Surveys, the history of accretion in the Universe and galaxy evolution Fabrizio Fiore and the HELLAS2XMM collaboration: (A. Baldi, M. Brusa, N. Carangelo, P. Ciliegi, F. Cocchia, A. Comastri, V. D’Elia, C. Feruglio, F. La Franca, R. Maiolino, G. Matt, M. Mignoli, S. Molendi, G.C. Perola, S. Puccetti, C. Vignali) +
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High Energy Large Area Surveys, the history of accretion in the Universe and galaxy evolution Fabrizio Fiore and the HELLAS2XMM collaboration: (A. Baldi,
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High Energy Large Area Surveys, the history of accretion in the Universe
and galaxy evolution
Fabrizio Fiore and the HELLAS2XMM collaboration:
(A. Baldi, M. Brusa, N. Carangelo, P. Ciliegi, F.
Cocchia, A. Comastri, V. D’Elia, C. Feruglio, F. La Franca, R. Maiolino, G. Matt, M. Mignoli, S. Molendi, G.C. Perola, S. Puccetti, C. Vignali)
+ M. Elvis, P. Severgnini, N. Sacchi, N. Menci, A.
Cavaliere, G. Pareschi, O. Citterio...
Hard X-ray Surveys
Most direct probe of the super-massive black hole (SMBH) accretion activity, recorded in the CXB spectral energy density
SMBH census
Strong constraints to models for the formation and evolution of structure in the Universe
AGN number and luminosity evolution
AGN clustering and its evolution
The Cosmic X-ray Background
Hard X-ray Surveys
Most direct probe of the super-massive black hole (SMBH) accretion activity, recorded in the CXB spectral energy density
SMBH census
Strong constraints to models for the formation and evolution of structure in the Universe
AGN number and luminosity evolution
AGN clustering and its evolution
XMM/Chandra Surveys
Wide and medium-deep several deg2
30-100 sources/XMM field,
Fx 10-14 50% of the CXB
LX-Z diagram coverage
Rare and peculiar sources, avoid cosmic variance Relatively “easy” multi-
The HELLAS2XMM survey- 1.5 deg2 of sky covered, 232 2-10keV sources down to F 2-10keV=610-15 cgs
- nearly complete photometry down to R~25- nearly complete spectroscopy down to R~24: 160 z
- 100 broad line AGN; 41 narrow line AGN and gal. 16 have logLX>44 QSO2!- 11 XBONGs; 1 star; 3 groups of galaxies
- 40 sources with X/O>8, 19 z - 6 broad line AGN; 13 narrow line AGN (12 QSO2!)
Fiore et al. 2003 A&A, Cocchia et al. in
preparation
X-ray to optical flux ratio15-20% of the sources have X/O>10 over a large flux range30-40% have X/O>3. Optical identification of sources with X/O>3-10 is possible in the shallower surveys! HELLAS2XMM CDFN SSA13 Lockman Hole
Large area surveysat Fx10-14 can beused to gain infoon the fainter sources, making the remaininghalf of the CXB!!!
High X/O = QSO2!
Mignoli, Cocchia et al. 2004
X-ray obscured AGNPerola, Puccetti et al. 2004 A&A
LDDE with constant NH distribution La Franca et al. 2005
Solid = observed dashed = best fit
2-10 keV AGN luminosity function models
LDDE with variable absorbed AGN fraction La Franca et al. 2005
Fraction of obscured AGN
La Franca et al. 2005
Comparison with CDM HC models
Menci,Fiore,Perola & Cavaliere 2004
Processes of galaxy formation and evolution described by a semi-analytic model.
Galaxy interactions: main triggers of accretion (Cavaliere & Vittorini 2000)
L(2-10keV)=0.01 L(bol.)
no other parameter tuning
Comparison with CDM HC models
Menci,Fiore,Perola & Cavaliere 2004
CXB Resolved fraction
LogL<43.5
43.5<LogL<44.5
LogL>44.5
Menci et al 2004
Summary most of the CXB <6-8keV is resolved in sources Black Hole mass density ~2 times higher than that
estimated from optical and soft X-rays: better agreement with CXB estimates and with local space density
Differential evolution of number and luminosity densities.
Nice agreement between the evolution of luminous QSO and CDM HC models. Problems with low luminosity AGN?
Revision of Unified Schemes
Revision of Unified Schemes
. Mild
Revision of Unified Schemes Strong:Low L Seyfers and powerful QSO: different populations.A working scenario:Seyferts – associated to galaxies with merging histories
characterized by small mass progenitors. Feedback is effective in self-regulating accretion and SF, cold gas is left available for subsequent nuclear activation produced by loose galaxy encounters (fly-by).
QSOs – associated to galaxies with large mass progenitors. Feedback is less effective, most gas is quickly converted in stars and accreted during a few major mergers at high Eddington rates.
The obscuration properties of the two populations can be different in term of geometry, gas density, covering factor, ionization state, metallicity, dust content etc..
What’s next ?
1) Paucity of high z logLX<44.5 sources? Real or are we missing highly obscured AGNs?
2) Compare the obscuration properties of Seyfert 2 galaxies and QSO2
3) Deconvolve accr. rate and BH mass:4) Seyfert-QSO/galaxy clustering and
its evolution
1) Paucity of Seyfert like sources @ z>1 is real? Or, is it, at least partly, a selection effect?
