Star formation and black hole activity evolution from deep radio survey
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Transcript of Star formation and black hole activity evolution from deep radio survey
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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
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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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Margherita Bonzini
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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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)
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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?
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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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Margherita Bonzini
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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Margherita Bonzini
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
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- U-B rest-frame colors- Stellar masses
(AGN+galaxy SED fitting)- Sersic index (HST images)
Margherita Bonzini
Host galaxy properties
(Bonzini et al., 2013)
SFGRQ AGNRL AGN
SFGRQ AGNRL AGN
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Margherita Bonzini
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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Margherita Bonzini
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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Margherita Bonzini
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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Margherita Bonzini
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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Margherita Bonzini
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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Margherita Bonzini
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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Margherita Bonzini
SFR vs Stellar Mass
z < 1 1 < z < 2.5
Elbaz+07Daddi+07
Flux density
limit
SFGRQ AGNRL AGN
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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
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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
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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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Margherita Bonzini
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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Margherita Bonzini
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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Margherita Bonzini
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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Margherita Bonzini
Summary & OutlookJVLA
MeerKAT
SKA