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VST ATLAS

VST ATLAS. Mike Irwin, Nigel Metcalfe, Tom Shanks, et al. +2QDES. Michael Drinkwater, Scott Croom et al. Featuring Utane Sawangwit, PhD. VST ATLAS Survey. VST ATLAS (+VHS) ➝ Southern SDSS in ugriz (+YJHK)!

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VST ATLAS

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  1. VST ATLAS Mike Irwin, Nigel Metcalfe, Tom Shanks, et al +2QDES Michael Drinkwater, Scott Croom et al Featuring Utane Sawangwit, PhD

  2. VST ATLAS Survey • VST ATLAS (+VHS) ➝ Southern SDSS in ugriz (+YJHK)! • Exposures u: 2x60s, g: 2x50s, riz: 2x45s – one filter per hourly concatenations – ugr (dark), iz (gray.bright) • Newsflash – ESO Chilean VST time doubles u exposure to 4x60s • 2-tile dither – 84" in Dec, 24" in RA • Offsets 58' in RA and Dec – 2' overlap • 1"-1."4 seeing – better than SDSS median 1."4 –complements KIDS • No guide star needed so no overhead • ~45 nights per year for 2 years – accelerated! • Footprint ~2500deg2 in SGC and ~2000deg2 in NGC

  3. OmegaCAM 80" gap ~20" gap

  4. VST ATLAS Survey Area b=30o b=-30o

  5. VST ATLAS Core Team • CASU (Mike Irwin et al, Cambridge) does the basic reduction using the VST Data Flow pipeline • Steve Maddox (Nottingham) leads the overall global calibration process • Nigel Metcalfe + Peter Draper (Durham) – OB submission + QC on the ATLAS products • WFAU (Bob Mann et al, Edinburgh) to provide archiving facilities, additional to the ESO archive

  6. VST ATLAS Status – 6/2/12 ~750 deg2 ugriz observed

  7. SDSS-ATLAS zoom - r SDSS ATLAS

  8. SDSS-ATLAS zoom - g SDSS ATLAS

  9. SDSS-ATLAS zoom - u SDSS ATLAS

  10. ATLAS CASU ids – improve! ATLAS ids ATLAS

  11. WHDF v ATLAS + SDSS - u

  12. WHDF v ATLAS + SDSS – b vs g D. Karagiannis et al

  13. WHDF vs ATLAS+SDSS – i

  14. ATLAS Science Summary • VST ATLAS – "Southern Sloan" – SDSS depth + ~1."2 resolution in ugriz over ~4500deg2 • Cosmology Package to rival WFIRST! • 2QDES survey of up to ~500000 QSOs • BAO at z~1.6 via ATLAS+2dF UVX QSO clustering • Gravitational Growth rate at z~1.6 via QSOs • QSO Lensing vs galaxy ugrizYJHK photo-z • Probe of primordial large-scale Non-Gaussianity • ISW via LRGs • Other Science • Stellar Streams + Galactic Archaeology • Z~7 QSOs via ATLAS+VHS z dropouts • Beyond the Great Attractor + Fornax etc

  15. 2QDES BAO vs BOSS • 80deg-2 0.4<z<2.2 +3000deg2 • ~3s BAO detection • ⇒±3% BAO • 105deg-2 1<z<2.2 and 4500deg2 • ~6s BAO detection • ⇒±1.7% BAO Sawangwit et al (2012), MNRAS, 420, 1916

  16. 2QDES BAO vs BOSS • 80deg-2 0.3<z<2.2 + 3000deg2 • ~3s BAO detection • ⇒±3% BAO • 105deg-2 1<z<2.2 + 4500deg2 • ~6s BAO detection • ⇒±1.7% BAO • Competitive with BOSS! Sawangwit et al (2012), MNRAS, 420, 1916

  17. 2QDES Pilot: 5 ATLAS fields → 2dF

  18. ATLAS 2QDES ugri QSO selection • Simple selection in ugr and gri • + KDE selection of Bovy et al • Limit g<22.5

  19. 2QDES 2dF AAOmega Pilot • 50 min exposure on 20 December AAT Director's night • ATLAS field observed at RA 2h30 Dec-30 • 176 high quality QSO spectra observed! • ~66% QSO in fibres 1-200 but 38% QSO in fibres 201-400 • 2dF fibre positional problem – no guide stars in N half • Assuming 66% -> already achieving ~80deg-2 • Compare to ~105deg-2 required to beat BOSS

  20. Pilot Sample QSO Spectra

  21. VST ATLAS 2QDES Pilot Loss of fibre flux caused by lack of allocated guide stars in Northern half of 2dF field

  22. Fibre-ATLAS mag v fibre no. Significant light loss in fibres 201-400 caused by unallocated guide stars in half the field

  23. 2MASS v ATLAS astrometry check

  24. AAOmega Pilot z vs 2QZ z

  25. AAOmega Pilot QSO N(z)

  26. AAOmega Pilot QSO n(g) ~50% success rate being maintained at g~22 in only 50 min exposure

  27. Summary • ~750deg2 surveyed by ATLAS already • More or less achieving SDSS depth in ugriz • Chilean proposal to double u exposure time accepted • 2dF AAOmega pilot already hitting QSO sky density of 80deg-2 to g~22 in 50min exposure • 105deg-2 1<z<2.2 QSO target for April run • 2QDES survey of ~0.5million QSOs still a possibility… • … for z~1.6 6s BAO, RSD, QSO Lensing + fNL+ QSO BH-halo mass relation

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