High Energy Large Area Surveys,

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

Optical (and soft X-ray) surveys gives values 2-3 times lower than those obtained from the CXB (and of the F.&M. and G. et al. estimates)

XMM/Chandra Surveys Wide and medium-deep 2 several deg 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 multiwavelength follow-up (ESOVLT,3.6m, ATCA, VLA, TNG & Chandra) HELLAS2XMM CDFN CDFS Lockman Hole

Some 2-10 kev surveys CDFN-CDFS 0.03deg2-16 XMM LH 0.12deg 2 50% z spec. XMM/ELAIS 0.5deg 2 Cont. XMM/COSMOS 2deg 2 Cont. Log Flux -15-14 CHAMP - SEXSI % z spec.? Kim/Green/Wilkes Harrison/Helfand 1-10 deg2 HELLAS2XMM 1-4deg2 80% z spec. -13 XMM BSS-HS 25deg 2-12 nearly 100% z spec. Caccianiga/Della Ceca 2004

The HELLAS2XMM survey - 1.5 deg2 of sky covered, 232 2-10keV sources down to F 2-10keV=6 10-15 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 ratio 15-20% of the sources have X/O>10 over a large flux range 30-40% have X/O>3. Optical identification of sources with X/O>3-10 is possible in the shallower surveys! HELLAS2XMM CDFN SSA13 Large area surveys at Fx 10-14 can be used to gain info on the fainter sources, making the remaining half of the CXB!!! Lockman Hole

High X/O = QSO2! Mignoli, Cocchia et al. 2004

X-ray obscured AGN Perola, Puccetti et al. 2004 A&A PKS0312_22 PKS0537_111 QSO1 z=2.14 X/O=3.1 R=25 X/O=50 lognh=22.8 lognh 23 PKS0537_153 R>25 X/O>21 lognh 23 PKS0537_11a QSO2 z=0.981 LX=44.2 X/O=30 lognh=22.2

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 cgs Fiore et al. 2003 Lockman Hole - 0.09 deg2-55 sources F2-10keV 5 10-15 cgs (Mainieri et al 2002) CDFN - 0.037 deg2-88 sources F2-10keV 10-15 cgs CDFN - 0.051 deg2-44 sources F2-10keV 3 10-15 cgs (Barger et al. 2002) CDFS - 0.037 deg2-80 sources F2-10keV 10-15 cgs CDFS - 0.051 deg2-43 sources F2-10keV 3 10-15 cgs SSA13-0.015 deg2-20 sources F2-10keV 4 10-15 cgs Barger et al. 2001 HEAO1 (Grossan) - 26,000 deg2-63 sources F2-10keV 2 10-11 cgs

452 sources (Hellas2XMM + LH + CDFN + CDFS +SSA13) -15<logFx<-13.3, 304 z-spec + (29 z-phot) Broad line AGN Non Broad line AGN Fiore et al. 2003 A&A

X/O of optically obscured AGN

X/O of optically obscured AGN (including EROs photo-z limits from Mignoli et al. 2004)

X/O-LX X-photometric z! z/(1+z)=0.21 139 opticaly obscured AGN with logl(2-10)>42 from H2, CDFS, CDFN, LH and SSA13 with robust z-spec.

High z optically obscured AGN

High z optically obscured AGN: the X-ray K correction 2 3 Z=4

High X/O = high NH QSO2! EROs Unobscured Obscured Perola et al. 2004

Luminosity Function and Redshift distribution Combined sample (Opt + stat. ids) all fluxes 10-15<F(2-10keV)<10-14 cgs

The evolution of number and luminosity densities Non parametric determination Fiore et al. 2003 A&A

Black hole mass density A ~ 5x1039 erg s-1mpc-3 A (1- ) LBol. BH ~ c2 =0.1 LX LBol/LX=40. BH ~ 3x10-5 M? Yr-1 Mpc-3 BH ~ 4x105 M? Mpc-3

2-10 kev AGN luminosity function models Solid = observed dashed = best fit LDDE with constant NH distribution La Franca et al. 2005

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

Type 2 QSOs number density

Lx-z plane: source number density

Comparison with CDM HC models Menci,Fiore,Perola & Cavaliere 2004 Processes of galaxy formation and evolution described by a semianalytic 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 (NH 1024 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)< 7 10-15 cgs or 0.75 µcrab 10-15 cgs or 0.1 µcrab F(10-30keV)< 10-14 cgs or 0.65 µcrab 2 10-15 cgs or 0.13 µcrab

What s next (3) Franceschini et al. 1999 Marconi et al 2004 Deconvolve accr. rate and BH mass: Optically unobscured AGN: MBH from broad line FWHM Optically obscured AGN: MBH from bulge light

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 MBH Mclure & Jarvis 2002 Vestergaard 2002

Obscured sources The nucleus is obscured so we can study the host galaxy Imaging Morphology Bulge MBH Mc Lure et al. 2002 Log(MBH/Mo) = -0.5 MR 2.96

Hellas2XMM BPM16274 #69 B/T = 1 Pks0312 #31 B/T = 0.8

The GOODS sample We 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 clustering D Elia et al. 2004 0=10

ELAIS S1 XMM-SWIRE X-ray sources clustering and evolution XMM PN+MOS 50ks net expo. 0.5 deg2 479 X-ray sources R=16.8 R=17.1

FX=1.5 10-13 cgs

ELAIS S1 XMM-SWIRE 6 extended sources in the 0.5 deg2 field R=19.5 FX=1.5 10-14 R=20.3

XMM survey of ELAIS S1: detections Palermo waveleth detection algorithm: 0.5-10 kev 479 sources 396 with optical counterpart (85 %) 2-10 kev 204 sources 3 10-15-3.2 10-13 187 with optical counterpart (92.5%) 30 have X/O>10 (15%) 5 sources not detected in the 0.5-10 kev band 0.5-2 kev 371 sources 28 sources not detected in the 0.5-10 kev band 5-10 kev 31 sources

ELAIS-S1 number counts Unobscured Obscured

Clustering in the ELAIS-S1 field 2-10 kev: 0=11+/-6 arcsec 0.5-2keV 0=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 COSMOS is an HST/ACS Treasury project (..) Goal: Interplay between Large Scake Structure, evolution and formation of galaxies, dark matter and AGNs Need to go to larger scales 2 sq. deg.

