Exploring the link between C <scp>iv</scp> outflow kinematics and sublimation-temperature dust in quasars

Temple, Matthew J.; Banerji, M.; Hewett, Paul C.; Rankine, Amy L.; Richards, Gordon T.

doi:10.1093/mnras/staa3842

Cited by 24 publications

(19 citation statements)

References 78 publications

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“…A number of observational studies have reported significant correlations between C IV BEL/BAL properties (i.e., blueshift and EW) and dust properties traced by rest-frame 2-6 μm emission and UV/NIR spectral slopes (e.g., Zhang et al 2014;Baron & Netzer 2019;Rankine et al 2020;Yi et al 2020;Temple et al 2021), suggestive of an underlying link between quasar wind and dust across 1-1000 pc scales. However, these studies suffered from large uncertainties in distance for both wind and dust, making robust assessments difficult.…”

Section: Implications From the Sedmentioning

confidence: 99%

A Quasar Shedding Its Dust Cocoon at Redshift 2

Brandt

et al. 2022

ApJ

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We present the first near-IR spectroscopy and joint analyses of multiwavelength observations for SDSS J082747.14+425241.1, a dust-reddened, weak broad emission-line quasar (WLQ) undergoing a remarkable broad-absorption line (BAL) transformation. The systemic redshift is more precisely measured to be z = 2.070 ± 0.001 using Hβ compared to z = 2.040 ± 0.003 using Mg ii from the literature, signifying an extreme Mg ii blueshift of 2140 ± 530 km s−1 relative to Hβ. Using the Hβ-based single-epoch scaling relation with a systematic uncertainty of 0.3 dex, its black hole (BH) mass and Eddington ratio are estimated to be M BH ∼ 6.1 × 108 M ⊙ and λ Edd ∼ 0.71, indicative of being in a rapidly accreting phase. Our investigations confirm the WLQ nature and the LoBAL → HiBAL transformation, along with a factor of 2 increase in the Mg ii+Fe ii emission strength and a decrease of 0.1 in E(B − V) over two decades. The kinetic power of this LoBAL wind at R ∼ 15 pc from its BH is estimated to be ∼43% of the Eddington luminosity, sufficient for quasar feedback upon its host galaxy albeit with an order-of-magnitude uncertainty. This quasar provides a clear example of the long-sought scenario where LoBAL quasars are surrounded by dust cocoons, and wide-angle nuclear winds play a key role in the transition of red quasars evolving into the commonly seen blue quasars.

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Section: Implications From the Sedmentioning

confidence: 99%

A Quasar Shedding Its Dust Cocoon at Redshift 2

Brandt

et al. 2022

ApJ

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“…Such models provide predictions of the optical through near-infrared colours of an accuracy sufficient to allow the estimation of photometric redshifts. Of particular note was the parametrization of the quasar 'continuum' longward of ≈10 000 Å. Observations of individual quasars (Glikman et al 2006) and near-infrared photometry of luminous quasars (Maddox & Hewett 2006;Maddox et al 2008) resulted in the identification of a component that can be reproduced by emission from a blackbody with temperature ≈1200 K (see Temple et al 2021a, for a recent investigation).…”

Section: Early Quasar Sed Modelsmentioning

confidence: 99%

Modelling type 1 quasar colours in the era of Rubin and Euclid

Temple

Hewett

Banerji

2021

Monthly Notices of the Royal Astronomical Society

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We construct a parametric SED model which is able to reproduce the average observed SDSS-UKIDSS-WISE quasar colours to within one tenth of a magnitude across a wide range of redshift (0 < z < 5) and luminosity (−22 > Mi > −29). This model is shown to provide accurate predictions for the colours of known quasars which are less luminous than those used to calibrate the model parameters, and also those at higher redshifts z > 5. Using a single parameter, the model encapsulates an up-to-date understanding of the intra-population variance in the rest-frame ultraviolet and optical emission lines of luminous quasars. At fixed redshift, there are systematic changes in the average quasar colours with apparent i-band magnitude, which we find to be well explained by the contribution from the host galaxy and our parametrization of the emission-line properties. By including redshift as an additional free parameter, the model could be used to provide photometric redshifts for individual objects. For the population as a whole we find that the average emission line and host galaxy contributions can be well described by simple functions of luminosity which account for the observed changes in the average quasar colours across 18.1 < iAB < 21.5. We use these trends to provide predictions for quasar colours at the luminosities and redshifts which will be probed by the Rubin Observatory LSST and ESA-Euclid wide survey. The model code is applicable to a wide range of upcoming photometric and spectroscopic surveys, and is made publicly available.

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“…Eddington ratios are calculated assuming a constant bolometric correction of 𝐿 bol = 5.15 × 𝐿 3000 . However, we note that this correction may in fact be changing systematically as a function of C blueshift, as discussed by Temple et al (2021). The properties of the 39 833 object subsample are shown in Fig.…”

Section: 𝑀mentioning

confidence: 71%

“…In particular, given the large velocity gradients which must be present in the outflowing wind, thermal line widths are clearly inappropriate for this component. We suggest that the line broadening in highionization BLR winds could plausibly range from 10 2−3 km s −1 ; here we have chosen to adopt 𝜈 turb = 300 km s −1 ≈ 10 2.5 km s −1 to maintain consistency with Temple et al (2021). A full discussion of the effect of varying 𝜈 turb is beyond the scope of this paper; here we simply aim to show that there exist plausible solutions which do not require the metallicity of the BLR to vary.…”

Section: Photoionization Modelling Resultsmentioning

confidence: 99%

High-ionization emission line ratios from quasar broad line regions: metallicity or density?

Temple,

Ferland,

Rankine

et al. 2021

Preprint

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The flux ratios of high-ionization lines are commonly assumed to indicate the metallicity of the broad emission line region in luminous quasars. When accounting for the variation in their kinematic profiles, we show that the N /C , (Si +O ])/C and N /Ly 𝛼 line ratios do not vary as a function of the quasar continuum luminosity, black hole mass, or accretion rate. Using photoionization models from CLOUDY, we further show that the observed changes in these line ratios can be explained by emission from gas with solar abundances, if the physical conditions of the emitting gas are allowed to vary over a broad range of densities and ionizing fluxes. The diversity of broad line emission in quasar spectra can be explained by a model with emission from two kinematically distinct regions, where the line ratios suggest that these regions have either very different metallicity or density. Both simplicity and current galaxy evolution models suggest that near-solar abundances, with parts of the spectrum forming in high-density clouds, are more likely. Within this paradigm, objects with stronger outflow signatures show stronger emission from gas which is denser and located closer to the ionizing source, at radii consistent with simulations of line-driven disc-winds. Studies using broad-line ratios to infer chemical enrichment histories should consider changes in density and ionizing flux before estimating metallicities.

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Exploring the link between C iv outflow kinematics and sublimation-temperature dust in quasars

Cited by 24 publications

References 78 publications

A Quasar Shedding Its Dust Cocoon at Redshift 2

A Quasar Shedding Its Dust Cocoon at Redshift 2

Modelling type 1 quasar colours in the era of Rubin and Euclid

High-ionization emission line ratios from quasar broad line regions: metallicity or density?

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