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UKIRT Infrared Deep Sky Survey

UKIRT Infrared Deep Sky Survey. Omar Almaini Royal Observatory Edinburgh. UKIRT Wide Field Camera (WFCAM) Public surveys - UKIDSS Ultradeep Survey (UDS). Near infrared camera for UKIRT Construction at ATC, Edinburgh Widest IR field ever attempted Delivery to Hawaii March ‘04

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UKIRT Infrared Deep Sky Survey

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  1. UKIRT Infrared Deep Sky Survey Omar Almaini Royal Observatory Edinburgh • UKIRT Wide Field Camera (WFCAM) • Public surveys - UKIDSS • Ultradeep Survey (UDS)

  2. Near infrared camera for UKIRT • Construction at ATC, Edinburgh • Widest IR field ever attempted • Delivery to Hawaii March ‘04 • Plan to undertake public surveys using ~50% of UKIRT time - but there will be open time! Project Scientist: Mark Casali

  3. IR detectors • 4 Rockwell Hawaii-II devices • HgCdTe hybrids • J, H, K (+Y, Z) • 2048 x 2048 18 m pixels • detector packaging prevents close packing - 90% is optimum if optics can be achieved

  4. The Pixel Scale • Competing requirements… • Survey Speed – big pixels • Resolution, point source sensitivity – small pixels •  Compromise using 0.4" pixels + MICROSTEPPING

  5. Footprint on the Sky ISAC (VLT) UFTI (UKIRT) WFCAM WFIRC (du Pont) 0.66 deg

  6. Focal Plane configuration • 90% spacing of 4 detectors • four exposures give filled 0.88° square (0.77 sq. °) • diameter of field required = 0.93° (151 mm)

  7. Survey Performance • The minimum WFCAM standard tile • 4 microsteps (10 sec per stare) • 4 macrosteps  = 0.77 sq. deg. in t = 211 sec K=18.4 H=18.9 J=20.0 • = 0.77 sq. deg. in t = 4 hours K=20.7 H=21.2 J=22.3

  8. Current status Integration and testing complete Cryostat temp to spec Detectors & electronics in place Good q.e. > 60% in z’ Y J Two outstanding components I. Tertiary mirror ii. Corrector plate NEW - both delivered Dec 2003 (under testing)

  9. Asembled WFCAM cryostat The WFCAM Cryostat Two outstanding optical components Integration and testing complete Cryostat temp to spec Detectors & electronics in place Good q.e.: 60% in z’ Y J

  10. Footprint on the Sky ISAC (VLT) UFTI (UKIRT) WFCAM WFIRC (du Pont) 0.66 deg

  11. Small projects won’t fully exploit the capabilities • Consortium formed to propose a very large public survey • We proposed ~50% of all UKIRT time for 7 years • "UKIRT infra-red deep sky survey“ • Final approval granted (2 year roller) • Immediately public to ESO community • World public 18 months after observation UKIDSS

  12. The UKIDSS Consortium • Chair: Andy Lawrence • Survey Scientist: Steve Warren • Survey design heads: Almaini,Edge, Hambly, Jameson, Lucas • + ~50 others within ESO • + Subaru FMOS team • "UKIRT infra-red deep sky survey“ UKIDSS

  13. wedding cake strategy • five year plan 2004-2009 Ultradeep Survey K=23, 0.8 sq. deg The Deep Survey K=21, 30 sq. deg Galactic Plane Survey K=19, b= +/- 5 deg Large Area Survey K=18.4, 4000 sq. deg Galactic Cluster Survey K=18.4, 1600 sq. deg

  14. 5 sigma, point source At any depth UKIDSS will cover an area between 1 and 2 orders of mag larger than any existing or planned near-ir survey

  15. The UKIDSS Ultra-Deep Survey • UDS • 0.8 deg 2 • K=23, H=24 , J=25 • z~3 Large-scale structure • 104 EROs • LF and clustering of z>2 massive galaxies

  16. The UKIDSS Ultra-Deep Survey • UDS • 0.8 deg 2 • K=23, H=24 , J=25 • z~3 Large-scale structure • 104 EROs • LF and clustering of z>2 massive galaxies FIRES (Labbe et al. 2002)

  17. The formation of massive spheroids How many massive galaxies in place at z>2 ?? A fundamental test of galaxy formation theories. • e.g. how many galaxies in place more massive than present day 2L* ellipticals at 2<z<4? • Passive evolution models: ~1000 deg-2 • Hierarchical Lambda CDM: ~100 deg-2 Requires depth (K>22) and area (~1sq deg) z~1 c.f. ERO studies at z~1.5 Daddi et al. 2001, Smith et al. 2002, Roche et al. 2002

  18. Predicted IR colours vs redshift

  19. B=27.5, R=27.5, i’=27.2, z’=26.3 RA: 02 h Dec: –5 deg

  20. B=27.5, R=27.5, i’=27.2, z’=26.3

  21. 82 sq. arcmin (now 160) 29 > 3.0 sigma 13 > 3.5 sigma 6 > 4.0 sigma

  22. Summary of data in UDS field * Proposed/in prep.

  23. UDS - Plans For Year One K = 22.5 [0.8 sq deg] (best 60% seeing) J = 23.5 [0.8 sq deg] (best 70% seeing)

  24. Early science from UDS? • Space density and clustering of z=3 massive galaxies (>L*) (select e.g. using J-K>2) • can we construct a mass function of galaxies as a fn of redshift? etc… FIRES (Labbe et al. 2002)

  25. WFCAM – 0.2 sq deg IR field • Delivery to Hawaii May 2004 • Plan to undertake public surveys using ~50% of UKIRT time UKIDSS www.ukidss.org

  26. END

  27. Predictions of passive evolution K-z predictions for L* ellipticals (full aperture magnitudes)

  28. UKIDSS overview LAS DXS UDS GPS GCS

  29. UKIDSS overview2-year plan LAS DXS UDS GPS GCS

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