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