1. 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, …

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

3. 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

4. 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

5. 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

6. SL2S GROUPS

7. STRAIGHT ARC BETWEEN THE TWO GALAXIES
SL2SJ
z = 0.30 (PHOT)
STRAIGHT ARC BETWEEN THE TWO GALAXIES
SL RE = 6.8“

8. SL2SJ
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”

9. SL2SJ
z = 0.444
MULTIPLE IMAGES (SOUTHERN ARC MAYBE NOT ASSOCIATED)
SL RE = 7.3“ ± 0.5”

10. 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

11. 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 RE = 2.5“)
XMM SNAPSHOTS OF 5-10 ks TO SECURE FLUXES FOR DEEPER CHANDRA OBSERVATION. ENOUGH PHOTONS FOR MORPHOLOGY AND POSSIBLY TEMPERATURE

12. SL2SJ
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

13. SL2SJ
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)

14. 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

15. 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

16. SL2SJ
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)

17. 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).