the$changing$life$of$agn$and$their$role$ …gee/gee2/ppts/gee2_bardelli.pdf · blue: non-passive...
TRANSCRIPT
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The Changing life of AGN and their role In the Feedback
Sandro Bardelli
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OPTICAL PROPERTIES OF RADIOGALAXIES IN THE VLA-‐VVDS SURVEY +zCOSMOS
Sandro Bardelli INAF-‐OABo
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Feedback required
From Hopkins
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WHAT IS AN AGN? From the observaQonal point of view
X-‐Ray
OpQcal
IR
Radio
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Hickox et al. (2009) AEGIS survey 0.2<z<0.8
Overlap between AGN classes
CorrelaQon funcQon
Bias relaQve to all galaxies
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Two type of AGN “modes”
1) Quasar mode: cold disk gas is driven onto central black hole (X-‐Ray emission)
2) Radio mode: sub-‐Eddington accreQon from hot gas Efficient at late Qmes, ongoing heaQng source Mechanism observed in central part of clusters (Bubbles) Radio emission
See Croton et al. (2006)
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If there is AGN Feedback that stop the star formaQon, there should be a clear co-‐evoluQon between AGN and normal galaxies
We know how evolves the stellar mass funcQon (Micol talk), but AGN?
DIFFICULTIES
1)What type of AGN (Spectral, X-‐ray, Radio ……) 2) Occurrence (different life Qme ) 3) Different detectability
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Dying sequence
Galaxies from zCOSMOS 20K sample (z<1)
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The RADIO SIDE
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VLA-‐COSMOS (Schinnerer et al. ,2007; 2010)
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1.4 GHz over 2x2 deg2 ~2417 sources 1.5 arcsec resoluQon to 11µ Jy
VLA-‐COSMOS Bondi et al. (2008)
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EMISSION FROM AGNE
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A 6cm MERLIN/VLA image of nearby starburst galaxy M82. The discrete sources are mostly supernova remnants with ages less than 1000 years and compact HIIregions. The non-‐thermal extended background is mainly due to relaQvisQc electrons generated by older remnants M>8 M0 Qme ~10**8 yrs
Radio emission associated to late type galaxies
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COLORS DISTRIBUTION
Red points: Type 1 radiogalaxies
Blue points: Type 3+4 radiogalaxies
NORMALLY the Division between AGN and star forming is done on the basis of optical properties
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673 radio sources with spectroscopic sample
140 AGN AGN region
Star forming relaQon
Bardelli et al. (2010) A new method for idenQfying Radio AGN
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XMM perspecQve
Lflux limit of ~1.7 10-‐15 erg cm-‐2 s-‐1 in the 0.5-‐2 keV band over 1.92 deg2
CappelluQ et al. (2009)
282 X-‐ray sources in zCOSMOS and z<1.0
243 AGN 34 type 1
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PASSIVE AGN
NON-PASSIVE AGN
64 passive radio 28 Xray
49 passive radio 105 Xray
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Hickox et al. (2009) Signature of evolution?
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ENVIRONMENT
High density environment low density
environment
1) Nearest Neighbour StaQsQc Kovac et al. (2008)
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Red: Passive radio AGN
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Blue: Non-passive radio AGN
Red: Passive radio AGN ProbKS pass-nonpass=0.00002 ProbKS pass-Xray = 10-5 ProbKS nonpass-Xray=0.53
SAME ENVIRONMENT NON-PASSIVE AND X_RAY
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Green: X-ray AGN ProbKS pass-nonpass=0.00002 ProbKS pass-Xray = 10-5 ProbKS nonpass-Xray=0.53
SAME ENVIRONMENT NON-PASSIVE AND X_RAY
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PASSIVE AGN
NON-PASSIVE AGN
64 passive radio 28 Xray
49 passive radio 105 Xray
What about Non emitting Galaxies?
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Passive PKS=10-5 nonPassive ProbKS=0.28 Xray ProbKS=0.89
Overdensity distribution with respect the Parent population
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Passive PKS=10-5 nonPassive ProbKS=0.28 Xray ProbKS=0.89
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Passive PKS=10-5 nonPassive ProbKS=0.28 Xray ProbKS=0.89
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XMM Groups Finoguenov et al. (2011)
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XMM Groups Finoguenov et al. (2011)
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XMM Groups Finoguenov et al. (2011)
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36 radio AGN in groups 30 are passive (red) 21 are the most massive galaxies (yellow)
28 xray AGN are in groups (black) 9 are the most massive (green crosses)
Knobel et al. (in prep)
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Morphologies Nair et al. (in prep)
12 %
12 %
38 %
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10 %
18%
52 %
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13 %
11 %
20 %
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Radio AGN
Increaese of num With decreasing z
Control sample
radio sample
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RADIO AGN
Different masses ranges for passive and non passive AGN
Solid points: all galaxies Open points radio sources
Red:passive blue:non passive
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Passive AGN and Galaxies : Mass range [10.55 – 11.45]
Diff radio 11.23 10 -‐5 diff control 23.5 10-‐5
RATIO= 0.47
RaQo of stellar masses lowz= 0.31 highz=0.10
Higher fracQon of AGN transit to passive
Non Passive Mass range [9,95-‐10.85] Diff radio 5.2 10-‐5 diff control 4.38 10-‐4 RATIO =0.12 consistent with stellar masses raQos Constant flow?
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+6.5 10-‐5
-‐2.5 10-‐5
+4.8 10-‐5
+9.28 10-‐6
R~1
R~0.26
R~0.02 +4.3 10-‐5 R~0.20
R~0.02
+9.28 10-‐6
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Red passive Blue non-‐passive
As a funcQon of Overdensity (with all the caveats)
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Luminosity-‐Stellar mass RaQo (vmax corrected)
Increase of low lum radio AGN
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Xray AGN same mass range As non passive radio AGN
X-ray AGN
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Conclusions
-‐Non passive radio AGN and type 2 x-‐ray AGN occupy same Stellar mass range and environment same populaQon
-‐constat flow of both radio non passive and x-‐ray AGN With respect the general populaQon (i.e. raQos are constant)
-‐New passive galaxies have almost all a central radio AGN And become ellipQcals at high densiQes but with lower radio power with respect to pre-‐exisQng AGN