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Star formation and black hole activity evolution from deep radio survey

Star formation and black hole activity evolution from deep radio survey . Margherita Bonzini Collaborators: V. Mainieri , P. Padovani , N. Miller, K. I. Kellermann , P. Tozzi , , P. Rosati , S. Vattakunnel , A. Bongiorno ,

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Star formation and black hole activity evolution from deep radio survey

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  1. Star formation and black hole activity evolution from deep radio survey Margherita Bonzini Collaborators: V. Mainieri, P. Padovani, N. Miller, K. I. Kellermann, P. Tozzi, , P. Rosati, S. Vattakunnel, A. Bongiorno, P. Andreani, D. Rosario, S. Berta, D. Lutz., M. Bethermin

  2. AGN & hosts co-evolution (yesterday talks) “Starburst” sSFRMS declines by 20since z = 2 SFR Main Sequence • What triggers the starburst activity? • What quenches the star formation? • Where are the AGN in this plane? “quenched” passive Stellar mass ( Noeske+07, Daddi+07, Elbaz+07, Peng+10, Lilly+13 ) Margherita Bonzini

  3. A radio perspective • Observed AGN feedback : “radio mode” • Unaffected by dust obscuration • Tons of data are coming! JVLA ASKAP (Fabian & Sanders 2009) SKA Margherita Bonzini

  4. A radio perspective The extragalactic faint radio sky is a complex mixture of different emission mechanisms (e.g., Condon+84, Seymour+04,Smolčić+08, Padovani+09, Bonzini+13) Jets Star Formation Margherita Bonzini

  5. A radio perspective The extragalactic faint radio sky is a complex mixture of different emission mechanisms (e.g., Condon+84, Seymour+04,Smolčić+08, Padovani+09, Bonzini+13) Jets Star Formation Not only radio-loud (RL) AGNs (>10% of all AGNs) but also radio-quiet (RQ) AGNs What is the origin of radio emission in RQ AGNs? Margherita Bonzini

  6. Sample & ancillary data E-CDFS • ~ 900 sources 5σ flux density limit: ~30 μJy • (Miller+13) • X-ray: Chandra: 250 ks + 4 Ms(Lemer+05, Xue+11) • Optical: GEMS/ACS, VLT/FORS + ISAAC, Subaru, NTT/SOFI, ESO2.2m/WFI, HST/ACS • Mid infrared: Spitzer/IRAC+MIPS 1.4 GHz / VLA 30 arcmin Optical-infrared counterparts: 94% with redshift: 78% (40% spectroscopic), <z>≈1 (Bonzini et al., 2012) Margherita Bonzini

  7. AGN or SFG? • Fir/radio ratio • X-ray luminosity • Mid-IR colors SFG locus q24 (Sargent+10) Power law sources Lx >1042 erg s-1 AGN AGN ( Szokoly+04) ( Donley+12) Margherita Bonzini (Bonzini+13)

  8. The faint radio sky 63% SFG 20% RQ AGN 17% RL AGN • Below 0.1mJy: • SFGs are the majority • RQ AGNs outnumber RL AGNs (Bonzini et al., 2013) Margherita Bonzini

  9. Host galaxy properties SFG RQ AGN RL AGN SFG RQ AGN RL AGN • - U-B rest-frame colors • Stellar masses (AGN+galaxy SED fitting) • Sersicindex (HST images) Margherita Bonzini (Bonzini et al., 2013)

  10. Host galaxy properties SFG RQ AGN RL AGN SFG RQ AGN RL AGN RQ and RL are two evolutionary phases in the AGN-galaxy evolution Radio emission in RQ AGNs from star formation rather then from accretion Margherita Bonzini (Bonzini et al., 2013)

  11. Radio-FIR correlation (RFC) SFGs ONLY PACS/Herschel data (PI: D. Lutz) The RFC holds for radio selected SFG up to z=3 Radio power and LFIR both good SFR tracers for SFGs Margherita Bonzini (Bonzini et al., in prep)

  12. SFR comparison Good agreement for SFG and RQ AGN RL AGN off correlation because of jets contribution to the radio power Margherita Bonzini (Bonzini et al., in prep)

  13. SFR comparison Good agreement for SFG and RQ AGN 5% outliers due to misclassification RL AGN off correlation because of jets contribution to the radio power Margherita Bonzini (Bonzini et al., in prep)

  14. SFR comparison Good agreement for SFG and RQ AGN FIR brightness dependence? Stacking analysis for PACS undetected sources Large points: Stacking results Margherita Bonzini (Bonzini et al., in prep)

  15. SFR comparison Good agreement for SFG and RQ AGN FIR brightness dependence? Stacking analysis for PACS undetected sources Large points: Stacking results Radio emission in RQ AGN mainly due to star formation Margherita Bonzini (Bonzini et al., in prep)

  16. SFR vsStellar Mass Daddi+07 Flux density limit Elbaz+07 SFG RQ AGN RL AGN z < 1 1 < z < 2.5 Margherita Bonzini

  17. SFR vsStellar Mass Daddi+07 Elbaz+07 SFG RQ AGN RL AGN z < 1 1 < z < 2.5 Two regimes of SF activity: starburst and MS galaxies (Sargent+12) Starburst: 0.6 dex above the MS (Rodighiero+11) (see Bethermin’s talk)

  18. AGN content across the MS Passive MS Starburst • Not all the RL AGN hosts are quenched (Caldwell’s poster) • The majority (75%) of RQ AGN are hosted in MS galaxies (Silverman’s, Polletta’s.. talk) • The relative fraction of AGN increases as the sSFR increases

  19. AGN content across the MS Passive MS Starburst Ongoing quenching? • Not all the RL AGN hosts are quenched (Caldwell’s poster) • The majority (75%) of RQ AGN are hosted in MS galaxies (Silverman’s, Polletta’s.. talk) • The relative fraction of AGN increases as the sSFR increases

  20. Cosmic SF history with radio surveys One example: The fraction of starburst increases up to z~1 and then flattens (Sargent+12, Hopkins+10) Margherita Bonzini

  21. Need for deep and large radio surveys Fraction of starburst as a function of the radio flux density limit Our VLA survey (Based on the model of Bethermin+12, Sargent+12) Margherita Bonzini

  22. Summary & Outlook • Deep radio surveys detect the same populations (SFG & RQ AGNs) observed in other bands, not only RL AGNs • Host galaxy properties vs radio loudness: from RQ AGN (late type, Mstar~1010.5M) to RL AGN (early type, Mstar~1011M) • Radio emission in RQ AGN due to SF • AGN content as a function of the distance from the MS • Deep radio surveys as tool to study the cosmic SFH Excitation and accretion state SFR for AGNs hosts! Optical and IFU spectroscopy (KMOS) to look for feedback signature Margherita Bonzini

  23. Summary & Outlook JVLA MeerKAT SKA Margherita Bonzini

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