Post on 22-Feb-2016
description
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
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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
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