2016
Publication Year
2020-10-19T10:06:20Z
Acceptance in OA@INAF
The WISSH Project: Winds In The BLR
Title
VIETRI, GIUSTINA; PICONCELLI, Enrico; FIORE, Fabrizio; BONGIORNO, ANGELA; Bischetti, M.; et al.
Authors
10.5281/zenodo.163618
DOI
http://hdl.handle.net/20.500.12386/27884
!
The WISSH project: Winds in the BLR
!
GIUSTINA VIETRI
INAF-OAR Università di Roma “La Sapienza”
The quasars project
!
E.Piconcelli, F.Fiore, A. Bongiorno, M. Bischetti, F. Duras, S. Martocchia, L. Zappacosta INAF OAR M. Brusa, C. Vignali UNIBO - INAF OABO
A. Marconi, G. Cresci INAF Arcetri … and many others
XMM & Chandra X-rays
LBT/LUCI - TNG Hβ + [OIII]
SINFONI IFU Spec Hβ + [OIII] + Hα
X-shooter Hβ + CIV + MgII
ALMA CII + FIR continuum
+ Herschel - WISE - 2MASS - SDSS
public data
Targeting WISSH Quasars
Extensive multi-λ observing program
Panchromatic view of
Hyper-Lum QSOs
!
Goal: Nuclear, winds & host
galaxy properties
This Talk
SMBH mass and Eddington ratio estimate
[OIII] outflows
Disk Winds
Data
LBT/LUCI: performed observations 18 3/18 SINFONI data
!
SDSS public data
WISSH Quasars
86 broad-line Quasars with
WISE/SDSS Selected Hyper-luminous Quasars
L
Spectral overview of WISSH Quasars
Very complex spectra, different from those typically observed !
Narrow [OIII] emission weak or absent in all of them !
If present, [OIII] shows broad blue-shifted profiles (in 5/18 quasars) indicative of outflows
!
Strong, complex FeII emission
SDSS J1326-0005 z=3.303
lack of [OIII]
70 % SDSS J1201-0116 z=3.247
70% lack of [OIII] emission 30% prominent broad
[OIII] emission
SDSS J2123-0050! ! z=2.283 SDSS J0958+2827 z= 3.436
SDSS J1236+6554 z=3.424
Strong, complex FeII emission !
Upper limits on [OIII]: FWHM~500 km/s !
Weak [OIII] emission line? Iron residual?
70% lack of [OIII] emission
Revealing ultra-massive, highly accreting SMBH
•
Hβ-based SMBH massesfrom
~ 2 × 10
9M⊙
up to
∼ 2 × 10
10M⊙
! !•
L
Bolfrom multi-component
broad-band (far-IR to UV)
SED fitting
m LBol=L Edd LBol =0.5 xLEd d(Duras et al. in prep)
WISSH QSOs populate the massive end
of the BH mass function at z ~ 2.5 - 3.5
•
high accretion rates0.4 < λ
Edd< 3
Opportunity of collecting high-mass, highly accreting SMBHs at the peak of the quasars number density
WISSH vs “typical” AGN SMBHs
BLR
Accretion Disk
Torus
gravitationally
bounded clouds
<0.1pc
<0.01pc
1pc-10pc
Hβ
[OIII] outflows
NLR
Kpc
Winds in WISSH Quasars
(Manuela Bischetti talk)
High ionization emission
lines winds (i.e. CIV)
BLR winds in WISSH Quasars
50000 10000 15000 20000 20 40 60 80LUCI/LBT
Optical rest-frame
Hβ λ4861
Observed wavelength (A)
Fl
ux
[1
0
-17e
rg/
s/
cm
2/A
]
SDSS
UV rest-frame
CIV λ1549
SDSSJ1201-0116
BLR winds vs [OIII] winds: a dichotomy
Radiatively driven winds dominating the BLR kinematics
−2×104 −1×104 0 1×104 2×104 velocity shift (km/s) 0.2 0.4 0.6 0.8 1.0 1.2
Flux in arbritary unit
CIV-H
βvelocity shift
SDSS −2×104 −1×104 0 1×104 2×104 velocity shift (km/s) 0.6 0.7 0.8 0.9 1.0 1.1 1.2
Flux in arbritary unit
no[OIII]
SDSS LBT LBT CIV CIV Hbeta HbetaCIV velocity shift (km/s)
SDSS DR7 Shen et al. 2011No OIII
OIII outflow
Evidence of dichotomy
CIV vshift > 2000 km/s if no [OIII]
CIV vshift < 2000 km/s if [OIII]
[OIII]
Gaskell 1982 Marziani+1996 Richards+2011
-2000 0 2000 4000 6000 8000 CIV velocity shift (km/s)
0.0 0.5 1.0 1.5 2.0 2.5 3.0
log REW CIV (A)
WISSH NoOIII WISSH OIII
WLQ (Luo+15,Wu+11,Plotkin+15) PG (Baskin+04,Tang+12)
BLR winds vs [OIII] winds: a dichotomy
(Vietri et al. in prep)
Contours: SDSS DR7 Shen11
no [OIII] [OIII]
WISSH selection very effective in collecting the highest CIV winds
higher EWCIV and lower velocity shift lower EWCIV and higher velocity shift
[OIII]: NO [OIII]:
Corbin & Boroson 1996
Richards et al. 2002a
Weak Line Quasars
0.01 0.10 1.00 10.00 Edd ratio -2000 0 2000 4000 6000 8000
Log velocity shift Civ-hbeta km/s
44 45 46 47 48 49 Log Lbol -2000 0 2000 4000 6000 8000
Log velocity shift Civ-hbeta km/s
BLR winds vs EDD ratio and Bolometric Luminosity
Higher velocity shift with increasing L
Bol(Vietri et al. in prep)
[OIII]
NO [OIII]
BUT what else..?
SMBH from Hbeta ~183 QSOs
SMBH from Hbeta
~183 QSOs NO [OIII]
[OIII]
EDD ratio Log Lbol
CIV velo city shif t (km/s) CIV velo city shif t (km/s)
Conclusions
The WISSH sample
86 hyper-luminous, IR-loud, broad-line quasars at 2 < z < 5 with LBol > 2 x 1047 erg s-1
Ongoing multi-lambda observing programs (LBT, SINFONI, CHANDRA, ALMA,…)
Results from LBT/SINFONI observations (18 targets):
• SMBH (2 × 109 M⊙ up to 2 × 1010 M⊙) at the massive end of the BH mass function • High accretion rates (0.4 < λEdd < 3)
• Narrow [OIII] emissions weak/absent
• If present (30%), broad [OIII] (FWHM ~ 2000 km/s) indicative of outflows highest broad [OIII] luminosities observed so far (up to 1045 erg s-1)
• BLR winds with CIV shifts 2000 - 7000 km/s (70%) • BLR winds - [OIII] winds dichotomy
• Dependence of CIV velocity shift on Bolometric Luminosity but there is …..
(Manuela talk)
SED properties? Xray weakness?