M. LIMOUSIN & THE SL2S COLLABORATION X-RAY FOLLOW-UP AND DETECTION OF SL2S GROUPS: A NEW ERA OF X-RAY – LENSING COMPARISON FABIO GASTALDELLO (IASF-MILAN, UCI) M. LIMOUSIN & THE SL2S COLLABORATION S. ETTORI, …

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

IMAGE SEPARATION DISTRIBUTION OF SL GALAXY GROUPS – POOR CLUSTERS WITH IMAGE SEPARATION IN THE RANGE 6”-16” HAVE BEEN SCARCELY REPORTED The standard model appears to have withstood every test, the problems at very small scale (LSB rotation curves, number of MW satellites) can be explained by astrophysical processes (Primack 2006). Testing the model on smaller scales, fully into the non-linear regime (δ ›› 1) will further our understanding of structure formation and evolution and refine the fundamental parameters of the cosmological model itself OGURI 2006

IMAGE SEPARATION DISTRIBUTION OF SL NO 6”-15” IMAGE SEPARATION LENSES IN THE CLASS SURVEY (PHILLIPS+01,McKEAN10) The standard model appears to have withstood every test, the problems at very small scale (LSB rotation curves, number of MW satellites) can be explained by astrophysical processes (Primack 2006). Testing the model on smaller scales, fully into the non-linear regime (δ ›› 1) will further our understanding of structure formation and evolution and refine the fundamental parameters of the cosmological model itself OGURI 2006

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 = 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

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

SL2SJ08544-0053 z = 0.351 BIMODAL LUMINOSITY DISTRIBUTION (TWO DISTRINCT SUBGROUPS FROM SPECTROSCOPY, MUNOZ+11, IN PREP.). PERTURBED LENSING CONFIGURATION WHICH REQUIRES EXTERNAL MASS (LIMOUSIN+10) SL RE = 5.5“ ± 0.1”

SL2SJ02140-0532 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

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 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

SL2SJ09013-0158 The standard model appears to have withstood every test, the problems at very small scale (LSB rotation curves, number of MW satellites) can be explained by astrophysical processes (Primack 2006). Testing the model on smaller scales, fully into the non-linear regime (δ ›› 1) will further our understanding of structure formation and evolution and refine the fundamental parameters of the cosmological model itself 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

SL2SJ09013-0158 The standard model appears to have withstood every test, the problems at very small scale (LSB rotation curves, number of MW satellites) can be explained by astrophysical processes (Primack 2006). Testing the model on smaller scales, fully into the non-linear regime (δ ›› 1) will further our understanding of structure formation and evolution and refine the fundamental parameters of the cosmological model itself CLEARLY EXTENDED SOURCE (rc = 150 ± 60 kpc, 34” ± 13”, ß = 0.58 ± 0.12)

SL2SJ08544-0053 ELONGATED X-RAY EMISSION The standard model appears to have withstood every test, the problems at very small scale (LSB rotation curves, number of MW satellites) can be explained by astrophysical processes (Primack 2006). Testing the model on smaller scales, fully into the non-linear regime (δ ›› 1) will further our understanding of structure formation and evolution and refine the fundamental parameters of the cosmological model itself

SL2SJ08544-0053 SEPARATION BETWEEN X-RAY GAS AND GALAXIES The standard model appears to have withstood every test, the problems at very small scale (LSB rotation curves, number of MW satellites) can be explained by astrophysical processes (Primack 2006). Testing the model on smaller scales, fully into the non-linear regime (δ ›› 1) will further our understanding of structure formation and evolution and refine the fundamental parameters of the cosmological model itself SEPARATION BETWEEN X-RAY GAS AND GALAXIES

SL2SJ02140-0535 The standard model appears to have withstood every test, the problems at very small scale (LSB rotation curves, number of MW satellites) can be explained by astrophysical processes (Primack 2006). Testing the model on smaller scales, fully into the non-linear regime (δ ›› 1) will further our understanding of structure formation and evolution and refine the fundamental parameters of the cosmological model itself EVIDENCE FOR A SINGLE HALO: FIT A SINGLE HALO IN SL, NO OPTICAL SUBSTRUCTURE (MUNOZ+11, IN PREP)

CONCLUSIONS 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, SUN+09, HUMPHREY+11).