Quasars in the epoch of reioniza1on

Transcription

1 Big Bang Dark Ages Quasars in the epoch of reioniza1on Carnegie-Princeton Fellow Illumina9ng the Dark Ages June 27, Heidelberg, Germany Universe Today

2 Quasars and galaxies in the reioniza1on epoch

3 Quasars as a phase of a galaxy

4 Outline The search of the most distant quasars (z>5.5) Quasars as probes of the intergalac9c medium Quasar host galaxies

5 The search for distant quasars The challenge: Quasars at z>5.5 are very rare Not found in deep HST blank fields Requirement: Large area mul9-color surveys

6 The search for distant quasars M Redshift 1 2 z>5.6 quasars Total = Year

7 The search for distant quasars M Redshift 1 2 See talk by Linhua Jiang z>5.6 quasars Total = 23 SDSS Year Fan+ 2-26

8 The search for distant quasars M Redshift 1 2 See talk by Linhua Jiang z>5.6 quasars Total = 56 SDSS Stripe 82 CFHQS UKIDSS Year Fan Jiang Willoc

9 The search for distant quasars M Redshift 1 2 See talk by Linhua Jiang z>5.6 quasars Total = 58 SDSS Stripe 82 CFHQS UKIDSS Year Fan Jiang Willoc Mortlock+ 211

10 The search for distant quasars M Redshift 1 2 See talks by Chiara Mazzucchelli, Sophie Reed, and Yoshiki Matsuoka z>5.6 quasars Total = 179 SDSS Stripe 82 CFHQS UKIDSS PanSTARRS VIKING DES, HSC Year Bañados Jiang+ 215 Venemans+213,215 Reed+ 215 Matsuoka+216

11 The search for distant quasars M Redshift 1 2 Pan-STARRS Sample See talks by Chiara Mazzucchelli, Sophie Reed, and Yoshiki Matsuoka z>5.6 quasars Total = 179 SDSS Stripe 82 CFHQS UKIDSS PanSTARRS VIKING DES, HSC Year Bañados+ 214,215,216 Venemans, Bañados+ 215 Mazzucchelli+ in prep.

12 The search for distant quasars M PanSTARRS DES SDSS PanSTARRS DES HSC Redshift 1 2 See talks by Chiara Mazzucchelli, Sophie Reed, and Yoshiki Matsuoka z>5.6 quasars Total = 179 SDSS Stripe 82 CFHQS UKIDSS PanSTARRS VIKING DES, HSC Year

13 Variety of spectral proper9es Ly N V Si II O I + Si II Si IV +OIV] 12 f (Arbitrary units) 8 Strong Ly Weak Ly 4 PS1 high composite z N Rest frame wavelength (Å) Bañados+ subm.

14 Variety of spectral proper9es Ly N V Si II O I + Si II Si IV +OIV] 12 Weak-line quasars: 14% at z=6 1-6% at z=2-4 f (Arbitrary units) 8 4 Strong Ly Weak Ly Diamond-Stanic+ 29 Bañados+ 214, 216 subm. N 11 8 PS1 high composite z Rest frame wavelength (Å) Bañados+ subm.

15 Radio-loud frac9on Bañados+ 215a

16 Radio-loud frac9on Bañados+ 215a

17 Does it evolve with redshim?? Bañados+ 215a

18 No evolu9on up to z=6 Bañados+ 215a

19 The most distant quasar M Redshift 1 2 See talks by Chiara Mazzucchelli, Sophie Reed, and Yoshiki Matsuoka z>5.6 quasars Total = 179 SDSS Stripe 82 CFHQS UKIDSS PanSTARRS VIKING DES, HSC Year

20 The most distant quasar Quasar at z=7.1 (Age of Universe:.75 Gyr) Black hole mass: 2 x 1 9 M M 145 = J AB = 2.4 Mortlock + 211

21 The most luminous and massive quasar M Redshift 1 2 z>5.6 quasars Total = 179 SDSS Stripe 82 CFHQS UKIDSS PanSTARRS VIKING DES, HSC Year

22 The most luminous and massive quasar Flux (1 16 erg s 1 cm 2 Å 1 ) Lyα C IV.4.35 Mg II Fe II PL 2,7 2,8 2,9 3, Rest-frame wavelength (Å) Mg II z=6.3 (Age of Universe:.88 Gyr) Black hole mass: 12 x 1 9 M M 145 = J AB = Observed wavelength (Å) Wu+ 215

23 Constraints on black hole growth Black hole mass (M ) Time (Gyr) M at z = M at z =6.3 L Bol =.5 L Edd L Bol =L Edd Redshift 15 1 But see also Volonteri+ 215, La9f+ 216, Li+ 27, Inayoshi+ 216

24 Quasars as probes of the IGM

25 Quasars as probes of the IGM Flux Wavelength Eilers+ in prep.

26 End of reioniza9on at z~6 Neutral Hydrogen Fan+ 26 Gunn-Peterson effect saturates at low neutral frac9on x HI <1 4 Redshim See also Becker+ 215 and McGreer+ 215

