spectral energy distribution of hyper-luminous infrared...

Spectral Energy Distribution of Spectral Energy Distribution of Hyper-Luminous Infrared GalaxiesHyper-Luminous Infrared Galaxies

Ángel Ruiz1 Francisco J. Carrera1, Francesca Panessa2, Giovanni Miniutti3

1: Instituto de Física de Cantabria (CSIC-UC)2: INAF/IASF – Roma3: Laboratoire APC - Paris

May 30May 30thth 2008 – X-ray Universe 2008 – Granada, Spain 2008 – X-ray Universe 2008 – Granada, Spain

Thanks to ESA & ESA Education Office for financial support

What is all the fuss about?

Supermassive Black Holes in centers of most local galaxies (Kormendy & Gebhardt, 2001)

Correlation between mass of central BH and spheroid (Magorrian et al. 1998; McLure & Dunlop,2002)

Similar evolution of X-ray AGN and optical galaxies (Silvermann et al. 2005)

What is all the fuss about?

Supermassive Black Holes in centers of most local galaxies (Kormendy & Gebhardt, 2001)

Correlation between mass of central BH and spheroid (Magorrian et al. 1998; McLure & Dunlop 2002)

Similar evolution of X-ray AGN and optical galaxies (Silvermann et al. 2005)

Conected growth of central BH through accretion and spheroid through star formation

AGN-galaxy co-evolution

Strong evidence of AGN-galaxy co-evolution: Conection between the growth of central SMBH through accretion and

spheroid through star formation

How to observe AGN-galaxy coeval:

Star formation takes place in heavily obscured environments: need penetrating radiation:

X-rays (of course!): thermal bremsstrahlung, binaries MIR-FIR-submm: radiation absorbed and re-emitted Radio

SMBH growth through accretion produces AGN activity: X-rays are the ”smoking gun”, but:

Most accretion power in the Universe absorbed (Fabian & Iwasawa 1999) X-ray background synthesis model require most AGN in the Universe absorbed (Gilli et al. 1999)

”Warm” MIR-FIR colours: direct emission absorbed and re-emitted Radio

AGN-galaxy co-evolution

Strong evidence of AGN-galaxy co-evolution: Connection between the growth of central SMBH through accretion and

spheroid through star formation

How to observe AGN-galaxy coeval:

Star formation takes place in heavily obscured environments: need penetrating radiation:

X-rays (of course!): thermal bremsstrahlung, binaries MIR-FIR-submm: radiation absorbed and re-emitted Radio

SMBH growth through accretion produces AGN activity: X-rays are the ”smoking gun”, but:

Most accretion power in the Universe absorbed (Fabian & Iwasawa 1999) X-ray background synthesis model require most AGN in the Universe absorbed (Gilli et al. 1999)

”Warm” MIR-FIR colours: direct emission absorbed and re-emitted Radio

Happy marriage of X-ray and MIR-FIR astronomy: coincidence in time of

Chandra, XMM-Newton, Suzaku, Spitzer, Akari, Herschel...

Observing AGN-galaxy co-evolution in X-rays and MIR-FIR

Multi-wavelength surveys: AEGIS, GOODS, COSMOS (see Brusa's talk)

Targeted MIR observations of X-ray sources: X-ray absorbed broad line QSO (see Page's talk)

Targeted X-ray observations of MIR-FIR-emiting objects:

Ultraluminous IR Galaxies (Franceschini et al. 2003, Teng et al. 2005, Poster G-1 by Anabuki)

Hyperluminous IR Galaxies (this talk, Ruiz et al. 2007)

Why HLIRGs?

L8-1000µm

= 1012-1013 Lsol: ULIRGS Powered by starburst (STB) and some (~50%) harbour AGN (Farrah et al. 2003)

Fraction of AGN increases with IR luminosity(Veilleux et al. 1999)

Most in interacting systems (Farrah et al. 2001) Sample in X-rays: composite, STB dominated (Franceschini et al. 2003; Teng et al. 2005)

L8-1000µm

> 1013 Lsol: HLIRGS (Rowan-Robinson 2000 [RROO]) Most with AGN contribution (RR00, Farrah et al. 2002a) Only some interacting (~30%) (Farrah et al. 2002b)

Not trivially high luminosity tail of ULIRGs Some present heavy obscuration in X-rays, even Compton-Thick (Wilman et al. 2003, Iwasawa et al. 2005; Nandra et al. 2007)

Why HLIRGs?

