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The ionising radiation of AGN: Ultraviolet quasar composite from WFC3 Elisabeta Lusso INAF - Arcetri Observatory, Italy J. F. Hennawi (MPIA), G. Worseck (MPIA), J. X. Prochaska (UCSC), J. M. OMeara (Saint Michael's College), J.

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SLIDE 1

The ionising radiation of AGN: Ultraviolet quasar composite from WFC3

Elisabeta Lusso

INAF - Arcetri Observatory, Italy

  • J. F. Hennawi (MPIA), G. Worseck (MPIA), J. X. Prochaska (UCSC), J. M. O’Meara (Saint

Michael's College), J. Stern (MPIA), and C.Vignali (Unibo)

  • “Quenching & Quiescence”

Heidelberg, Germany. July 14-18, 2014

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SLIDE 2

Broad band quasar SEDs

Lusso+10

? ?

Big-blue bump Hot-dust Cold-dust X-ray corona

but see also Edelson&Malkan+86, Ward+87, Kriss+88, Sanders+89, Elvis+94, Richards+06, Krawczyk+13, Shang+11, Elvis+12

ALMA WILL FILL THE FIR GAP! PROBLEM SOLVED

Absorption by neutral hydrogen along the l.o.s. makes detection at these λ challenging

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SLIDE 3

Broad band quasar SEDs

Lusso+10

? ?

Big-blue bump Hot-dust Cold-dust X-ray corona

but see also Edelson&Malkan+86, Ward+87, Kriss+88, Sanders+89, Elvis+94, Richards+06, Krawczyk+13, Shang+11, Elvis+12

0.0001 pc (~10 RS) X-ray “corona”

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SLIDE 4

Broad band quasar SEDs

Lusso+10

? ?

Big-blue bump Hot-dust Cold-dust X-ray corona

but see also Edelson&Malkan+86, Ward+87, Kriss+88, Sanders+89, Elvis+94, Richards+06, Krawczyk+13, Shang+11, Elvis+12

0.0001-0.001 pc (10-100 RS) UV continuum “Big Blue Bump”

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SLIDE 5

Broad band quasar SEDs

Lusso+10

? ?

Big-blue bump Hot-dust Cold-dust X-ray corona

but see also Edelson&Malkan+86, Ward+87, Kriss+88, Sanders+89, Elvis+94, Richards+06, Krawczyk+13, Shang+11, Elvis+12

<1 pc (1000-105 RS) High ionization broad em lines CIV, HeII, OVI, Coronal lines?

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SLIDE 6

Broad band quasar SEDs

Lusso+10

? ?

Big-blue bump Hot-dust Cold-dust X-ray corona

but see also Edelson&Malkan+86, Ward+87, Kriss+88, Sanders+89, Elvis+94, Richards+06, Krawczyk+13, Shang+11, Elvis+12

<1 pc (1000-105 RS) Low ionization broad em lines MgII, Balmer, Paschen series (crossing 2000 K = 1μm dip)

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SLIDE 7

Broad band quasar SEDs

Lusso+10

? ?

Big-blue bump Hot-dust Cold-dust X-ray corona

but see also Edelson&Malkan+86, Ward+87, Kriss+88, Sanders+89, Elvis+94, Richards+06, Krawczyk+13, Shang+11, Elvis+12

>1 pc (up to few tens of parsec) near-IR and mid-IR continuum Dusty “torus” Hα, [OIII]

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SLIDE 8

Broad band quasar SEDs

Lusso+10

? ?

Big-blue bump Hot-dust Cold-dust X-ray corona

but see also Edelson&Malkan+86, Ward+87, Kriss+88, Sanders+89, Elvis+94, Richards+06, Krawczyk+13, Shang+11, Elvis+12

~100 pc far-IR continuum Molecular dust (~20 K) CO, H2 transition region: from nucleus to galaxy

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SLIDE 9

Broad band quasar SEDs

Lusso+10

? ?

Big-blue bump Hot-dust Cold-dust X-ray corona

but see also Edelson&Malkan+86, Ward+87, Kriss+88, Sanders+89, Elvis+94, Richards+06, Krawczyk+13, Shang+11, Elvis+12

~100 pc far-IR continuum Molecular dust (~20 K) CO, H2 transition region: from nucleus to galaxy

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SLIDE 10

Broad band quasar SEDs

Lusso+10

? ?

