The XMM Large Scale The XMM Large Scale Structure (XMM-LSS) Survey: Structure (XMM-LSS) Survey: X-ray X-ray analysis analysis and and first first results results Andy Read Andy Read University University of of Leicester Leicester For the XMM-LSS consortium For the XMM-LSS consortium EPIC Consortium Meeting, Palermo, October 2003 EPIC Consortium Meeting, Palermo, October 2003
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The XMM Large Scale Structure (XMM-LSS) Survey: X-ray analysis and first results Andy Read University of Leicester University of Leicester For the XMM-LSS.
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The XMM Large Scale Structure The XMM Large Scale Structure (XMM-LSS) Survey:(XMM-LSS) Survey:
For the XMM-LSS consortiumFor the XMM-LSS consortium
EPIC Consortium Meeting, Palermo, October 2003EPIC Consortium Meeting, Palermo, October 2003
EPIC Consortium Meeting EPIC Consortium Meeting Palermo 14-16 Oct 2003Palermo 14-16 Oct 2003
Andy Read, University of LeicesterAndy Read, University of LeicesterFor the XMM-LSS consortiumFor the XMM-LSS consortium
A EuropeA Europe/Chile/Chile Consortium Consortium
Birmingham Birmingham BristolBristol CopenhagenCopenhagen DublinDublin ESO/ SantiagoESO/ Santiago LeidenLeiden LiègeLiège
Marseille (LAM)Marseille (LAM) Milano (AOB)Milano (AOB) Milano (IFCTR)Milano (IFCTR) Munich (MPA)Munich (MPA) Paris (IAP)Paris (IAP) Santiago (Uni. Cato.)Santiago (Uni. Cato.)
PI : Saclay, France
EPIC Consortium Meeting EPIC Consortium Meeting Palermo 14-16 Oct 2003Palermo 14-16 Oct 2003
Andy Read, University of LeicesterAndy Read, University of LeicesterFor the XMM-LSS consortiumFor the XMM-LSS consortium
XMM sensitivityXMM sensitivity
12.5Å 1.25Å
EPIC Consortium Meeting EPIC Consortium Meeting Palermo 14-16 Oct 2003Palermo 14-16 Oct 2003
Andy Read, University of LeicesterAndy Read, University of LeicesterFor the XMM-LSS consortiumFor the XMM-LSS consortium
The XMM-LSS SurveyThe XMM-LSS Survey
- Goal: determine the cluster correlation function in two redshift bins 0 < z < 0.5, 0.5 < z < 1, each bin containing 450 clusters
- Fixes the XMM-LSS survey characteristics: 8x8 sq.deg. area covered by 10 ksec XMM pointings
- Sensitivity: 5e-15 ergs/s/cm² in [0.5-2 keV] band
- XMM’s unrivalled sensitivity, large FOV and good PSFopens a new area for the study of the cluster LSS
- Able to Map the evolution of the LSS of the universe out to z~1, with both the galaxy cluster and the QSO
populations for the first time
EPIC Consortium Meeting EPIC Consortium Meeting Palermo 14-16 Oct 2003Palermo 14-16 Oct 2003
Andy Read, University of LeicesterAndy Read, University of LeicesterFor the XMM-LSS consortiumFor the XMM-LSS consortium
Expected numbers of objectsExpected numbers of objects
EPIC Consortium Meeting EPIC Consortium Meeting Palermo 14-16 Oct 2003Palermo 14-16 Oct 2003
Andy Read, University of LeicesterAndy Read, University of LeicesterFor the XMM-LSS consortiumFor the XMM-LSS consortium
XMM Subaru Deep Survey
VIRMOS VVDS wide
XMDS & VIRMOS VVDS deep
SIRTF Legacy : SWIRE
NOAO Deep Survey
Galex
XMM-LSS
Survey Survey LocationLocation
HI map NH~1.4-3.5 e20
EPIC Consortium Meeting EPIC Consortium Meeting Palermo 14-16 Oct 2003Palermo 14-16 Oct 2003
Andy Read, University of LeicesterAndy Read, University of LeicesterFor the XMM-LSS consortiumFor the XMM-LSS consortium
