radioagn host galaxy properties out to z~5hiddenmonsters/talks/delveccio.pdf · radio agn in the...
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Dartmouth – Hidden Monsters August 10th, 2016
RadioAGN host galaxy properties RadioAGN host galaxy properties out to z~5out to z~5
Ivan Delvecchio (University of Zagreb)
On behalf of:V. Smolčić, G. Zamorani, C. Del P. Lagos, S. Berta, J. Delhaize, N. Baran, D. Alexander, D. Rosario,
V. GonzalezPerez, O. Ilbert, C. Lacey, O. Le Fèvre, O. Miettinen, M. Bondi, C. Carilli, P. Ciliegi, K. Mooley, M. Novak, E. Schinnerer, M. Aravena, P. Capak, F. Civano, N. Fanidakis, N. HerreraRuiz,
A. Karim, C. Laigle, S. Marchesi, H. McCracken, E. Middleberg, M. Salvato and L. Tasca
Are Are radioradio AGN special? AGN special?
Hickox et al. (2009)
Goulding et al. (2014)
More massive
Red
der
Radio AGN in the local Universe: Radio AGN in the local Universe: a twofold populationa twofold population
HERAGNHERAGN vs vs LERAGNLERAGN Green vs Red Low vs High M* High vs Low M
BH rate
Thin Disc vs ADAF
Smolčić (2009)
AGN dichotomy in the local Universe is reflected alsoin the properties of their host galaxies
SDSS + NVSS local sampleOptical spectroscopy: Highexcitation Radio AGN (HERAGN)
Lowexcitation Radio AGN (LERAGN)
PI: V. SmolčićV. Smolčić
Beyond the local Universe:Beyond the local Universe:The 3 GHz VLACOSMOS surveyThe 3 GHz VLACOSMOS survey
10,830 radio sources selected at 3 GHz (10 cm) with 0.75'' resolution over 2.6 deg2 of the COSMOS field (Smolčić et al. 2016, accepted)Smolčić et al. 2016, accepted)
~85% have optical/NIR counterpart in the COSMOS2015 catalog (Baran et al., in prep).
Accurate redshifts and photometry from the COSMOS2015 catalogue (Laigle et al., 2016)
FINAL SAMPLE:
7,339 radio sources + multi λ
rms ~ 2.3 uJy/beam
rms ~ 2.3 uJy/beamrms ~ 2.3 uJy/beam
PI: V. SmolčićV. Smolčić
OpticalnearIR midIR
FarIR/submm
Beyond the local Universe:Beyond the local Universe:The 3 GHz VLACOSMOS surveyThe 3 GHz VLACOSMOS survey
10,830 radio sources selected at 3 GHz (10 cm) with 0.75'' resolution over 2.6 deg2 of the COSMOS field (Smolčić et al. 2016, accepted)Smolčić et al. 2016, accepted)
~85% have optical/NIR counterpart in the COSMOS2015 catalog (Baran et al., in prep).
Accurate redshifts and photometry from the COSMOS2015 catalogue (Laigle et al., 2016)
FINAL SAMPLE:
7,339 radio sources + multi λ
Galaxy templates (MAGPHYS,da Cunha et al. 2008)consistency between absorbed stellar light and IR emission of the galaxy(= energy balance argument).
AGN library of templates physicallymotivated models of accretion disc and dusty torus emission (Fritz et al. 2006; Feltre et al. 2012)
(1) Decomposing AGN emission from hostgalaxy light(2) Classification: AGN or galaxy (statistical and incomplete method)
(1) Decomposing AGN emission from hostgalaxy light(2) Classification: AGN or galaxy (statistical and incomplete method)
3component SED fitting code SED3fit (Berta et al. 2013)http://cosmos.astro.caltech.edu/page/othertools
SEDfitting decompositionSEDfitting decomposition
~ 21% radiatively Efficient AGN~ 21% radiatively Efficient AGN
Xray + midIR + SED fitting (#1516)
AGN populations in RadioAGN populations in Radio Rad. Eff. AGN
(Radiative AGN activity) 1) Lx > 1042 erg/s (e.g. Szokoly et al. 2004)
2) MidIR colourcolour diagram (Donley et al. 2012)
3) SEDfitting identified AGN
Radioexcess AGNRadioexcess AGN
Considering 79% of non Rad. Eff. AGN
Radio 1.4 GHz luminositySFR_IR from galaxy's SF luminosity (Kennicutt 1998)
Distribution oflog(L
RADIO / SFR
IR )
RadiativelyInefficient AGN
Radiatively Inefficient AGN show up only in RadioRadioexcess threshold in good agreement with Del Moro et al. (2013)
Radiatively Inefficient AGN show up only in RadioRadioexcess threshold in good agreement with Del Moro et al. (2013)
(Delvecchio et al. 2016, submitted)
~ 21% radiatively Efficient AGN(7% shows >3σ radioexcess) ~ 21% radiatively Efficient AGN
(7% shows >3σ radioexcess)
Xray + midIR + SED fitting (#1516)
AGN populations in RadioAGN populations in Radio Rad. Eff. AGN Rad. Ineff. AGN
~ 17% radiatively Inefficient AGN~ 17% radiatively Inefficient AGN
Non Rad. Eff. AGN and Radioexcess (#1247)
(Radiative AGN activity) (Mechanical AGN activity)
Radio AGN in the SFRM* planeRadio AGN in the SFRM* plane
(noise)
Rad. Eff. AGN lie around the MS, while Rad. Ineff. AGN are 23 times below Rad. Eff. AGN lie around the MS, while Rad. Ineff. AGN are 23 times below
(Agreement with local Universe)
(Delvecchio et al. 2016, submitted)
(in agreement with local Universe)
(noise)
M* distributionsM* distributions
Rad. Eff. AGN typically hosted in less massive galaxies than Rad. Ineff. AGNRad. Eff. AGN typically hosted in less massive galaxies than Rad. Ineff. AGN
(Delvecchio et al. 2016, submitted)
z=1.5: similar M* distributions z=2: possible reversal (5.7 σ) of the M* behaviour (galaxy ''downsizing''?)
z=1.5: similar M* distributions z=2: possible reversal (5.7 σ) of the M* behaviour (galaxy ''downsizing''?)
