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

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

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 UFTI (UKIRT) WFCAM ISAC (VLT) WFIRC (du Pont) 0.66 deg

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

7.   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 Survey Performance

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. 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 Asembled WFCAM cryostat

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

11. n Small projects won’t fully exploit the capabilities n 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

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

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

14. Large Area Survey (4000 sq deg) SDSSK = 18.4 H = 18.8 J = 20.0 Y = 20.5 Deep Extragalactic Survey (30 sq deg) Lockman Hole XMM-LSS ELAIS N1 VIRMOS-4 K = 21.0 H = 22.0 J = 22.5 Ultra Deep Survey (0.8 sq deg) SXDF (02hr –5)K = 23.0 H = 24.0 J = 25.0

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

16. The UKIDSS Ultra-Deep Survey n n UDS –0.8 deg 2 –K=23, H=24, J=25 –z~3 Large-scale structure –10 4 EROs –LF and clustering of z>2 massive galaxies

17. The UKIDSS Ultra-Deep Survey n n UDS –0.8 deg 2 –K=23, H=24, J=25 –z~3 Large-scale structure –10 4 EROs –LF and clustering of z>2 massive galaxies FIRES (Labbe et al. 2002)

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

19. Predicted IR colours vs redshift

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

22. B=27.5, R=27.5, i’=27.2, z’=26.3

23. 82 sq. arcmin (now 160) 29 > 3.0 sigma 13 > 3.5 sigma 6 > 4.0 sigma

24. Optical * Subaru Suprimecam VLT VIMOS HST? (c.f. COSMOS) B=27.5 R=27.5 i’=27.2 z’=26.3 u=27.5 X-ray * XMM-Newton (Watson) Chandra ( Almaini/Page ) 100ks + 6x50ks ? Mid/FIR * SIRTF – SWIRE (Lonsdale) + GO ( Simpson ) 3.6-160  m (22 AB at 3.6  m) Mm/Sub-mmSCUBA (SHADES – Dunlop) BLAST 8mJy @850 250, 350, 500 RadioVLA (A,B,C Array) ( Rawlings, Simpson et al.) 5  = 50  Jy Summary of data in UDS field * Proposed/in prep.

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

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

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

28. END

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

30. UKIDSS overview LAS DXS UDS GPS GCS

31. UKIDSS overview 2-year plan LAS DXS UDS GPS GCS