1 / 26

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

The µJy Sky and the Radio-FIR relation vs. z. 1) µJy radio properties Radio-FIR relation vs z 3) Implications, future directions. Outline of Talk. G. Morrison (UH) M. Pannella, V. Strazzullo, W-H. Wang (NRAO) M. Polletta (Milan) C. Lonsdale (NRAO) A. Baker, Matt Klimek (Rutgers)

halen
Télécharger la présentation

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

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. The µJy Sky and the Radio-FIR relation vs. z EVLA Vision December 17, 2008

  2. 1) µJy radio properties • Radio-FIR relation vs z 3) Implications, future directions Outline of Talk EVLA Vision December 17, 2008

  3. 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) Short List of Collaborators EVLA Vision December 17, 2008

  4. 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 (1st priority) to come. SWIRE Deep Field: 1046+59 EVLA Vision December 17, 2008

  5. EVLA Vision December 17, 2008

  6. Pannella/Strazzullo Radio Source Photo-z’s UgrizJHK3.6µ4.5µ EVLA Vision December 17, 2008

  7. Radio Luminosities vs. z Majority of sources > 10^23 W/Hz, more luminous than Arp 220 EVLA Vision December 17, 2008

  8. 1) µJysources are resolvedmedian size ~ 1 arcsecor ~10 kpc,unlike local ULIRGs < 100pc. EVLA Vision December 17, 2008

  9. Median Sizes from 1046+59 Large median size for sources continues down to bottom of the survey. EVLA Vision December 17, 2008

  10. Log N-log S continues flat to bottom of survey. 6 sources/sq arcmin. 20cm Log N –Log S Huyng et al 2005 EVLA: 10X deeper: natural confusion ? EVLA Vision December 17, 2008

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

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

  13. Condon et al 2002 Radio SF vs. AGN Locally, AGN/SF luminosity functions cross at 10^23 W/Hz. <10^23 SF >10^23 AGN EVLA Vision December 17, 2008

  14. Generic Radio/FIR Spectrum EVLA Vision December 17, 2008

  15. For SF q=2.3 σ(q)~0.2 Radio-FIR Relation Condon et al 2002 EVLA Vision December 17, 2008

  16. 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 EVLA Vision December 17, 2008

  17. 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 Radio-FIR Relation vs. z from Stacking Spitzer MIPS data EVLA Vision December 17, 2008

  18. EVLA Vision December 17, 2008

  19. EVLA Vision December 17, 2008

  20. EVLA Vision December 17, 2008

  21. EVLA Vision December 17, 2008

  22. EVLA Vision December 17, 2008

  23. EVLA Vision December 17, 2008

  24. Best fit opt/NIRSEDsStrazzullo et al(2009) EVLA Vision December 17, 2008

  25. 5) X-rays EVLA Vision December 17, 2008

  26. 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. Conclusions/Speculations EVLA Vision December 17, 2008

More Related