Illuminating the Dark Ages: Luminous Quasars in the Epoch of Reionisation. Bram Venemans MPIA Heidelberg
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1 Illuminating the Dark Ages: Luminous Quasars in the Epoch of Reionisation Bram Venemans MPIA Heidelberg Workshop The Reionization History of the Universe Bielefeld University, March
2 History of the Universe Big Bang Years after the Big Bang million 1 billion 13.8 billion Dark Ages Today Credits: NRAO Redshift
3 Recombination Big Bang History of the Universe Years after the Big Bang million 1 billion 13.8 billion Dark Ages Today Credits: NRAO Redshift
4 History of the Universe Recombination Big Bang Formation of first luminous sources Years after the Big Bang million 1 billion 13.8 billion Dark Ages Today Credits: NRAO Redshift
5 The Epoch of Reionisation (EoR) Recombination Big Bang Formation of first luminous sources Years after the Big Bang million 1 billion 13.8 billion Dark Ages Today Credits: NRAO Redshift
6 Constraints on reionisation from CMB Neutral Ionized Neutral fraction xhi, Neutral fraction Planck XLVII 2016 CMB + ksz + z 6 quasars Redshift Redshift Time (Gyr)? 6 Planck XLVII 2016
7 The first sources: galaxies in the EoR z= Example of galaxies in the Hubble Ultra Deep Field: very faint (mag 26) difficult to confirm their distance nearly impossible to measure properties JWST (launch 2019) Bouwens+ 2016
8 High luminosity objects: quasars - powered by accreting black holes - brightest sources in universe - UV/optical spectrum: power-law cont. by accretion disk + broad emission lines - line width+continuum black hole mass
9 Quasars: beacons in the early Universe Luminous quasar are found up to! > 7: >10 9 M black holes exist within first Gyr Hosted by starburst galaxies (SFR > 100 M /yr) Study the formation of massive galaxies Excellent probes of the Epoch of Reionisation
10 Quasars: sources of UV photons Lyα + luminous + very blue + high escape fraction Wavelength (Å) Lusso+ 2015
11 High-! quasar luminosity function! = 6 Willott Onoue+ 2017
12 Ionising photon production of quasars Probability factor ~20 Needed to keep Universe reionised at! ~ 6 Willott Onoue Log ionising photon emission density
13 Probes of the Intergalactic Medium (IGM)
14 Quasars: probes of the EoR Use quasars to X-ray the early Universe Investigate redshift evolution of absorption in the Lyα forest ionised region around quasars (near zone) damping wing 08/03/2018 Luminous Quasars in the Epoch of Reionisation, Bielefeld University Bram Venemans
15 Quasar absorption due to Lyα forest Credits: B. Keel, N. Wright Strong absorption at! > 6 Fan+ 2006
16 Probing the neutral IGM 8400 Wavelength (Å) SDSS J Lyβ Flux density Flux (10-18 erg cm -2 s -1 A -1 ) Redshift Redshift Wavelength SDSS J Lyα Lyβ Lyα Redshift e.g. White+ 03
17 Evolution of the optical depth Optical depth Redshift
18 Evolution of the optical depth Optical depth GP (z) ¼ 1:8 ; 10 5 h 1 1=2 m b h 2 1 þ z 0:02 7 3=2 n H i n H (Gunn & Peterson 1965) Redshift
19 X HI from Lyα forest 10-3 Neutral Hydrogen <F HI > V 10 3 Absorption saturates at X HI ~ 10-4 fraction X HI gure z ! e.g. Fan+ 2006
20 Lyα absorption saturates 30 hour spectrum with the VLT of a quasar at!=7.1 Barnett+ 2017
21 Weak constraints on X HI from Lyα forest X HI 10-4 Barnett+ 2017
22 Dark pixel statistics Count fraction of zero flux pixels upper limit on X HI + Not dependent on model or quasar spectrum Reionisation ending at!~6 McGreer+ 2015
23 Quasar ionisation regions HI HII R NZ
24 Quasar ionisation regions Quasar near zone: HI R NZ ~ X HI -1/3 (t Q L) 1/3 (e.g. Fan+ 2006) HII X HI neutral H fraction t Q quasar age L quasar luminosity R NZ
25 Quasar ionisation region Distance to quasar (Mpc) Normalised flux density R p R NZ Lyα at! Q Wavelength Eilers Patzer Co!oquium December 8th, 2
26 Quasar ionisation region Near zone sizes scaled to same luminosity Fan Carilli BV+ 2015
27 Quasar ionisation region Decreasing near zone, increasing X HI at!=6 7 X HI few % at "=7 factor 6.5 Fan Carilli BV+ 2015
28 However: near zone ionisation front New simulations show: R NZ ~ L 1/2.35 R NZ (proper Mpc) R NZ ~ L 1/3 Simulations M 1450 Eilers see also Bolton & Haehnelt 2007
