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-

wavelength follow-up (ESO-VLT,3.6m, ATCA, VLA, TNG & Chandra)

HELLAS2XMM CDFN CDFS Lockman Hole

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

PKS0312_22QSO1 z=2.14 X/O=3.1 logNH=22.8

PKS0537_111R=25 X/O=50 logNH 23

PKS0537_11aQSO2 z=0.981 LX=44.2 X/O=30 logNH=22.2

PKS0537_153R>25 X/O>21 logNH 23

XBONGs

O = type 1 AGN =type 2 AGN = Early type Gals.

The HELLAS2XMM survey in a context

HELLAS2XMM – 1.5 deg2 - 232 sources F2-10keV 10-14 cgsFiore et al. 2003

Lockman Hole - 0.09 deg2 - 55 sources F2-10keV 510-15 cgs (Mainieri et al 2002)

CDFN - 0.037 deg2 - 88 sources F2-10keV 10-15 cgsCDFN - 0.051 deg2 - 44 sources F2-10keV 310-15 cgs(Barger et al. 2002)

CDFS - 0.037 deg2 - 80 sources F2-10keV 10-15 cgsCDFS - 0.051 deg2 - 43 sources F2-10keV 310-15 cgs

SSA13 - 0.015 deg2 - 20 sources F2-10keV 410-15 cgsBarger et al. 2001

HEAO1 (Grossan) - 26,000 deg2 - 63 sources F2-10keV 210-11 cgs

The evolution of number and luminosity densities

Fiore et al. 2003 A&ANon parametric determination

Black hole mass density

A ~ 5x1039 erg s-1Mpc-3

A (1-) LBol

BH ~ ——————

c2 LX

=0.1 LBol/LX=40

BH ~ 3x10-5 MΘ Yr-1 Mpc-3

BH ~ 4x105 MΘ Mpc-3

.

.

2-10 keV AGN luminosity function models

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)

50% of CXB @ 20-40keV

CXB fraction>50% res.CXB>80% res.CXB

F(20-40keV)<710-15 cgs or0.75 Crab10-15 cgs or0.1 Crab

F(10-30keV)<10-14 cgs or0.65 Crab210-15 cgs or0.13 Crab

What’s next (3)

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”

COSMOS project: COSMOS project: overviewoverview

MULTIWAVELENGTH DATA

Scheduled/observed:HST/ACS (600 orbits), XMM-Newton (0.8 Ms), SUBARU (b,v,r,i,z), VLA, GALEX, CFHT, Mambo …

proposed:Chandra (1.4 Ms), XMM (additional 0.8 Ms)+ Spitzer (200 orbits), VLT/VIMOS (70 nights)

http://www.astro.caltech.edu/cosmos/

http://www.ifa.hawaii.edu/~Eaussel/Cosmos/multiwavelength.html

800 ksec XMM-Newton Cosmos field

XMM pn true color image (courtesy I. Lehmann)

PI: G. Hasinger; 25 pointings 32 ksec each

Direct Imaging at E=10-80 keV

1Crab = 250 sources deg2 = 12 sources X 15’ diam. FOV0.5 Crab = 550 deg2 = 27 sources X 15’ diam. FOV0.1Crab = 2350 deg2 = 120 sources X 15’ diam. FOV

RFLA inceff228

F = focal lenght R = reflectivity

L = mirror height

= inclination angle

Designing a mission concept:Goals ≤Crab sensitivity, 15’15’ FOV;

1 Crab=0.2 cts/Msec/cm2 20-40 keV; S/N=3, Csource=Cbkg 20 cts/Msec Aeff100cm2 @ 30 keV.

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

• Telescope 30cm diameter 0.1-0.3deg, 8-12m F.L., + multilayer coatings + multiple units: HEXIT-SAT Focal plane of 15-20’ FWHM

•Telescope 90cm diameter, 0.1-0.3deg, 20-30m F.L., + multilayer coatings: Simbol-X development study Focal plane of 15-20’ FWHM

Image quality: which PSF do we need?

