Quasar evolution at high redshift Ian McGreer Steward Observatory - - PowerPoint PPT Presentation

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Quasar evolution at high redshift Ian McGreer Steward Observatory - - PowerPoint PPT Presentation

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Quasar evolution at high redshift Ian McGreer Steward Observatory a brief history of quasars a brief history of quasars 1964: 1 st quasar redshift 1968: z=2 quasars ~1970: BH accretion theory a brief history of quasars 1964: 1 st quasar

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Quasar evolution at high redshift

Ian McGreer Steward Observatory

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a brief history of quasars

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a brief history of quasars

1964: 1st quasar redshift 1968: z=2 quasars ~1970: BH accretion theory

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a brief history of quasars

1964: 1st quasar redshift 1968: z=2 quasars ~1970: BH accretion theory early 1990s: unification late 1990s: BH-galaxy correlations

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a brief history of quasars

1964: 1st quasar redshift 1968: z=2 quasars ~1970: BH accretion theory early 1990s: unification late 1990s: BH-galaxy correlations 2000s: reionization epoch

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  • ne Gyr of quasar evolution

Richards+06 (SDSS)

density of luminous quasars

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SLIDE 7
  • ne Gyr of quasar evolution

Richards+06 (SDSS)

density of luminous quasars

Hopkins & Beacom (2006)

cosmic star formation density

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Characterizing the growth of SMBHs over cosmic time

seeds, role of mergers, lifetimes, outflows/winds/feedback, spin, radiative efficiency, spectral energy distributions, halo occupation…

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Characterizing the growth of SMBHs over cosmic time

seeds, role of mergers, lifetimes, outflows/winds/feedback, spin, radiative efficiency, spectral energy distributions, halo occupation…

Multiwavelength surveys, luminosity functions, clustering

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Part 1: Quasar SEDs

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Do quasar SEDs evolve?

  • no change in UV/optical spectra for observed quasars to z~7
  • nuclear region already chemically enriched (Kurk+07,Jiang+07,de Rosa+12)

Mortlock+11

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  • the ionizing continuum is poorly constrained
  • Lya forest: PCA methods (Lee+12, Paris+12), differential evolution (Becker+13)
  • mean spectral shape: UV spectra from space
  • Telfer+02: <z> ~1, 80-300 objects, ⍺uv=-1.57
  • Scott+04: z<0.7, far-UV (FUSE) ⍺uv=-0.6, ⍺uv ~ Luv
  • Shull+12/Stevans+14: <z>~0.4, 22 (159) AGN (COS), ⍺uv=-1.41
  • Lusso+15: z~2.4, 53 SDSS quasars (COS), ⍺uv=-1.7

Do quasar SEDs evolve?

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  • the ionizing continuum is poorly constrained
  • Lya forest: PCA methods (Lee+12, Paris+12), differential evolution (Becker+13)
  • mean spectral shape: UV spectra from space
  • Telfer+02: <z> ~1, 80-300 objects, ⍺uv=-1.57
  • Scott+04: z<0.7, far-UV (FUSE) ⍺uv=-0.6, ⍺uv ~ Luv
  • Shull+12/Stevans+14: <z>~0.4, 22 (159) AGN (COS), ⍺uv=-1.41
  • Lusso+15: z~2.4, 53 SDSS quasars (COS), ⍺uv=-1.7

Do quasar SEDs evolve?

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  • the ionizing continuum is poorly constrained
  • Lya forest: PCA methods (Lee+12, Paris+12), differential evolution (Becker+13)
  • mean spectral shape: UV spectra from space
  • Telfer+02: <z> ~1, 80-300 objects, ⍺uv=-1.57
  • Scott+04: z<0.7, far-UV (FUSE) ⍺uv=-0.6, ⍺uv ~ Luv
  • Shull+12/Stevans+14: <z>~0.4, 22 (159) AGN (COS), ⍺uv=-1.41
  • Lusso+15: z~2.4, 53 SDSS quasars (COS), ⍺uv=-1.7

Do quasar SEDs evolve?

inhomogeneous samples, low-z, small numbers, no dust corrections

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correlations dust

Scott+04 (also Wyithe & Bolton 2010) Hopkins+04, IDM+ in prep

characterizing far-UV slopes

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Part II: the luminosity function

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Hopkins, Richards, & Hernquist 2007

The quasar luminosity function

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State of the quasar census: z=2.2–3.5 QLF

  • only 1/6th of data analyzed
  • systematics-limited
  • little evolution in bright end
  • strong density evolution, PLE ruled
  • ut LDDE (e.g., HRH07) strongly

disfavored

  • independent luminosity and density

evolution (LEDE)

BOSS DR9 (Ross, IDM et al. 2013)

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  • factor of ~5 discrepancy at faint end
  • NDWFS (Glikman+11)
  • COSMOS (Masters+12)
  • GOODS fields (Giallongo+15)
  • faint slope appears to steepen

State of the quasar census: z=4 QLF

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State of the quasar census: z=5 QLF

  • SDSS main + deep (IDM+14)
  • GOODS fields (Giallongo+15)
  • faint quasars with Gemini

spectroscopy (IDM+, in prep)

  • consistent with steep faint end slope

and high break luminosity

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State of the quasar census: z=5 QLF

