2018A&A...617A..81V


C.D.S. - SIMBAD4 rel 1.7 - 2020.04.07CEST12:43:35

2018A&A...617A..81V - Astronomy and Astrophysics, volume 617A, 81-81 (2018/9-1)

The WISSH quasars project. IV. Broad line region versus kiloparsec-scale winds.

VIETRI G., PICONCELLI E., BISCHETTI M., DURAS F., MARTOCCHIA S., BONGIORNO A., MARCONI A., ZAPPACOSTA L., BISOGNI S., BRUNI G., BRUSA M., COMASTRI A., CRESCI G., FERUGLIO C., GIALLONGO E., LA FRANCA F., MAINIERI V., MANNUCCI F., RICCI F., SANI E., TESTA V., TOMBESI F., VIGNALI C. and FIORE F.

Abstract (from CDS):

Winds accelerated by active galactic nuclei (AGNs) are invoked in the most successful models of galaxy evolution to explain the observed physical and evolutionary properties of massive galaxies. Winds are expected to deposit energy and momentum into the interstellar medium (ISM), thus regulating both star formation and supermassive black hole (SMBH) growth. We undertook a multiband observing program aimed at obtaining a complete census of winds in a sample of WISE/SDSS selected hyper-luminous (WISSH) quasars (QSOs) at z~=2-4. We analyzed the rest-frame optical (i.e. LBT/LUCI and VLT/SINFONI) and UV (i.e. SDSS) spectra of 18 randomly selected WISSH QSOs to measure the SMBH mass and study the properties of winds both in the narrow line region (NLR) and broad line region (BLR) traced by blueshifted or skewed [OIII] and CIV emission lines, respectively. These WISSH QSOs are powered by SMBH with masses ≥109M accreting at 0.4<λEdd<3.1. We found the existence of two subpopulations of hyper-luminous QSOs characterized by the presence of outflows at different distances from the SMBH. One population (i.e. [OIII] sources) exhibits powerful [OIII] outflows, a rest-frame equivalent width (REW) of the CIV emission REWCIV~=20-40Å, and modest CIV velocity shift (vCIVpeak) with respect to the systemic redshift (vCIVpeak≲2000km/s). The second population (i.e. Weak [OIII] sources), representing ∼70% of the analyzed WISSH QSOs, shows weak or absent [OIII] emission and an extremely large blueshifted CIV emission (vCIVpeak up to ∼8000km/s and REWCIV≲20Å). We propose two explanations for the observed behavior of the strength of the [OIII] emission in terms of the orientation effects of the line of sight and ionization cone. The dichotomy in the presence of BLR and NLR winds could be likely due to inclination effects considering a polar geometry scenario for the BLR winds. In a few cases these winds are remarkably as powerful as those revealed in the NLR in the [OIII] QSOs (Ekin∼1044–45erg/s). We also investigated the dependence of these CIV winds on fundamental AGN parameters such as bolometric luminosity (LBol), Eddington ratio (λEdd), and UV-to-X-ray continuum slope (αOX). We found a strong correlation with LBol and an anti-correlation with αOX whereby the higher the luminosity, the steeper the ionizing continuum described by means of αOX and the larger the blueshift of the CIV emission line. Finally, the observed dependence vCIVpeak∝LBol0.28±0.04 is consistent with a radiatively-driven-winds scenario, where a strong UV continuum is necessary to launch the wind and a weakness of the X-rayemission is fundamental to prevent overionization of the wind itself.

Abstract Copyright: © ESO 2018

Journal keyword(s): galaxies: active - galaxies: nuclei - quasars: emission lines - quasars: general - quasars: supermassive black holes - ISM: jets and outflows

Status at CDS:  

Simbad objects: 22

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Number of rows : 22

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9298 1
2 QSO J0745+4734 QSO 07 45 21.7881463456 +47 34 36.191344902   16.76 16.44     ~ 83 0
3 QSO J0801+5210 QSO 08 01 17.7968518079 +52 10 34.600380950   17.41 17.04     ~ 42 0
4 QSO B0900+42 QSO 09 00 33.5093000271 +42 15 47.031257024   17.63 17.18     ~ 62 0
5 2MASS J09584122+2827291 QSO 09 58 41.2178939144 +28 27 29.567298382   19.02 18.44     ~ 14 0
6 QSO B1103+6416 QSO 11 06 10.7342664415 +64 00 09.646278482   16.36 16.16     ~ 55 0
7 QSO J1111+1336 QSO 11 11 19.1031733986 +13 36 03.821438785   18.59 17.96     ~ 28 0
8 IRAS 11119+3257 Sy1 11 14 38.8904034667 +32 41 33.481055206   19.22 17.96     ~ 110 1
9 2MASS J11574799+2724595 QSO 11 57 47.9892881842 +27 24 59.651671606   19.70 18.99     ~ 9 0
10 QSO J1201+0116 QSO 12 01 44.3651168135 +01 16 11.738588370   18.09 17.74 17.4   ~ 48 2
11 QSO B1159+123 QSO 12 01 47.9113685833 +12 06 30.254501010   18.85 18.16     ~ 84 0
12 [VV2006] J123641.5+655441 QSO 12 36 41.4593292099 +65 54 42.187925135   18.21 17.72     ~ 26 0
13 Mrk 231 Sy1 12 56 14.2340989340 +56 52 25.238555193   14.68 13.84     ~ 1765 3
14 [VV2006] J132655.0-000531 QSO 13 26 54.9510725223 -00 05 30.128528420   21.22 20.81     ~ 28 0
15 [VV2006] J142124.0+463318 QSO 14 21 23.9851528711 +46 33 17.955335686   18.53 17.99     ~ 30 0
16 [VV2006] J142243.0+441721 QSO 14 22 43.0266144858 +44 17 21.324202449   19.96 19.08     ~ 27 0
17 2MASS J15215647+5202387 QSO 15 21 56.4822619037 +52 02 38.598808258   16.02 15.70     ~ 39 0
18 QSO J1538+0855 QSO 15 38 30.5594703954 +08 55 17.150684209   18.77 17.98     ~ 19 0
19 2MASS J15493872+1245092 QSO 15 49 38.7150556228 +12 45 09.160054709   19.21 18.54 17.61   ~ 22 0
20 QSO J2123-0050 QSO 21 23 29.4639237667 -00 50 52.916067995   16.91 16.62     ~ 83 0
21 QSO J2155-0922 Sy1 21 55 01.5123415724 -09 22 24.351917710   13.9 16.8 14.1   ~ 154 0
22 QSO J2346-0016 QSO 23 46 25.6713273667 -00 16 00.425283243   19.44 18.73     ~ 50 0

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2020.04.07-12:43:35

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