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Octiber 30, 2002 Santiago, Chile 1
SWIRE
The SIRTF Wide-Area Infra-Red Extragalactic
SurveyCarol J. Lonsdale
IPAC, Caltech
October 30, 2002 Santiago, Chile Carol Lonsdale 2
SIRTF & SWIRE
85 cm cryogenic telescope– Launch mid-April 2003, heliocentric orbit
– 3-5 year lifetime; 75% open time: 1st call Nov 8, 2002
– 3 instruments: 3-160μm imaging & spectroscopy
Legacy Program– 6 large programs; 3 of them extragalactic
– To be completed in first year
– Non-proprietary: immediate community follow-up
SWIRE: largest Legacy program: 851 hours– 63 sq degs, 7 fields
– 3-160 μm imaging, to z~3
– SPHEROIDS, DISKS, STARBURSTS, AGN
– 100s of 100Mpc-scale cells
October 30, 2002 Santiago, Chile Carol Lonsdale 3
IR Galaxy Populations
Luminous IR Galaxies are the dominant population L > 1011Lo
~30% of local energy density is in the IR
IR GalaxyLuminosityFunction
Optical LF
Soifer et al 1989
October 30, 2002 Santiago, Chile Carol Lonsdale 4
IR Galaxy Populations: LIRGs
Interactions/mergers
IR does not coincide with UV-optical – younger stellar
population
October 30, 2002 Santiago, Chile Carol Lonsdale 5
IR Galaxy Populations: ULIRGs
Surace et al (2001) Scoville et al. (2000), Soifer et al. (2000), Goldader et al (2002)
Compact core: 80% of mid-IR
<7% in far-UV
Arp 220
Av>100
October 30, 2002 Santiago, Chile Carol Lonsdale 6
Strong Evolution of the Infrared Galaxy
Population First discovered for IRAS
sources
ISO surveys confirm strong evolution
Also seen in the submm
Xu et al. (2001) model fits multi-λ data:– L α (1+z)4
– ρ α (1+z)2
October 30, 2002 Santiago, Chile Carol Lonsdale 7
IR Dominates the Global Backgrounds
50% or more is in IR
Franceschini et al 2001
October 30, 2002 Santiago, Chile Carol Lonsdale 8
CIRB Resembles M82
Elbaz et al 2002
Franceschini et al 2001
October 30, 2002 Santiago, Chile Carol Lonsdale 9
IR & X-Ray Backgrounds
Cosmic X-Ray Background models require a population of highly obscured AGN which increases with z(Comastri et al., Gilli et al, Polletta et al 2002)
What fraction of the CIRB is powered by accretion?
Hasinger
Salvati & Maiolino
Even MIR and hard X-ray highly obscured
October 30, 2002 Santiago, Chile Carol Lonsdale 10
Deep ISO 15µm & X-ray
XMM image: Hasinger et al. (2001)ISO image: Fadda et al. (2001)
They are Type II QSOs
October 30, 2002 Santiago, Chile Carol Lonsdale 11
The Mid & Far-IR Universe Evolution to z~1 is
greater in IR than UVO
IR is <30% locally but dominates at z>1
ULIRGs <1% locally but major population at z>1 (SCUBA sources)
AGN account for ~20% of the CIRB
Chary and Elbaz 2001
ISO/IRAS/SCUBA
UVO
October 30, 2002 Santiago, Chile Carol Lonsdale 12
Old Stellar Populations
Slow evolution in color, line strengths, velocity dispersion of spheroids since z>~1
Stronger morphological than color evolution: red mergers (Van Dokkum)
Large spiral disks in place by z~1 (Vogt)
Van Dokkum et al. 2000; z=0.83 cluster Zf for spheroids vs. assembly ?
