The WISSH quasars project

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 bot...

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Bibliographic Details
Published in:Astronomy and astrophysics (Berlin) 2018-09, Vol.617
Main Authors: 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., Fiore, F.
Format: Article
Language:English
Subjects:
Active galactic nuclei
Astronomical models
Bolometers
Dependence
Deposition
Emission analysis
Galactic evolution
Galaxies
galaxies: active
galaxies: nuclei
Inclination
Interstellar matter
Ionization
ISM: jets and outflows
Luminosity
Quasars
quasars: emission lines
quasars: general
quasars: supermassive black holes
Red shift
Star & galaxy formation
Star formation
Stellar winds
Subpopulations
X ray spectra
Citations: Items that cite this one
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Description
Summary: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 ≳109 M⊙ 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 ≈ 20–40 Å, and modest CIV velocity shift ( vCIVpeak $v_{\textrm{CIV}}^{\textrm{peak}}$ vCIVpeak) with respect to the systemic redshift ( vCIVpeak $v_{\textrm{CIV}}^{\textrm{peak}}$vCIVpeak
ISSN:0004-6361
1432-0746
DOI:10.1051/0004-6361/201732335