3 Chandra ACIS I + S 370 ksec 280 ksec C12 PI JSantos HST/ACS ~ 7500 cts 9 bins spec analysis Santos, Tozzi, Rosati, Nonino, Giovannini, 2012 A&A 539,105 WARPJ1415, z=1

4. 4 ACS i775-z850 Surface Brightness: β –model fit and c SB c SB = 0.150 ± 0.007 (dividing line mod / strong CC )

5. 5 ACS i775-z850 T drop: 4.6 – 8.0 keV Fe peak: 3.6 -0.9 +1.5 Z sun 2  detections Si, S, Ni Temperature and Metallicity Leccardi & Molendi 2008 low-z M fe exc =1.8 -0.5 +0.7 x10 9 M sun

6. Joana Santos - ESA6 ACS i775-z850 Entropy & Cooling time profiles

7. Joana Santos - ESA7 CC parameterArchival 90 ksecTotal 370 ksec T drop --4.6 – 8.0 – 5.7 (keV) Z fe,c --3.6 -0.9 +1.5 Z sun c SB 0.144±0.0160.150±0.007 t cool,c 3.4 Gyr0.06±0.01 Gyr K0K0 80 keV.cm 2 9.9±2.0 keV.cm 2 X-ray cool core estimators The importance of deep data for high-z clusters!!

8. Joana Santos - ESA8 ACS i775-z850 Mass profile HE T profile n e profile Total mass Gas mass WL (Jee et al. 2011)

9. Joana Santos - ESA9 ACS i775-z850 Radio VLA (res ~ 2”) Residual Chandra -β model 1’ Nuclear emission: L 1.4GHz = 2.0x10 25 W/Hz + one sided jet/tail feature X-rays + radio interaction 80 kpc Asymmetry in SB: reg. 1 is 25% less luminous than reg. 2 1’ (480 kpc)

10. 10 BCG - OII The BCG Subaru/Suprime BVR HST/ACS i 775 - z 850 EW[OII]=-25 A SFR=2-8 M s /yr

11. Joana Santos - ESA11 Summary I WARPJ1415 is a “classical” cool-core cluster at z=1 With the deepest Chandra data of a high-z cluster (370 ksec) we measure: - temperature drop similar to the ones in local cc clusters - high Fe peak: timescale for the build-up of Fe peak [2.4-3.5] Gyr Feedback in action - radio source in the center + OII emission in the BCG: The X-ray properties of the cool-core in WARPJ1415 are very similar to the ones of low-z cool-cores Ideal high-z cluster to study different components of the cool-core phenomenon (optical, radio)

12. Joana Santos - ESA12 BONUS! Serendipitous discovery of a massive, z~1.5 cluster in the field of WARPJ1415

13. Joana Santos - ESA

14. 14 CXO1415 at z X =1.46 : ICM best Chandra data of a z>1.4 cluster (~660 net counts) T=5.9 keV Fe= 1.3 Z/Z sun Mass=M 200 =5x10 14 M sun

15. Joana Santos - ESA15 Subaru/Suprime BVR

16. Joana Santos - ESA16 red-sequence in place (>10 galaxies) few galaxies with distorted morphologies CXO1415 at z X =1.46: galaxy population

17. Joana Santos - ESA17 CXO1415 at z X =1.46: galaxy population 8 band photometry z phot =1.50 (consistent with z X )

18. Joana Santos - ESA18 To be continued in Tozzi et al. in prep. … CXO1415 at z X =1.46