The µJy Sky and the Radio-FIR relation vs. z

1 Frazer Owen NRAO EVLA Vision December 17, 2008

Outline of Talk

1) µJy radio properties 2) Radio-FIR relation vs z 3) Implications, future directions Frazer Owen NRAO EVLA Vision December 17, 2008 2

Short List of Collaborators

• G. Morrison (UH) • M. Pannella, V. Strazzullo, W-H. Wang (NRAO) • M. Polletta (Milan) • C. Lonsdale (NRAO) • A. Baker, Matt Klimek (Rutgers) • R. Ivison, A. Biggs (ROE) • D. Shupe (Herschel) • B. Wilkes (CFA) • R. Kilgard (Wesleyan) Frazer Owen NRAO EVLA Vision December 17, 2008 3

SWIRE Deep Field: 1046+59

• Deepest existing radio survey at 20cm (rms 2.7µJy), also 50cm (10µJy), 90cm (70µJy) • GALEX UV, ground-based optical, NIR, Spitzer IRAC, confusion-limited MIPS (24,70,160 µm),MAMBO 1.2mm, Chandra imaging, spectroscopy.

• XMM, SCUBA2, Herschel HerMES 100 500µm (1 st priority) to come.

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Radio Source Photo-z’s

UgrizJHK3.6µ4.5µ Frazer Owen NRAO EVLA Vision December 17, 2008 Pannella/Strazzullo 6

Radio Luminosities vs. z

Majority of sources > 10^23 W/Hz, more luminous than Arp 220 Frazer Owen NRAO EVLA Vision December 17, 2008 7

1) µJy sources are resolved median size ~ 1 arcsec or ~10 kpc, unlike local ULIRGs < 100pc.

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Median Sizes from 1046+59 Large median size for sources continues down to bottom of the survey.

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Huyng et al 2005

20cm Log N –Log S

Log N-log S continues flat to bottom of survey. 6 sources/sq arcmin.

Frazer Owen NRAO EVLA: 10X deeper: natural confusion ?

EVLA Vision December 17, 2008 10

Radio SF or AGN ?

M84: AGN (Mechanical Energy) M82: SF Frazer Owen NRAO Both ~ galaxy size, but different relation to optical light. EVLA Vision December 17, 2008 11

Relation of Radio and Optical Brightness distributions (GOODS-N) Frazer Owen NRAO EVLA Vision December 17, 2008 12

Radio SF vs. AGN

Locally, AGN/SF luminosity functions cross at 10^23 W/Hz.

<10^23 SF >10^23 AGN Frazer Owen NRAO Condon et al 2002 EVLA Vision December 17, 2008 13

Generic Radio/FIR Spectrum Frazer Owen NRAO EVLA Vision December 17, 2008 14

Radio-FIR Relation

Frazer Owen NRAO For SF q=2.3

σ(q)~0.2

Condon et al 2002 EVLA Vision December 17, 2008 15

ULIRGs ( Ultraluminous Infrared Galaxies ) L_FIR > 10^12 L_sun Local examples have radio size < 100pc (LIRGs > 10^11 L_sun) Frazer Owen NRAO Arp220 L_20cm=2.3x10^23 W/Hz L_FIR=1.2x10^12 L_sun EVLA Vision December 17, 2008 16

Radio-FIR Relation vs. z from Stacking Spitzer MIPS data • 24, 70 and 160 µm sources stacked at the radio source positions in ranges of L_20cm and z.

• 160/70 µm ratio and error calculated.

• Using redshifted templates with different dust temperatures, rest-frame: T(dust), L_FIR and q=log(L_20cm/L_FIR) are calculated.

24µ 70µ 160µ Frazer Owen NRAO EVLA Vision December 17, 2008 17

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Best fit opt/NIR SEDs Strazzullo et al (2009) Frazer Owen NRAO EVLA Vision December 17, 2008 24

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Conclusions/Speculations

• Star-formation and AGN activity go together: composites • Relation of AGN activity to evolutionary sequence still unclear but probably not related by a simple, one-time event. Too many star-forming galaxies with AGN evidence. • Deeper Herschel, XMM, EVLA data should make the picture clearer. • Deep EVLA imaging will probably be dominated by more extreme star-forming objects. May reach natural confusion.

• Higher resolution radio observations from EVLA, eMerlin and SKA may be most productive path for more understanding.

• Need new imaging algorithms for EVLA /eMerlin to make deep, wide-field images.

26 Frazer Owen NRAO EVLA Vision December 17, 2008