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,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)

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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)

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

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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

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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!

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Summary & OutlookJVLA

MeerKAT

SKA