Next Generation Deep 2m Survey:

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Next Generation Deep 2m Survey Reconnoitering
the Dark Ages
Jeremy Mould, Swinburne University Recent
Progress in theoretical and observational
cosmology Beijing, Nov 6, 2011
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A vital goal of astronomy today is to understand
the evolution of galaxies
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The earliest galaxies emit in the infrared where
for maximum sensitivity telescopes should be
based in Antarctica
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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.

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Spectra and images of the first galaxies

• JWST

• PILOT Survey Telescope

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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
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UKIDSS

• 7500 square degrees of the Northern sky,
  extending over both high and low Galactic
  latitudes, in JHK to K18.3.
• 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 K21, and the other reaching
  K23 over 0.77 square degrees.

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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 gt 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.

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PILOT 2m survey

• Offner relay reflective cold stop design
  (diffraction limited) by Jon Lawrence
• On chip guiding
• 8K x 8K arrays gt 16'x 16' _at_ 0.125"/pixel
• Assumed K background 1mJy/?" 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 gt16 times longer, that is 4hr.
  

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Jon Lawrence, M. Ashley, M. Burton J. Storey
Design of DMT
citeseerx.ist.psu.edu/viewdoc/download?doi10.1.1.
147.5241.pdf
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Image Quality Tip-Tilt removed PSF from SPIE 4836

• D

Diffraction limited
Best 25 South Pole
The other two curves are MK and average SP
arcsec
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PILOT survey NIRSpec 70 nJy
2p sr
23 nJy is K 26.2 mag
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Plan AClone the GSAOI focal plane
Type Rockwell HAWAII-2RG HgCdTe 
Array sizes 2048 x 2048 pixels each (2040 x 2040 active)
 Detector area 4080 x 4080 pixels ( 85" x 85")
Physical Pixel size 18 µm
Pixel scale 0.02" (TBC)
Spectral Response 0.9  µm to 2.6 µm (data / plot)
Gains 2.8 e-/ADU (TBC)
 Dark current   0.01 e-/s/pix (12 e- in the maximum integration time of 20 minutes)
 Saturation 48,000 ADU (TBC)
On-Detector Guide Windows (ODGW)  One programmable ODGW per detector
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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

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Plan BSOFRADIR SATURN SW HgCdTe SWIR
ARRAY FEATURES Format 1000x256 Pixel pitch 30 µmx30 µm Material spectral response 0.8µm 2.5 µm FPA Operating Temperature up to 200 K ROIC FEATURES Modes snap shot operation, integrate while read mode, programmable integration time, anti blooming system Input stage Capacitance TransImpedance Amplifier (CTIA) Charge handling capacity 0.4 106 / 10.6 106 (for 100 well fill) Electrical dynamic range gt 2 V (75 dB) Readout noise lt 150 e- (for 0.4 Me- gain) and lt 450 e- (for 1.6 Me- gain) Signal outputs 4 or 8 (user selectable)
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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 gt 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

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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 arXiv1108.1992
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The competition is space WFIRST
Exoplanets and dark energy
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WFIRST (or Euclid) vs PILOT

• Advantages of WFIRST

• Disadvantages of WFIRST

• Top ranked in ASTRO 2010
• Broader band possible, e.g. 1.6-3.6m
• No clouds

• 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

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PILOT Survey logistics

• Implement 20 field 26 years/sr
• assuming 180 x 24 clear hours per year
• but thats probably faster than WFIRST
• ARENAs 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 Moores Law
• data could be served from CAASTRO website
• Will not be obsolete until KDUST 8 is operational
• That will reach ABK 29 mag

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Stellar pops in the EOR
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2 micron background
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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.

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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

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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

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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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CAASTRO Project Criteria

• Align with core CAASTRO Science Goals (must be
  All-sky and be in at least one Theme ? Dark,
  Dynamic or Evolving)
• All three themes. Genuinely all-sky project (2p
  sr)
• Involve strong collaboration across a number of
  CAASTRO nodes to achieve the research outcomes
  and/or involve international partners
• Possible camera/telescope integration work in
  WA.
• CAASTRO could serve the data (100 Pb) from
  caastro.org.au , physically probably from
  Pawsey.
•