29 Shallower trend with redshift Recent publications: New observations Higher S/N Homogeneous analysis Better systemic redshifts R NZ (Mpc) + simulations show same trend for neutral and ionised IGM neutral IGM ionised IGM Eilers Redshift 6.6
30 Shallower trend with redshift Recent publications: New observations Higher S/N Homogeneous analysis Better systemic redshifts + simulations show same trend for neutral and ionised IGM R NZ (Mpc) ionised IGM Eilers Redshift 6.6
31 Near zone size as function of age ~10% of quasars have a very small R NZ No evidence for proximate DLAs Short quasar lifetime of t Q < 10 5 yr R NZ (Mpc) Quasar lifetime 1 Myr? Inconsistent with rapid growth of black holes Log t Q (years) Eilers+ 2017
32 IGM damping wing Damping wing of the IGM: sensitive to neutral fractions >0.1 challenge: unknown intrinsic spectrum see, e.g., Miralda-Escude 1998
33 Tentative detection of damping wing J at!=7.1 shows a damping wing signature (Mortlock+ 11): X HI = 0.4 +/- 0.2 However, claim disputed Bosman & Becker 2015: no need for damping wing Mortlock+ 2011; see also Bolton+ 2011; Greig+ 2016
34 Principle Component Analysis Wavelength Davies Model red side of spectrum to predict blue side Use! 2 quasars as training set
35 Damping wing modeling Model IGM neutral fraction and quasar age simultaneously log t Q (years) X HI Davies+ 2018; Bolton+ 2011
36 Evolution of neutral Hydrogen fraction Neutral xhi, Neutral fraction X HI Planck XLVII 2016 CMB + ksz + z 6 quasars 9 Redshift Redshift Time (Gyr) Time (Gyr) 7 6
37 Evolution of neutral Hydrogen fraction Neutral xhi, Neutral fraction X HI Planck XLVII 2016 CMB + ksz + z 6 quasars 9 Redshift Redshift z =7.1 QSO damping wing Time (Gyr) Time (Gyr) 7 6
38 Evolution of neutral Hydrogen fraction Neutral xhi, Neutral fraction X HI Planck XLVII 2016 CMB + ksz + z 6 quasars 9 Redshift Redshift z =7.1 QSO damping wing Time (Gyr) Time (Gyr) 7 6
39 New quasar at record redshift:!=7.54! Age of universe: 690 Myr à ~10% younger than at!=7.1 Z J1 J H Ks Observed wavelength (µm) f (10 18 erg s 1 cm 2 Å 1 ) Transmission Z Ly C IV C III] Mg II J1 J H Ks Observed wavelength (µm) Bañados, BV+ 2018
40 New quasar at record redshift:!=7.54! Very accurate measurement of systemic redshift BV+ 2017
41 IGM damping wing at!=7.5 Observed wavelength (µm) f 6 PDF Rest frame wavelength (Å) Lyα at systemic redshift Bañados, BV x HI X HI
42 Neutral xhi, Neutral fraction X HI Reionisation occurred late? Lyα at systemic Redshift redshift Planck XLVII 2016 CMB + ksz + z 6 quasars Redshift 2 1 J damping wing Bañados et al Time (Gyr) Time (Gyr) C A B Bañados, BV
43 Conclusions Luminous quasars are ideal objects to study the Epoch of Reionisation Quasar do not contribute to ionising photon density Analysis of Lyα forest suggests reionisation ended around!=6 Size of near zones insensitive to neutral fraction Damping wing in two most distant quasars indicate a highly neutral Universe at!>7
44 Conclusions Luminous quasars are ideal probes to study the Epoch of Reionisation Quasar do not contribute significantly to the ionising photon rate density Analysis of Lyα forest suggests reionisation ended around!=6 Size of near zones insensitive to neutral fraction Damping wing in two most distant quasars indicate a highly neutral Universe at!>7 Probability factor ~20 Log ionising photon emission density
45 Conclusions Luminous quasars are ideal probes to study the Epoch of Reionisation Quasar do not contribute significantly to the ionising photon rate density Analysis of Lyα forest suggests reionisation ended around!=6 Size of near zones insensitive to neutral fraction Damping wing in two most distant quasars indicate a highly neutral Universe at!>7 Probability factor ~20 Log ionising photon emission density
46 Conclusions Luminous quasars are ideal probes to study the Epoch of Reionisation Quasar do not contribute significantly to the ionising photon rate density Analysis of Lyα forest suggests reionisation ended around!=6 Size of near zones insensitive to neutral fraction Damping wing in two most distant quasars indicate a highly neutral Universe at!>7 Probability factor ~20 Log ionising photon emission density xhi, Neutral fraction Planck XLVII 2016 CMB + ksz + z 6 quasars Redshift J damping wing Bañados et al Time (Gyr) C A B 7 6
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