COSMOS project: overview 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 PI: G. Hasinger; 25 pointings 32 ksec each XMM pn true color image (courtesy I. Lehmann)

Direct Imaging at E=10-80 kev 1µCrab = 250 sources deg2 = 12 sources X 15 diam. FOV 0.5 µcrab = 550 deg2 = 27 sources X 15 diam. FOV 0.1µCrab = 2350 deg2 = 120 sources X 15 diam. FOV

Designing a mission concept: Goals?µCrab sensitivity, 15 15 FOV; 1 µcrab=0.2 cts/msec/cm2 20-40 kev; S/N=3, Csource=Cbkg cts/msec Aeff 100cm2 @ 30 kev. 20 T. Area - grazing angle - t. diameter/focal length mirror coating tradeoffs: Aeff 2 2 8 FL inc R F = focal lenght R = reflectivity L = mirror height θ= inclination angle

Possible solutions based on Wolter-1 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? 50 HPD; eq. 2 Crab 10 1 10 1 10 30 HPD Eq.2 Crab 1 15 HPD Eq.0.2 Crab

Image quality: which PSF do we need?

HEXIT-SAT 4 mirror modules (XMM technology) 8m focal length 33cm diameter 200 bilayers W/Si 400 cm2 @30keV 200 cm2 @50keV 1400 cm2 @1 kev

HEXIT-SAT flux limit 1Msec: 20-40 1/3 µcrab 10-30keV 1/10 µcrab

Flux limits

Flux limits S/N=3 1Msec Markarian 3: a highly obscured (NH=5 1023cm-2), high luminosity (logl20-100kev=43.8) Seyfert at 60Mpc BeppoSAX MECS-PDS data Mark3 X 10 a QSO2

Flux limits S/N=3 1Msec Circinus galaxy: a nearby (4Mpc), highly obscured (NH=2 1024cm-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 Mpc observed 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 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

Wide band Multilayer (supermirrors) 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 34 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

Main characteristics Number of modules 4 Number of nested mirror shells 50 Reflecting coating Geometrical profile 200 bilayers W/Si Wolter I (lin. approx) Focal Length 8000 mm Total Shell Height 800 mm Plate scale Total Shell Height Material of the mirror walls Min-MaxTop Diameter 26 arcsec/mm 800 mm electroformed Ni 112-330 mm Min - Max angle of incidence 0.096-0.295 deg Min-Max wallweight thickness Total Mirror (1 0.120-0.350 mm module) Field-of-View (diameter 65 FWHM) Single module effective area 15 arcmin 75 cm 2 @40 kev

XEUS-I Multilayer optimization From Pareschi & Cotroneo: 50m focal lenght 200 W/Si bi-layers on shells from 1.3m to 2.8m diameter. 30 W/Si bi-layers on shells From 2.8m to 4m 2000-3000 cm2 @20-40 kev

Background LEO Active shields instrument Sky+particle ind. Dark Earth BeppoSAX PDS: CXB Phoswich NaI(Tl) 3mm detector CsI(Na) 50mm active shield

Internal Background LEO Low inclination (4 degrees) orbit: low and regular background Total average BKG = 5.6 10-5 cts/s/cm2/kev/mm PL average BKG = 4 10-5 cts/s/cm2/kev/mm 13-60keV

Internal Background HEO Active shield instrument EXOSAT 200,000 km apogee 500 km perigee ME Argon 1-15 kev ME Xenon 5-50 kev 1.5cm thick ME Xenon total internal BKG 10-50 kev = 50-60 cts/s/detector 3 10-3 cts/s/kev/cm2 = 2 10-4 cts/s/kev/cm2/mm 10 times less than XMM MOS

Internal Background HEO Simulations From Armstrong et al. 1999 Montecarlo 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)=1.38 10-11 erg/s/cm2/deg2 =8.6 10-3 ph/s/cm2/deg2 Det. Spot= (HPR/plate scale)2 #mod. Spot(HX)= (7.5 /260 /cm)2 4 = 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) = 9 10-5 counts/s/deg2 PIB(HX) = 2 10-5 counts/s CXB(Xeus) =4 10-4 counts/s/deg2 PIB(Xeus) = 4.6 10-5 counts/s CXB(SXB) = 1.3 10-3 counts/s/deg2 PIB(SXB) = 1.5 10-4 counts/s CXB(SXM) = 3.2 10-4 counts/s/deg2 PIB(SXM) = 3.7 10-5 counts/s

Conclusions To improve the present knowledge on the sources making the CXB, to have a more complete census of SMBH up to z=1-2, i.e. the golden age of AGN and galaxy activity, we should go down to fluxes where: 80% of the 10-30keV CXB is resolved in sources (0.1 Crab); 50% of the 20-40keV CXB is resolved in sources (0.75 Crab) This can be done with lightweight (<400kg), multilayer optics with Aeff 500 cm2 @20-30 kev and 15 HPD