1’

1’

1’

10’

10’

10’

50”HPD; eq. 2Crab

30”HPDEq.2Crab

15”HPDEq.0.2Crab

HEXIT-SAT

4 mirror modules(XMM technology)8m focal length33cm diameter200 bilayers W/Si

400 cm2 @30keV200 cm2 @50keV1400 cm2 @1 keV

HEXIT-SAT flux limit

1Msec: 20-40 1/3 Crab 10-30keV 1/10 Crab

Flux limits

Flux limits S/N=3 1Msec

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

Reflecting coatingReflecting coating 200 bilayers W/Si

Geometrical profile Geometrical profile Wolter I (lin. approx)

Focal LengthFocal Length 8000 mm

Total Shell HeightTotal Shell Height 800 mm

Plate scalePlate scale 26 arcsec/mm

Total Shell Height Total Shell Height 800 mm

Material of the mirror wallsMaterial of the mirror walls electroformed Ni

Min-MaxTop DiameterMin-MaxTop Diameter 112 - 330 mm

Min - Max angle of incidenceMin - Max angle of incidence 0.096 - 0.295 deg

Min-Max wall thicknessMin-Max wall thickness 0.120 - 0.350 mm

Total Mirror Weight (1 module)Total Mirror Weight (1 module) 65

Field-of-View (diameter FWHM)Field-of-View (diameter FWHM) 15 arcmin

Single module effective areaSingle module effective area 75 cm2 @40 keV

Main characteristicsMain characteristics

XEUS-I Multilayer optimization

From Pareschi & Cotroneo:

50m focal lenght

200 W/Si bi-layers on shellsfrom 1.3m to 2.8m diameter.30 W/Si bi-layers on shellsFrom 2.8m to 4m

2000-3000 cm2 @20-40 keV

Background LEOActive shields instrument

BeppoSAX PDS:

Phoswich NaI(Tl) 3mm detector CsI(Na) 50mm active shield

Sky+particle ind.

Dark Earth

CXB

Internal Background LEOLow inclination (4 degrees) orbit: low and regular background

Total average BKG = 5.610-5 cts/s/cm2/keV/mmPL average BKG = 410-5 cts/s/cm2/keV/mm

13-60keV

Internal Background HEOActive shield instrument

EXOSAT 200,000 km apogee500 km perigee

ME Argon 1-15 keV

ME Xenon 5-50 keV1.5cm thick

ME Xenon total internal BKG 10-50 keV = 50-60 cts/s/detector310-3 cts/s/keV/cm2 = 210-4 cts/s/keV/cm2/mm 10 times less than XMM MOS

Internal Background HEOSimulations

From Armstrong et al. 1999Montecarlo for an L2 orbit

Assuming 90% efficiency anticoincidences, total BKG=10-4 cts/s/cm2/keV/mm

Within a factor of 2 of that seen by EXOSAT ME

20 times less than XMM MOS

2-3 times higher than LEO low inclination orbit BKG

CXB from outside the FOV

Reference PIB=10-4 counts/s/cm2/keV

CXB(20-40keV)=1.3810-11 erg/s/cm2/deg2 =8.610-3 ph/s/cm2/deg2

Det. Spot= (HPR/plate scale)2 #mod.

Spot(HX)=(7.5”/260”/cm)24 = 0.01 cm2

Spot(Xeus)=(5”/41.3”/cm)2 = 0.046 cm2

Spot(SXB)=(15”/69”/cm)2 = 0.15 cm2

Spot(SXM)=(7.5”/69”/cm)2 = 0.037 cm2

CXB(HX) = 910-5 counts/s/deg2 PIB(HX) = 210-5 counts/sCXB(Xeus) =410-4 counts/s/deg2 PIB(Xeus) = 4.610-5 counts/sCXB(SXB) = 1.310-3 counts/s/deg2 PIB(SXB) = 1.510-4 counts/sCXB(SXM) = 3.210-4 counts/s/deg2 PIB(SXM) = 3.710-5 counts/s

Conclusions

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