October 30, 2002 Santiago, Chile Carol Lonsdale 13
IRAC & Old Stellar Populations
Sawicki 2002
IRAC will sample low-mass stellar populations in high-z galsand measure baryonic mass to high-z
October 30, 2002 Santiago, Chile Carol Lonsdale 14
Space InfraRed Telescope Facility M. Werner, Project Scientist
85 cm telescope
Diffraction limited at 6.5µm
Delta launch: April 15th 2003
Earth-trailing orbit No eclipses or occultations, continuous operations
only seven distinct observing modes (AOTs) Single instrument campaigns last 3-to-10 days
Science Center at IPAC, Caltech Community Time >75%
Cycle 1 Call November 8
Legacy data are non-proprietary:
Archive opens early 2004
October 30, 2002 Santiago, Chile Carol Lonsdale 15
SIRTF: MIPS
24, 70 & 160 µm imaging, G. Rieke, PI
U Arizona
Freeze-frame scanning with secondary mirror
λ(µm)
Array size
Detector FOV Pixsize
24 128x128 Si:As 5' x 5 ' 7"
70 32x32 Ge:Ga 5' x 5 ' 17 "
160 2x20 Ge:Ga(stressed)
0.5x5 ' 40 "
October 30, 2002 Santiago, Chile Carol Lonsdale 16
SIRTF: IRAC
256 x 256 1.2" pixels 5' x 5'
3.6 & 4.5 µm: In:Sb
5.8 & 8.0 µm: Si:As
3.6, 4.5, 5.8, 8.0 µm imaging G. Fazio, PI, SAO
October 30, 2002 Santiago, Chile Carol Lonsdale 17
SIRTF: IRS
IRS: 5.0 – 40 µm spectroscopy, J. Houck PI, Cornell
Short Low: 5.3-14um 62-124 resolution Si:As
Short-High 10.3-19.5 600 Si:As
Long-Low 14-42 62-124 Si:Sb
Long-High 19-37 600 Si:Sb
128 x 128, all modules
October 30, 2002 Santiago, Chile Carol Lonsdale 18
The SWIRE Survey
63 square degrees all 7 SIRTF MIPS & IRAC imaging bands 851 hours – largest SIRTF Program
17.5 mJy160 m
2.75 mJy70 m
0.45 mJy24 m
32.5 Jy8.0 m
27.5 Jy5.8 m
9.7 Jy4.5 m
7.3 Jy3.6 m
SIRTF is ideally designed for detailed study of the history of star formation
IRAC is optimized for old and reddened stellar populations
MIPS is optimized for star-forming galaxies and AGN
5σ sensitivities
October 30, 2002 Santiago, Chile Carol Lonsdale 19
Galaxies in the IR
IRAC MIPS
Polletta et al 2002
r
StarsDust
October 30, 2002 Santiago, Chile Carol Lonsdale 20
GOODS: Great Observatories Origins Deep Survey Mark Dickinson (STScI) 300h 300 sq arcmin/50 sq arcmin IRAC/MIPS 24m
SINGS: The SIRTF Nearby Galaxies SurveyRob Kennicutt (U. Arizona) 512h 75 nearby galaxies
IRAC/MIPS/IRS
SWIRE: The SIRTF Wide-area Infrared Extragalactic SurveyCarol Lonsdale (IPAC/Caltech) 851h 63 sq deg; 2x106 galaxies IRAC/MIPS
SIRTF Legacy Surveys: Extragalactic
October 30, 2002 Santiago, Chile Carol Lonsdale 21
Carol Lonsdale PI IPAC, CaltechHarding E (Gene) Smith Deputy PI, ground-based program UCSDMichael Rowan-Robinson Deputy PI for Science Imperial CollegeDave Shupe Liaison Scientist SSC/IPACDeborah Padgett MIPS SSC/IPACJason Surace Data Processing/IRAC SSC/IPAC
Cong Xu Models IPACSeb Oliver Large Scale Structure Sussex University
