UKIRT Infrared Deep Sky Survey

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UKIRT Infrared Deep Sky Survey
Omar Almaini Royal Observatory Edinburgh

• UKIRT Wide Field Camera (WFCAM)
• Public surveys - UKIDSS
• Ultradeep Survey (UDS)

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• 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
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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

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The Pixel Scale

• Competing requirements
• Survey Speed big pixels
• Resolution, point source sensitivity small
  pixels
• ? Compromise using 0.4" pixels
  MICROSTEPPING

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

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Survey Performance

• The minimum WFCAM standard tile
• 4 microsteps (10 sec per stare)
• 4 macrosteps
• ? 0.77 sq. deg. in t 211 sec
• K18.4 H18.9 J20.0
• 0.77 sq. deg. in t 4 hours
• K20.7 H21.2 J22.3

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Current status
Integration and testing complete Cryostat temp to
spec Detectors electronics in place Good q.e.
gt 60 in z Y J Two outstanding components I.
Tertiary mirror ii. Corrector plate NEW -
both delivered Dec 2003 (under testing)
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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
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Footprint on the Sky
ISAC (VLT)
UFTI (UKIRT)
WFCAM
WFIRC (du Pont)
0.66 deg
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• Small projects wont 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
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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
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wedding cake strategy

• five year plan 2004-2009

Ultradeep Survey K23, 0.8 sq. deg
The Deep Survey K21, 30 sq. deg
Galactic Plane Survey K19, b /- 5 deg
Large Area Survey K18.4, 4000 sq. deg
Galactic Cluster Survey K18.4, 1600 sq. deg
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Large Area Survey (4000 sq deg) SDSS K 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
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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
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The UKIDSS Ultra-Deep Survey

• UDS
• 0.8 deg 2
• K23, H24 , J25
• z3 Large-scale structure
• 104 EROs
• LF and clustering of zgt2 massive galaxies

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The UKIDSS Ultra-Deep Survey

• UDS
• 0.8 deg 2
• K23, H24 , J25
• z3 Large-scale structure
• 104 EROs
• LF and clustering of zgt2 massive galaxies

FIRES (Labbe et al. 2002)
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The formation of massive spheroids
How many massive galaxies in place at zgt2 ?? A
fundamental test of galaxy formation theories.

• e.g. how many galaxies in place more massive
  than present day 2L ellipticals at 2ltzlt4?
• Passive evolution models 1000 deg-2
• Hierarchical Lambda CDM 100 deg-2

Requires depth (Kgt22) and area (1sq deg)
z1 c.f. ERO studies at z1.5 Daddi
et al. 2001, Smith et al. 2002, Roche et al. 2002
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Predicted IR colours vs redshift
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B27.5, R27.5, i27.2, z26.3
RA 02 h Dec 5 deg
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(No Transcript)
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B27.5, R27.5, i27.2, z26.3
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82 sq. arcmin (now 160) 29 gt 3.0 sigma 13 gt
3.5 sigma 6 gt 4.0 sigma
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Summary of data in UDS field
Optical Subaru Suprimecam VLT VIMOS HST? (c.f. COSMOS) B27.5 R27.5 i27.2 z26.3 u27.5
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-mm SCUBA (SHADES Dunlop) BLAST 8mJy _at_850 250, 350, 500
Radio VLA (A,B,C Array) (Rawlings, Simpson et al.) 5? 50 ?Jy
Proposed/in prep.
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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)

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Early science from UDS?

• Space density and clustering
• of z3 massive galaxies (gtL)
• (select e.g. using J-Kgt2)
• can we construct a mass function of galaxies as a
  fn
• of redshift?
• etc

FIRES (Labbe et al. 2002)
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• 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
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END
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Predictions of passive evolution

K-z predictions for L ellipticals (full
aperture magnitudes)
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UKIDSS overview
LAS DXS UDS GPS GCS
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UKIDSS overview2-year plan
LAS DXS UDS GPS GCS