SWIRE Octiber 30, 2002Santiago, Chile1 The SIRTF Wide-Area Infra-Red Extragalactic Survey Carol J....

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


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


IR Galaxy Populations: LIRGs

Interactions/mergers

IR does not coincide with UV-optical – younger stellar

population


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


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


IR Dominates the Global Backgrounds

50% or more is in IR

Franceschini et al 2001


CIRB Resembles M82

Elbaz et al 2002

Franceschini et al 2001


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


Deep ISO 15µm & X-ray

XMM image: Hasinger et al. (2001)ISO image: Fadda et al. (2001)

They are Type II QSOs


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


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 ?


IRAC & Old Stellar Populations

Sawicki 2002

IRAC will sample low-mass stellar populations in high-z galsand measure baryonic mass to high-z


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


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 "


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


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


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


Galaxies in the IR

IRAC MIPS

Polletta et al 2002

r

StarsDust


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


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


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


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


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


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


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


Fields We Didn’t Select

Groth Strip SSA68


Cirrus Holes Too Small

HDF-South HDF-North


SWIRE Survey Fields

Lockman Hole ELAIS-N1

IRAS 100 m images


SWIRE Survey Fields

ELAIS N2

ELAIS S1


CDF-S

Lonsdale Hole

SWIRE Survey Fields


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


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


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


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


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


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


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


Mosiaced IRAC Simulation

0.2 sq degEROs

Las Campanas NIR HDF Survey (Chen et al. 2001).

LCIRS limit


SWIRE Starbursts & AGN

1 sq degree SWIRE survey (excluding spheroids)

8μm 7200 sources

24μm 3300

70μm 2700

Warm AGN: 1000

Starbursts & obscured AGN: 4500


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)


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


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


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

SWIRE Octiber 30, 2002Santiago, Chile1 The SIRTF Wide-Area Infra-Red Extragalactic Survey Carol J....

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