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X-RAY FOLLOW-UP OF STRONG LENSING OBJECTS: SL2S GROUPS (AND A1703)

X-RAY FOLLOW-UP OF STRONG LENSING OBJECTS: SL2S GROUPS (AND A1703). FABIO GASTALDELLO (IASF-MILAN, UCI) M. LIMOUSIN & THE SL2S COLLABORATION. INTRODUCTION TO GROUPS IN SL2S XMM SNAPSHOT PROGRAM FOR X-RAY FOLLOW-UP OF SL2S GROUPS: DETECTIONS AND PRELIMINARY INITIAL INFORMATION

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X-RAY FOLLOW-UP OF STRONG LENSING OBJECTS: SL2S GROUPS (AND A1703)

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

  2. 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 OUTLINE

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

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

  5. 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 = 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 SL2S GROUPS

  6. SL2S GROUPS

  7. 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 B2108+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 X-RAY FOLLOW-UP

  8. SL2SJ09013-0158 z = 0.30 (PHOT) STRAIGHT ARC BETWEEN THE TWO GALAXIES SL RE = 6.8“

  9. SL2SJ09013-0158 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 kT = 3.4 ± 0.6 keV

  10. SL2SJ09013-0158 CLEARLY EXTENDED SOURCE (rc = 150 ± 60 kpc, 34” ± 13”, ß = 0.58 ± 0.12)

  11. SL2SJ22214-0053 z = 0.334 STRAIGHT ARC BETWEEN THE TWO GALAXIES SL RE = 6.83±0.15“

  12. SL2SJ22214-0053 JUST A POINT SOURCE DETECTED, HOWEVER VERY SHALLOW XMM EXPOSURE (5 KS)

  13. SL2SJ09413-1100 z = 0.385 EXTENDED STELLAR HALO FOR CENTRAL GALAXY SL RE = 7.50±0.81“

  14. RATHER REGULAR X-RAY EMISSION TEMPERATURE OF KT=3.6±0.4 SL2SJ09413-1100

  15. SL2SJ09413-1100 CLEARLY EXTENDED SOURCE

  16. SL2SJ02140-0532 z = 0.444 MULTIPLE IMAGES (SOUTHERN ARC MAYBE NOT ASSOCIATED) SL RE = 7.3“ ± 0.5”

  17. 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

  18. SL2SJ02140-0535 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

  19. SL2SJ08544-0053 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”

  20. ELONGATED X-RAY EMISSION TEMPERATURE OF KT=2.7±0.4 SL2SJ08544-0053

  21. SL2SJ08544-0053 CLEARLY EXTENDED SOURCE (rc = 128 ± 56 kpc, 26” ± 11”, ß = 0.52 ± 0.07)

  22. SL2SJ08544-0053:THE BULLET GROUP SEPARATION BETWEEN X-RAY GAS AND GALAXIES

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

  24. WHY LOOKING FOR BULLETS ?

  25. Intra-cluster medium (ICM) Thermal plasma X-rays (10-30%) Galaxies (5%) Dark Matter Gravitational potential 1E 0657-156 THE BULLET CLUSTER MARKEVITCH+04

  26. CONSTRAINTS ON DM SELF-INTERACTION CROSS SECTION RANDALL+08

  27. BABY BULLET (MACS J0025) BRADAČ+08

  28. SL2S J08544 SL2S J08544 SHAN+10

  29. ABELL 1703 LIMOUSIN+08 RICHARD+09

  30. ABELL 1703 RICHARD+09 UNIMODAL REGULAR CLUSTER

  31. ABELL 1703

  32. ABELL 1703

  33. ABELL 1703 TEMPERATURE OF KT=7.9±1.2 keV

  34. 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 SUMMARY

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