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The µJy Sky and the Radio-FIR relation vs. z
Frazer Owen NRAO EVLA Vision December 17, 2008
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Outline of Talk 1) µJy radio properties Radio-FIR relation vs z
3) Implications, future directions Frazer Owen NRAO EVLA Vision December 17, 2008
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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
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SWIRE Deep Field: 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 µm (1st priority) to come. Frazer Owen NRAO EVLA Vision December 17, 2008
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Frazer Owen NRAO EVLA Vision December 17, 2008
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Radio Source Photo-z’s
UgrizJHK3.6µ4.5µ Pannella/Strazzullo Frazer Owen NRAO EVLA Vision December 17, 2008
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Radio Luminosities vs. z
Majority of sources > 10^23 W/Hz, more luminous than Arp 220 Frazer Owen NRAO EVLA Vision December 17, 2008
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1) µJy sources are resolved median size ~ 1 arcsec or ~10 kpc, unlike local ULIRGs < 100pc.
Frazer Owen NRAO EVLA Vision December 17, 2008
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Median Sizes from Large median size for sources continues down to bottom of the survey. Frazer Owen NRAO EVLA Vision December 17, 2008
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20cm Log N –Log S Log N-log S continues flat to bottom of survey.
Huyng et al 2005 Log N-log S continues flat to bottom of survey. 6 sources/sq arcmin. EVLA: 10X deeper: natural confusion ? Frazer Owen NRAO EVLA Vision December 17, 2008
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Radio SF or AGN ? M84: AGN (Mechanical Energy) M82: SF Both ~ galaxy size, but different relation to optical light. Frazer Owen NRAO EVLA Vision December 17, 2008
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Relation of Radio and Optical Brightness distributions (GOODS-N)
Frazer Owen NRAO EVLA Vision December 17, 2008
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Radio SF vs. AGN Locally, AGN/SF luminosity functions cross at 10^23 W/Hz. <10^23 SF >10^23 AGN Condon et al 2002 Frazer Owen NRAO EVLA Vision December 17, 2008
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Generic Radio/FIR Spectrum
Frazer Owen NRAO EVLA Vision December 17, 2008
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Radio-FIR Relation For SF q=2.3 σ(q)~0.2 Frazer Owen NRAO EVLA Vision
Condon et al 2002 Frazer Owen NRAO EVLA Vision December 17, 2008
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ULIRGs (Ultraluminous Infrared Galaxies)
L_FIR > 10^12 L_sun Local examples have radio size < 100pc (LIRGs > 10^11 L_sun) Arp220 L_20cm=2.3x10^23 W/Hz L_FIR=1.2x10^12 L_sun Frazer Owen NRAO EVLA Vision December 17, 2008
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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 µ µ Frazer Owen NRAO EVLA Vision December 17, 2008
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Frazer Owen NRAO EVLA Vision December 17, 2008
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Frazer Owen NRAO EVLA Vision December 17, 2008
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Frazer Owen NRAO EVLA Vision December 17, 2008
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Frazer Owen NRAO EVLA Vision December 17, 2008
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Frazer Owen NRAO EVLA Vision December 17, 2008
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Frazer Owen NRAO EVLA Vision December 17, 2008
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Best fit opt/NIR SEDs Strazzullo et al (2009)
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5) X-rays Frazer Owen NRAO EVLA Vision December 17, 2008
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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. Frazer Owen NRAO EVLA Vision December 17, 2008
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