Astrophysics and Evolution Astrophysics and Evolution of Supermassive Black of Supermassive Black

HolesHoles

INAF - Osservatorio Astronomico di BolognaINAF - Osservatorio Astronomico di Bologna

IASF – CNR sezione di BolognaIASF – CNR sezione di Bologna

Dipartimento di Astronomia – Universita’ Dipartimento di Astronomia – Universita’ BolognaBologna

WHY WHY

Probe the inner regions Probe the inner regions strong field limit of GR strong field limit of GR

Unbiased (Unobscured) view of accretion history Unbiased (Unobscured) view of accretion history

AIMS AIMS

Mapping physics and geometry of central BH Mapping physics and geometry of central BH

Space density and evolution of obscured accreting BH Space density and evolution of obscured accreting BH

WHEN WHEN

since early 2000 (launch of XMM and Chandra) based since early 2000 (launch of XMM and Chandra) based

on the BeppoSAX heritage on the BeppoSAX heritage up to the foreseen life of up to the foreseen life of

NASA and ESA cornerstones (2008-2010)NASA and ESA cornerstones (2008-2010)

STRATEGYSTRATEGY: HIGH ENERGY OBSERVATIONS : HIGH ENERGY OBSERVATIONS and and MULTIWAVELENGTH FOLLOW- MULTIWAVELENGTH FOLLOW-UPUP

OAB OAB

P. Ciliegi (RA)P. Ciliegi (RA)

A. Comastri (AA)A. Comastri (AA)

C. Gruppioni (RA) C. Gruppioni (RA)

M. Mignoli (RA) M. Mignoli (RA)

G.M. Stirpe (AA) G.M. Stirpe (AA)

V. Zitelli (AA) V. Zitelli (AA)

C. Vignali (Post-Doc) C. Vignali (Post-Doc)

M. Brusa (PhD 3+ yr.)M. Brusa (PhD 3+ yr.)

P. Ranalli (PhD 3+ yr.)P. Ranalli (PhD 3+ yr.)

F. Civano (PhD 1 yr.)F. Civano (PhD 1 yr.)

IASFIASF M. Cappi (Ric.)M. Cappi (Ric.)G. Di Cocco (Dir.) G. Di Cocco (Dir.) P. Grandi (Ric.)P. Grandi (Ric.)G. Malaguti (Ric.) G. Malaguti (Ric.) M. Dadina (art. 23) M. Dadina (art. 23) L. Foschini (art. 23) L. Foschini (art. 23)

F. Panessa (PhD 3+ F. Panessa (PhD 3+ yr.)yr.)

G. Ponti (PhD 1 yr.) G. Ponti (PhD 1 yr.) N. Cappelluti (student) N. Cappelluti (student)

UNIBO UNIBO G. G. C. Palumbo (PO)G. G. C. Palumbo (PO)

SMBH ASTROPHYSICS SMBH ASTROPHYSICS o Deep high energy observations of Deep high energy observations of

bright Seyfert galaxies and quasarsbright Seyfert galaxies and quasarso Direct (unabsorbed) probe of the Direct (unabsorbed) probe of the

disc/BH system inner regionsdisc/BH system inner regionso High quality spectroscopy (continuum + High quality spectroscopy (continuum +

emission/absorption line parameters)emission/absorption line parameters)o High throughput (variability, High throughput (variability,

reverberation mapping)reverberation mapping)o High-quality imaging of high z QSOHigh-quality imaging of high z QSO

o Reverberation mapping in Opt/UVReverberation mapping in Opt/UV

Broad-band (0.1-100 keV) X-ray Observations of AGNs

Importance of high-energy coverage for the astrophysics of

AGNs

Cappi et al., ‘99, Malaguti et al. ‘98, ‘01, etc. (single objects)Dadina et al., in preparation ( all the AGNs (z<0.1) in BeppoSAX archive)

BeppoSAX spectra up to 100 keV for about 100 AGNs

R and Ec for about 20 AGNs

N.

of

sou

rces

Gamma R

EcN

. of

sou

rces

N.

of

sou

rces

X-ray mapping of the Inner regions of AGNs

First model-independent confirmation of the existence of a

broad FeK line in MCG-6-30-15

Ponti et al. 2003, Dadina & Cappi 2003, Longinotti et al. 2003, etc

First reverberation mapping of the FeK line (r<100 rs)

continuum FeK line

Diffuse emission from AGN : Diffuse emission from AGN :

e.g. NGC 5252 with Chandrae.g. NGC 5252 with Chandra

(Joint XMM and Chandra observation)

Monitoraggio di QSO a Loiano

• Zitelli e Stirpe + Trevese (Univ. Roma)

• Avviato nel 2003

• 2 PG QSO con z > 1, V 15

• Osservazioni fotometriche e spettroscopiche a Loiano (1.5m) con cadenza mensile