M* distributionsM* distributions(Delvecchio et al. 2016, submitted)
Hint of ''downsizing''?Hint of ''downsizing''? Rad. Eff. AGN live preferentially in MS galaxies
Molecular gas fraction increases with redshift fgas ~ (1+z)2 in MS galaxies (Saintonge et al. 2013)
AGN accretion occurs more likely in gasrich galaxies (e.g. Vito et al. 2014)
Saintonge et al. (2013)
ffgasgas
Massive galaxies at high redshift host Rad. Eff. AGN activity more commonly than less massive galaxies
Galaxies below the MS have less cold gas, meaning less efficient SMBH accretion
RadioAGN dichotomy at highz?RadioAGN dichotomy at highz?
Rad. Eff. AGN
Rad. Ineff. AGN typically live in less starforming and more massive galaxies than Rad. Eff. AGN (highz analogs of Low/High Excitation AGN?)
Rad. Ineff. AGN
AGN populations in the AGN populations in the COSMOS fieldCOSMOS field
COSMOS2015catalog
midIR AGN[Donley+2012]
Xray AGN [Lx > 1042 erg/s]Civano et al. (2016);
Marchesi et al. (2016)
Radio AGN(Eff + Ineff) [this work]
AGN populations in the AGN populations in the COSMOS fieldCOSMOS field
COSMOS2015catalog
midIR AGN[Donley+2012]
Radio AGN(Eff + Ineff) [this work]
Xray AGN [Lx > 1042 erg/s]Civano et al. (2016);
Marchesi et al. (2016)
AGN populations in the AGN populations in the COSMOS fieldCOSMOS field
COSMOS2015catalog
midIR AGN[Donley+2012]
Radio AGN(Eff + Ineff) [this work]
Xray AGN [Lx > 1042 erg/s]Civano et al. (2016);
Marchesi et al. (2016)
Xray stacking of Rad. Ineff. AGNXray stacking of Rad. Ineff. AGNz<0.3
Log Lx = 40.61±0.260.3<z<0.7
Log Lx = 41.10±0.08 0.7<z<1.2Log Lx = 41.56±0.06
1.2<z<1.8Log Lx = 41.94±0.06
1.8<z<2.5Log Lx = 42.39±0.06
2.5<z<3.5Log Lx = 42.60±0.15
soft-x hard-x soft-x hard-x soft-x hard-x
soft-x hard-xsoft-x hard-xsoft-x hard-x
Xray excess wrt IRbased SFR: misclassified obscured AGN, or intrinsically lowluminosity AGN?
Hints of additional Xray emission from Xray stacking on larger scales (16''/32'' aperture, A. Finoguenov). Hot halo?
Xray stacking of Rad. Ineff. AGNXray stacking of Rad. Ineff. AGN**
* CSTACK (T. Miyaji)http://lambic.astrosen.unam.mx/cstack/
Xray excess
from Symeonidis et al. (2014)
3)
Rad. Ineff. AGN lie at lower Eddington ratio (~104 103)compared to Rad. Eff. AGN
Radiativeto mechanical luminosity
(sBHAR = Lx/M*)
Moreradiative
Moremechanical
Takehome messagesTakehome messages
Radio observations are crucial to unveil a population of lowaccreting AGN missed by Xray/midIR diagnostics
Twofold AGN population in Radio:Rad. Eff. AGN (21%) and Rad. Ineff. AGN (17%)
The differences in their galaxy properties (SFR, M*) are plausible in the context of the evolution
of the cold gas content.
Radio emission (345 sources):
~50% core (20100pc)~50% outer regions
<TOTAL / CORE radio emission> ~ 0.250.3 dex
VLBA – vs – VLA emissionVLBA – vs – VLA emission
redshift
Lx (
log
erg/
s)Contamination of Rad. Ineff. AGNContamination of Rad. Ineff. AGN
from undetected Xray AGN?from undetected Xray AGN?
15% contaminationat 0.5<z<3
AGN populations in RadioAGN populations in Radio3GHz VLA(+ multiλ)
midIR AGN (6%)[Donley+2012]
Xray AGN (12%)[Lx > 1042 erg/s]
+ + =~ 21% radiatively efficient AGN~ 21% radiatively efficient AGN
SEDfitting AGN (15%)[this work]
SED examples of Rad. Eff. AGNSED examples of Rad. Eff. AGN
SED+MIR+Xray AGN SEDonly AGN Xrayonly AGN
Specific SFR (sSFR) distributionsSpecific SFR (sSFR) distributions
Rad. Eff. AGN are hosted in more star forming galaxies than Rad. Ineff. AGNRad. Eff. AGN are hosted in more star forming galaxies than Rad. Ineff. AGN
(Delvecchio et al. 2016, submitted)
(NUVr) colour distributions(NUVr) colour distributions
Rad. Eff. AGN ''bluer'' than Rad. Ineff. AGN. Rad. Eff. AGN with radioexcess show intermediate colours
Rad. Eff. AGN ''bluer'' than Rad. Ineff. AGN. Rad. Eff. AGN with radioexcess show intermediate colours
Blue cloud(NUVr) < 1.2
Green valley1.2 < (NUVr) < 3.5
Red sequence(NUVr) > 3.5
(Delvecchio et al. 2016, submitted)