X-RAY FOLLOW-UP OF STRONG X-RAY FOLLOW-UP OF STRONG LENSING OBJECTS:LENSING OBJECTS:
SL2S GROUPS (AND A1703)SL2S GROUPS (AND A1703)
FABIO GASTALDELLO
(IASF-MILAN, UCI)
M. LIMOUSIN & THE SL2S COLLABORATION
OUTLINEOUTLINE
• 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 IMAGE SEPARATION DISTRIBUTION OF SLDISTRIBUTION OF SL
OGURI 2006
GALAXY GROUPS – POOR CLUSTERS WITH
IMAGE SEPARATION IN THE RANGE 6”-16”
HAVE BEEN SCARCELY REPORTED
IMAGE SEPARATION IMAGE SEPARATION DISTRIBUTION OF SLDISTRIBUTION OF SL
OGURI 2006
NO 6”-15” IMAGE SEPARATION
LENSES IN THE CLASS SURVEY (PHILLIPS+01,
McKEAN10)
SL2S GROUPSSL2S 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 GROUPSSL2S GROUPS
X-RAY FOLLOW-UPX-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
z = 0.30 (PHOT)
STRAIGHT ARC BETWEEN THE TWO GALAXIES
SL RE = 6.8“
SL2SJ09013-0158SL2SJ09013-0158
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
SL2SJ09013-0158SL2SJ09013-0158
CLEARLY EXTENDED SOURCE (rc = 150 ± 60 kpc, 34” ± 13”, ß = 0.58 ± 0.12)
SL2SJ22214-0053
z = 0.334
STRAIGHT ARC BETWEEN THE TWO GALAXIES
SL RE = 6.83±0.15“
SL2SJ22214-0053SL2SJ22214-0053
JUST A POINT SOURCE DETECTED, HOWEVER VERY SHALLOW XMM EXPOSURE (5 KS)
SL2SJ09413-1100
z = 0.385
EXTENDED STELLAR HALO FOR CENTRAL GALAXY
SL RE = 7.50±0.81“
SL2SJ09413-1100SL2SJ09413-1100
RATHER REGULAR X-RAY EMISSION
TEMPERATURE OF KT=3.6±0.4
SL2SJ09413-1100SL2SJ09413-1100
CLEARLY EXTENDED SOURCE
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
SL2SJ02140-0535SL2SJ02140-0535
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
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”
SL2SJ08544-0053SL2SJ08544-0053
ELONGATED X-RAY EMISSION
TEMPERATURE OF KT=2.7±0.4
SL2SJ08544-0053SL2SJ08544-0053
CLEARLY EXTENDED SOURCE (rc = 128 ± 56 kpc, 26” ± 11”, ß = 0.52 ± 0.07)
SL2SJ08544-0053:SL2SJ08544-0053:THE BULLET GROUPTHE BULLET GROUP
SEPARATION BETWEEN X-RAY GAS AND GALAXIES
THE BULLET GROUPTHE BULLET GROUP
SEPARATION BETWEEN THE X-RAY PEAK AND THE GALAXY ASSOCIATED WITH THE LENS OF 22” (109 Kpc)
WHY LOOKING FOR BULLETS ?WHY LOOKING FOR BULLETS ?
Galaxies (5%)Galaxies (5%)
Intra-cluster medium (ICM)Intra-cluster medium (ICM)
Thermal plasmaThermal plasma
X-rays (10-30%)X-rays (10-30%)
Dark MatterDark Matter
Gravitational potentialGravitational potential
1E 0657-156 THE BULLET CLUSTER1E 0657-156 THE BULLET CLUSTER
MARKEVITCH+04
CONSTRAINTS ON DM SELF-CONSTRAINTS ON DM SELF-INTERACTION CROSS SECTIONINTERACTION CROSS SECTION
RANDALL+08
BABY BULLET (MACS J0025)BABY BULLET (MACS J0025)
BRADAČ+08
SHAN+10
SL2S J08544
SL2S J08544
ABELL 1703ABELL 1703
LIMOUSIN+08RICHARD+09
ABELL 1703ABELL 1703
RICHARD+09
UNIMODAL REGULAR CLUSTER
ABELL 1703ABELL 1703
ABELL 1703ABELL 1703
ABELL 1703ABELL 1703
TEMPERATURE OF KT=7.9±1.2 keV
SUMMARYSUMMARY
• 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
