Blue outliers among intermediate redshift quasars

Marziani, Paola; Sulentic, J. W.; Stirpe, G. M.; Dultzin, D.; Olmo, A. del; Martínez-Carballo, M. A.

doi:10.1007/s10509-015-2590-2

Cited by 52 publications

(76 citation statements)

References 61 publications

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“…We note that there is a known small systematic offset of δv r ≈ +19 km/s, frequently found in [O III]-strong AGN (e.g., Eracleous & Halpern 2003;Hu et al 2008;Komossa et al 2008;Marziani et al 2016, and references therein). The velocity zero point was set on the peak wavelength of [O III] λ5007, as [O III] λ5007 is a very sharp feature of high S/N, less influenced by the underlying broad Hβ profile.…”

Section: Line and Continuum Fittingssupporting

confidence: 58%

Evidence for Periodicity in 43 Year-Long Monitoring of NGC 5548

Bon¹,

Zucker²,

Netzer³

et al. 2016

ApJS

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113

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We present an analysis of 43 years (1972 to 2015) of spectroscopic observations of the Seyfert 1 galaxy NGC 5548. This includes 12 years of new unpublished observations (2003 to 2015). We compiled about 1600 Hβ spectra and analyzed the long-term spectral variations of the 5100Å continuum and the Hβ line. Our analysis is based on standard procedures, including the LombScargle method, which is known to be rather limited to such heterogeneous data sets, and a new method developed specifically for this project that is more robust and reveals a -2 -∼5700 day periodicity in the continuum light curve, the Hβ light curve, and the radial velocity curve of the red wing of the Hβ line. The data are consistent with orbital motion inside the broad emission line region of the source. We discuss several possible mechanisms that can explain this periodicity, including orbiting dusty and dust-free clouds, a binary black hole system, tidal disruption events, and the effect of an orbiting star periodically passing through an accretion disk.

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Section: Line and Continuum Fittingssupporting

confidence: 58%

Evidence for Periodicity in 43 Year-Long Monitoring of NGC 5548

Bon¹,

Zucker²,

Netzer³

et al. 2016

ApJS

Self Cite

113

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“…Harrison et al 2016) samples, it is becoming clear that powerful outflows may be very common in AGN hosts, especially at high redshifts (see e.g. Marziani et al 2016). However, to uncover the kinematics and physical properties of the wind, high-resolution and high S/N observations, such as those presented in this paper, are needed.…”

Section: Discussionmentioning

confidence: 97%

A fast ionised wind in a star-forming quasar system atz~ 1.5 resolved through adaptive optics assisted near-infrared data

Brusa

Perna

Cresci

et al. 2016

A&A

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Aims. Outflow winds are invoked in co-evolutionary models to link the growth of SMBH and galaxies through feedback phenomena, and from the analysis of both galaxies and active galactic nuclei (AGN) samples at z ∼ 1−3, it is becoming clear that powerful outflows may be very common in AGN hosts. High-resolution and high S/N observations are needed to uncover the physical properties of the wind through kinematics analysis. Methods. We exploited VLT/VIMOS, VLT/SINFONI, and Subaru/IRCS adaptive optics (AO) data to study the kinematics properties on the scale of the host galaxy of XID5395; this galaxy is a luminous, X-ray obscured starburst/quasar (SB-QSO) merging system at z ∼ 1.5, detected in the XMM-COSMOS field, associated with an extreme [O II] emitter (with equivalent width, EW, ∼200 Å). For the first time, we mapped the kinematics of the [O III] and Hα line complexes and linked them with the [O II] emission at high resolution. The high spatial resolution achieved allowed us to resolve all the components of the SB-QSO system. Results. Our analysis, with a resolution of few kpc, reveals complexities and asymmetries in and around the nucleus of XID5395. The velocity field measured via non-parametric analysis reveals different kinematic components with maximum blueshifted and redshifted velocities up to > ∼ 1300 km s −1 that are not spatially coincident with the nuclear core. These extreme values of the observed velocities and spatial location can be explained by the presence of fast moving material. We also spectroscopically confirm the presence of a merging system at the same redshift as the AGN host. Conclusions. We propose that EW as large as >150 Å in X-ray selected AGN may be an efficient criterion to isolate objects associated with the short, transition phase of "feedback" in the AGN-galaxy co-evolutionary path. This co-evolutionary path subsequently evolves into an unobscured QSO, as suggested from the different observational evidence (e.g. merger, compact radio emission, and outflow) we accumulated for XID5395.

