X-RAY FOLLOW-UP OF STRONG LENSING OBJECTS: SL2S GROUPS (AND A1703) FABIO GASTALDELLO (IASF-MILAN, UCI) M. LIMOUSIN & THE SL2S COLLABORATION

OUTLINE INTRODUCTION TO GROUPS IN SL2S XMM SNAPSHOT PROGRAM FOR X-RAY FOLLOW-UP OF SL2S GROUPS: DETECTIONS AND PRELIMINARY INITIAL INFORMATION THE BULLET GROUP A1703

IMAGE SEPARATION DISTRIBUTION OF SL OGURI 2006 GALAXY GROUPS – POOR CLUSTERS WITH IMAGE SEPARATION IN THE RANGE 6”-16” HAVE BEEN SCARCELY REPORTED

IMAGE SEPARATION DISTRIBUTION OF SL OGURI 2006 NO 6”-15” IMAGE SEPARATION LENSES IN THE CLASS SURVEY (PHILLIPS+01, McKEAN10)

SL2S GROUPS INITIAL SAMPLE OF 13 OBJECTS, A SUBSAMPLE OF THE SL2S BASED ON MULTI-COLOUR CFHTLS, IDEAL TO DETECT SL FEATURES AND FOLLOW-UP HUBBLE IMAGING (z = ) LUMINOSITY MAPS BASED ON LIGHT DISTRIBUTION OF ELLIPTICALS HAVE FOR SOME OBJECTS COMPLICATED SHAPE. WEAK LENSING SIGNAL DETECTED FOR 6 GROUPS

SL2S GROUPS

X-RAY FOLLOW-UP CLEARLY DIFFICULT BECAUSE WE ARE TARGETING LOW FLUX OBJECTS, HOWEVER MORE MASSIVE OBJECTS THAN PREVIOUS STUDIES (E.G., LARGEST IMAGE SEPARATION IN FASSNACHT+08 IS CLASS B WITH R E = 2.5“) XMM SNAPSHOTS OF 5-10 ks TO SECURE FLUXES FOR DEEPER CHANDRA OBSERVATION. ENOUGH PHOTONS FOR MORPHOLOGY AND POSSIBLY TEMPERATURE

SL2SJ z = 0.30 (PHOT) STRAIGHT ARC BETWEEN THE TWO GALAXIES SL R E = 6.8“

SL2SJ TWO GROUPS DETECTED, THE N-ONE CONSISTENT WITH THE ELONGATION IN LUMINOSITY CONTOURS. THE S-ONE ASSOCIATED WITH THE LENS HAS A TEMPERATURE CONSISTENT WITH A POOR CLUSTER kT = 3.4 ± 0.6 keV

SL2SJ CLEARLY EXTENDED SOURCE (r c = 150 ± 60 kpc, 34” ± 13”, ß = 0.58 ± 0.12)

SL2SJ z = STRAIGHT ARC BETWEEN THE TWO GALAXIES SL R E = 6.83±0.15“

SL2SJ JUST A POINT SOURCE DETECTED, HOWEVER VERY SHALLOW XMM EXPOSURE (5 KS)

SL2SJ z = EXTENDED STELLAR HALO FOR CENTRAL GALAXY SL R E = 7.50±0.81“

SL2SJ RATHER REGULAR X-RAY EMISSION TEMPERATURE OF KT=3.6±0.4

SL2SJ CLEARLY EXTENDED SOURCE

SL2SJ z = MULTIPLE IMAGES (SOUTHERN ARC MAYBE NOT ASSOCIATED) SL R E = 7.3“ ± 0.5”

SL+WL+GALAXY DYNAMICS (VERDUGO+11) UNIMODAL NFW W/ c_200 = 6.0±0.6 AND M_200 ≈ 1.0 x REPRODUCES WELL ALL THE CONSTRAINTS

SL2SJ EVIDENCE FOR A SINGLE HALO: FIT A SINGLE HALO IN SL, NO OPTICAL SUBSTRUCTURE (MUNOZ+11, IN PREP) X-RAY EXTENDED BUT NOT ENOUGH COUNTS FOR SPECTRAL INFORMATION

SL2SJ z = BIMODAL LUMINOSITY DISTRIBUTION (TWO DISTRINCT SUBGROUPS FROM SPECTROSCOPY WITH A VELOCITY DIFFERENCE OF 1200 km/s, MUNOZ+12, IN PREP.). PERTURBED LENSING CONFIGURATION WHICH REQUIRES EXTERNAL MASS (LIMOUSIN+10) SL R E = 5.5“ ± 0.1”

SL2SJ ELONGATED X-RAY EMISSION TEMPERATURE OF KT=2.7±0.4

SL2SJ CLEARLY EXTENDED SOURCE (r c = 128 ± 56 kpc, 26” ± 11”, ß = 0.52 ± 0.07)

SL2SJ : THE BULLET GROUP SEPARATION BETWEEN X-RAY GAS AND GALAXIES

THE BULLET GROUP SEPARATION BETWEEN THE X-RAY PEAK AND THE GALAXY ASSOCIATED WITH THE LENS OF 22” (109 Kpc)

WHY LOOKING FOR BULLETS ?

Galaxies (5%) Intra-cluster medium (ICM) Thermal plasma X-rays (10-30%) Dark Matter Gravitational potential 1E THE BULLET CLUSTER MARKEVITCH+04

CONSTRAINTS ON DM SELF- INTERACTION CROSS SECTION RANDALL+08

BABY BULLET (MACS J0025) BRADAČ+08

SHAN+10 SL2S J08544

ABELL 1703 LIMOUSIN+08 RICHARD+09

ABELL 1703 RICHARD+09 UNIMODAL REGULAR CLUSTER

ABELL 1703

TEMPERATURE OF KT=7.9±1.2 keV

SUMMARY SL2S IS FINALLY PROVIDING A GOOD SAMPLE OF LENSING GROUPS/POOR CLUSTERS, OPENING A NEW WINDOW OF THE MASS SPECTRUM FOR LENSING/X-RAY COMPARISON STAY TUNED FOR MORE TARGETS AND MORE DATA: THE GOAL IS TO OBTAIN CHANDRA OBSERVATIONS TO ALLOW X-RAY HE MASS RECONSTRUCTION, AS DONE FOR LOCAL (z < 0.1) GROUPS (GASTALDELLO+07) THE BULLET GROUP IS THE FIRST GROUP MASS-SIZE EXAMPLE OF A BULLET AND A GOOOD PROMISE FOR A STATISTICAL DETECTION OF BULLETICITY (Massey+11) A1703 IS REALLY AN EXCEPTIONAL TARGET AND WE HOPE TO GET BETTER X-RAY DATA WITH CHANDRA

SL2SJ z = RADIO SOURCE COINCIDENT WITH CENTRAL GALAXY SL R E = 6.0“ ± 0.3”

SL2SJ z = VERY EXOTIC SL CONFIGURATION, DIFFICULT TO KNOW HOW MANY MULTIPLE IMAGES ARE OBSERVED SL R E = 8“

IMAGE SEPARATION OF SL Fraction of lensing by satellites peaks at 1” and decreases rapidly with increasing image separation 14% and 4 percent of lenses in groups and clusters, half of them expected to be by satellites Separation enhanced significantly by surrounding haloes OGURI 2006