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Synergies with multi-wavelength surveys

Synergies with multi-wavelength surveys. Matt Jarvis University of Hertfordshire. Facilities for the next decade. SDSS1-2 Pan-STARRS SDSS-3 SkyM DES LSST. Optical. Now. . 2009. . 2010. . 2011. 2015. . UKIDSS VISTA JWST ELT. Near-IR. Now. . 2009. . 2013. .

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Synergies with multi-wavelength surveys

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  1. Synergies with multi-wavelength surveys Matt Jarvis University of Hertfordshire

  2. Facilities for the next decade SDSS1-2 Pan-STARRS SDSS-3 SkyM DES LSST Optical Now  2009  2010  2011 2015  UKIDSSVISTA JWSTELT Near-IR Now  2009  2013  2020 SpitzerSCUBA2HerschelWISE ALMA Mid/Far-IR Now  2009  2009  2010  2012 eMerlinLOFAR EVLAKAT/ASKAPSKA Radio 2009  2010  2013  2020

  3. ESO-VISTA public surveys • VHS (Richard McMahon) ~17000sq.deg (z<0.6ish) • VIKING (Will Sutherland) ~1000sq.deg (z<1.2ish) • VIDEO (Matt Jarvis) ~13sq.deg (1<z<6ish) • Ultra-VISTA (LeFevre/Dunlop/Franx/Fynbo)~1sq.deg (z>5) • VVV (Dante Minitti & Phil Lucas) • VMC Survey (Maria-Rosa Cioni)

  4. VISTA Hemiphere Survey (McMahon) Lowest mass and nearest stars Merger history of the Galaxy LSS to z~1 Dark Energy z > 7 QSOs. 3 components; VHS-ATLAS ~5000sq.deg Y=20.9, J=20.9, H=20.3, Ks=19.8 (5s AB mags) VHS-DES ~4500sq.deg J=21.2, H=20.8, Ks=20.2 VHS-GPS ~8200sq.deg J=21.1, Ks=19.8

  5. VIKING (PI Sutherland) Combine with KIDS to provide a deep 9-band photometric survey. Photo-zs for cosmology, dark energy, weak lensing. Z > 7 QSOs, galaxy morphologies, galactic structure, brown dwarfs Z=23.1, Y=22.3, J=22.0, H=21.5, Ks=21.2 (AB)

  6. VIDEO Survey (starting 2009)(also UKIDSS-DXS fields in the north) Z=25.7, Y=24.6, J=24.5, H=24.0, Ks=23.5 (5 AB mag) Deep enough to probe an L* elliptical galaxy out to z~4 Over 12 square degrees Wide enough to sample the full range of galaxy environments, from the richest clusters to the field galaxy population.

  7. VIDEO Survey • Trace the formation and evolution of massive galaxies from z~1 up to and above z~6 • Measure the clustering of the most massive galaxy up to and above z~6 • Trace the evolution of galaxy clusters from their formation epoch until the present day, ~80 massive (>1014) clusters at z>1 . • Quantify the obscured and unobscured accretion activity over the history of the Universe. • Determine the quasar luminosity function at z>6 • Determine near-infrared light curves for Sne • Determine the nature of SNe host galaxies to high redshift Elais-S1 XMM-LSS CDF-S

  8. VIDEO+SERVs+DES Spitzer Representative Volume Survey (SERVS) approved to cover VIDEO survey regions + LH and Elais-N1 (1400hours over next few years) Will provide 3.6 and 4.5um data to slightly deeper levels than the VIDEO depths (L* at z>5) VIDEO entering data sharing agreement with the Dark Energy Survey. DES will have grizy photometry over VIDEO regions to depths of AB~27 (5sigma) Concentrating on SNe science initially. Elais-S1 XMM-LSS CDF-S

  9. Herschel

  10. HerMES

  11. Herschel-ATLAS SurveySteve Eales, Loretta Dunne, Matt Jarvis, ++ Aim is to survey ~550sq.deg with Herschel at 110, 170, 250, 350 and 550mm. (600hrs allocated) • Local(ish) Galaxies • Planck synergies • Efficient lens survey • Rare object science • Large-scale structure • Clusters • Galactic science

  12. Herschel-ATLAS Survey Synergies with Planck • One of the Planck survey’s main goals is to detect 1000s of high-z clusters through ths SZ-effect. • H1K will be able to determine the composition of the distant clusters in 1/40 of the Planck sky. H1K lens survey • Submm surveys possibly ideal way to find lenses. Large -ve k-correction means sources at z>1. • H1K will contain ~3000, 1600 and 700 strongly lensed galaxies at 250, 350 and 500um, with a lens yield of ~100% at 500um. high-z gals FSQs low-z gals

  13. North+Equatorial GAMA South

  14. EUCLID/IDECS 1.2m telescope in Space with 0.5sq.deg FoV Visible and near-infrared telescope with both imaging and spectroscopic capabilities Broad science aims but particularly in determining the Dark Energy equation of state with a combination of weak lensing, SNe and Baryon Acoustic Oscillations. 20000 sq.deg survey to H=24 and spectroscopic survey to H=22. Deep field to H=26 spectroscopy to H=24. Would be able to do VIDEO science over the whole hemisphere Projected launch 2017/2018 if approved in the Cosmic Visions process later this year.

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