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“…It also provides an explanation for the larger blueshifts (v b ) of the CIV with respect to low-ionization emission lines such as MgII and Hβ found at higher luminosities in the "wind-dominated" quasar population (e.g. Richards et al 2011;Marziani et al 2016), and the observed anti-correlation between v b and the EW of the CIV emission line (Korista et al 1998; Krawczyk et al 2013). This SED-based scenario for "wind-dominated" quasars rules out orientation as a major cause of these blueshifts.…”

Section: Discussionmentioning

confidence: 98%

The WISSH quasars project

Martocchia

Piconcelli

Zappacosta

et al. 2017

A&A

126

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We perform a survey of the X-ray properties of 41 objects from the WISE/SDSS selected Hyper-luminous (WISSH) quasars sample, which includes 86 broad-line quasars with bolometric luminosity L Bol > ∼ 2 × 10 47 erg s −1 shining at z ∼ 2-4. We use both proprietary and archival Chandra and XMM-Newton observations. Twenty-one quasars have sufficient quality data to perform a spectroscopic analysis, while for the remaining sources, X-ray properties are derived through hardness-ratio analysis (apart for six sources which result to be undetected). The bulk (∼ 70%) of the detected WISSH quasars exhibit N H < 5 × 10 22 cm −2 , in agreement with their optical Type 1 AGN classification. All but three quasars show unabsorbed 2-10 keV luminosities L 2−10 ≥ 10 45 erg s −1 . Thanks to their extreme radiative output across the Mid-IR-to-X-ray range, WISSH quasars therefore offer the opportunity to significantly extend and validate the existing relations involving L 2−10 . Specifically, we study the X-ray luminosity as a function of (i) X-ray-to-Optical (X/O) flux ratio, (ii) mid-IR luminosity (L MIR ), (iii) L Bol as well as (iv) α OX versus the 2500Å luminosity. We find that the WISSH quasars show (i) unreported very low X/O (< 0.1) compared to typical AGN values; (ii) L 2−10 /L MIR ratios significantly smaller than those derived for AGN with lower luminosity; (iii) a large X-ray bolometric correction k Bol,X ≈ 100-1000; and (iv) steep -2 > ∼ α OX > ∼ -1.7. These results lead to a scenario in which the X-ray emission of hyper-luminous quasars is relatively weaker compared to lower-luminosity AGN. Models predict that such an X-ray weakness can be relevant for the acceleration of powerful high-ionization emission line-driven winds, commonly detected in the UV spectra of WISSH quasars, which can in turn perturb the X-ray corona and weaken its emission. Accordingly, hyper-luminous quasars represent the ideal laboratory to study the link between the AGN energy output and wind acceleration. Additionally, WISSH quasars exhibit very large SMBH masses (log[M BH /M ] > ∼ 9.5). This enables a more robust modeling of the Γ-M BH relation by increasing the statistics at high masses. We derive a flatter Γ dependence than previously found over the broad range 5 < ∼ log(M BH /M ) < ∼ 11. Finally, we estimate that only 300 ks observation of X-IFU on board Athena will offer a detailed view of the properties of absorption features associated to powerful X-ray SMBH winds for a representative sample of WISSH quasars.

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Blue outliers among intermediate redshift quasars

Cited by 52 publications

References 61 publications

Evidence for Periodicity in 43 Year-Long Monitoring of NGC 5548

Evidence for Periodicity in 43 Year-Long Monitoring of NGC 5548

A fast ionised wind in a star-forming quasar system atz~ 1.5 resolved through adaptive optics assisted near-infrared data

The WISSH quasars project

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