Shedding light on hyperluminous quasars at the golden epoch of AGN/galaxy coevolu<on L. Zappacosta (INAF- OAR) E. Piconcelli, S. Martocchia, F. Fiore, M. BischeL, A. Bongiorno, F. Duras, G. Vietri (INAF- OAR), M. Brusa, G. Lanzuisi (INAF- OABO), C. Vignali (Univ. Bologna), S. Bianchi (Univ Roma Tre), C. Feruglio (SNS)
Hun<ng for the most luminous monsters Adapted from Alexander & Hickox 2012 Obscured quasar Dust- enshrouded High obscura<on High SFR Blow- out phase AGN- driven winds Feedback in ac<on Unobscured QSO Blue Op<cally bright X- ray unobscured Aim: probe and study the AGN- driven feedback phase? From theory: the strength of ouilows is proporaonal to L bol 0.5 (Menci et al. 2008, Faucher- Giguère & Quataert 2012) The most luminous QSOs at the epoch in which their acavity peaks (2<z<4) Efficient IR selec<on: search for dust- reddened/ir loud QSOs over large sky areas
Dust enshrouded phase: Hot Dust Obscured Galaxies (Hot DOGs) ~1000 Hot DOGs at z~2.5 - WISE All Sky survey W1W2- dropout (Eisenhardt et al. 2012) (3.4/4.6μm undetected/faint, 12/22 μm detected) Wu et al. 2012 Hot Dust Obscured Galaxies High MIR/submm à Hot dust Hyperluminous à L bol > 10 13-14 L In overdense regions (Jones+2014) Extended Lyα blobs à QSO feedback op<cal narrow lines (mainly) X- ray obscured (Stern et al. 2014) Bridge et al. 2013 W1/W2 W3/W4 W1W2- dropout Assef et al. 2015 Rare, hyperluminous, obscured à Short- lived obscured QSO phase
First X- ray spectrum of a Hot DOG: A heavily buried QSO at z=2.3 W1835+4355: First X- ray spectrum of a Hot DOG Flat spectrum (Γ~0.8) Reflec<on dominated Strong Fe line complex (cold, ionized, EW > 1 kev) SED filng L bol =1.3 10 14 L ~75% of L IR à QSO SFR ~ 2000 M /yr XMM- PN XMM- MOS Piconcelli, Vignali, Bianchi, LZ et al. 2015
NuSTAR observa<on: peering through the obscurer Detected in 150 ks NuSTAR observa<on 35 and 16 net- counts in FPMA and FPMB. 57:00.0 FPMA 57:00.0 FPMB First W1W2- dropout detected by NuSTAR! 43:56:00.0 43:56:00.0 Broad- band spectrum: 0.5-24 kev 55:00.0 42.0 38.0 34.0 18:35:30.0 26.0 55:00.0 42.0 38.0 34.0 18:35:30.0 26.0 Model: absorbed power- law + Compton reflec<on + Gaussian for Fe XXV line + low energy scapered component N H = 1.6 +1.6-0.6 1024 cm - 2 L 2-10 =7.0 10 44 L 10-40 =6.9 10 44 erg/s Pure reflec<on dominated sta<s<cally equally acceptable kev 2 (Photons cm 2 s 1 kev 1 ) 10 6 10 5 XMM- PN XMM- MOS NuSTAR FPMA NuSTAR FPMB Pwlaw Reflect Scap Zappacosta et al. In prep. 1 2 5 10 20 Energy (kev)
Physically mo<vated models Brightman & Nandra 2012 torus model (Spherical geometry with conical polar openings) Edge- on geometry (i=85 deg) opening angle: 60 deg N H = 1.7±0.4 10 24 cm - 2 Torus Scap Spherical model N H = 1.1±0.3 10 24 cm - 2 Scapered flux: 12% Contribu<on from star forma<on alone? à >20000 M /yr (Ranalli et al. 2003) à From SED filng 2000 M /yr à The remainder gives scapered flux of 10%. Torus Scap kev 2 (Photons cm 2 s 1 kev 1 ) 10 6 10 5 kev 2 (Photons cm 2 s 1 kev 1 ) 10 6 10 5 1 2 5 10 20 Energy (kev) 1 2 5 10 20 Energy (kev)
Red quasars: J- K > 2.5 Hyperluminous QSOs selected for unusual red colors. UKIDSS Large Area Survey à Banerji et al. 2012, 2015 normalized counts s 1 kev 1 10 4 10 3 0.01 0.01 10 3 4 ULAS J1539+0557 (z=2.658) PN, MOS XMM proprietary (PI: LZ) 1 2 5 Energy (kev) ULAS J2315+0143 (z=2.56) PN XMM archival Low obscuraaon N H < 7 10 22 cm - 2 Very luminous L 2-10 =1-3 10 45 erg/s Consistent with Reddest Type 1 QSO known ULAS J1234+0907 (z=2.503) (Banerji+2014) Banerji+2012 Hyperluminous, Type 1 low X- ray obscura<on Dust- reddened high Eddington ra<o (>0.1) 3 2 1 1 2 5 Energy (kev) STRONG OUTFLOWS RADIATIVE PRESSURE ON DUST TRANSITIONAL PHASE?