  • SDSS main + deep (IDM+14)
  • GOODS fields (Giallongo+15)
  • faint quasars with Gemini

spectroscopy (IDM+, in prep)

  • consistent with steep faint end slope

and high break luminosity

IDM+, in prep Yang, IDM+, in prep

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  • now ~140 quasars
  • Pan-STARRS filling out bright end
  • constraints from gravitational lensing

agree with high M* (IDM+, in prep)

State of the quasar census: z=6 QLF

Willott+11

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  • 1 z>7 QSO from UKIDSS (Mortlock+11)
  • 3 z>6.5 QSOs from

VIKING (Venemans

+13)

  • 3 z>6.5 QSOs from Pan-STARRS

(Venemans+15)

State of the quasar census: z=7 QLF

Venemans+13

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  • 1 z>7 QSO from UKIDSS (Mortlock+11)
  • 3 z>6.5 QSOs from

VIKING (Venemans

+13)

  • 3 z>6.5 QSOs from Pan-STARRS

(Venemans+15)

State of the quasar census: z=7 QLF

Venemans+13 Fan+04 IDM+14

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State of the quasar census: evolutionary models

gray: HRH07

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State of the quasar census: evolutionary models

gray: HRH07

BOSS (Ross, IDM +14) COSMOS (Masters+12) SDSS (IDM+14) CFHTQS (Willott+12)

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ionizing emissivity from z=4 QLF

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evolution of quasar ionizing background

Data from Faucher-Giguere+08, Wyithe+Bolton`10, Calverley+11

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evolution of quasar ionizing background

Data from Faucher-Giguere+08, Wyithe+Bolton`10, Calverley+11 Giallongo+15

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He reionization (McQuinn+09)

  • sensitive to UV spectral index
  • driven by L* quasars

➡more sensitive to shot noise than clustering …assuming HRH07 QLF

evolution of quasar ionizing background

Data from Faucher-Giguere+08, Wyithe+Bolton`10, Calverley+11 Giallongo+15

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Part III: clustering

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high redshift quasar clustering: measurements

2.9<z<3.5 z>3.5

Shen+07

  • SDSS ~4K quasars (Shen+07)
  • BOSS ~27K quasars (White+12)
  • Transverse Proximity Effect /

absorber correlations (Prochaska+13)

  • quasar pairs at z>4 (Schneider+00,

Hennawi+06, Shen+10)

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  • SDSS ~4K quasars (Shen+07)
  • BOSS ~27K quasars (White+12)
  • Transverse Proximity Effect /

absorber correlations (Prochaska+13)

  • quasar pairs at z>4 (Schneider+00,

Hennawi+06, Shen+10)

  • weak luminosity dependence at low-z

(Adelberger+Steidel`05,Lidz+06, Shen+13,…)

high redshift quasar clustering: measurements

2.9<z<3.5 z>3.5

White+12

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high redshift quasar clustering: a new z=5 binary

10 20 Lyα NV OI SiIV CIV

QSO-A

7000 7500 8000 8500 9000 9500

wavelength [ ˚ A]

1 2

QSO-B fλ [relative units]

IDM, Eftekharzadeh, in prep

r0 > 30 Mpc

130 kpc i=19.4 i=21.4

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high redshift quasar clustering: a new z=5 binary

10 20 Lyα NV OI SiIV CIV

QSO-A

7000 7500 8000 8500 9000 9500

wavelength [ ˚ A]

1 2

QSO-B fλ [relative units]

IDM, Eftekharzadeh, in prep

r0 > 30 Mpc

130 kpc i=19.4 i=21.4 Ross+09, after Hopkins+07

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Part IV: bright, reionization-epoch sources

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~140 quasars known at z>5.7 today

Ongoing wide-area searches:

  • Pan-STARRS (Morganson+12, Banados+14,

Venemans+15)

  • ~20 reported to date, reaching z~6.7
  • SDSS+WISE (Wu+12)
  • expanding on Fan et al. selection
  • VST ATLAS (Carnall et al. 2015)
  • 5000 deg2 SDSS-like in Southern Hem., ~40% of data so far
  • 3 z~6 QSOs with z~19.6

Prospects for bright reionization-epoch quasars

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SDSS+WISE Ultra-luminous quasars

Wu et al. 2015 Nature 518, 7540, 512

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SDSS+WISE Ultra-luminous quasars

Wu et al. 2015 Nature 518, 7540, 512

luminosity BH mass

Wang et al. 2015 (submitted)

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SDSS+WISE Ultra-luminous quasars

Wu et al. 2015 Nature 518, 7540, 512

luminosity BH mass

Wang et al. 2015 (submitted)

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luminosity BH mass

Wang et al. 2015 (submitted)

SDSS+WISE Ultra-luminous quasars

Wu et al. 2015 Nature 518, 7540, 512

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SDSS+WISE Ultra-luminous quasars

Wang et al. 2015 (submitted)

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SDSS+WISE Ultra-luminous quasars

Wang et al. 2015 (submitted)

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Part IV: future surveys

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Quasar survey landscape, 2000-2030

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Summary (hopefully not too depressing)

  • Ionizing spectrum of quasars is poorly constrained,

key input to (He) reionization models

  • Factor of ~5 (or more) uncertainty in faint end

QLF at z>3

  • Quasars are strongly clustered at z>3, but tQSO,

BH mass -- halo mass relation poorly constrained