Big and young SMBHs in the early Universe

Colloquium talk given at ASTRON/JIVE (Dwingeloo, The Netherland)

1. BIG AND YOUNG SMBHS IN THE EARLY UNIVERSE TULLIA SBARRATO UNIVERSITÀ DEGLI STUDI DI MILANO-BICOCCA in collaboration with: G. Ghisellini, G. Tagliaferri, F. Haardt, and the NuSTAR blazar scientific team ASTRON/JIVE, 12 November 2015
2. ACTIVE GALACTIC NUCLEI ASTRON/JIVE, 12 November 2015 Urry & Padovani 1995
3. ACTIVE GALACTIC NUCLEI ASTRON/JIVE, 12 November 2015 Blazar Urry & Padovani 1995
4. BLAZAR: SPECTRAL ENERGY DISTRIBUTION Fossati et al. 1998 Donato et al. 2001 ASTRON/JIVE, 12 November 2015
5. BLAZARS: A REAL SED torus corona disc ASTRON/JIVE, 12 November 2015
6. QUESTIONS What do we observe at very high redshift? Looking for blazars at high redshift …
 
 What can we learn about formation of the first SMBHs? ASTRON/JIVE, 12 November 2015 what is the population of jetted quasars at high z? what is the role of the jet in SMBH early formation?
7. WHAT DO WE OBSERVE AT VERY HIGH REDSHIFT?
8. WHAT DO WE OBSERVE AT VERY HIGH REDSHIFT? THE HIGHEST REDSHIFT ASTRON/JIVE, 12 November 2015 Mortlock et al. 2011 M ⇠ 2 ⇥ 109M z = 7.085
9. WHAT DO WE OBSERVE AT VERY HIGH REDSHIFT? THE MOST MASSIVES ASTRON/JIVE, 12 November 2015
10. WHAT DO WE OBSERVE AT VERY HIGH REDSHIFT? THE MOST MASSIVES ASTRON/JIVE, 12 November 2015 non-jetted quasar: SDSS J0100+2802 M ' 1010M z = 6.30 { Wu et al. 2015
11. WHAT DO WE OBSERVE AT VERY HIGH REDSHIFT? THE MOST MASSIVES ASTRON/JIVE, 12 November 2015 jetted quasar: SDSS J0306+1853 M ' 1010M z = 5.363 { Wang et al. 2015
12. WHAT DO WE OBSERVE AT VERY HIGH REDSHIFT? FOCUS ON JETTED SOURCES ASTRON/JIVE, 12 November 2015 extremely massive blazars at z>4 efficiently trace their parent population project to systematically look for and classify new blazars! M > 109M
13. LOOKING FOR BLAZARS AT HIGH Z
14. LOOKING FOR BLAZARS AT HIGH Z WHY BLAZARS? finding extremely massive SMBHs hosted in jetted AGN constraints on SMBH formation models clues on jets role in SMBH formation M > 109M z > 4 ✓b = 1/ ✓v ASTRON/JIVE, 12 November 2015
15. LOOKING FOR BLAZARS AT HIGH Z WHY BLAZARS? finding extremely massive SMBHs hosted in jetted AGN constraints on SMBH formation models clues on jets role in SMBH formation M > 109M z > 4 ✓b = 1/ ✓v ✓v < 1/ 2 2 ⇠ 340 450 ASTRON/JIVE, 12 November 2015 viewing angle: analogous jetted AGN, randomly oriented:
16. LOOKING FOR BLAZARS AT HIGH Z each blazar counts for ~340-450 jetted AGN not aligned efficiently provide clues on jet-accretion relation But: very few blazars known at z>4, all serendipitous ASTRON/JIVE, 12 November 2015 WHY BLAZARS?
17. LOOKING FOR BLAZARS AT HIGH Z each blazar counts for ~340-450 jetted AGN not aligned efficiently provide clues on jet-accretion relation But: very few blazars known at z>4, all serendipitous SYSTEMATIC SEARCH! ASTRON/JIVE, 12 November 2015 WHY BLAZARS?
18. LOOKING FOR BLAZARS AT HIGH Z SERENDIPITOUS LOW Z HIGH Z ASTRON/JIVE, 12 November 2015 high redshift most powerful most massive
19. LOOKING FOR BLAZARS AT HIGH Z SERENDIPITOUS LOW Z HIGH Z ASTRON/JIVE, 12 November 2015 high redshift most powerful most massive
20. LOOKING FOR BLAZARS AT HIGH Z SERENDIPITOUS LOW Z HIGH Z ASTRON/JIVE, 12 November 2015 high redshift most powerful most massive
21. LOOKING FOR BLAZARS AT HIGH Z SYSTEMATIC SEARCH ASTRON/JIVE, 12 November 2015 naked disc blazars found in optical quasar catalogs SDSS + FIRST quasar catalog z > 4 radio—detected >1mJy R > 100 105783 1248 53 31 R = F5GHz /FB
