XRAY FOLLOWUP OF STRONG LENSING OBJECTS SL 2
X-RAY FOLLOW-UP OF STRONG LENSING OBJECTS: SL 2 S GROUPS (AND A 1703) FABIO GASTALDELLO (IASF-MILAN, UCI) M. LIMOUSIN & THE SL 2 S COLLABORATION
OUTLINE • INTRODUCTION TO GROUPS IN SL 2 S • XMM SNAPSHOT PROGRAM FOR X-RAY FOLLOW-UP OF SL 2 S GROUPS: DETECTIONS AND PRELIMINARY INITIAL INFORMATION • THE BULLET GROUP • A 1703
IMAGE SEPARATION DISTRIBUTION OF SL GALAXY GROUPS – POOR CLUSTERS WITH IMAGE SEPARATION IN THE RANGE 6”-16” HAVE BEEN SCARCELY REPORTED OGURI 2006
IMAGE SEPARATION DISTRIBUTION OF SL NO 6”-15” IMAGE SEPARATION LENSES IN THE CLASS SURVEY (PHILLIPS+01, Mc. KEAN 10) OGURI 2006
SL 2 S GROUPS • INITIAL SAMPLE OF 13 OBJECTS, A SUBSAMPLE OF THE SL 2 S BASED ON MULTI-COLOUR CFHTLS, IDEAL TO DETECT SL FEATURES AND FOLLOW-UP HUBBLE IMAGING (z = 0. 3 -0. 8) • LUMINOSITY MAPS BASED ON LIGHT DISTRIBUTION OF ELLIPTICALS HAVE FOR SOME OBJECTS COMPLICATED SHAPE. WEAK LENSING SIGNAL DETECTED FOR 6 GROUPS
SL 2 S 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 2108+213 WITH RE = 2. 5“) • XMM SNAPSHOTS OF 5 -10 ks TO SECURE FLUXES FOR DEEPER CHANDRA OBSERVATION. ENOUGH PHOTONS FOR MORPHOLOGY AND POSSIBLY TEMPERATURE
SL 2 SJ 09013 -0158 z = 0. 30 (PHOT) STRAIGHT ARC BETWEEN THE TWO GALAXIES SL RE = 6. 8“
SL 2 SJ 09013 -0158 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 k. T = 3. 4 ± 0. 6 ke. V
SL 2 SJ 09013 -0158 CLEARLY EXTENDED SOURCE (rc = 150 ± 60 kpc, 34” ± 13”, ß = 0. 58 ± 0. 12)
SL 2 SJ 22214 -0053 z = 0. 334 STRAIGHT ARC BETWEEN THE TWO GALAXIES SL RE = 6. 83± 0. 15“
SL 2 SJ 22214 -0053 JUST A POINT SOURCE DETECTED, HOWEVER VERY SHALLOW XMM EXPOSURE (5 KS)
SL 2 SJ 09413 -1100 z = 0. 385 EXTENDED STELLAR HALO FOR CENTRAL GALAXY SL RE = 7. 50± 0. 81“
SL 2 SJ 09413 -1100 RATHER REGULAR XRAY EMISSION TEMPERATURE OF KT=3. 6± 0. 4
SL 2 SJ 09413 -1100 CLEARLY EXTENDED SOURCE
SL 2 SJ 02140 -0532 z = 0. 444 MULTIPLE IMAGES (SOUTHERN ARC MAYBE NOT ASSOCIATED) SL RE = 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 1014 REPRODUCES WELL ALL THE CONSTRAINTS
SL 2 SJ 02140 -0535 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
SL 2 SJ 08544 -0053 z = 0. 351 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 RE = 5. 5“ ± 0. 1”
SL 2 SJ 08544 -0053 ELONGATED X-RAY EMISSION TEMPERATURE OF KT=2. 7± 0. 4
SL 2 SJ 08544 -0053 CLEARLY EXTENDED SOURCE (rc = 128 ± 56 kpc, 26” ± 11”, ß = 0. 52 ± 0. 07)
SL 2 SJ 08544 -0053: 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 ?
Intra-cluster medium (ICM) Thermal plasma X-rays (10 -30%) Galaxies (5%) Dark Matter Gravitational potential 1 E 0657 -156 THE BULLET CLUSTER MARKEVITCH+04
CONSTRAINTS ON DM SELFINTERACTION CROSS SECTION RANDALL+08
BABY BULLET (MACS J 0025) BRADAČ+08
SL 2 S J 08544 SHAN+10
ABELL 1703 LIMOUSIN+08 RICHARD+09
ABELL 1703 RICHARD+09 UNIMODAL REGULAR CLUSTER
ABELL 1703
ABELL 1703
ABELL 1703 TEMPERATURE OF KT=7. 9± 1. 2 ke. V
SUMMARY • SL 2 S 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) • A 1703 IS REALLY AN EXCEPTIONAL TARGET AND WE HOPE TO GET BETTER X-RAY DATA WITH CHANDRA
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