The First Data: 15 GO PointingsThe First Data: 15 GO Pointings 15 Pointings (MOS1, MOS2 & pn, all with ~10 ksec)15 Pointings (MOS1, MOS2 & pn, all with ~10 ksec) Standard SAS (emchain and epchain) processingStandard SAS (emchain and epchain) processing Flare-cleaned to common level of low backgroundFlare-cleaned to common level of low background Bad pixel analysis and removalBad pixel analysis and removal RGB mosaic constructed (0.3-1, 1-2.5, 2.5-10 keV)RGB mosaic constructed (0.3-1, 1-2.5, 2.5-10 keV) Rigorous background subtraction, to account for Rigorous background subtraction, to account for
-Subtract to calculate ‘soft excess’ at large-R for particular energy
- Start `soft excess’ loop over several small energy bands
- End Loop over energies to accumulate total energy, full field `soft excess’ image
-Add `soft excess’ to Scaled BG image to create double background
-Add double background to scaled particles image to create total background
EPIC Consortium Meeting EPIC Consortium Meeting Palermo 14-16 Oct 2003Palermo 14-16 Oct 2003
Andy Read, University of LeicesterAndy Read, University of LeicesterFor the XMM-LSS consortiumFor the XMM-LSS consortium
The First Data: Flare-cleaned exposure The First Data: Flare-cleaned exposure
EPIC Consortium Meeting EPIC Consortium Meeting Palermo 14-16 Oct 2003Palermo 14-16 Oct 2003
Andy Read, University of LeicesterAndy Read, University of LeicesterFor the XMM-LSS consortiumFor the XMM-LSS consortium
Part of the XMM-LSS mosaic : 15 pointings (~1.6 sq.deg.) Part of the XMM-LSS mosaic : 15 pointings (~1.6 sq.deg.)
Red[0.3-1]keV Green[1-2.5]keV Blue[2.5-10]keV
Andy ReadAndy Read
Circles:RASS
EPIC Consortium Meeting EPIC Consortium Meeting Palermo 14-16 Oct 2003Palermo 14-16 Oct 2003
Andy Read, University of LeicesterAndy Read, University of LeicesterFor the XMM-LSS consortiumFor the XMM-LSS consortium
‘‘Big C’ – XMMUJ022540-031111Big C’ – XMMUJ022540-031111Hardness map of centre
-Hotter at interface (kT~7.6keV)
All-EPIC, BG-sub, exp-corr. contours on CFHT I band imagez~0.29, kT~6.2 keV, Lx~3e44 erg/s
EPIC Consortium Meeting EPIC Consortium Meeting Palermo 14-16 Oct 2003Palermo 14-16 Oct 2003
Andy Read, University of LeicesterAndy Read, University of LeicesterFor the XMM-LSS consortiumFor the XMM-LSS consortium
Detection Algorithm OverviewDetection Algorithm Overview- Standard SAS processing - emchain & epchain + flare removal- Wavelet filtering of images (M1-M2-PN) - in counts (preserving Poisson stats) - computing threshold by histogram auto-convolution- Exposure correction on a per instrument basis- Addition of exposure-corrected images- 1st detection step: Sextractor
- on co-added images - with low detection threshold, to avoid missing faint sources - with parameters adjusted for X-ray filtered images- Max. Likelihood fit step: EMLdetect (with extension fit & CAL psf) - source input list from Sextractor - X/Y & Ext. tied for 3 instruments, normalization free - ML min = 8.5 - Final X-ray catalogue: - Mix of Sextractor/EMLdetect results
Sergio Dos Santos, Saclay
EPIC Consortium Meeting EPIC Consortium Meeting Palermo 14-16 Oct 2003Palermo 14-16 Oct 2003
Andy Read, University of LeicesterAndy Read, University of LeicesterFor the XMM-LSS consortiumFor the XMM-LSS consortium
-Results encouraging: - Most, if not all clusters (T>4keV) up to z~1 can be detected using 10 ksec XMM pointings - Richest clusters should be detected at z<2 (if they exist!) - Very small rate of spurious detections (<1 per pointing), due to 2-stage process
Sergio Dos Santos, Saclay
EPIC Consortium Meeting EPIC Consortium Meeting Palermo 14-16 Oct 2003Palermo 14-16 Oct 2003
Andy Read, University of LeicesterAndy Read, University of LeicesterFor the XMM-LSS consortiumFor the XMM-LSS consortium
• 55 Candidate extended sources over ~ 3.5 sq.deg. i.e. as expected ~15 extended sources per sq.deg.
