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Next Generation Deep 2 m Survey: Reconnoitering the Dark Ages

Next Generation Deep 2 m Survey: Reconnoitering the Dark Ages. Jeremy Mould, Swinburne University Recent Progress in theoretical and observational cosmology Beijing, Nov 6, 2011. A vital goal of astronomy today is to understand the evolution of galaxies.

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Next Generation Deep 2 m Survey: Reconnoitering the Dark Ages

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  1. Next Generation Deep 2m Survey: Reconnoitering the Dark Ages Jeremy Mould, Swinburne University Recent Progress in theoretical and observational cosmology Beijing, Nov 6, 2011

  2. A vital goal of astronomy today is to understand the evolution of galaxies

  3. The earliest galaxies emit in the infrared where for maximum sensitivity telescopes should be based in Antarctica

  4. The End of the Dark Ages: First Light and Reionization • Until around 400 million years after the Big Bang, the Universe was a very dark place.  There were no stars, and there were no galaxies. • Scientists would like to unravel the story of exactly what happened after the Big Bang.  • The PILOT survey telescope and the James Webb Space Telescope will pierce this veil of mystery and reveal the story of the formation of the first stars and galaxies in the Universe.

  5. Spectra and images of the first galaxies JWST PILOT Survey Telescope

  6. The PILOT telescope is to be erected on a tower on the Antarctic plateau, as that is how and where the best images are obtained. http://www.aao.gov.au/pilot/ Project Leader: John Storey Project Manager: Roger Haynes Telescope Scientist: Will Saunders

  7. UKIDSS • 7500 square degrees of the Northern sky, extending over both high and low Galactic latitudes, in JHK to K=18.3. • three magnitudes deeper than 2MASS. • UKIDSS = near-infrared SDSS • Also a panoramic atlas of the Galactic plane. • UKIDSS = five surveys • two deep extra-Galactic elements, one covering 35 square degrees to K=21, and the other reaching K=23 over 0.77 square degrees.

  8. The Current State of the ArtVIKING - VISTA Kilo-Degree Infrared Galaxy Survey. PI Will Sutherland • The VIKING survey will image the same 1500 square degrees of the sky in Z, Y, J, H, and Ks to a limiting magnitude 1.4 mag deeper than the UKIDSS Large Area Survey. • very accurate photometric redshifts, especially at z > 1, important step in weak lensing analysis and observation of Baryon Acoustic Oscillations. • Other science drivers include the hunt for high redshift quasars, galaxy clusters, and the study of • galaxy stellar masses.

  9. PILOT 2m survey • Offner relay reflective cold stop design (diffraction limited) by Jon Lawrence • On chip guiding • 8K x 8K arrays => 16'x 16' @ 0.125"/pixel • Assumed K background 1mJy/ﬦ" i.e. 14.54 mag. • 0.2 arcsec aperture background is K = 14.54 - 2.5log(p0.01) = 20.8 mag • NICMOS sensitivity is H = 25, gives S/N = 0.5 in 900s with background adjusted for aperture. • To reach S/N = 2 =>16 times longer, that is 4hr.

  10. D Image Quality Tip-Tilt removed PSF from SPIE 4836 Diffraction limited Best 25% South Pole The other two curves are MK and average SP arcsec

  11. PILOT survey NIRSpec 70 nJy 2p sr 23 nJy is K = 26.2 mag

  12. Plan AClone the GSAOI focal plane

  13. Cost of Infrared Camera • $750,000 per 20482 • $125,000 per ASIC (one for each chip) • 40962 totals $3.5M (8.5 arcmin field) • 2 x 40962 totals $7M (8.5 x 17 arcmin) • Plus cost of dewar and filters • Plus cost of labour

  14. Plan BSOFRADIR SATURN SW HgCdTe SWIR

  15. Science Goals • Although there are many science goals for a survey deeper than any previous one, • e.g. the lowest mass stars • Star formation regions in our galaxy • See also ARENA and Dome F proposals • one of the most exciting is finding galaxies at redshift > 10 from the H dropout method. • These have no flux at 1.6m • But are detected at 2.2m • Redshift = 1.6/0.09 – 1 = 16.8 • Spectra of these objects would be obtained with JWST

  16. The Antarctic advantage • Almost diffraction limited images • Wide field • Low 2m background • This combination is only available from • the Antarctic plateau • high altitude balloons • space More details http://www.kdust.org/KDUST/KDUST.html and arXiv:1108.1992

  17. The competition is space: WFIRST Exoplanets and dark energy

  18. WFIRST (or Euclid) vs PILOT Advantages of WFIRST Disadvantages of WFIRST Smaller aperture, 1.5 metre Lower resolution 3 year mission lifetime 2020 launch Order of magnitude higher cost 200 nJy limit vs 70 nJy with PILOT • Top ranked in ASTRO 2010 • Broader band possible, e.g. 1.6-3.6m • No clouds

  19. PILOT Survey logistics • Implement 20’ field: 26 years/sr • assuming 180 x 24 clear hours per year • but that’s probably faster than WFIRST • ARENA’s PLT design offers 40’, 6 years/sr • If K background is 0.1mJy/sq” then 0.26 years/sr • other wavelengths also become doable in a 5 year ‘mission’ • ~100 Pb of data to cover 2p sr • not a problem according to Moore’s Law • data could be served from CAASTRO website • Will not be obsolete until KDUST 8 is operational • That will reach ABK = 29 mag

  20. Stellar pops in the EOR

  21. 2 micron background

  22. Denizens of the epoch of reionization • 1m band dropouts at z = 1.1/0.09 -1 = 11 • J band dropouts at z = 1.4/0.09 -1 = 14 • Galaxies with 108 year old stellar pops at z = 6 • Pair production SNe (massive stars) at MK = -23 • Activity from progenitors of supermassive black holes • Young globular clusters with 106 year free fall times and M/L approaching 10-4 • Rare bright objects require wide field survey, then JWST or GMT spectra.

  23. The next steps • Is this project compatible with KDUST 2.5 ? • Finalize camera configuration • Find LIEF partners • Swinburne University, J. Mould • UNSW, M. Burton • Macquarie University, J. Lawrence • Melbourne University, S. Wyithe • ANU, P. McGregor • CAASTRO and AAO ? • Texas A & M University

  24. ARC LIEF facts of life • $9M is a very big proposal • Funding spread over 2013,4,5 • But the chips need purchasing in 2013 • Most proposals are unfunded • This proposal needs to be very strong • Universities must contribute 25% cash • CAASTRO may be able to contribute a postdoc

  25. Construction and operations schedule (tentative) • January 2013 LIEF funding • Preliminary Design Review • 2013 Texas A & M purchases Teledyne arrays • ANU purchases dewar and filters • 2014 Integrate and test focal plane at ANU • January 2015 Integrate telescope and camera in Fremantle • 2015-2019 operations (within the international antarctic science region) at Kunlun Station • 2020 return of focal plane to USA

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