The blow- out phase: WISSH sample 86 WISE/SDSS Hyperluminous (L bol > 10 14 L ) QSOs (WISSH) WISE selected W4(22μm)>3mJy SDSS broad line QSOs 1.5 < z < 4.5 Brightest mid- IR Type 1 AGN Primary targets to search for AGN- driven ou{lows Extensive mul<- λ follow- up programs (observed/approved): X- ray proper<es (Chandra/XMM) [OIII] ou{lows (LBT/LUCI,VLT/SINFONI/X- SHOOTER) Nuclear ou{lows (LBT/LUCI/MODS + SDSS) Map of ionized gas (VLT/SINFONI IFU) Map of molecular gas (ALMA) SED (Herschel/WISE/2MASS/SDSS) Redshi 0.6 1.5 2 3 4 5.3 3C 273 BAT sample WISE/SDSS + HotDOGs Δ Weedman+2012 Link nuclear and galac<c- scale proper<es à clues on AGN feedback
Pervasive signs of ou{lows Strong [OIII] ou{lows ~30% Remarkable nuclear winds ~70% (CIV blueshis) Flux Hβ CIV CIII - 20000-10000 0 10000 20000 Velocity [km s - 1 ] BAL 20%
WISSH: X- ray/nuclear proper<es X- ray WISSH sample 41 sources 34 Chandra + 7 XMM 8 proprietary (PI: LZ, Piconcelli) Very low absorp<on Martocchia et al. in prep 5x10 21 10 22 5x10 22 10 23 5x10 23 N H [cm - 2 ]
Op<cal/UV vs X- ray Reprocessing UV/op<cal à X- ray è progressively less efficient at high Luminosity
The mid- IR reprocessor Intrinsic Log [L 2-10 /erg s - 1 ] Hyp. Red QSOs W1835 Stern+2014 X- ray weakness or IR loudness? Biases IR/X selec<on à IR/X loud AGNs Mateos+15 à from X- ray Lanzuisi+09 à from Mid IR Low α ox à X- ray emission quenched MIR selec<on à large dust reservoir? Stern+15 rela<on for op<cally selected Hyperluminous QSOs à Good! à Probably not IR bias à X- ray weakness!
Connec<ng radia<ve output to galaxy- wide AGN ou{lowing proper<es BischeL et al. submiped CIV blueshi [km/s] - 2000 Log EW(CIV) [Å] - 1 0 1 2 3 0 +2000-4000 - 6000 SDSS- DR7 NO BAL BAL [OIII] NO [OIII] - 8000 Vietri et al. in prep
Connec<ng radia<ve output to galaxy- wide AGN ou{lowing proper<es BischeL et al. submiped CIV blueshi [km/s] - 2000 Log EW(CIV) [Å] - 1 0 1 2 3 0 +2000 Low L X à No galaxy scale winds strong nuclear winds High L X à Galaxy- scale winds weak nuclear winds - 4000-6000 SDSS- DR7 NO BAL BAL [OIII] NO [OIII] - 8000 Vietri et al. in prep
Conclusions Merger- induced QSO forma<on scenario The best strategy to study feedback: à hyperluminous sources (L bol > 10 47-48, L MIR > 10 47 ) Hot DOGs: obscured accre<on First NuSTAR detec<on and broad band X- ray spectrum at z~2.3 à Reflec<on dominated /Compton thick possibly not spherically obscured Type 1 Dusty Red and Hyperlum. WISSH QSOs: unobscured wind- dominated Low X- ray obscura<on X- ray weakness: Coronal X- ray emission rela<ve to Opt/UV depressed at high L à coronal quenching from strong radia<ve output? Perturbed by AGN- driven winds? Hint of X- ray output correla<ng with presence of [OIII] (kpc scales) and an<correla<ng with blueshi of CIV (sub- pc scales). How do they talk to each other?!