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