• Finalizzato a misurare il ritardo delle variazioni delle righe rispetto a quelle del continuo ottenere dimensioni della Broad Line Region e, combinando con la larghezza delle righe, la massa del buco nero centrale

• Non ancora fatto per alte luminosità

Primi spettri

Vista variabilità, misura preliminare di ritardo (ca. 60 d) in UM 87

Monitoraggio di QSO ad alto z al VLT con ISAAC

• Stirpe + Marconi e Salvati (Arcetri), Capetti (Torino), Axon e Robinson (Rochester, NY), Horne (St. Andrews)

• Finalità simili al programma di Loiano, ma per z più alti e righe di ionizzazione più bassa

•Avviato nel 2001, cadenze mensili in service mode (6 h/semestre)

• 2 QSO con z=2.3, K=15

X-ray Lighthouses at the Dawn X-ray Lighthouses at the Dawn of the Modern Universe (C. of the Modern Universe (C. Vignali) Vignali)

>500 QSOs at z>4

~90 detected by Chandra/XMMX-ray emission is

a universal property of QSOs

Spectral shape constantup to z=6

UV to X-ray ratio higher for brighter quasars

X-RAY COSMOLOGY X-RAY COSMOLOGY o HARD X-RAY SURVEYSHARD X-RAY SURVEYS Insensitive to absorption up to large column Insensitive to absorption up to large column

densities (log NH < 24, Compton-thin) densities (log NH < 24, Compton-thin)

Most direct probe of the super-massive black Most direct probe of the super-massive black holes (SMBH) accretion activity recorded in the holes (SMBH) accretion activity recorded in the XRB spectral energy density XRB spectral energy density

Test of XRB models Test of XRB models test of AGN unified test of AGN unified schemes schemes physics and geometry of obscuring physics and geometry of obscuring gas and dust gas and dust

o MULTIWAVELENGTH FOLLOW-UPMULTIWAVELENGTH FOLLOW-UP Optical Identifications Optical Identifications Redshift, Luminosity and Absorption distributionsRedshift, Luminosity and Absorption distributions X-ray properties (individual and stacked) of other X-ray properties (individual and stacked) of other

classes non-AGN objects (Starburst, galaxies, classes non-AGN objects (Starburst, galaxies, EROs, etc..)EROs, etc..)

The deepest X-ray The deepest X-ray skysky

CDF-N (Alexander et al. 2003) CDF-S (Giacconi et al. 2002)

Chandra Surveys, 1-2 Ms exposures

The HELLAS2XMM surveyThe HELLAS2XMM surveyCollaborators: A. Baldi (Harvard-CFA),

N. Carangelo, S. Molendi (IASF-Mi) F. Fiore, F. Cocchia, V. D’Elia, S. Puccetti (INAF-OAR), F. La Franca, G. Matt, G.C. Perola (Uni Roma3),

R. Maiolino (INAF-OAA),

Beginning: Early 2001Main goal: to trace the history of accretion in the UniverseStrategy: public XMM-Newton fields large area (4 deg2)

To date: 122 sources in ~1 deg2 (5 fields) Optical Photometry (R band): ESO 3.6m (complete to R=24)Spectroscopy: ESO 3.6m + VLT/FORS2 (96/122)Near-Infrared photometry: VLT/ISAAC (11 targets with R>24)Radio: ATCA + VLA (complete)Additional X: Chandra (2 fields)

Selected Results Selected Results•Starburst (P. Ranalli)

•XBONGs(A.Comastri)

•EROs (M. Brusa)

•High X/O (M. Mignoli)

High X/O sources High X/O sources HELLAS2XMMHELLAS2XMM

ISAAC observationsISAAC observations: : 11 sources with R > 24 11 sources with R > 24 F(2-10) > 1.2 x 10-14F(2-10) > 1.2 x 10-14 K-band morphologyK-band morphology::

Most (7/10) are ellipticalsMost (7/10) are ellipticals Redshift rangeRedshift range: : z=0.8-2.4z=0.8-2.4 (from colour-morphology (from colour-morphology

redshift tracks)redshift tracks) X-ray analysis:X-ray analysis: (Perola et al. in prep.)(Perola et al. in prep.)

Highly obscuredHighly obscured

L(2-10 keV)=10L(2-10 keV)=104444-10-1045 45 erg/serg/s ALLALL: R-K>5 : R-K>5 EROs EROs 3 near-IR counterparts 3 near-IR counterparts

are unique are unique

Mignoli, Pozzetti et al. 2004, A&A, in press

R-band image K-band image

High quality imaging

Surface brightness

and effective radius

Fit with a de Vaucouleurs profile

2 pointlike1 disky7 ellipticals

Piercing obscured AGN among EROs with XMM-Newton

M. BRUSA Comastri, Mignoli, Vignali, Pozzetti, Zamorani+ Daddi (ESO) + Cimatti (INAF-Arcetri)

R band K band

Included in the XMM-Newton Image Gallery(section: Cosmology/Deep Fields)

