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The Build-up of Quasars. Gordon Richards Drexel University. With thanks to Michael Strauss, Yue Shen (Princeton), Don Schneider, Nic Ross (Penn State), Adam Myers (Illinois ), Phil Hopkins ( Berkeley ), and a host of other people from the SDSS Collaboration. Caveats.

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the build up of quasars
The Build-up of Quasars

Gordon Richards

Drexel University

With thanks to Michael Strauss, YueShen (Princeton), Don Schneider, Nic Ross (Penn State), Adam Myers (Illinois), Phil Hopkins (Berkeley), and a host of other people from the SDSS Collaboration

caveats
Caveats

I tend to be biased towards:

  • High redshift (z>1)
  • High luminosity
  • Optical Selection
  • “Quasar” mode accretion
  • Unobscured (i.e., type 1)
  • Quasar=QSO=AGN=any actively accreting supermassive black hole
the redshift desert
The Redshift Desert
  • Redshift desert for galaxies due to lack of spectral features in the optical octave at z~2.
  • No redshift desert for quasars (in the galaxy sense), but there is in reality. And just as frustrating.

Galaxy

Franx 2003

Quasar

the z 2 7 quasar desert
The z~2.7 Quasar Desert

Observed

Corrected

Schneider et al. 2007

z 2 7 quasar colors
Z~2.7 Quasar Colors

At 2.5<z<3.0 quasars cross through the locus of stars, making those quasars harder to identify (efficiently).

x ray and ir selection
X-ray and IR Selection
  • X-ray and IR selection don’t suffer from the same problem (and they allow selection of obscured quasars).
  • But they do have their own problems.
  • Area surveyed by X-ray is tiny.
  • Mid-IR has its own 3.5<z<5 desert.
  • Not clear that optical/radio/MIR/X-ray selecting same objects (at least at lower luminosity), see Hickox et al. 2008.
quasar luminosity function
Quasar Luminosity Function

As with star formation rate, quasars peaked at redshift 2-3.

The rise and fall is even more dramatic in time than redshift.

Richards et al. 2006

the rise of quasars at z 6
The Rise of Quasars at z~6

Sets an upper limit to the luminosity for a given mass, orequivalentlya minimum mass for a given luminosity.

LE = 1.38x1038 M/Msun erg/s

ME = 8x107L46Msun

Mere existence z~6 quasars constrains formation models

Eddington argument: If the luminosity of a quasar is high enough, then radiation pressure from electron scattering will prevent further gravitational infall.

making smbhs at z 6
Making SMBHs at z~6

The luminosities of the z~6 quasars imply BH masses in excess of 109MSun.

But z~6 is <1Gyr after the Big Bang.

Assembling that much mass in so little time is difficult (but not impossible).

Tanaka & Haiman 2009

quasar luminosity function1
Quasar Luminosity Function

e.g., Richards et al. 2006

SDSS is relatively shallow.

It probes only the tip of the iceberg.

Need fainter surveys to get full picture.

cosmic downsizing
Cosmic Downsizing

Hasinger et al. 2005

X-ray surveys probe much deeper. Here we see that peak depends on the luminosity.

Ueda et al. 2003

cosmic downsizing1
Cosmic Downsizing

Hasinger et al. 2005

X-ray surveys probe much

larger dynamic range.

SDSS+2SLAQ

Croom et al. 2009

slide13

How does the quasar luminosity function relate to the physics of BH accretion and galaxy evolution?

quasar luminosity function2
Quasar Luminosity Function

Space density of quasars as a function of redshift and luminosity

Typically fit by double power-law

Croom et al. 2004

density evolution
Density Evolution

Number of quasars is changing as a function of time.

luminosity evolution
Luminosity Evolution

Space density of quasars is constant.

Brightness of individual (long-lived) quasars is changing.

luminosity vs redshift
Luminosity vs. Redshift

2.5

1.5

4.5

3.5

0.5

Usually we split into L or z instead of making a 3-D plot, but the information is the same.

luminosity evolution1
Luminosity Evolution

Cosmic Downsizing

  • Pure density or pure luminosity evolution don’t lead to cosmic downsizing.
  • The slopes must evolve with redshift.
luminosity dependent density evolution
Luminosity Dependent Density Evolution

To get cosmic downsizing, the number of quasar must change as a function of time, as a function of luminosity. i.e., the slopes must evolve.

bolometric qlf
Bolometric QLF

Hopkins, Richards, & Hernquist 2007

hopkins et al 2005
Hopkins et al. 2005

Most QLF models assume they are either “on” or “off” and that there is a mass/luminosity hierarchy.

Hopkins et al.: quasar phase is episodic with a much smaller range of mass than previously thought.

QLF is the convolution of the formation rate and the lifetime.

Hopkins et al. 2006

qso qlf galaxy qlf
QSO QLF != Galaxy QLF

Benson et al. 2003

hopkins et al 20051
Hopkins et al. 2005

Most QLF models assume they are either “on” or “off” and that there is a mass/luminosity hierarchy.

Hopkins et al.: quasar phase is episodic and “all quasars are created equal” (with regard to mass/peak luminosity).

QLF is the convolution of the formation rate and the lifetime.

