BH growth and the impact of AGN feedback on galaxy evolution

27 Pages·2014·21.17 MB·English

BH growth and the impact of AGN
feedback on galaxy evolution
Yohan Dubois – Institut d’Astrophysique de Paris (IAP)
Collaborators:
Julien Devriendt, Raphaël Gavazzi, Martin Haehnelt, Sébastien Peirani, Christophe
Pichon, Joe Silk, Adrianne Slyz, Romain Teyssier, Marta Volonteri
Horizon-AGN simulation
http://horizon-AGN.projet-horizon.fr
The Horizon-AGN simulation
•  Ramses code (AMR) Teyssier (2002)
•  L =100 Mpc/h
box
•  10243 DM particles
M =8x107 M
•  z=0.6 using 6.7 Mhours on 4096 cores
DM,res sun
•  Finest cell resolution dx=1 kpc •  150 000 galaxies per snapshot (> 50 part.)
•  Gas cooling & UV background •  7 billions leaf cells (> Illustris or EAGLE)
heating
•  Low efficiency star formation
•  Stellar winds + SNII + SNIa
•  O, Fe, C, N, Si, Mg, H
•  AGN feedback radio/quasar
-  Dubois et al, 2014
-  Welker et al, 2014
-  Codis et al, sub.
http://horizon-AGN.projet-horizon.fr
Green: gas density / Red: temperature / Blue: metallicity
29/07/14 AGN vs SF
A visual inspection of the impact of AGN feedback on
large-scale structures
Green: gas density / Red: temperature / Blue: metallicity
Without AGN With AGN
z=2.5 z=2.5
29/07/14 AGN vs SF
AGN are responsible for turning discs into ellipticals
Central galaxies at z=0 in groups 1013<M <1014 M
halo sun
Increasing mass
No AGN
AGN
140 kpc
Dubois, Gavazzi, Peirani, Silk, 2013
29/07/14 AGN vs SF
Radio mode or quasar mode ?
2
0 �
1
=
z=0 � z=1
no AGN
AGN
z=4
z=3

y
t
i z=2
s
o
n z=1
i
m
z=0.5
u
l

n z=0
o
i
t
e
r
c
c z=2 z=4
A
Galaxies are gas-rich at high-redshift
Star formation and feedback
consumes/removes/prevents from
collapsing the gas
BH mass
Dubois, Devriendt, Slyz, Teyssier, 2012
29/07/14 AGN vs SF
Growing the first bright quasars
Observationnal facts:
-  Very bright quasars in the SDSS with z>6
(Willott et al., 2003; Fan et al., 2006; Jiang et al., 2009)
-  Detection of a 2.109 M BH at z=7
sun
(Mortlock et al., 2011)
Requirement:
-  Need to grow from 105-106 M up to 109 M in less
sun sun
than 700 Myrs ! Eddington limit provides an e-folding
time = 45 Myr
Question:
-  How to bring gas sufficiently rapidly into the bulge of
the galaxy ?
15
Eddington
10
)un Mortlock
Ms direct
(H Eddington/3 collapse
B
M
g Eddington/10
o
l 5
pop III
remnant
0
29/07/14 AGN vs SF 6 10 20
z
Growing the first bright quasars
-  Direct accretion from the cosmic
cold flows (Di Matteo et al., 2012) Observationnal facts:
Cosmological context with large
-  Very bright quasars in the SDSS with z>6
statistics but low resolution (~1kpc)
(Willott et al., 2003; Fan et al., 2006; Jiang et al., 2009)
Versus -  Detection of a 2.109 M BH at z=7
sun
-  Violent disc instabilities (Mortlock et al., 2011)
(Bournaud et al., 2011)
High resolution (1pc) but isolated disc Requirement:
-  Need to grow from 105-106 M up to 109 M in less
sun sun
than 700 Myrs ! Eddington limit provides an e-folding
time = 45 Myr
Bournaud et al., 2011
Question:
-  How to bring gas sufficiently rapidly into the bulge of
the galaxy ?
15
Eddington
10
Di Matteo et al., 2012 )un Mortlock
Ms direct
(H Eddington/3 collapse
B
M
g Eddington/10
o
l 5
pop III
remnant
0
29/07/14 6 10 20
z
Growing the first bright quasars
-  Direct accretion from the cosmic
cold flows (Di Matteo et al., 2012) M =5.1011 M at z=6 M =2.1012 M at z=6
h sun h sun
Cosmological context with large
statistics but low resolution (~1kpc)
Versus
-  Violent disc instabilities
(Bournaud et al., 2011)
High resolution (1pc) but isolated disc

Bournaud et al., 2011 Cosmological zooms
10 pc resolution
Dubois, Pichon,
Haehnelt et al., 2012
Di Matteo et al., 2012
29/07/14
Growing the first bright quasars
-  Direct accretion from the cosmic
cold flows (Di Matteo et al., 2012) M =5.1011 M at z=6 M =2.1012 M at z=6
h sun h sun
Cosmological context with large
statistics but low resolution (~1kpc)
Versus
-  Violent disc instabilities
(Bournaud et al., 2011)
High resolution (1pc) but isolated disc

Bournaud et al., 2011
Cold flows
Di Matteo et al., 2012 Disc instabilities
Dubois, Pichon, Haehnelt et al., 2012
29/07/14