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

AGN & hosts co-evolution

Margherita Bonzini

“quenched” passive

SFR

Main Sequence

Stellar mass

sSFRMS declines by 20 since z = 2

“Starburst”

• What triggers the starburst activity?

• What quenches the star formation?

• Where are the AGN in this plane?

(yesterday talks)

( Noeske+07, Daddi+07, Elbaz+07, Peng+10, Lilly+13 )

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A radio perspective • Observed AGN feedback : “radio mode”

• Unaffected by dust obscuration

• Tons of data are coming!

ASKAP JVLA

SKA

(Fabian & Sanders 2009)

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Jets Star Formation

The extragalactic faint radio sky is a complex mixture of different emission mechanisms

A radio perspective

(e.g., Condon+84, Seymour+04, Smolčić+08, Padovani+09, Bonzini+13)

Margherita Bonzini

Jets Star Formation

The extragalactic faint radio sky is a complex mixture of different emission mechanisms

A radio perspective

(e.g., Condon+84, Seymour+04, Smolčić+08, Padovani+09, Bonzini+13)

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?

Sample & ancillary data

Margherita Bonzini

30 arcmin

1.4 GHz / VLA • ~ 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 Optical-infrared counterparts: 94%

with redshift: 78% (40% spectroscopic), <z>≈1(Bonzini et al., 2012)

E-CDFS

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AGN or SFG?

( Donley+12)

Lx >1042 erg s-1 Power law

sources

AGNAGN

SFG locus

(Sargent+10)

• Fir/radio ratio• X-ray

luminosity• Mid-IR colors

q24

(Bonzini+13)

( Szokoly+04)

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The faint radio sky

(Bonzini et al., 2013)

63% SFG 20% RQ AGN 17% RL AGN

Below 0.1mJy:• SFGs are the

majority• RQ AGNs

outnumber RL AGNs

- U-B rest-frame colors- Stellar masses

(AGN+galaxy SED fitting)- Sersic index (HST images)

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Host galaxy properties

(Bonzini et al., 2013)

SFGRQ AGNRL AGN

SFGRQ AGNRL AGN

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Host galaxy properties

(Bonzini et al., 2013)

SFGRQ AGNRL AGN

SFGRQ AGNRL AGN

1. RQ and RL are two evolutionary phases in the AGN-galaxy evolution

2. Radio emission in RQ AGNs from star formation rather then from accretion

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Radio-FIR correlation (RFC)

(Bonzini et al., in prep)

The RFC holds for radio selected SFG up to z=3Radio power and LFIR both good SFR tracers for SFGs

PACS/Herschel data (PI: D. Lutz)

SFGs ONLY

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SFR comparison

(Bonzini et al., in prep)

Good agreement for SFG and RQ AGN

RL AGN off correlation because of jets contribution to the radio power

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SFR comparison

(Bonzini et al., in prep)

Good agreement for SFG and RQ AGN

5% outliers due to misclassification

RL AGN off correlation because of jets contribution to the radio power

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SFR comparison

(Bonzini et al., in prep)

Good agreement for SFG and RQ AGN

Large points:Stacking results

FIR brightness dependence?

Stacking analysis for PACS undetected

sources

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SFR comparison

(Bonzini et al., in prep)

Good agreement for SFG and RQ AGN

Large points:Stacking results

FIR brightness dependence?

Stacking analysis for PACS undetected

sources

Radio emission in RQ AGN

mainly due to star formation

Margherita Bonzini

SFR vs Stellar Mass

z < 1 1 < z < 2.5

Elbaz+07Daddi+07

Flux density

limit

SFGRQ AGNRL AGN

SFR vs Stellar Mass

z < 1 1 < z < 2.5

Elbaz+07Daddi+07

Starburst: 0.6 dex above the MS (Rodighiero+11)

Two regimes of SF activity: starburst and MS galaxies (Sargent+12)

(see Bethermin’s talk)

SFGRQ AGNRL AGN

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

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

Ongoing quenching?

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Cosmic SF history with radio surveys

The fraction of starburst increases up to z~1 and then flattens (Sargent+12, Hopkins+10)

One example:

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Need for deep and large radio surveys

(Based on the model of Bethermin+12, Sargent+12)

Fraction of starburst as a function of the radio flux density limit

Our VLA survey

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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

Optical and IFU spectroscopy (KMOS) to look for feedback signature

Excitation and accretion state

SFR for AGNs hosts!

Margherita Bonzini

Summary & OutlookJVLA

MeerKAT

SKA