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Testing AGN impact on SF: a single source and a statistical sample.
Vincenzo Mainieri!
!
G. Cresci, M. Brusa, A. Marconi
M. Bonzini, J. Silverman, M. Perna
F. Fiore, C. Feruglio, R. Maiolino Motivations/goals
²  Study how radio-quiet AGNs can affect their host galaxies
(e.g. quenching/triggering SF).
²  In the redshift range 1<z<3 (e.g. peak of the AGN activity,
peak of the SFRD)
bian+03
A single source in
great details (IFU)
A statistical sample
(stacking of opt spectra)
AGN vs SF, Durham, July 31st 2014
A single source in great details AGN vs SF, Durham, July 31st 2014
Catching an AGN where the gas is being expelled
SINFONI noAO J-band observations (Feb-Mar 2014, PI Mainieri)
AGN vs SF, Durham, July 31st 2014
Ingredients MBH
Silverman+13
Matsuoka+13
Lbol
Lusso+12
NH
Mainieri+07
Lanzuisi+12
AGN vs SF, Durham, July 31st 2014
SINFONI/VLT J-band
1”x1”
Scale 250x125 mas, noAO
6 hours on target
z=1.594
L(AGN)~2 x 10^46 erg/s
q24=1.36
MBH(Hα)~2.7 x 10^9 M¤
AGN vs SF, Durham, July 31st 2014
SINFONI/VLT J-band
[OIII]
core
1.296-1.300
micron
1”x1”
1.296<λ<1.300 μm
Scale 250x125 mas, noAO
6 hours on target
z=1.594
L(AGN)~2 x 10^46 erg/s
q24=1.36
MBH(Hα)~2.7 x 10^9 M¤
AGN vs SF, Durham, July 31st 2014
SINFONI/VLT J-band
[OIII]
core
1.296-1.300
micron
1”x1”
1.296<λ<1.300 μm
[OIII] blue wing
Scale 250x125 mas, noAO
6 hours on target
z=1.594
L(AGN)~2 x 10^46 erg/s
q24=1.36
MBH(Hα)~2.7 x 10^9 M¤
13 kpc
1.294<λ<1.296 μm
AGN vs SF, Durham, July 31st 2014
SINFONI/VLT J-band: outflow properties
V10
•  V10 ~ -1500 km/s
W80
AGN vs SF, Durham, July 31st 2014
SINFONI/VLT J-band: outflow properties
V10
•  V10 ~ -1500 km/s
•  Mion > 8.5 x108 M¤ −1
" LH β
%" ne %
M ion = 2.82 •10 $ 43
−1 ' $
−3 '
# 10 ergs &# 100cm &
9
W80
[Osterbrock & Ferland 2006]
Assuming ne =100 cm-3
AGN vs SF, Durham, July 31st 2014
SINFONI/VLT J-band: outflow properties
V10
V10 ~ -1500 km/s
Mion > 8.5 x108 M¤ Td ≈ Rout / vout ~ 8.5 Myr
Mout,ion > 300 M¤/yr
• 
• 
• 
• 
•
2
out
M ≈ 〈 ρout 〉V •ΩR • vout
W80
M out
= 3• vout •
R out
Bi-conical outflow uniformly filled with outflowing clouds
AGN vs SF, Durham, July 31st 2014
SINFONI/VLT J-band: outflow properties
V10
• 
• 
• 
• 
• 
V10 ~ -1500 km/s
Mion > 8.5 x108 M¤ Td ≈ Rout / vout ~ 8.5 Myr
Mout,ion > 300 M¤/yr
Pkin,tot > 0.5 Mout vout2 =5.3 x 1044 erg s-1
What powers the outflow?
W80
P(SF) ~7 x 1041 x SFR(M¤/yr) [Veilleux+05]
Pkin,tot / P(SF) ~ 2.5
AGN vs SF, Durham, July 31st 2014
X-shooter/VLT spectroscopy (PI Brusa)
(Perna et al., in preparation)
[OIII]5007
XID2028
(a) centre
(b) outflow
(c) no outflow
Brusa+14
AGN vs SF, Durham, July 31st 2014
SINFONI/VLT H-band
1”x1”
H+K archival observations
Scale 250x125 mas, noAO
20 min on target
SFR (narrow Ha) ~ 230 M¤/yr
SFR (PACS Herschel) ~ 275 M¤/yr
AGN vs SF, Durham, July 31st 2014
SINFONI/VLT H-band: positive and negative feedback
Cresci,VM, et al., submitted
AGN vs SF, Durham, July 31st 2014
SINFONI/VLT H-band: positive and negative feedback
Cresci,VM, et al., submitted
AGN vs SF, Durham, July 31st 2014
SINFONI/VLT H-band: positive and negative feedback
Cresci,VM, et al., submitted
o  SF in blobs A&B: log([NII]/Hα)<-1.1
o  Casual connection outflow-SF: highly asymmetric shape of the SF regions
AGN vs SF, Durham, July 31st 2014
A statistical sample: stacking
AGN vs SF, Durham, July 31st 2014
Testing AGN impact on SF: the SFR vs M* plane
AGN vs SF, Durham, July 31st 2014
Testing AGN impact on SF: the SFR vs M* plane
•  X-ray selected sample of AGN: LX(2-10keV) > 1042 erg s-1
CDF-S
E-CDFS
COSMOS
AGN vs SF, Durham, July 31st 2014
Testing AGN impact on SF: the SFR vs M* plane
•  X-ray selected sample of AGN: LX(2-10keV) > 1042 erg s-1
•  High quality optical spectra: VIMOS, FORS1-2, IMACS
AGN vs SF, Durham, July 31st 2014
Testing AGN impact on SF: the SFR vs M* plane
•  X-ray selected sample of AGN: LX(2-10keV) > 1042 erg s-1
•  High quality optical spectra: VIMOS, FORS1-2, IMACS
•  PACS/Herschel detection or PACS ul and 24μm detection
Bonzini+13,+14
2361 AGNs
AGN vs SF, Durham, July 31st 2014
Testing AGN impact on SF: the SFR vs M* plane
•  X-ray selected sample of AGN: LX(2-10keV) > 1042 erg s-1
•  High quality optical spectra: VIMOS, FORS1-2, IMACS
•  PACS/Herschel detection or PACS ul and 24μm detection
AGN vs SF, Durham, July 31st 2014
SFR vs Mstar
AGN vs SF, Durham, July 31st 2014
SFR vs Mstar
AGN vs SF, Durham, July 31st 2014
SFR vs Mstar
AGN vs SF, Durham, July 31st 2014
Average spectra
2.5
2200
redshift
0.5
wavelength
5500
AGN vs SF, Durham, July 31st 2014
Velocity offsets: [NeV]λ3346 and FeIIλ2586-2600
0.5
redshift
2.5
VM, Bonzini in prep
outflow
AGN vs SF, Durham, July 31st 2014
Summary and outlook
²  An AGN driven outflow on kpc scale is quenching SF along its
way and triggering new SF at its edges.
²  AGN hosts show blue shifted ISM lines mostly above the MS.
AGN or SF? à comparison sample of inactive galaxies Single source
• Molecular outflow: PdBI (PI Brusa)
• High resolution map of the SF: VLT/SINFONI AO H band (PI Cresci)
Statistical samples
• Gas content in MS AGN hosts: ALMA band 3 in Cycle-2 (PI Mainieri)
AGN vs SF, Durham, July 31st 2014
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