The WISSH Project: Winds In The BLR

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

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The WISSH project: Winds in the BLR

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GIUSTINA VIETRI

INAF-OAR Università di Roma “La Sapienza”

The quasars project

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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

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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

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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

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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

•

~ 2 × 10

_M⊙

_{∼ 2 × 10}

M⊙

•

L

from multi-component

broad-band (far-IR to UV)

SED fitting

(Duras et al. in prep)

WISSH QSOs populate the massive end

of the BH mass function at z ~ 2.5 - 3.5

•

0.4 < λ

< 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

LUCI/LBT

Optical rest-frame

Hβ λ4861

Observed wavelength (A)

Fl

ux

[1

0

e

rg/

s/

cm

/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

velocity 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]

CIV velocity shift (km/s)

No 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

(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 < λ_Edd < 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?