A 3-D map of the AGN distribution and relation to the zCOSMOS

A 3-D map of the AGN distribution and
relation to the zCOSMOS density field
John Silverman (ETH-Zurich)
XMM/COSMOS: G. Hasinger (PI; MPE), M. Brusa (MPE), V. Mainieri (ESO),
Nico Cappelluti (MPE), A. Finoguenov (MPE), H. Brunner (MPE), A. Comastri
(INAF-Bologna), R. Gilli (INAF-Bologna), C. Vignali (INAF-Bologna) & others
zCOSMOS: S. Lilly (PI; ETH), Katarina Kovac (ETH), V. Mainieri (ESO), G.
Zamorani (INAF-Bologna), O. Le Fevre (LAM-Marseille), T. Contini (LATTToulouse), M. Bolzonella (INAF-Bologna), M. Scodeggio (INAF-Milan) & other
zCOSMOS members
& many other COSMOS folks
How does the local environment influence
AGN activity?
• Merger-driven accretion onto supermassive black holes
- Numerical simulations demonstrate that mergers are efficient at transferring gas to the
nucleus (Mihos & Hernquist 1996) thus powering AGN (e.g. Hopkins et al. 2008)
- Ultraluminous infrared galaxies have high central gas concentrations (see Sanders &
Mirabel 1996).
• Depletion of fuel (gas) in dense environments
- galaxy harrassment or tidal interactions
- low redshift (z < 0.3 ) obscured AGN prefer to reside
in underdense regions (Kaufmann et al. 2003)
- analgous to star formation (e.g. Cooper et al. 2008)
Extend environmental studies to higher redshifts (z~1)
where the star formation and AGN accretion history peak
(e.g. Merloni et al. 2004) and the galaxy merger rate may
be higher (e.g. Kartaltepe et al. 2007).
JDS et al. 2008, ApJ, 679, 118
COSMOS
Galaxy evolution over a wide range of scales up to high redshift
PI: Nick Scoville (CalTech)
HST/ACS: i’ (Scoville)
Spitzer: (Sanders)
IRAC-3.6, 4.5, 5.6 8.0µm
MIPS-24, 70, 160µm
VLA: (Schinnerer)
GALEX: (Schiminovich)
XMM: (Hasinger)
Chandra: (Elvis)
VLT: (Lilly)
Subaru: (B, V, g, r, i, z; Taniguichi)
CFHT (u,i,Ks; McCraken)
GEMS
Blue: Fully exploited here
Red: Derived stellar masses, rest-frame
colors
(M. Bolzonella et al. in preparation)
Scoville et al. 2007
XMM survey of the COSMOS field
PI: G. Hasinger (MPE); 1848 point sources (Cappelluti et al. 2007, Hasinger et al. 2007)
f0.5-2.0 keV > 5 x 10-16 erg cm-2 s-1 (Soft band)
f2-10 keV > 2 x10-15 “
“ (Hard band)
~40% have optical
spectroscopic redshifts
Magellan (Trump et al.
2007), SDSS, MMT,
zCOSMOS
1
(Mpc)
84% have optical/NIR
counterpart (Brusa et al.
2007)
z
0.7
0.5
0.3
• 321 AGN (0.1 < z <1) having LX > 1042 erg s-1
• Most with 1042 < LX < 1043.7 erg s-1
- cleanly study their hosts properties (e.g. stellar mass)
See JDS et al. 2008, ApJ, 675, 1025
0.1
zCOSMOS
ETH-Zurich, LAM Marseille, LAMP Toulouse, INAF-Milan, INAF-Bologna,
MPE-Garching
PI. Simon Lilly (ETH)
Large VLT/VIMOS program (600 hrs)
10k ‘Bright’ sample (1.5 sq. deg)
• ‘Bright program’: 20k spectra i<22.5 (1.7 deg2)
~5500-9600 Å
z < 1.2
• ‘Deep program’: 10k spectra R < 25 (0.9 deg2)
~3300-6700 Å
1.5 < z < 2.5
High sampling rate (~70%)
Compulsory targets: X-ray (XMM, Chandra) and
VLA radio sources
7543 galaxies with secure spectroscopic redshifts
152 AGN (0.1 < z <1) identified by zCOSMOS
having LX > 1042 erg s-1
AGN
zCOSMOS
ETH-Zurich, LAM Marseille, LAMP Toulouse, INAF-Milan, INAF-Bologna,
MPE-Garching
PI. Simon Lilly (ETH)
Large VLT/VIMOS program (600 hrs)
10k ‘Bright’ sample (1.5 sq. deg)
• ‘Bright program’: 20k spectra i<22.5 (1.7 deg2)
~5500-9600 Å
z < 1.2
• ‘Deep program’: 10k spectra R < 25 (0.9 deg2)
~3300-6700 Å
1.5 < z < 2.5
High sampling rate (~70%)
Compulsory targets: X-ray (XMM, Chandra) and
VLA radio sources
7543 galaxies with secure spectroscopic redshifts
152 AGN (0.1 < z <1) identified by zCOSMOS
having LX > 1042 erg s-1
zCOSMOS: 3-D density field
zCOSMOS galaxy density field
Katarina Kovac et al. 2008, (in preparation)
• Zurich developed density estimator
10k (spectroscopic) +
30k (photometric)
• Nearest neighbor (3rd, 5th, 10th, 20th)
• Projected density (± 1000 km s-1)
Overdensity (δ): 1 + δ = ρ/<ρ>
z
1
0.7
0.5
0.3
0.1
Yingjie Peng (ETH-Zurich)
1000-1500 Mpc h-1
500-1000 Mpc h-1
AGN
X-ray clusters (Finoguenov et al. in prep)
Yingjie Peng (ETH-Zurich)
2000-2500 Mpc h-1
1500-2000 Mpc h-1
AGN
X-ray clusters (Finoguenov et al. in prep)
Local environments of AGN
Log M* > 10.4
AGN
Galaxies
• No apparent dependence on environment for
all galaxies (Miller et al. 2003)
• Mass dependency
- high mass hosts reside in underdense
environments (Kauffmann et al. 2004)
• No dependence on X-ray luminosity or absorption
Local environments of AGN
Log M* > 10.4
AGN
Galaxies
• No apparent dependence on environment for
all galaxies (Miller et al. 2003)
• Mass dependency
- high mass hosts reside in underdense
environments (Kauffmann et al. 2004)
• No dependence on X-ray luminosity or absorption
Concluding remarks
Environment
• X-ray selected AGN trace the overall galaxy distribution
• AGN in massive host galaxies (log M* > 11) prefer
underdense environments
Similar environmental/mass dependence of AGN activity
and star formation
JDS et al. 2008b, soon to be submitted to ApJ
What factors are critical for AGN activity?
• Massive, bulge-dominated galaxy (log M* > 10.5)
• Plentiful gas supply as inferred through concurrent star
formation (1-100 M* yr-1)
JDS et al. 2008a, companion paper, ApJ
Posters: N. Cappelluti “Coevolution of AGN and galaxy clusters in COSMOS”
T- Miyaji “X-ray AGN-galaxy cross-correlation and AGN halo occupation”
Talk:
R. Gilli “Spatial clustering of X-ray selected AGN at z~1”