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Transcript of SDSS and UKIDSS Jon Loveday University of Sussex.
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SDSS and UKIDSS
Jon Loveday
University of Sussex
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Outline
• Sloan Digital Sky Survey status
• UK Infrared Deep Sky Survey overview and status
• K-band luminosity function from matched SDSS-UKIDSS sample
• Future prospects
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SDSS1 Survey Goals
• Make definitive map of local universe• Image quarter-sky in five colours ugriz• Measure 50 million galaxy images to r~22• Obtain spectra for 1 million galaxies and
100,000 quasars• SDSS1 ended June 2005, immediately
followed by SDSS2
http://www.sdss.org
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SDSS2 - commenced July 2005
• Legacy survey– complete SDSS1 goals
• SEGUE – Galactic structure
• Supernovae– Repeated imaging of southern equatorial stripe
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SDSS Status (March 2006)
• Unique area imaged (sq deg)– North: 7561 essentially completed 30 Jan 2006– South: 739– 210 million objects detected
• Spectroscopy: 1819 plates inc spectra of– 697,757 galaxies– 93,083 QSOs– 253,261 stars
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Data Release 4
• Published July 2005
• Imaging area 6670 deg2
• Photometry of 180 million unique objects
• Spectra of 849,920 objects over 4783 deg2:
565,715 galaxies 76,483 quasars
102,714 stars
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Imaging
Spectroscopy
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Data Release 5
• Due summer 2006• Imaging area 8000 deg2
• Photometry of 215 million unique objects • Spectra of 1,048,960 objects over 5740
deg2: 674,749 galaxies 90,611 quasars
154,925 stars
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Imaging
Spectroscopy
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SDSS Cosmological Highlights
• Highest known redshift quasar (z = 6.4)• Large scale structure cosmological
constraints• Galaxy properties and environment• Detection of baryon acoustic peak• More than 1000 publications using SDSS
data, with 29,000 citations
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z=6.4 Quasar
Gunn-PetersonTrough
Fan et al 2003
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Cmbgg OmOlCMB
+
LSS
WMAP only+ SDSS
Tegmarket al 2004
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UKIDSS
• UK Infrared Deep Sky Survey • Consortium of most UK astronomy departments• UKIRT 3.8m telescope plus WFCAM
(4x20482 Hawaii-II arrays, 0.21 deg2)• Etendue of 2.38 m2 deg2 largest of any IR camera
until VISTA• zYJHK (1 ~ 2.5 ) near-IR filters• 5 surveys, 3 extragalactic• Significantly deeper than 2MASS
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UKIDSS (contd)
• Observing started May 2005• 7 year observing plan (~50% of UKIRT time)• Pipeline processing in Cambridge, archive in
Edinburgh• No proprietary data period• Data immediately available to ESO members once
verified• Rest of world 18 months later
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UKIDSS filters
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Why Near-IR?
• 2 light traces mass in evolved stars - provides good estimate of stellar mass
• Helps identify cool dwarf stars and high-z quasars (optical dropouts)
• Less sensitive than optical light to dust reddening and type-dependent K-corrections
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T6 brown dwarfz =7 quasar
Quasars vs dwarf stars
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UKIDSS Surveys
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Lawrence et al 2006 in prep
Comparison with 2MASS
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http://apm14.ast.cam.ac.uk/status/wfcam/
UKIDSS Status
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UKIDSS Early Data Release
• Available to ESO community 2006 Feb 10
• ~1% of final sample, comparable to 2MASS
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Data Access
• Via WFCAM Science Archive (Edinburgh) http://surveys.roe.ac.uk/wsa
• Need to register with your community contact
• SQL interface will be familiar to SDSS CAS users
• NB: EDR data not all of final survey quality
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Early application of SDSS + UKIDSS
• K-band luminosity function
• UKIDSS K-band photometry
• SDSS redshifts
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Bell et al 2003
Grey:Cole et al
2001
Currentestimates
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K-band luminosity function
• Use UKIDSS “EDR+” sample: includes areas of sky with incomplete filter coverage
• Match UKIDSS EDR+ LAS with SDSS DR5 main sample galaxies (r < 17.7)
• Tolerance 2 arcsec (nearly all matches within 1 arcsec)
• Use Petrosian magnitudes
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Sky Coverage
“EDR+” inc. areas with incomplete filter coverage
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Sky Coverage
Matched with SDSS DR5 main galaxy target
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Sky Coverage
Has redshift and K-band detection
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K-band Completeness
LAS galaxies 16.0SDSS matches 14.0
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r-K colours
Completeness of matched sample (K=14) limited by SDSS r limit (17.77) and reddest r-K colour (~3.8)
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LF Estimate
• Use complete sample (K < 14) 1287 galaxies (fewer than 50%)
• K-corrections to z = 0.1 from template fit to SDSS ugriz using kcorrect v4
• STY, SWML estimators of (MK) - independent of density inhomogeneities
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Bivariate LF
• Use entire matched sample by estimating SWML bivariate (Mr, MK) allowing for SDSS r flux limit (r < 17.7)
• Sample size 3249 galaxies, but faintest galaxies will now be bluer than average
• Integrate over Mr to obtain (MK)
• Fit Schechter function by least squares
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Conclusions/Future Prospects
• UKIDSS-SDSS K-band LF consistent with earlier estimates using 2MASS
• Measurements will improve considerably with more data
• UKIDSS Data Release 1 (DR1) due mid-2006 will have ~10 times as much data
• Two year goals:• LAS half complete• DXS full depth in JK over 3.1 deg2
• UDS K = 22.8, J = 23.8
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Future Plans
• Investigate type-dependence of K-band LF and its evolution
• Comparison with optical distinguishes stellar mass accumulation with star formation history
• Evolution to z ~ 0.3 with SDSS redshifts• Higher-redshift evolution using photometric
redshifts
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Future Plans (2)
• SDSS Southern stripe co-added data plus UKIDSS DXS excellent for photo-z
• Possible volume-limited redshift survey using AAOmega
• Clustering evolution of K-limited (stellar mass selected) samples
• VISTA …
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Websites
• http://www.sdss.org
• http://www.ukidss.org
• http://surveys.roe.ac.uk/wsa