L8-1000µm

= 1012-1013 Lsol: ULIRGS Powered by starburst (STB) and some (~50%) harbour AGN (Farrah et al. 2003)

Fraction of AGN increases with IR luminosity(Veilleux et al. 1999)

Most in interacting systems (Farrah et al. 2001) Sample in X-rays: composite, STB dominated (Franceschini et al. 2003; Teng et al. 2005)

L8-1000µm

> 1013 Lsol: HLIRGS (Rowan-Robinson 2000 [RROO]) Most with AGN contribution (RR00, Farrah et al. 2002a) Only some interacting (~30%) (Farrah et al. 2002b)

Not trivially high luminosity tail of ULIRGs Some present heavy obscuration in X-rays, even Compton-Thick (Wilman et al. 2003, Iwasawa et al. 2005; Nandra et al. 2007)

● HLIRGs:●Strong star formation: > 1000 M⊙ / yr

●High AGN fraction

● Good laboratory to investigate star formation and BH growth:● Young galaxies experiencing burst of star formation?● Transient phase in AGN evolution?● ....

An XMM-Newton study of HLIRGs:Sample

Out of the 45 RR00 sample, those with: Public XMM-Newton data as of Dec. 2004 Own XMM-Newton AO-5 data z < ~2: avoid strong biasing due to high z QSOs

14 objects in final sample: All SED fitting in MIR/FIR (RR00, Farrah et al. 2002, Verma et al. 2002)

X0.6/0.40.323QSO 1.5IRAS 14026+4341

X0.7/0.30.36QSOIRAS 13279+3401

X0.6/0.40.780QSOIRAS F12509+3122

X1/02.038QSOPG 1247+267

X0.6/0.40.292StarburstIRAS 07380-2342

0.5/0.50.575StarburstIRAS F00235+1024

X1/01.158QSOPG 1206+459

X0.8/0.21.334QSOIRAS 16347+7037

X0.2/0.81.21QSOIRAS F14218+3845

X0.6/0.40.297QSOIRAS 18216+6418

0.7/0.30.926Seyfert 2IRAS F15307+3252

0.4/0.60.3Seyfert 2IRAS 12514+1027

1/00.442QSO 2IRAS 09104+4109

0.35/0.650.327QSO 2IRAS 00182-7112

CT?AGN / STB

(IR SED fitting)z

Type(opt)

Source

88

44

2

X<42.6-3σ upper limitIRAS 14026+4341


X44.343.8“thermal”+directIRAS F12509+3122

X45.945.5“thermal”+directPG 1247+267

X<42.5-3σ upper limitIRAS 07380-2342

<42.4-3σ upper limitIRAS F00235+1024

X45.1<44.0directPG 1206+459

X46.045.7“thermal”+directIRAS 16347+7037

X44.6<43.8directIRAS F14218+3845


43.7→45.5<43.1“direct”IRAS F15307+3252

43.342.2thermal+absorbed direct (4x1023)IRAS 12514+1027

45.344.2“thermal”+reflected+narrow lineIRAS 09104+4109

44.8<41.9reflected+narrow line (0.8keV)IRAS 00182-7112

CT?log L2-10log L0.5-2ModelSourceN

ot

dete

cted

wit

h X

MM

-New

ton







X45.1<44.0directPG 1206+459


X44.6<43.8directIRAS F14218+3845


43.7→45.5<43.1“direct”IRAS F15307+3252




CT?log L2-10log L0.5-2ModelSourceS

tong

ly a

bso

rbed o

r no d

irect

conti

nuu

m







X45.1<44.0directPG 1206+459


X44.6<43.8directIRAS F14218+3845


43.7→45.5<43.1“direct”IRAS F15307+3252




CT?log L2-10log L0.5-2ModelSourceSoft

exce

ss:

too b

right

to c

om

e f

rom

STB







X45.1<44.0directPG 1206+459


X44.6<43.8directIRAS F14218+3845


43.7→45.5<43.1“direct”IRAS F15307+3252




CT?log L2-10log L0.5-2ModelSourceO

nly

on

e d

ete

ctio

n o

f th

erm

al em

issi

on

fro

m S

TB

Risaliti & Elvis

Risaliti & Elvis

AGN

Risaliti & Elvis

STARBURST

AGN

AGN-dominated ULIRG

Risaliti & Elvis

STARBURST

AGN

STB-dominated ULIRG

AGN-dominated ULIRG

Risaliti & Elvis

STARBURST

AGN

STB-dominated ULIRG

AGN-dominated ULIRG

High-z HLIRGS

Risaliti & Elvis

STARBURST

AGN

STB-dominated ULIRG

AGN-dominated ULIRG

High-z HLIRGS

Risaliti & Elvis

AGN-dominated HLIRG

STARBURST

AGN

STB-dominated ULIRG

AGN-dominated ULIRG

High-z HLIRGS

Risaliti & Elvis

AGN-dominated HLIRG

“Mixed”

STARBURST

AGN

STB-dominated ULIRG

AGN-dominated ULIRG

High-z HLIRGS

Risaliti & Elvis

AGN-dominated HLIRG

STB-dominatedHLIRG

“Mixed”

STARBURST

AGN

STB-dominated ULIRG

AGN-dominated ULIRG

High-z HLIRGS

Risaliti & Elvis

AGN-dominated HLIRG

STB-dominatedHLIRG

“Mixed”

STARBURST

AGN

IRAS 14026+4341

H consistent with

z = 0.32

STB-dominated ULIRG

AGN-dominated ULIRG

High-z HLIRGS

Risaliti & Elvis

AGN-dominated HLIRG

STB-dominatedHLIRG

“Mixed”

STARBURST

AGN

IRAS 13279+3401

QSO; z ~ 0.3 Rowan-Robinson 2002

STB-dominated ULIRG

AGN-dominated ULIRG

High-z HLIRGS

Risaliti & Elvis

AGN-dominated HLIRG

STB-dominatedHLIRG

“Mixed”

STARBURST

AGN

IRAS 13279+3401


IRS-Spitzer MIR spectrum

Observed frame:

10 m absorption feature

Starburst shape(Nardini et al. 2008)

STB-dominated ULIRG

AGN-dominated ULIRG

High-z HLIRGS

Risaliti & Elvis

AGN-dominated HLIRG

STB-dominatedHLIRG

“Mixed”

STARBURST

AGN

IRAS 13279+3401


Luminosity overestimated!!!Strong evidence on IRAS13279+3401 is NOT AN HLIRG

STB-dominated ULIRG

AGN-dominated ULIRG

High-z HLIRGS

Risaliti & Elvis

AGN-dominated HLIRG

STB-dominatedHLIRG

“Mixed”

STARBURST

AGN

Spectral Energy Distributions

Systematic IR excess (or underluminous in X-rays) with respect to local QSO SED: X-ray obscuration? Starburst excess? Departure from standard local SED?

STB and AGN relative contribution to the total output

Spectral Energy Distributions

Systematic IR excess (or underluminous in X-rays) with respect to local QSO SED: X-ray obscuration? Starburst excess? Departure from standard local SED?

STB and AGN relative contribution to the total output

Build and model the SED of each source in our sample (from radio to X-rays)

STB1: NGC 1482

STB2: NGC 4102

STB3: NGC 5253

STB4: NGC 7714

Starburst:

Templates

Well observed SED of local STB and AGN

Different obscuration, width, intensity and peak

wavelength

F

[arb

itra

ry u

nit

s]

(Hz)

Type 1 RQ QSO mean SED: Elvis et al. 1994: log < 12 Richards et al. 2006: log > 12

RQ QSO luminosity-dependent SED: Hopkins, Richards & Hernquist 2007

OX

increase with LBOL

Templates


F

[arb

itra

ry u

nit

s]