Complementary programon EROs

The 2-10 keV luminosity as a The 2-10 keV luminosity as a Star Formation Rate indicatorStar Formation Rate indicator

Blue: Local starburst

Red: HDFN high-z galaxies

SFR=2x10-40L2-10

(from Ranalli, Comastri & Setti, 2003, A&A 399, 39)

XBONGs:Featureless optical spectra

LX>1042 erg/s

Relatively hard X-ray spectra

Discovered both in shallow and deep surveys (e.g. Barger et al. 2002)

X-ray bright optically normal X-ray bright optically normal galaxiesgalaxies PROTOTYPE: Source

P3 in the PKS0312 field (Comastri et al. 2002, ApJ,

571, 771)

KKs s (VLT/ISAAC) imaging of (VLT/ISAAC) imaging of XBONGsXBONGs

________________________ 30 arcsec

________________________ 30 arcsec

________________________ 30 arcsec

________________________ 30 arcsec

AGN surveys in the Marano AGN surveys in the Marano FieldField(Mignoli, Zamorani, Marano + MPE) (Mignoli, Zamorani, Marano + MPE)

WFI composite (BVR) image.WFI composite (BVR) image.~55000 objects, ~300 color-selected AGN ~55000 objects, ~300 color-selected AGN candidates down to B=23.5 (>100 spect. observed)candidates down to B=23.5 (>100 spect. observed)CorrectedCorrected quasar density at B=23.5 ~340/sq. deg quasar density at B=23.5 ~340/sq. deg

XMM-Newton ESO-WFI

~500 X-ray sources~500 X-ray sources

ContestoContesto NazionaleNazionale e e InternazionaleInternazionale

13 staff a BO (wrt ~ 100 in Italia) 13 staff a BO (wrt ~ 100 in Italia) Hellas2XMM e’ una collaborazione INAF-Hellas2XMM e’ una collaborazione INAF-

Universita’-CNR Universita’-CNR Cambridge e IC (UK) e UCLA (USA) per Cambridge e IC (UK) e UCLA (USA) per

studi di timing e LLAGNstudi di timing e LLAGN MPE (D) e CfA (USA) per le surveysMPE (D) e CfA (USA) per le surveys Partner di COSMOS (2 gradi quadri con Partner di COSMOS (2 gradi quadri con

HST PI: Scoville - Caltech) official HST PI: Scoville - Caltech) official commitment for XMM e Chandra follow-up commitment for XMM e Chandra follow-up (Co-PI) (Co-PI)

Partner of european RTN FP6 Partner of european RTN FP6

2000 2001 2002 2003+ Refereed Journals + Invited Talks 20+1 17+1 20+1 30+4

International Review Committees Chandra/XMM TAC + XMM User Group XEUS Astrophysics WG

Telescopes Time (X-rays) --- kiloseconds 420 320 770 600 Telescope Time (other lambda, mostly ESO) ---

nights 6 6 12 9+

Several hundreds of kiloseconds in large international programs (COSMOS/ELAIS etc..)

2000 2001 2002 2003+ (k€)

Personale 30 35 30 13(ASI+CNR+Cofin)

Ricerca 11 16 40 17(ASI)

Ricerca - 20 25 10 Inaf

(COFIN + INAF) 52 approved

FINANZIAMENTI

Problemi Problemi PROGRAMMAZIONEPROGRAMMAZIONE: : necessita’ all’interno del budget necessita’ all’interno del budget

assegnato/disponibile, di un piano organico a assegnato/disponibile, di un piano organico a medio/lungo terminemedio/lungo termine

VALUTAZIONEVALUTAZIONE: : Interna (comitati esterni internazionali) delle Interna (comitati esterni internazionali) delle

attivita’/proposte/strategie scientificheattivita’/proposte/strategie scientifiche

OUTREACH: : necessita’ di un’ Interfaccia- struttura INAF necessita’ di un’ Interfaccia- struttura INAF

dedicata alla diffusione dell’attivita’ scientificadedicata alla diffusione dell’attivita’ scientifica

Future developmentsFuture developments

X-RAY COSMOLOGY X-RAY COSMOLOGY :: high redshift Universe / LSS of X-ray high redshift Universe / LSS of X-ray

sources (X—rays + SIRTF) sources (X—rays + SIRTF)

Hellas2xmm 4 degHellas2xmm 4 deg22, @ 10, @ 10-14 -14 cgscgs ELAIS-S1 0.5 degELAIS-S1 0.5 deg2 2 @ 2x10 @ 2x10-15 -15 cgscgs COSMOS 2 degCOSMOS 2 deg2 2 @ 2x10@ 2x10-15 -15 cgscgs

X-RAY ASTROPHYSICS:X-RAY ASTROPHYSICS: Physical observables down to ~ Rg (within Physical observables down to ~ Rg (within

XMM-Chandra framework) XMM-Chandra framework) Physics of accretion up to z ~ 4-5 Physics of accretion up to z ~ 4-5