Jim Condon VLA Survey NRAOTim Conrow System IPACHerve Dole MIPS U. ArizonaFan Fang Simulation/Models SSC/IPACAlberto Franceschini Spheroids, AGN Padua Dave Frayer MIPS SSC/IPACNick Gautier Cirrus JPLMatt Griffin Herschel/SPIRE CardiffPerry Hacking Models Vanguard Tom Jarrett Nearby Galaxies IPAC, CaltechFrank Masci MIPS 24um SSCGlenn Morrison Radio VanguardJoAnn O’Linger Disks SSCFrazer Owen Radio NRAOIsmael Perez-Fournon QSOs IAC, TenerifeMarguerite Pierre X-ray/XMM CEA, SaclayRick Puetter Pixons UCSDSteve Serjeant ELAIS U. KentGordon Stacey Molecular lines CornellMike Werner IRS JPL
October 30, 2002 Santiago, Chile Carol Lonsdale 22
SWIRE: Environment & LSS
Kauffmann et al. (1999); 21x21x8 (Mpc/h)3
red blue: increasing SFR
Resolving
Star Formation History
&
AGN Accretion
&
Spheroid Evolution
in Time and Space
in context of
Structure Formation
z=3
z=0z=1
z=2
October 30, 2002 Santiago, Chile Carol Lonsdale 23
The SWIRE Survey
24m / 70m / 160m
1 x 1 degree
Rowan-Robinson 2001
3.6 m / 8 m / 24 m
10’ x 10’
Xu et al. 2001
• 0.5 < z < 3 • 100s of ~100Mpc cells• 1000s sources in each cell• > 106 galaxies• >104 Type 1 AGN
October 30, 2002 Santiago, Chile Carol Lonsdale 24
FIELD RA
(J2000)
Dec ISSA
MJy/sr
E(B-V) Size
Sq. deg
ELAIS-S1 00h 38m 30s -44º 00' 0.42 0.008 14.0
XMM-LSS 02h 21m 00s -05º 00' 1.3 0.027 8.8
Chandra-S 03h 32m 00s -28º 16' 0.46 0.001 6.9
Lockman 10h 45m 00s +58º 00' 0.38 0.006 14.0
Lonsdale 14h 41m00s +59º 25' 0.47 0.012 6.5
ELAIS-N1 16h 11m00s +55º 00' 0.44 0.007 8.8
ELAIS-N2 16h 36m48s +41º 01‘ 45" 0.42 0.007 4.3
SWIRE Fields
7 large fields: large scale sizes combat cosmic variance
October 30, 2002 Santiago, Chile Carol Lonsdale 25
Field Selection Strategy
1. Low extinction, cirrus noise: extensive survey for fields with
I100µm < 0.5MJy/Sr; b > 40º, β > 40º. See:
http://star-www.cpes.susx.ac.uk/~sjo/swire/I100/index2.html
2. Avoid bright stars, galaxies, radio sources
3. Favor prior or planned complementary surveys with either:• large investment of time, or • large effort to repeat
October 30, 2002 Santiago, Chile Carol Lonsdale 26
Minimize NH & Cirrus
B100 Contours at 1 and 2 MJy/sr
CHANDRA-S
ELAIS-S1 XMM-LSS
LOCKMANELAIS-N1
LONSDALE
ELAIS-N2
Schlegel et al. 1998 DIRBE-calibrated IRAS 100m map
October 30, 2002 Santiago, Chile Carol Lonsdale 27
Fields We Didn’t Select
Groth Strip SSA68
October 30, 2002 Santiago, Chile Carol Lonsdale 28
Cirrus Holes Too Small
HDF-South HDF-North
October 30, 2002 Santiago, Chile Carol Lonsdale 29
SWIRE Survey Fields
Lockman Hole ELAIS-N1
IRAS 100 m images
October 30, 2002 Santiago, Chile Carol Lonsdale 30
SWIRE Survey Fields
ELAIS N2
ELAIS S1
October 30, 2002 Santiago, Chile Carol Lonsdale 31
CDF-S
Lonsdale Hole
SWIRE Survey Fields
October 30, 2002 Santiago, Chile Carol Lonsdale 32
SWIRE Survey Fields
XMM-LSS
SWIRE
XMM-LSS
M. Pierre, PI
LH
Xray surveys are typically very small (eg: Lockman Hole survey below).