(Hz)

Type 2 AGN (different obscuration level)

C. THINC. THIN

C. THICKC. THICK

AGN3: NGC 5506 (N

H=3x1022 cm-2)

AGN4: NGC 4507 (N

H=4x1023 cm-2)

AGN5: Mrk 3 (N

H=1x1024 cm-2)

AGN6: NGC 3393 (N

H > 1025 cm-2)

Templates


F

[arb

itra

ry u

nit

s]

(Hz)

From Bianchi et al. 2006Sy2 sample with

minimal starburst contribution

SEDs of HLIRGs

Starburst (opt.)

SEDs of HLIRGs

Type 2 AGN sources (opt.)

SEDs of HLIRGs


non-Luminosity-dependent SED

SEDs of HLIRGs


Luminosity-dependent SED

1 2 30

1

2

3

4

5N

um

be

r o

f s

ou

rce

s

SED of HLIRGs


LX>L

X

temp LX~L

X

temp LX<L

X

temp

non-Luminosity-dependent SED

1 2 3

0

1

2

3

4

5N

um

be

r o

f so

urc

es

SED of HLIRGs


LX>L

X

temp LX~L

X

temp LX<L

X

temp

Luminosity-dependent SED

X0.3 / 0.746.8IRAS 14026+4341

X1 / 047.4IRAS F12509+3122

X1 / 049.2PG 1247+267

X1 / 0 46.6IRAS 07380-2342

1 / 0 46.0AGN3IRAS F00235+1024

X1 / 048.4PG 1206+459

X1 / 048.9IRAS 16347+7037

X1 /047.0IRAS F14218+3845

X0.8 / 0.247.4IRAS 18216+6418

0.2 / 0.847.0IRAS F15307+3252

0.9 / 0.146.4IRAS 12514+1027

0.9 / 0.147.0IRAS 09104+4109

1 / 046.5IRAS 00182-7112

CT?AGN / STBlog LBOLBest fitSource

AGN3

AGN3

AGN3

AGN3

AGN1

AGN1

AGN1

AGN1

AGN1

AGN1

AGN1

AGN1

STB4

STB4

STB1

STB4

STB1

Fitt

ing w

ith

ou

t X

-ray d

ata

X0 / 146.8IRAS 14026+4341

X1 / 047.4IRAS F12509+3122

X1 / 049.2PG 1247+267

X0 / 146.2IRAS 07380-2342

0 / 145.6IRAS F00235+1024

X1 / 048.4PG 1206+459

X1 / 048.9IRAS 16347+7037

X1 /047.0IRAS F14218+3845

X0.7 / 0.347.5IRAS 18216+6418

0.8 / 0.247.0IRAS F15307+3252

0.5 / 0.547.2IRAS 12514+1027

0.6 / 0.446.9IRAS 09104+4109

0 / 146.1IRAS 00182-7112


AGN3

AGN5

AGN5

AGN1

AGN1

AGN1

AGN1

AGN1

AGN1

STB4

STB1

STB1

STB1

STB2

STB4

STB4

STB1

Fitt

ing

wit

h X

-ray d

ata

X0 / 146.8IRAS 14026+4341

X1 / 047.4IRAS F12509+3122

X1 / 049.2PG 1247+267

X0 / 146.2IRAS 07380-2342

0 / 145.6IRAS F00235+1024

X1 / 048.4PG 1206+459

X1 / 048.9IRAS 16347+7037

X1 /047.0IRAS F14218+3845

X0.7 / 0.347.5IRAS 18216+6418

0.8 / 0.247.0IRAS F15307+3252

0.5 / 0.547.2IRAS 12514+1027

0.6 / 0.446.9IRAS 09104+4109

0 / 146.1IRAS 00182-7112


AGN3

AGN5

AGN5

AGN1

AGN1

AGN1

AGN1

AGN1

AGN1

STB4

STB1

STB1

STB1

STB2

STB4

STB4

STB1

Com

pto

n T

hic

k

X0 / 146.8IRAS 14026+4341

X1 / 047.4IRAS F12509+3122

X1 / 049.2PG 1247+267

X0 / 146.2IRAS 07380-2342

0 / 145.6IRAS F00235+1024

X1 / 048.4PG 1206+459

X1 / 048.9IRAS 16347+7037

X1 /047.0IRAS F14218+3845

