The technicolor "big picture" of black hole evolution: Multiwavelength views of AGN, galaxies, and largescale

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1 The technicolor "big picture" of black hole evolution: Multiwavelength views of AGN, galaxies, and largescale structures Image courtesy ESO AGN clustering workshop 2014 Ryan C. Hickox AGN: what s in a name? ESO, Garching 1 July 2016

2 A galaxy An AGN The big question: How is black hole growth connected to the growth of galaxies and large-scale structures?

3 Some context: Galaxies and halos Mhalo ~ 1013 M Moster et al. (2010) Redder More star formation Mhalo 1012 M More luminous Galaxy formation is most efficient in 12 ~10 M halos Blanton (2006)

4 objects populate dark matter halos two-point correlation function

5 Optical quasars reside in halos of ~constant mass with redshift exhausted systems QSOs maximal quenching star-forming systems See Alexander & Hickox (2012) for references

6 Infrared optical/uv X-ray LUMINOSITY CUTS: X-ray, radio COLOR/SPECTRAL CUTS: Infrared, optical/uv Very different selection effects! (e.g. Hopkins, Hickox et al., 2009) Radio C. Harrison PhD thesis (2014)

7 TAKE-HOME MESSAGE 1: To fully understand the full AGN population, need to select and study sources in multiple wavebands

8 Infrared optical/uv X-ray Radio

9 Mackenzie Jones (PhD student) optical/uv X-ray POSTER B6 Infrared optical/uv Infrared X-ray Parker Gardner (undergrad) Raphael Hviding (undergrad) POSTER G8 POSTER B5 Radio Vivyan Yan (PhD student) Chris Carroll (PhD student) POSTER F2 Mike DiPompeo (postdoc) Parker Gardner (undergrad) POSTER G6 Kevin Hainline (now postdoc at Steward) TALK YESTERDAY Chien-Ting Chen (now postdoc at Penn State) Infrared optical/uv X-ray

10 An example: Hickox et al. (2009) AGN populations at z ~ 0.5 (observed; uncorrected for depth, etc.) Radio: Lbol/LEdd < 10-3 X-ray: 10-3 < Lbol/LEdd < 1 IRAC: Lbol/LEdd > 10-2

11 Redder Radio X-ray Infrared IRAC Galaxy luminosity Redder Hickox et al. (2009)

12 Radio X-ray QSOs exhausted systems maximal quenching IRAC star-forming systems

13 Radio exhausted systems X-ray QSOs maximal quenching High-Eddington, radiative AGN X-ray, Infrared, optical/uv are found in star-forming halos Mechanical AGN (mostly low-eddington) radio are found in massive, passive halos IRAC star-forming systems

14 Rujopakarn et al. (2010) Assef et al. (2010) Cowley et al. (2016) Kozlowski et al. (2013) Hickox et al. (2009) Juneau et al. (2013) Mendez et al. (2013)

15 Rujopakarn et al. (2010) Assef et al. (2010) Cowley et al. (2016) Kozlowski et al. (2013) Hickox et al. (2009) Mendez et al. (2013) Juneau et al. (2013) Mendez et al. (2013)

16 SFRs, colors, and masses Radio Radio X-ray z~0.1 z~0.5 z~1.0 Optical Infrared Infrared Ellison et al. (2016) Goulding et al. (2014) Infrared Cowley et al. (2016) X-ray Radio X-ray Also MOSDEF (Alison Coil s talk today) Radio Infrared Mendez et al. (2015)

17 Average black hole accretion tracks star formation Average BH accretion rate star formation rate Hickox et al. (2014)

18 TAKE-HOME MESSAGE 2: Efficient BH growth broadly follows star formation, and AGN hosts are otherwise indistinguishable from normal galaxies of similar mass

19 The importance of stochasticity in the AGN population [OIII] light echoes from AGN (Keel et al. 2014) Hickox et al. (2014)

20 The importance of stochasticity in the AGN population [OIII] light echoes from AGN (Keel et al. 2014) Must think of AGN in terms of probability distributions Hickox et al. (2014)

21 The AGN Eddington ratio distribution How likely is an black hole to be active as a function of L/LEdd? star-forming Aird et al. (2016, in prep) Jones et al. (2016) POSTER B6

22 The AGN halo occupation distribution How likely is a DM halo to host an AGN as a function of halo mass? Are AGN primarily in central or satellite halos? The HOD formalism One-halo term Two-halo term Miyaji et al. (2011) satellites centrals Also direct measures of AGN HOD flat or declining with halo mass? (e.g., Allevato et al. 2012; Martini et al. 2013, DiPompeo et al. 2016) Credit: I. Kayo

23 TAKE-HOME MESSAGE 3: AGN activity is a stochastic process, and we need to measure the distribution of AGN properties

24 Di Matteo et al. (2005) Obscured quasars as an evolutionary phase? Alexander & Hickox (2012) obscured unobscured obscured fraction DiPompeo et al. (2014, 2015a,b, 2016) star formation rate Chen et al. (2015)

25 TAKE-HOME MESSAGE 4: Some support for evolutionary models of obscured quasars?

26 Take-home messages 1. To fully understand the full AGN population, need to select and study sources in multiple wavebands 2. Efficient BH growth broadly follows star formation, and AGN hosts are otherwise indistinguishable from normal galaxies of similar mass 3. AGN activity is a stochastic process, and we need to measure the distribution of AGN properties 4. Some support for evolutionary models of obscured quasars? Thanks to

27 We look forward to seeing many of you next month!

The High-Redshift Universe Bologna, June 5-6

The High-Redshift Universe Bologna, June 5-6 Why a workshop on the High-redshift Universe? To report on the state of the art in the high-redshift Universe field To combine expertise in high-redshift AGN