• 10 ksec XMM + 2h VLT allow T (±1 keV) measurement and velocity dispersion at z~0.8
• Intermediate mass systems are being uncovered by XMM
• First results described in four papers• Pierre et al, 2003, astro-ph/0305191• Valtchanov et al, 2003, astro-ph/0305192• Willis et al, 2003, in prep• Andreon et al, in prep
EPIC Consortium Meeting EPIC Consortium Meeting Palermo 14-16 Oct 2003Palermo 14-16 Oct 2003
Andy Read, University of LeicesterAndy Read, University of LeicesterFor the XMM-LSS consortiumFor the XMM-LSS consortium
photo-zphoto-z
CFHT I-band image
EPIC contours
EPIC Consortium Meeting EPIC Consortium Meeting Palermo 14-16 Oct 2003Palermo 14-16 Oct 2003
Andy Read, University of LeicesterAndy Read, University of LeicesterFor the XMM-LSS consortiumFor the XMM-LSS consortium
Predicted z (photometric): Predicted z (photometric):
MeasuredMeasuredz = 0.61 !z = 0.61 !
Sources ~1’ from centre
All sources
EPIC Consortium Meeting EPIC Consortium Meeting Palermo 14-16 Oct 2003Palermo 14-16 Oct 2003
Andy Read, University of LeicesterAndy Read, University of LeicesterFor the XMM-LSS consortiumFor the XMM-LSS consortium
CFH12k I-bandCFH12k I-band
EPIC contours
Nearby group
EPIC Consortium Meeting EPIC Consortium Meeting Palermo 14-16 Oct 2003Palermo 14-16 Oct 2003
Andy Read, University of LeicesterAndy Read, University of LeicesterFor the XMM-LSS consortiumFor the XMM-LSS consortium
Cluster without X-ray counterpart
(‘red sequence’ detection, z~0.3-0.4)
Image: zImage: z´́-band CTIO-band CTIO
EPIC contours
EPIC Consortium Meeting EPIC Consortium Meeting Palermo 14-16 Oct 2003Palermo 14-16 Oct 2003
Andy Read, University of LeicesterAndy Read, University of LeicesterFor the XMM-LSS consortiumFor the XMM-LSS consortium
A structure at z~1
EPIC Consortium Meeting EPIC Consortium Meeting Palermo 14-16 Oct 2003Palermo 14-16 Oct 2003
Andy Read, University of LeicesterAndy Read, University of LeicesterFor the XMM-LSS consortiumFor the XMM-LSS consortium
006 012
EPIC contours on CFHT images
EPIC Consortium Meeting EPIC Consortium Meeting Palermo 14-16 Oct 2003Palermo 14-16 Oct 2003
Andy Read, University of LeicesterAndy Read, University of LeicesterFor the XMM-LSS consortiumFor the XMM-LSS consortium
2-D fitting of X-ray emission2-D fitting of X-ray emission• Simultaneous fitting of MOS1, MOS2 and pn images
- Images and exposure maps required• PSF images required (created via SAS-calview)• Masks can be used to ignore e.g. nearby point sources• Source (src) and background (BG) boxes are chosen
2-D fitting: β-model (using CIAO-sherpa)
• 3 separate models (with tied parameters) for M1, M2, pn• Constant BG level(s) fit to BG emission• src+BG model fit to source emission (src = β-model)• Core radius Ro, slope β, ellipticity ε tied between 3
instruments, normalization free
EPIC Consortium Meeting EPIC Consortium Meeting Palermo 14-16 Oct 2003Palermo 14-16 Oct 2003
Andy Read, University of LeicesterAndy Read, University of LeicesterFor the XMM-LSS consortiumFor the XMM-LSS consortium
2-D model contours overlayed on EPIC X-ray emission