Hopkins et al. 2006

merger scenario w feedback
Merger Scenario w/ Feedback
  • merge gas-rich galaxies
  • form buried quasars
  • feedback expels the gas
  • revealing the quasar
  • shutting down accretion and star formation

e.g., Kauffmann & Haehnelt 2000

Granato et al. 2004, DiMatteo et al. 2005, Springel et al. 2005, Hopkins et al. 2005/6a-z

how can we test this
How Can We Test This?

In addition to the evolution of the QLF slopes, we can probe:

  • The Quasar Luminosity Function
    • active lifetime (e.g., Martini 2004)
    • accretion rate (e.g., Kollmeier et al. 2006)
    • MBH distribution (e.g., Vestergaard & Osmer 2009)
  • Quasar Clustering
    • L, zdependence (e.g., Lidz et al. 2006 ; Shen et al. 2009)
    • small scales (e.g., Hennawi et al. 2006; Myers et al. 2008)
clustering
Clustering
  • Red Points are, on average, randomly distributed, black points are clustered
  • Red points: ()=0
  • Black points: ()>0
  • Can vary as a function of, e.g., angular distance,  (blue circles)
  • Red: ()=0 on all scales
  • Black: () is larger on smaller scales

A. Myers

quasar clustering
Quasar Clustering
  • Quasars are more clustered on small scales than large scales.
  • Comparing with models of dark matter clustering gives the “bias” (overdensity of galaxies to DM)
  • Linear bias (bQ=1) ruled out at high significance.

Myers et al. 2007

galaxy clustering
The comoving clustering length of luminous galaxies is roughly independent of z at least to z~ 5.

Therefore, the distribution of galaxies must be increasingly biased relative to the dark matter at high redshift, galaxies=bdark matter

Galaxy Clustering

Ouchi et al. 2004

how about quasars
Quasars are powered by the ubiquitous super-massive black holes in the cores of ordinary massive galaxiesHow about quasars?

Therefore, we’d expect that the clustering of quasars should be similar to that of luminous galaxies, at the same redshift.

Bahcall, Kirhakos et al.

comoving correlation length
Comoving Correlation Length

SDSS Quasars

Ross et al. 2009

quasar bias evolution
Quasar Bias Evolution

As with galaxies, constant clustering length means strongly evolving bias.

Ross et al. 2009

what happens at higher redshift
What happens at higher redshift?
  • If very massiveBHsare associated with very massive DM halos, then high-redshift quasars should sit in very rare, many  peaks in the density field.
  • So we expect high-redshift quasars to be more strongly clustered.

For 2.9 < z < 3.5: r0=16.9±1.7 Mpc/h; b~10

For z > 3.5:

r0=24.3±2.4

b~15

Shen et al. 2007

slide33

Use ellipsoidal collapse model (Sheth, Mo & Tormen, 2001) to turn estimates of bQinto mass of halos hosting UVX quasars.

  • Find very little evolution in halo mass with redshift.
  • Our mean halo mass of ~5x1012h-1MSolar is halfway between characteristic masses from Croom et al. (2005) and Porciani et al. (2004).
  • This is comparable to the mass of galaxy groups, supporting the idea that quasars are triggered by mergers.
hierarchical halo merging
Lacey & Cole (1993)

Typical quasar hosts double in mass every Gyr or so

Constancy of quasar host halo mass thus limits quasar lifetime to around 106.5 to 107.5 yrs

Hierarchical Halo Merging

CDM theory tells us the expected space density of halos. Comparing with the observed quasar density allows us to determine the fraction of time a quasar is shining.

Time for 2x Mass

Time

Mass

clustering s luminosity dependence
Clustering’s Luminosity Dependence

Lidz et al. 2006

old model

new model

  • Quasars accreting over a wide range of luminosity are driven by a narrow range of black hole masses
  • M- relation mean a wide range of quasar luminosities will then occupy a narrow range of MDMH
no l dependence for quasars
No L Dependence for Quasars

galaxies

quasars

Zehavi et al. 2005

Shen et al. 2007

what next
What Next?

Measuring bias of faint high-z quasars will break degeneracies between feedback models.

faint quasars (e.g., LSST)

bright quasars (e.g., SDSS)

Richards et al. 2006

Hopkins et al. 2007

what we used to expect
What We (Used To) Expect

Galaxies (and their DM halos) grow through hierarchical mergers

Quasars inhabit rarer high-density peaks

If quasars long lived, their BHs grow with cosmic time

MBH-σ relation implies that the most luminous quasars are in the most massive halos.

More luminous quasars should be more strongly clustered (b/c sample higher mass peaks).

QLF from wide range of BH masses (DMH masses) and narrow range of accretion rates.

what we get
What We Get

Galaxies (and their DM halos) grow through hierarchical mergers

Something causes the growth of galaxies and their BHs to terminate even as DM halos continue to grow

Quasars always turn on in potential wells of a certain size (at earlier times these correspond to relatively higher density peaks).

Quasars turn off on timescales shorter than hierarchical merger times, are always seen in similar mass halos (on average).

MBH-σ relation then implies that quasars trace similar mass black holes (on average)

Thus little luminosity dependence to quasar clustering (L depends on accretion rate more than mass).

Need a wide range of accretion rates for a narrow range of MBH to be consistent with QLF.