Big-blue bump Hot-dust Cold-dust X-ray corona

but see also Edelson&Malkan+86, Ward+87, Kriss+88, Sanders+89, Elvis+94, Richards+06, Krawczyk+13, Shang+11, Elvis+12

~1 kpc Bulge Bicones extended NELR OIII, coronal lines Galaxy

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SLIDE 11

Broad band quasar SEDs

Lusso+10

? ?

Big-blue bump Hot-dust Cold-dust X-ray corona

but see also Edelson&Malkan+86, Ward+87, Kriss+88, Sanders+89, Elvis+94, Richards+06, Krawczyk+13, Shang+11, Elvis+12

~1 kpc Bulge Bicones extended NELR OIII, coronal lines Galaxy

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SLIDE 12

Broad band quasar SEDs

Lusso+10

? ?

Big-blue bump Hot-dust Cold-dust X-ray corona

but see also Edelson&Malkan+86, Ward+87, Kriss+88, Sanders+89, Elvis+94, Richards+06, Krawczyk+13, Shang+11, Elvis+12

>10 kpc Disk Galaxy

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SLIDE 13

Broad band quasar SEDs

Lusso+10

? ?

Big-blue bump Hot-dust Cold-dust X-ray corona

but see also Edelson&Malkan+86, Ward+87, Kriss+88, Sanders+89, Elvis+94, Richards+06, Krawczyk+13, Shang+11, Elvis+12

>10 kpc Disk Galaxy

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SLIDE 14

Broad band quasar SEDs

Lusso+10

? ?

Big-blue bump Hot-dust Cold-dust X-ray corona

but see also Edelson&Malkan+86, Ward+87, Kriss+88, Sanders+89, Elvis+94, Richards+06, Krawczyk+13, Shang+11, Elvis+12

>70% of the AGN emission is in the optical-UV corrected for absorption by neutral hydrogen along the l.o.s. (challenging)

  • According to the classical Soltan argument

LQSO = ε dM/dt c2 build up of SMBH is a fundamental ingredient in every galaxy/BH co-evolution studies

  • Radiative or quasar-mode feedback: strongly depends on LQSO and
  • n the (shape) quasar SED (zero-order assumption: one unique SED

at every quasar luminosity and redshift)

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SLIDE 15

UV spectra of BH accretion disks

αNUV = -0.72 αEUV = -1.57 Telfer+2002 (HST, >340 citations): 184 QSOs at ⟨z⟩~1.2 (~20 QSO z>2), break at ~ Lyα

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SLIDE 16

αEUV = -0.56 Scott+2004 (FUSE): 85 QSOs at ⟨z⟩~0.1 (z≲0.67), no break

UV spectra of BH accretion disks

Telfer+2002

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SLIDE 17

αNUV = -0.68 αEUV = -1.41 Shull+2012 (COS): 22 QSOs at ⟨z⟩~0.5, break at ~1000 Å

UV spectra of BH accretion disks

Scott+2004 Telfer+2002

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SLIDE 18

UV spectra of BH accretion disks

Scott+2004 Telfer+2002 Shull+2012

✤ Expect a break in the UV (black body) which depends

  • n BH mass (and on how the IGM correction is done)

✤ Expect less massive BH to be hotter

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SLIDE 19

If one assumes:

  • AGN luminosity derived by accretion
  • Particle erg dissipated locally at distance r and optically thick medium:

black body

  • Virial theorem

r = 3 RS ; λ=0.1 ; MBH = 106 M⦿ ⇒ T~5.0 ×105 K r = 3 RS ; λ=0.1 ; MBH = 108 M⦿ ⇒ T~1.5 ×105 K The disc temperature decreases as the black hole mass increases We expect to see the location of the break changing as a function of MBH MBH

Understanding the spectrum of BH AD

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SLIDE 20

Understanding the spectrum of BH AD

r = 3 RS ; λ=0.1 ; MBH = 106 M⦿ ⇒ T~5.0 ×105 K r = 3 RS ; λ=0.1 ; MBH = 108 M⦿ ⇒ T~1.5 ×105 K The disc temperature decreases as the black hole mass increases We expect to see the location of the break changing as a function of MBH MBH If one assumes:

  • AGN luminosity derived by accretion
  • Particle erg dissipated locally at distance r and optically thick medium:

black body

  • Virial theorem
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SLIDE 21

UV spectra of BH accretion disks

Scott+2004 Telfer+2002 Shull+2012

0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5

redshift

−30 −28 −26 −24 −22 −20 −18

Mi(z = 2)

Telfer+02

MBH ~ 108 M⦿ MBH ~ 107 M⦿ MBH ~ 109 M⦿

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SLIDE 22

UV spectra of BH accretion disks

Scott+2004 Telfer+2002 Shull+2012

0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5

redshift

−30 −28 −26 −24 −22 −20 −18

Mi(z = 2)

Telfer+02

Break at ~1100Å MBH ~ 108 M⦿ MBH ~ 107 M⦿ MBH ~ 109 M⦿

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SLIDE 23

0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5

redshift

−30 −28 −26 −24 −22 −20 −18

Mi(z = 2)

Telfer+02 Scott+04

UV spectra of BH accretion disks

Scott+2004 Telfer+2002 Shull+2012

Break at ~1100Å MBH ~ 108 M⦿ MBH ~ 107 M⦿ MBH ~ 109 M⦿ No break

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SLIDE 24

0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5

redshift

−30 −28 −26 −24 −22 −20 −18

Mi(z = 2)

Telfer+02 Scott+04 Shull+12

UV spectra of BH accretion disks

Scott+2004 Telfer+2002 Shull+2012

Break at ~1100Å MBH ~ 108 M⦿ MBH ~ 107 M⦿ MBH ~ 109 M⦿ Break at ~1000Å No break

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SLIDE 25

0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5

redshift

−30 −28 −26 −24 −22 −20 −18

Mi(z = 2)

Telfer+02 Scott+04 Shull+12

UV spectra of BH accretion disks

Scott+2004 Telfer+2002 Shull+2012

Break at ~1100Å MBH ~ 108 M⦿ MBH ~ 107 M⦿ MBH ~ 109 M⦿ Break at ~1000Å No break

T~L1/4 MBH -1/2 The thermal disk peaks further into the blue for small MBH

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SLIDE 26

0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5

redshift

−30 −28 −26 −24 −22 −20 −18

Mi(z = 2)

Telfer+02 Scott+04 Shull+12

UV spectra of BH accretion disks

Scott+2004 Telfer+2002 Shull+2012

Break at ~1100Å MBH ~ 108 M⦿ MBH ~ 107 M⦿ MBH ~ 109 M⦿ Break at ~1000Å No break

T~L1/4 MBH -1/2 The thermal disk peaks further into the blue for small MBH

maybe we are seeing the expected transaction, but…

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SLIDE 27

0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5

redshift

−30 −28 −26 −24 −22 −20 −18

Mi(z = 2)

Telfer+02 Scott+04 Shull+12

MBH ~ 108 M⦿ MBH ~ 107 M⦿ MBH ~ 109 M⦿ <20 QSOs at z>2 high redshift poorly explored

UV spectra of BH accretion disks

Scott+2004 Telfer+2002 Shull+2012

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SLIDE 28

✤ The most massive BH (redshift > 2) poorly explored ✤ Previous works used overly simplistic and outdated

models for the IGM correction

✤ Highly biased samples. Took whatever they find from

the HST/FUSE archives which tend to be the UV brightest and hence bluest objects

UV spectra of BH accretion disks

Scott+2004 Telfer+2002 Shull+2012

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SLIDE 29

BH growth at high z

✤ Construct for the first time the UV composite for QSO

at redshift > 2

✤ State-of-the-art IGM correction: proper estimate of the

uncertainties

✤ Clear sample selection

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SLIDE 30

The sample

53 SDSS QSOs with g<18.5 mag; 2.28 < z < 2.60; <z>~2.44 observed with WFC3/UVIS-G280 grism Cycle 17 O’Meara+11,+13

600 800 1000 1200 1400 1600 1800 2000 2200 2400 2600

λ rest-frame [ ˚ A]

0.2 0.6 1.0 1.4 1.8 2.2 2.6 3.0

fλ/f1450

λobs=2000-6000 Å λ=2500Å FWHM~60Å

  • S/N~30 at 1350 Å

WFC3 SDSS

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SLIDE 31

600 800 1000 1200 1400 1600 1800 2000 2200 2400 2600

λ rest-frame [ ˚ A]