Are we missing in Chandra and XMM surveys highly obscured (NH1024 cm-2) AGN? Which are common in the local Universe…
Imaging surveys up to 8-10 keV (ASCA,BSAX, Chandra, XMM):most of the CXB <6-7 keV is resolved in sources. But only 40-50% in the 5-10 keV band. Few % E>10keV.The light-up and evolution of obscured accreting SMBH is still largely unknown
Worsley et a. 2004
What’s needed?
Sensitive observations at the peak of the CXB (~20-40 keV) to probe highly X-ray obscured AGN
But.. How deep should we go?
…and how hard should we go?
Residual CXB after subtracting the resolved fraction below 10 keV
Comastri 2004
We need to resolve:
80% of CXB @10-30keV (similar to Chandra and XMM deep fields below 10 keV)
Deconvolve accr. rate and BH mass:•Optically unobscured AGN: MBH from broad line FWHM •Optically obscured AGN: MBH from bulge light
Franceschini et al. 1999 Marconi et al 2004
Unobscured sources A detailed spectral analysis allows to make use of the correlations between FWHM of the broad emission lines and BH masses
Spectroscopy FWHM emission lines MMBHBH
Mclure & Jarvis 2002
Vestergaard 2002
Obscured sources The nucleus is obscured so we can study the host galaxy
Imaging Morphology Bulge MMBHBH
Mc Lure et al. 2002
Log(MBH/Mo) = -0.5 MR – 2.96
BPM16274 #69
B/T = 1
Pks0312 #31
B/T = 0.8
Hellas2XMM
The GOODS sampleWe extended our analisys to a sample of optically obscured sources in the Great Observatories Origins Deep Survey (GOODS) fields taking advantage of the superior quality of the HST images
Z band Ks band
B/T =0.39
B/T =0.5
MBH, L/LEDD of obscured and unobscured AGN
* = broad line AGN
What’s next (4)
AGN clustering D’Elia et al. 2004
AGN clusteringD’Elia et al. 2004 0=10’’
ELAIS S1 XMM-SWIREX-ray sources clustering and evolution
45’
XMM PN+MOS 50ks net expo. 0.5 deg2 479 X-ray sources
R=16.8
R=17.1
FX=1.510-13 cgs
ELAIS S1 XMM-SWIRE 6 extended sources in the 0.5 deg2 field
R=19.5FX=1.510-14
R=20.3
Unobscured
Obscured
ELAIS-S1 number counts
Clustering in the ELAIS-S1 field
2-10 keV:0=11+/-6 arcsec
0.5-2keV0=4+/-2.5 arcsec
What’s next
How galaxy activity traces the cosmic WEB (direct comparison with models for the evolution of the structure in the universe)
COSMOS! ACS-XMM-VIMOS-Chandra
COSMOS multiwavelength project
Need to go to larger scales 2 sq. deg.
“COSMOS is an HST/ACS Treasury project (..) Goal: Interplay between Large Scake Structure, evolution and formation of galaxies,dark matter and AGNs”
T. Area - grazing angle - t. diameter/focal length -mirror coating tradeoffs:
Possible solutions based on Wolter-1 Possible solutions based on Wolter-1 design: design:
• Telescope 60cm diameter, <0.1deg, long focal lenght, e.g. 30-50m, small A/F.L. e.g. 0.02 – 0.01 Vs. 0.09 - 0.12 (XMM e Chandra): SIMBOL-X baseline Focal plane of 5-8’ FWHM
Markarian 3: a highly obscured (NH=51023cm-2), high luminosity (logL20-100keV=43.8) Seyfert at 60Mpc BeppoSAX MECS-PDS data Mark3 X 10 a QSO2
Flux limits S/N=3 1MsecCircinus galaxy: a nearby (4Mpc), highly obscured (NH=21024cm-2), low luminosity (logL20-100keV=41.7) AGN BeppoSAX MECS-PDS data Circinus X 100 a bright Seyfert
Flux limits S/N=3 1Msec
NGC1068: a Compton thick (NH=1025cm-2) AGN at 20 Mpcobserved luminosity logL20-100keV=42, unobscured luminosity logL20-100keV≈44,A nearby QSO2??!!BeppoSAX MECS,PDS NGC1068 X 10 a QSO2
Possible solutions based on Wolter-1 Possible solutions based on Wolter-1 design: design:
• Assume telescope diameter <60cm
• <0.1deg, long focal lenght, e.g. 30-50m, small A/F.L. e.g. 0.02 – 0.01 Vs. 0.09 - 0.12 (XMM e Chandra) Focal plane of 5-8’ FWHM
• 0.1-0.3deg, 8-12m F.L., + multilayer coatings + multiple units Focal plane of 15-20’ FWHM
• if the d-spacing is varied in a continuous way (supermirror) and the absorption is negligible (E > 10 keV) it is possible to reflection bands 3-4 times wider than those for total reflection in mirrors with a single layer of e.g. Au, Pt, Ir.
• The d-spacing follows a power law distribution:
d(i) = a / (b+i)c
i = bi-layer index a /(2 sin c) c 0.25 b> -1
Wide band Multilayer (supermirrors)Wide band Multilayer (supermirrors)
Number of modulesNumber of modules 4
Number of nested mirror shellsNumber of nested mirror shells 50
To improve the present knowledge on the sources making theCXB, to have a more complete census of SMBH up to z=1-2, i.e. the golden agegolden age of AGN and galaxy activity, we should go down to fluxes where:
80% of the 10-30keV CXB is resolved in sources (0.1Crab); 50% of the 20-40keV CXB is resolved in sources (0.75Crab)
This can be done with lightweight (<400kg), multilayer optics with Aeff500 cm2 @20-30 keV and 15” HPD