UKIRT Infrared Deep Sky Survey

UKIRT Infrared Deep Sky SurveyUKIRT Infrared Deep Sky Survey

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

Omar AlmainiRoyal Observatory Edinburgh

Project Scientist: Mark CasaliProject Scientist: Mark Casali

Near infrared camera for Near infrared camera for UKIRTUKIRT

Construction at ATC, Construction at ATC, EdinburghEdinburgh

Widest IR field ever Widest IR field ever attemptedattempted

Delivery to HawaiiDelivery to Hawaii March March ‘04 ‘04

Plan to undertake public Plan to undertake public surveyssurveys

using ~50% of UKIRT timeusing ~50% of UKIRT time

- but there will be open time!- but there will be open time!

IR detectorsIR 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

The Pixel ScaleThe Pixel ScaleCompeting requirements…

• Survey Speed – big pixels

• Resolution, point source sensitivity – small pixels

Compromise using 0.4" pixels + MICROSTEPPING

Footprint on the SkyFootprint on the Sky

UFTI (UKIRT)WFCAM

ISAC (VLT)

WFIRC (du Pont)

0.66 deg

•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

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

Current statusCurrent statusIntegration 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)

The WFCAM CryostatThe 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

Footprint on the SkyFootprint on the Sky

UFTI (UKIRT)WFCAM

ISAC (VLT)

WFIRC (du Pont)

0.66 deg

Small projects won’t fully exploit the capabilitiesSmall projects won’t fully exploit the capabilities Consortium formed to propose a very large public Consortium formed to propose a very large public

surveysurvey– We proposed ~50% of all UKIRT time for 7 yearsWe proposed ~50% of all UKIRT time for 7 years– "UKIRT infra-red deep sky survey“"UKIRT infra-red deep sky survey“– Final approvaFinal approval grantedl granted (2 year roller) (2 year roller)

– Immediately public to ESO communityImmediately public to ESO community– World public 18 months after observationWorld public 18 months after observation

Chair: Andy LawrenceChair: Andy Lawrence Survey Scientist: Steve WarrenSurvey Scientist: Steve Warren Survey design heads: Almaini,Survey design heads: Almaini, Edge, Hambly, Edge, Hambly,

Jameson, LucasJameson, Lucas ++ ~5 ~50 others within ESO0 others within ESO + Subaru FMOS team+ Subaru FMOS team

The UKIDSS ConsortiumThe UKIDSS Consortium

"UKIRT infra-red deep sky survey“"UKIRT infra-red deep sky survey“

– five year plan 2004-2009five year plan 2004-2009

wedding cake strategywedding cake strategy

Large Area Survey Large Area Survey K=18.4, 4000 sq. degK=18.4, 4000 sq. deg

Galactic Cluster Survey Galactic Cluster Survey K=18.4, 1600 sq. degK=18.4, 1600 sq. deg

Galactic Plane Survey Galactic Plane Survey K=19, b= +/- 5 degK=19, b= +/- 5 deg

The Deep Survey The Deep Survey K=21, 30 sq. degK=21, 30 sq. deg

Ultradeep SurveyUltradeep SurveyK=23, 0.8 sq. degK=23, 0.8 sq. deg

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

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

The UKIDSS Ultra-Deep SurveyThe UKIDSS Ultra-Deep Survey

UDS

– 0.8 deg0.8 deg 2 2

– K=23, H=24 , J=25K=23, H=24 , J=25

– z~3 Large-scale structure z~3 Large-scale structure – 10104 4 EROs EROs– LF and clustering of z>2 massive LF and clustering of z>2 massive

galaxiesgalaxies

The UKIDSS Ultra-Deep SurveyThe UKIDSS Ultra-Deep Survey

UDS

– 0.8 deg0.8 deg 2 2

– K=23, H=24 , J=25K=23, H=24 , J=25

– z~3 Large-scale structure z~3 Large-scale structure – 10104 4 EROs EROs– LF and clustering of z>2 massive LF and clustering of z>2 massive

galaxiesgalaxies

FIRES (Labbe et al. 2002)

The formation of massive The formation of massive spheroidsspheroids

e.g. how many galaxies in place more e.g. how many galaxies in place more massive than present day 2L* massive than present day 2L* ellipticals at 2<z<4? ellipticals at 2<z<4?

• Passive evolution models: ~1000 deg-Passive evolution models: ~1000 deg-22

• Hierarchical Lambda CDM: ~100 degHierarchical Lambda CDM: ~100 deg-2-2

z~1z~1 c.f. ERO studies at z~1.5 c.f. ERO studies at z~1.5Daddi et al. 2001, Smith et al. 2002, Roche et al. Daddi et al. 2001, Smith et al. 2002, Roche et al. 20022002

How many massive galaxies in place at z>2 ?? How many massive galaxies in place at z>2 ??

A fundamental test of galaxy formation theories.A fundamental test of galaxy formation theories.

Requires depth (K>22) and area (~1sq deg)Requires depth (K>22) and area (~1sq deg)

Predicted IR colours vs Predicted IR colours vs redshiftredshift

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

RA: 02 h RA: 02 h

Dec: –5 degDec: –5 deg

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

82 sq. arcmin(now 160)

29 > 3.0 sigma13 > 3.5 sigma6 > 4.0 sigma

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 3.6m)

Mm/Sub-mm SCUBA (SHADES – Dunlop)

BLAST

8mJy @850

250, 350, 500

Radio VLA (A,B,C Array)

(Rawlings, Simpson et al.)

5 = 50 Jy

Summary of data in UDS fieldSummary of data in UDS field

* Proposed/in prep.* Proposed/in prep.

UDS - Plans For Year OneUDS - Plans For Year One

K = 22.5 [0.8 sq deg]K = 22.5 [0.8 sq deg]

(best 60% seeing)(best 60% seeing)

J = 23.5 [0.8 sq deg]J = 23.5 [0.8 sq deg]

(best 70% seeing)(best 70% seeing)

Early science from UDS?Early science from UDS?

– Space density and clusteringSpace 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 can we construct a mass function of galaxies as a fna fn

of redshift?of redshift?

etc…etc…

FIRES (Labbe et al. 2002)

WFCAM – 0.2 sq deg IR fieldWFCAM – 0.2 sq deg IR field

Delivery to HawaiiDelivery to Hawaii May 2004 May 2004

Plan to undertake public surveysPlan to undertake public surveys

using ~50% of UKIRT timeusing ~50% of UKIRT time

www.ukidss.org

ENDEND

Predictions of passive Predictions of passive evolutionevolution

K-z predictions for K-z predictions for L* ellipticalsL* ellipticals

(full aperture magnitudes(full aperture magnitudes))

UKIDSS overviewUKIDSS overview

LAS

DXS

UDS

GPS

GCS

UKIDSS overviewUKIDSS overview2-year plan2-year plan

LAS

DXS

UDS

GPS

GCS