22. LOOKING FOR BLAZARS AT HIGH Z SYSTEMATIC SEARCH ASTRON/JIVE, 12 November 2015
23. LOOKING FOR BLAZARS AT HIGH Z SYSTEMATIC SEARCH ASTRON/JIVE, 12 November 2015 Sbarrato et al. 2013a disc emission fitted with 
 Shakura—Sunyaev model standard accretion on a non—spinning BH?
24. LOOKING FOR BLAZARS AT HIGH Z SUCCESSFUL CLASSIFICATIONS ASTRON/JIVE, 12 November 2015 Sbarrato et al. 2012; 2013b best blazar candidate: z = 5.3 R ⇠ 5200 F1.4GHz = 260mJy log Ld = 46 . 95 MBH = 2.8 ⇥ 109M NuSTAR + Swift/XRT 
 observations: hard and strong X-ray flux = 13 ✓v = 3 blazar!!
25. LOOKING FOR BLAZARS AT HIGH Z B2 1023+25: seen under viewing angle smaller than beaming angle SUCCESSFUL CLASSIFICATIONS ASTRON/JIVE, 12 November 2015 BUT: SDSS+FIRST covers ~1/4 of the sky = 13 ✓v = 3 } ✓v < 1/ 2 2 = 338 by classifying B2 1023+25 we can infer the presence of at least ~1540 analogous jetted quasars, randomly oriented
26. WHAT CAN WE LEARN ABOUT SMBH FORMATION?
27. WHAT CAN WE LEARN? ASTRON/JIVE, 12 November 2015 HOW MANY SMBHS DO THEY TRACE? SDSS+FIRST @ z>4: 11 blazars expected parents: ~3700 jetted quasars
28. WHAT CAN WE LEARN? ASTRON/JIVE, 12 November 2015 HOW MANY SMBHS DO THEY TRACE? SDSS+FIRST @ z>4: 11 blazars expected parents: ~3700 jetted quasars
29. WHAT CAN WE LEARN? ASTRON/JIVE, 12 November 2015 WHY DON’T WE SEE THE PARENT POPULATION? HOW MANY SMBHS DO THEY TRACE? SDSS+FIRST @ z>4: 11 blazars expected parents: ~3700 jetted quasars
30. WHAT CAN WE LEARN? ASTRON/JIVE, 12 November 2015 LACK OF MISALIGNED JETS are we missing radio or optical emission? discrepancy of a factor ~70 arises already at z~3, even if less pronounced
31. WHAT CAN WE LEARN? ASTRON/JIVE, 12 November 2015 CMB QUENCHING Ghisellini et al. 2014 UCMB / (1 + z)4 CMB energy density at z~3 becomes competitive with magnetic energy density of quasar lobes
32. WHAT CAN WE LEARN? ASTRON/JIVE, 12 November 2015 CMB QUENCHING Ghisellini et al. 2014 UCMB / (1 + z)4 CMB energy density at z~3 becomes competitive with magnetic energy density of quasar lobes
33. WHAT CAN WE LEARN? ASTRON/JIVE, 12 November 2015 CMB QUENCHING Ghisellini et al. 2014 UCMB / (1 + z)4 CMB energy density at z~3 becomes competitive with magnetic energy density of quasar lobes RADIO EMISSION IS QUENCHED! blazars: 
 best tracer for jetted quasars!
34. WHAT CAN WE LEARN? ASTRON/JIVE, 12 November 2015 INNER JET NOT QUENCHED! Frey et al. 2015 B2 1023+25
 @ 1.7 GHz @ 5 GHz
35. WHAT CAN WE LEARN? ASTRON/JIVE, 12 November 2015 HIGH MASSES AT HIGH REDSHIFT!
36. WHAT CAN WE LEARN? ASTRON/JIVE, 12 November 2015 HIGH MASSES AT HIGH REDSHIFT! updated from
 Sbarrato et al. 2015
37. WHAT CAN WE LEARN? ASTRON/JIVE, 12 November 2015 HIGH MASSES AT HIGH REDSHIFT! updated from
 Ghisellini et al. 2013 Ld = ⌘d ˙ Mc2 standard accretion at Eddington rate
38. WHAT CAN WE LEARN? ASTRON/JIVE, 12 November 2015 HIGH MASSES AT HIGH REDSHIFT! updated from
 Ghisellini et al. 2013 Ld = ⌘d ˙ Mc2 ⌘ = ⌘d + ⌘B standard accretion at Eddington rate … but what about the jet?
39. CONCLUSIONS blazars are efficient tracers of jetted AGN hosting extremely massive BHs at high redshift two different formation epochs for highly massive BHs: jetted systems preferentially form at z ~ 4
 non-jetted systems at z ~ 2-2.5 it’s hard to form such massive BHs in the early Universe
 the presence of a jet speeds up the process huge lack of misaligned AGN: CMB quenching? ASTRON/JIVE, 12 November 2015