0.2 0.6 1.0 1.4 1.8 2.2 2.6 3.0

fλ/f1450

The sample

53 SDSS QSOs with g<18.5 mag; 2.28 < z < 2.60; <z>~2.44 observed with WFC3/UVIS-G280 grism Cycle 17 O’Meara+11,+13 λobs=2000-6000 Å λ=2500Å FWHM~60Å

  • S/N~30 at 1350 Å

0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5

redshift

−30 −28 −26 −24 −22 −20 −18

Mi(z = 2)

Telfer+02 Scott+04 Shull+12

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SLIDE 32

The sample

53 SDSS QSOs with g<18.5 mag; 2.28 < z < 2.60; <z>~2.44 observed with WFC3/UVIS-G280 grism Cycle 17 O’Meara+11,+13

600 800 1000 1200 1400 1600 1800 2000 2200 2400 2600

λ rest-frame [ ˚ A]

0.2 0.6 1.0 1.4 1.8 2.2 2.6 3.0

fλ/f1450

λobs=2000-6000 Å λ=2500Å FWHM~60Å

  • S/N~30 at 1350 Å

0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5

redshift

−30 −28 −26 −24 −22 −20 −18

Mi(z = 2)

Telfer+02 Scott+04 Shull+12 Lusso+14

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SLIDE 33

The sample

53 SDSS QSOs with g<18.5 mag; 2.28 < z < 2.60; <z>~2.44 observed with WFC3/UVIS-G280 grism Cycle 17 O’Meara+11,+13

600 800 1000 1200 1400 1600 1800 2000 2200 2400 2600

λ rest-frame [ ˚ A]

0.2 0.6 1.0 1.4 1.8 2.2 2.6 3.0

fλ/f1450

λobs=2000-6000 Å λ=2500Å FWHM~60Å

  • S/N~30 at 1350 Å
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SLIDE 34

IGM absorption correction

600 800 1000 1200 1400

λ rest-frame [ ˚ A]

0.0 0.2 0.4 0.6 0.8 1.0

Tλ,f

10000 IGM transmission curves for a suite of different column densities via MCMC (calibrated from absorption lines)

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SLIDE 35

IGM absorption correction

600 800 1000 1200 1400

λ rest-frame [ ˚ A]

0.0 0.2 0.4 0.6 0.8 1.0

Tλ,f

S04

10000 IGM transmission curves for a suite of different column densities via MCMC (calibrated from absorption lines) single correction for a broad range

  • f redshift and models outdated
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SLIDE 36

UV quasar composite

600 800 1000 1200 1400

λ rest-frame [ ˚ A]

1 2 3

fλ/f1450

Lusso+14 O’Meara+13

Before IGM correction After IGM correction Lusso et al. , in prep.

Lusso+14 (observed)

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SLIDE 37

600 800 1000 1200 1400 1600 1800 2000 2200 2400 2600 2800

λ rest-frame [ ˚ A]

0.2 1.2 2.2 3.2

fλ/f1450

OIV OV NIII OIII − NeVIII + OIV OIII HI − Lyseries + SVI Lyγ + CIII] Lyβ + OVI FeII FeII + FeIII Lyα NV SiII OI + SiII CII SiIV + OIV] NIV] CIV HeII OIII] NIII] AlIII CIII] FeII − blend CII] [NIV] FeII − blend

Lusso+14 fλ ∝ λ−1.37±0.01(αν = −0.63)

UV quasar composite: continuum fit

αEUV ~ -1.9 αNUV = -0.63 ± 0.01 λbreak=922.18 ± 31.15 Lusso et al. , in prep.

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SLIDE 38

UV quasar composite: comparison

1015 1016

log ν [Hz]

1046 1047

νLν [erg s−1]

O’Meara (2013) Lusso (2014) continuum fit

3000 1000 400

λ [ ˚ A]

Lusso (2014) no corr.

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SLIDE 39

UV quasar composite: comparison

1015 1016

ν [Hz]

1046 1047

νLν [erg s−1]

O’Meara (2013) Lusso (2014) Telfer (2002) continuum fit

3000 1000 400

λ [ ˚ A]

Lusso (2014) no corr.

slide-40
SLIDE 40

UV quasar composite: comparison

1015 1016

ν [Hz]

1046 1047

νLν [erg s−1]

O’Meara (2013) Lusso (2014) Telfer (2002) continuum fit

3000 1000 400

λ [ ˚ A]

Lusso (2014) no corr.