X0.7 / 0.347.5IRAS 18216+6418

0.8 / 0.247.0IRAS F15307+3252

0.5 / 0.547.2IRAS 12514+1027

0.6 / 0.446.9IRAS 09104+4109

0 / 146.1IRAS 00182-7112


AGN3

AGN5

AGN5

AGN1

AGN1

AGN1

AGN1

AGN1

AGN1

STB4

STB1

STB1

STB1

STB2

STB4

STB4

STB1

AG

N o

nly

: 5

sourc

es

X0 / 146.8IRAS 14026+4341

X1 / 047.4IRAS F12509+3122

X1 / 049.2PG 1247+267

X0 / 146.2IRAS 07380-2342

0 / 145.6IRAS F00235+1024

X1 / 048.4PG 1206+459

X1 / 048.9IRAS 16347+7037

X1 /047.0IRAS F14218+3845

X0.7 / 0.347.5IRAS 18216+6418

0.8 / 0.247.0IRAS F15307+3252

0.5 / 0.547.2IRAS 12514+1027

0.6 / 0.446.9IRAS 09104+4109

0 / 146.1IRAS 00182-7112


AGN3

AGN5

AGN5

AGN1

AGN1

AGN1

AGN1

AGN1

AGN1

STB4

STB1

STB1

STB1

STB2

STB4

STB4

STB1

SB

on

ly:

4 s

ourc

es

X0 / 146.8IRAS 14026+4341

X1 / 047.4IRAS F12509+3122

X1 / 049.2PG 1247+267

X0 / 146.2IRAS 07380-2342

0 / 145.6IRAS F00235+1024

X1 / 048.4PG 1206+459

X1 / 048.9IRAS 16347+7037

X1 /047.0IRAS F14218+3845

X0.7 / 0.347.5IRAS 18216+6418

0.8 / 0.247.0IRAS F15307+3252

0.5 / 0.547.2IRAS 12514+1027

0.6 / 0.446.9IRAS 09104+4109

0 / 146.1IRAS 00182-7112


AGN3

AGN5

AGN5

AGN1

AGN1

AGN1

AGN1

AGN1

AGN1

STB4

STB1

STB1

STB1

STB2

STB4

STB4

STB1

Com

posi

te:

4 s

ourc

es

X0 / 146.8IRAS 14026+4341

X1 / 047.4IRAS F12509+3122

X1 / 049.2PG 1247+267

X0 / 146.2IRAS 07380-2342

0 / 145.6IRAS F00235+1024

X1 / 048.4PG 1206+459

X1 / 048.9IRAS 16347+7037

X1 /047.0IRAS F14218+3845

X0.7 / 0.347.5IRAS 18216+6418

0.8 / 0.247.0IRAS F15307+3252

0.5 / 0.547.2IRAS 12514+1027

0.6 / 0.446.9IRAS 09104+4109

0 / 146.1IRAS 00182-7112


AGN3

AGN5

AGN5

AGN1

AGN1

AGN1

AGN1

AGN1

AGN1

STB4

STB1

STB1

STB1

STB2

STB4

STB4

STB1

Bolometric output dominated by AGN emission

Conclusions XMM-Newton-selected sample of 13 HLIRGs:

10/13 detected and AGN-dominated in X-rays:

Under luminous in X-rays with respect to mean SED of local QSO

Modelling multi- SED (from radio to X-rays): SED fitting consistent with the optical classification

9/13 need an AGN component: 5 pure AGN, 4 composite STB templates preferred: NGC 1482 (aged bursts)

AGN component dominates the bolometric output

X-ray data are mandatory for an accurate estimation of the relative AGN / STB contribution

SED of type 1 AGN are consistent with a luminosity dependent SED

Thanks to ESA & ESA Education Office for financial support

spectral energy distribution of hyper-luminous infrared...

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