Marguerite PIERRE CEA Saclay ARCHES scientific workshop Paris - - PowerPoint PPT Presentation

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Marguerite PIERRE CEA Saclay ARCHES scientific workshop Paris - - PowerPoint PPT Presentation

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Marguerite PIERRE CEA Saclay ARCHES scientific workshop Paris December, 2015 XXL in short: 1) FIND ~ 500 X-ray clusters in 50 deg 2 2) DO COSMOLOGY Background image : CFHT i X-ray clusters ~ 5% Blue contours : XMM XLSSC 001 @ z=0.61

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Marguerite PIERRE CEA Saclay

ARCHES scientific workshop Paris December, 2015

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XXL in short:

1) FIND ~ 500 X-ray clusters in 50 deg2 2) DO COSMOLOGY

X-ray clusters ~ 5% Background image : CFHT i Blue contours : XMM

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XLSSC 001 @ z=0.61

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Working with these data : difficult ! : misleading (Poisson) : ambitious … but feasible and exciting !

XLSSC 008 @ z=0.30

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ž XMM VLP (2010) following XMM-LSS (2000-2010) :

  • 2 x 25 deg2 area
  • Total time > 6Ms
  • Largest XMM programme to date

ž An international consortium gathering ~ 100

scientists.

ž The 542 XMM observations were completed in

2013

ž First series of papers submitted to A&A in July

2015

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  • 1. Scientific motivations
  • 2. The XMM observations
  • 3. The follow-up programme
  • 4. The cluster catalogue
  • 5. Overview of the first results : 13 papers
  • 6. A comprehensive associated simulation
  • programme. Future
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ž Obtain a sample of ~ 500 clusters of

galaxies out to z~1

ž Well-defined selection effects ž Self-consistent cluster mass

measurements

ž Cluster counts AND cluster LSS

è Standalone cosmological constraints

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XXL Ref. Dark Energy Task Force *clusters* Pierre et al 2011

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LSS Surveys Roadmap

!

  • I. Shipsey

Stage IV Stage III

2014 2016 2018 2020 2022 2024 2026 2028 2030 2032

BOSS Dark Energy Survey HETDEX Hyper-Suprime D.E. Spectro. Instr. EUCLID Large Synoptic Survey Telescope WFIRST

  • AFTA

eBOSS Prime Focus Spectro.

spectroscopy imaging

High degree of complementary between missions

Image: Ian Shipsey XMM-XXL

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ž Cluster physics

~ 500 clusters

  • Scaling relations
  • Baryon budget
  • Galaxies in clusters

ž AGN physics

~ 25,000 AGNs

  • AGN evolution
  • AGNs in LSS
  • Search for exotic and very distant objects
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XXL standard processing 1: F. Pacaud Processing for the diffuse background: S. Snowden

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EXPO map

XXL-N 25 deg2

In CFHTLS-W1 2h23 -5d00 (extension of the XMM-LSS field)

Moon

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XXL-N

1 deg BKG map

XXL north

1 deg BKG map 13 pointings (+2 thanks to mosaic mode)

Observed Good Usable Lost

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EXPO map

XXL-S 25 deg2

23h30 -55d00 within the SPT 100 deg2 Deep Field

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XXL south

7 pointings (+1 with mosaic) 1 deg BKG map

Observed Good Usable Lost

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z = 0.053 z = 1.22

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I 3.6 µm 4.5 µm

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~ surface brightness limited

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Flux (cts/s) Core radius (arsec)

Not a flux limit ! Class 1 sample

Pacaud et al 2006

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ž Deep multi-band imaging

  • CFHTLS
  • DECam (Lidman et al)
  • HSC

ž Extensive spectroscopic follow-up

  • ESO LP – NTT & VLT (Adami et al)
  • WHT (Poggianti et al)
  • AAOmega (Lidman et al)
  • Associated with GAMA and VIPERS
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ž Full IR coverage

  • Spitzer
  • WIRCAM @ CFHT
  • VISTA

ž On-going radio surveys

  • GMRT (Raychaudury et al)
  • VLA, ATCA (Smolcic et al)
  • SPT, ACT

ž Existing public surveys

  • SDSS, Galex, . . .
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Selction: C1+C2 flux in r=1’ (>3 10-14)

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Brightest 100 cluster sample

Self-consistent analyses WMAP9 cosmology assumed

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Slope 2.66 +/- 0.15 E(z)1.46+/-0.80 !CAVEAT! Compatible with self-similar evolution

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38 XXL clusters with CFHT-Lens

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38 XXL clusters with CFHT-Lens Self-similarity 40%

  • ffset ?
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No evolution for F(Lx) !

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OWLS models

}

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Using

lensing masses

OWLS models

}

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. XXL 100 sample

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XMM photon map Optical galaxy density contours Image size 20’x13’

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  • First XXL results
  • 13 papers
  • General presentation
  • The 100 brightest clusters + science
  • A few interesting clusters
  • The 1000 brightest AGNs
  • VLA and ATCA catalogues
  • ESA-ESO-A&A press release on December 15th
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  • General catalogues (Milano)
  • X-ray
  • Optical
  • Radio

http://cosmosdb.iasf-milano.inaf.it/XXL/

  • Dedicated cluster database (Lyon)
  • X-ray parameters
  • X-ray, optical, IR images
  • Detail of the redshift measurements
  • Follow-up information

http://xmm-lss.in2p3.fr:8080/xxldb/index.html

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~ 500 clusters ~ 10 000 AGNs (5 10-15 erg/s/cm2, completeness limit) > 25 000 AGNs in total

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ž Reprocessing of the X-ray data – with overlap ž Cosmology with the full cluster sample (2016)

Simultaneous fit of:

  • Cosmology
  • Selection effects
  • Cluster physics evolution (scaling relations – baryon fraction)

ž Use numerical simulations to refine the selection function:

  • OWLS (McCarthty et al)
  • Aardvark (Evrard et al)
  • Horizon (Devriendt et al)
  • DEUS (Alimi et al)

ž And, of course, AGN LSS and AGN science ž Final multi-λ catalogues => Legacy

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OWLS simulations (X-ray flux) McCarthy, Le Brun, 2014 10ks XMM photon image Faccioli, Sauvageot et al in

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15 December 2015 ESA-ESO A&A press-release 13 papers

Stay tuned!