IGM correction employed by Telfer+02 less than 1%

  • ver the whole composite,

BUT

  • 1. in the forest the

correction should be >5% AND 2.at λ<600 (where there are <<20 z>2 quasars contributing) the correction is >>1% (~80%)!!

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SLIDE 41

UV quasar composite: comparison

1015 1016

ν [Hz]

1046 1047

νLν [erg s−1]

O’Meara (2013) Lusso (2014) Telfer (2002) continuum fit

3000 1000 400

λ [ ˚ A]

Lusso (2014) no corr.

slide-42
SLIDE 42

1015 1016

ν [Hz]

1046 1047

νLν [erg s−1]

O’Meara (2013) Lusso (2014) Telfer (2002) Shull (2012) continuum fit

3000 1000 400

λ [ ˚ A]

UV quasar composite: comparison

Lusso (2014) no corr.

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SLIDE 43

UV quasar composite: comparison

1015 1016

ν [Hz]

1046 1047

νLν [erg s−1]

O’Meara (2013) Lusso (2014) Telfer (2002) Shull (2012) Scott (2004) continuum fit

3000 1000 400

λ [ ˚ A]

Lusso (2014) no corr.

Softer EUV slope (αEUV~-1.9) than Scott+04 (αEUV~-0.56) and Shull+12 (αEUV~-1.41)

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SLIDE 44

Accretion disk models

Outer disk (Red) which emits as a (colour T corrected) BB Inner disk (Green) where the emission is Compton upscattered X-ray Corona (Blue) where also a fraction of the emission is Compton upscattered (power-law tail at high energies) Done+12

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SLIDE 45

Accretion disk models

15.0 15.5 16.0 16.5 17.0 17.5 18.0

log ν [Hz]

1045 1046 1047

νLν [erg s−1]

1 Ryd 4 Ryd

Lusso (2014) continuum fit αox=-1.37

3000 1000 400 100 50

λ [ ˚ A]

slide-46
SLIDE 46

15.0 15.5 16.0 16.5 17.0 17.5 18.0

log ν [Hz]

1045 1046 1047

νLν [erg s−1]

1 Ryd 4 Ryd

Lusso (2014) continuum fit αox=-1.37

3000 1000 400 100 50

λ [ ˚ A]

Accretion disk models

MBH = 6 ×109 M⦿ λEdd = 0.35 Γ = 1.9 (a=0.8) DATA{

slide-47
SLIDE 47

15.0 15.5 16.0 16.5 17.0 17.5 18.0

log ν [Hz]

1045 1046 1047

νLν [erg s−1]

1 Ryd 4 Ryd

Lusso (2014) continuum fit αox=-1.37

3000 1000 400 100 50

λ [ ˚ A]

Accretion disk models

MBH = 6 ×109 M⦿ λEdd = 0.35 Γ = 1.9 (a=0.8) DATA{ MBH = 1.2 ×1010 M⦿ λEdd = 0.17 Γ = 1.9 (a=1.0)

slide-48
SLIDE 48

15.0 15.5 16.0 16.5 17.0 17.5 18.0

log ν [Hz]

1045 1046 1047

νLν [erg s−1]

1 Ryd 4 Ryd

Lusso (2014) continuum fit αox=-1.37

3000 1000 400 100 50

λ [ ˚ A]

Accretion disk models

MBH = 6 ×109 M⦿ λEdd = 0.35 Γ = 1.9 (a=0.8) DATA{ MBH = 1.2 ×1010 M⦿ λEdd = 0.17 Γ = 1.9 (a=1.0) MBH = 3 ×109 M⦿ λEdd = 0.70 Γ = 1.9 (a=0.3)

slide-49
SLIDE 49

✤ Current estimates of AGN SEDs do not properly take into

account absorption by neutral hydrogen

✤ First UV quasar composite at redshift higher than 2 with

proper IGM absorption correction

✤ Softer EUV continuum than low luminous/low redshift

(low MBH) quasar samples

✤ The peak of the BBB does not depend on MBH only (but

BH spin is also involved)

Conclusions