The large XMM-LSS survey is unique
October 30, 2002 Santiago, Chile Carol Lonsdale 33
Next Generation “Cosmic Windows”
SWIRE is defining the best LARGE cirrus holes on sky which will be observed by many other survey instruments:
GALEX deep imaging survey: AB=25.5 mag UV 1350-3000Å, 50 cm telescope imaging and grism, 2003 launch (C. Martin)
SWIRE-GALEX very powerful in combination
October 30, 2002 Santiago, Chile Carol Lonsdale 34
Flu
x d
ensi
ty (
Jy)
10 100 1000
1012L
0.5
10
1
0.1
0.015
3
1
Z = 0.1
SP
IRE
(m)
Herschel/SPIRE 250, 350, 500μm imaging ~ 2007 launch
M. Griffin,Cardiff
October 30, 2002 Santiago, Chile Carol Lonsdale 35
Next Generation “Cosmic Windows”
VLA proposal 40μJy 20cm J. Condon
SWIRE/GALEX/XMM-LSS optical ground-based
Imaging Spectroscopy
Deep J & K (partial SWIRE field coverage); K=21 A. Lawrence
October 30, 2002 Santiago, Chile Carol Lonsdale 36
SWIRE SIRTF Observations
Lockman Field, incomplete map to illustrate strategy (4.0° x 3.75°)
MIPS Scan legs
GTO Deep Survey (2°x 0.25°)
IRAC Maps
October 30, 2002 Santiago, Chile Carol Lonsdale 37
SIRTF ObservationsTwo epochs & both instruments in one campaign
IRAC:• 2 dithers• 4x30 sec per point
MIPS:• 2 x 10 x 4 sec at 24 & 70μm• 2 x 1 x 4 sec at 160μm
October 30, 2002 Santiago, Chile Carol Lonsdale 38
Six-band simulation
3.6 4.5 5.8
8.0 24 70
Model of Xu et al, 2001, 2002
• 24μm LF
• 840 SEDs
• Starbursts
• Spirals
• AGN
• Ellipticals
5 x 5 arcmin
October 30, 2002 Santiago, Chile Carol Lonsdale 39
Mosiaced IRAC Simulation
0.2 sq degEROs
Las Campanas NIR HDF Survey (Chen et al. 2001).
LCIRS limit
October 30, 2002 Santiago, Chile Carol Lonsdale 40
SWIRE Starbursts & AGN
1 sq degree SWIRE survey (excluding spheroids)
8μm 7200 sources
24μm 3300
70μm 2700
Warm AGN: 1000
Starbursts & obscured AGN: 4500
October 30, 2002 Santiago, Chile Carol Lonsdale 41
Bias and SFR-Density Field
Would like to know evolution of the
mass density field
What we measure is the galaxy
density field:
δg = bδm
Complex astrophysics governs galaxy
light
– Did much star formation
happened early & fast in bursts ?
– Role of feedback ?Somerville et al 2001
(who conclude extinction & collisional starbursts important)
October 30, 2002 Santiago, Chile Carol Lonsdale 42
Bias and SFR-Density Field
So measure evolution of bias of
different populations:– Starburst vs Passive systems
– Young vs older starbursts
– Disks vs spheroids
– AGN vs starbursts
– Etc.
SWIRE is ideal
– Measures all populations
in same volume cells
optical IRAS
Oliver et al 1996
October 30, 2002 Santiago, Chile Carol Lonsdale 43
Additional Science
• Hundreds of field brown dwarfs, especially T (“methane”) dwarfs
• 50-60 circumstellar debris disks (to 100 pc), and HR4796A analogs to 1kpc
•Thermal emission at 8 and 24m from main belt asteroids as small as 1km
• Serendipitous discoveries; rare objects to 1-in-104 to 1-in-106
October 30, 2002 Santiago, Chile Carol Lonsdale 44
Bi-yearly releases: • source lists• fits images• cross-band identifications • coverage maps• documentation • ancillary data and cross-ids
Successive deliveries: Increased area coverageDecreasing SNR levels Cross-matching, increasing numbers of bands Image mosaics over increasing area
Data Products and Archive Services
SWIRE Data: Non-proprietary
1st release: early 2004