27 Quasar ioniza9on regions Near zone size: R ~ x HI -1/3 (Fan+ 26, Carilli+ 21) Quasar near zone (Mpc) But see also: Anna-Chris9na Eilers talk Bolton & Haehnelt 27 Kea9ng+ 215 Redshim Venemans, Bañados+ 215

28 IGM damping wing IGM absorp9on profile Transmiced Flux Sensi9ve to neutral IGM: x HI >.1 Wavelength Miralda-Escude 1998

29 First IGM damping wing at z~7? z=7.1 quasar (Mortlock+ 211) See also: Bradley Greig s talk Simcoe+ 212 Schroeder+ 213 Greig+ 216 Fig. 1 Estimated transmission towards the z = 7.8 quasar ULAS J obtained by dividing the observed spectrum by a model for its intrinsic emission based on lower redshift quasar spectra [29]. The resultant systematic uncertainty is shown at the bottom in red, along with the observational noise in black. Shown in blue are theoretical IGM damping wing profiles for the default No consensus on IGM absorp9on nature: e.g., Bosman & Becker 215

30 IGM damping wing Greig & Mesinger 1..8 Neutral Fraction,xH I But see also Bosman & Becker 215 z=7.1 QSO Damping wing 2 1 Dark pixels (1 ) Ly fraction (1 ) LAE Clust. (1 ) QSO DW (1 ) Planck (2 ) ksz (2 ). [h] Redshift, z Constraints on the EoR history, including all of the above-mentioned observational priors: (i) the dark fraction (McGreer et al. 2 Greig & Mesinger 216 Greig+ 216

31 IGM damping wing at z=6.4? f (1 17 erg s 1 cm 2 Å 1 ) Observed wavelength (Å) Bañados+ in prep.

32 Proximate DLA at z=6.4 DLA z = log N HI = 2.7 f (1 17 erg s 1 cm 2 Å 1 ) Observed wavelength (Å) Bañados+ in prep.

33 Proximate DLA at z=6.4 Normalized Flux Mg II 283 Fe II 2382 Si II 1526 Si II 134 Si II Relative velocity (km/s) Bañados+ in prep Mg II 2796 Al II 167 CII 1334 OI Relative velocity (km/s) ) ((. ( ) +8)6/7. ( ) 12++)-3(. ( ) *+),(-. ++),,/. ( ( /(( -(( ( -(( /(( /(( -(( ( -(( /(( v"#$%&' v"#$%&' Figure 2: Continuum-normalized spectral regions where key heavy z=7.41 if the absorber z=7.1 were quasar, typical of Simcoe+ a low redshift 212 DLA. 1" err the extraction aperture is indicated with horizontal bars. A Voigt pr by our column density upper limit is shown in red for each panel. V ) ( ) ( ) ( ) 45++)3(7. 9:++-;<

34 Quasar host galaxies

35 Quasar host galaxies Really hard (impossible?) in the UV/Op9cal (e.g., Decarli+ 212, Mechtley+ 212, Emanuele Farina s talk) Possible in the sub-mm/radio (e.g., see talks by Ran Wang, Bram Venemans, and Roberto Decarli) WALTER ET AL.The cer of molecbertoldi et al. nt, dense, and formation) is (a redshift of of 87 Myr, QL p.73, Astrophysical Journal, 773:44 Vol. 615(1pp), 213 August 1 CO at z=6.4 [CII] at z=6. servations of obtained with the first time, parsec scales constrain its s. al. (23) dej , p The ations at 1. 5 ndicated that d spectral res- Walter+ 24 Wang+ 213 Fig. 1. CO (3 2) map of J of the combined B- and C-array data sets (covering the total bandwidth, 37.5 MHz or 24 km s"1). Contours are shown at "2, "1.4, 1.4, 2, 2.8, and 4 # j (1 j p 43 mjy beam"1). The beam size (.Eduardo Bañados 35 #. 3) is shown in the bottom left corner; the plus sign

36 Quasar host galaxies [CII] 158um fine structure line: Principal ISM coolant Traces regions of ac9ve star forma9on One of the brightest lines in star-forming galaxies z > 5 à redshim to mm bands J at z=6.42 P36+3 at z=6.54 [CII] H 2 O Walter+ 29 Bañados+ 215b

37 ALMA [CII] survey [C I] [C I] [C I] 8.7kpc 2 [C I] 47kpc [C I] [C I] 6kpc [C I] [C I] 61kpc [C I] More in Roberto Decarli s talk

38 Bright ALMA companions... [C I] [C I] [C I] 8.7kpc 2 [C I] 47kpc [C I] [C I] 6kpc [C I] [C I] 61kpc [C I] See also Bañados+ 213 More in Roberto Decarli s talk

39 Summary & Outlook Summary Quasars are ideal targets to study the early universe Sample of ~2 quasars and increasing Mul9wavelength characteriza9on on-going ALMA, VLA, HST, Spitzer, Muse, Op9cal/NIR spectroscopy Outlook Push the redshim barrier (Euclid, WFIRST, LSST, ) QSO host galaxies and environments with ALMA Rest-frame op9cal proper9es with JWST (BH masses) Radio-loud quasars for 21cm forest with SKA