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doi:10.1111/mnr.2010.401.issue-1

Cited by 13 publications

(4 citation statements)

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“…Thus, the properties of the winds are almost the same when the quasi-steady state has been formed. The kinetic power of the winds is significantly higher than 0.5%L edd , so the winds can provide sufficient feedback to their host galaxies (Di Matteo et al 2005;Hopkins & Elvis 2010;Bu & Yang 2021).…”

Section: Discussionmentioning

confidence: 99%

“…The winds do not stop at the outer radial boundary of our simulations and can move out of the AGNs to interact with the interstellar medium of their host galaxies. The kinetic power of the winds is significantly higher than 0.5% L edd , so the winds can provide sufficient feedback to their host galaxies (Di Matteo et al 2005;Hopkins & Elvis 2010;Bu & Yang 2021). It is clear that the curves of the mass flux, momentum flux and kinetic power are almost same for model 1 and model 2.…”

Section: The Effect Of the Host Galaxy Potentialmentioning

confidence: 95%

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Large-scale Dynamics of Line-driven Winds with the Re-radiation Effect

Zhu,

Xie

2023

Res. Astron. Astrophys.

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Previous simulations studying winds only focus on the line force due to the photons from the central active galactic nucleis (AGNs). What the properties of the winds will be when including the re-radiation force due to the scattered and reprocessed photons (i.e., the re-radiation effect)? We perform simulations to study the large-scale dynamics of accretion disk winds driven by radiation line force and re-radiation force. For the fiducial run, we find that the re-radiation force drives stronger outflows during the early stages. When the flows get into the steadiness, the UV radiation due to spectral lines dominates total radiation and the re-radiation effect could be negligible. The opening angle of winds narrows as initial gas density increases. The larger the gas density is, the stronger the re-radiation effect will be. For $M_{BH}=10^6M_{\odot}$, $\varepsilon=0.3$, the outflows do become much stronger with the re-radiation effect and the winds still can not escape from gravitational potential. We find that the detection probability of ultra-fast outflows (UFOs) and the properties of the winds are both consistent with the observations.

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Section: Discussionmentioning

confidence: 99%

Section: The Effect Of the Host Galaxy Potentialmentioning

confidence: 95%

Large-scale Dynamics of Line-driven Winds with the Re-radiation Effect

Zhu,

Xie

2023

Res. Astron. Astrophys.

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“…Obtaining systemic redshifts (z sys ) for quasars to accuracies better than 1000 km s −1 is necessary for a variety of reasons. These include measuring the kinematics of outflowing material near the supermassive black hole that impact star formation rates in the quasar's host galaxy (e.g., Hopkins & Elvis 2010;Maiolino et al 2012;Carniani et al 2018) and cosmological studies that utilize redshifts as distance indicators, such as quasar clustering and the proximity effect at high redshift (e.g., Alcock & Paczynski 1979;Hogg 1999;Shen et al 2007;Dawson et al 2013;McGreer et al 2016;Zhao et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Gemini Near Infrared Spectrograph–Distant Quasar Survey: Augmented Spectroscopic Catalog and a Prescription for Correcting UV-based Quasar Redshifts

Matthews

Dix

Shemmer

et al. 2023

ApJ

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Quasars at z ≳ 1 most often have redshifts measured from rest-frame ultraviolet emission lines. One of the most common such lines, C iv λ1549, shows blueshifts up to ≈5000 km s−1 and in rare cases even higher. This blueshifting results in highly uncertain redshifts when compared to redshift determinations from rest-frame optical emission lines, e.g., from the narrow [O iii] λ5007 feature. We present spectroscopic measurements for 260 sources at 1.55 ≲ z ≲ 3.50 having −28.0 ≲ M i ≲ − 30.0 mag from the Gemini Near Infrared Spectrograph–Distant Quasar Survey (GNIRS-DQS) catalog, augmenting the previous iteration, which contained 226 of the 260 sources whose measurements are improved upon in this work. We obtain reliable systemic redshifts based on [O iii] λ5007 for a subset of 121 sources, which we use to calibrate prescriptions for correcting UV-based redshifts. These prescriptions are based on a regression analysis involving C iv full-width-at-half-maximum intensity and equivalent width, along with the UV continuum luminosity at a rest-frame wavelength of 1350 Å. Applying these corrections can improve the accuracy and the precision in the C iv-based redshift by up to ∼850 km s−1 and ∼150 km s−1, respectively, which correspond to ∼8.5 and ∼1.5 Mpc in comoving distance at z = 2.5. Our prescriptions also improve the accuracy of the best available multifeature redshift determination algorithm by ∼100 km s−1, indicating that the spectroscopic properties of the C iv emission line can provide robust redshift estimates for high-redshift quasars. We discuss the prospects of our prescriptions for cosmological and quasar studies utilizing upcoming large spectroscopic surveys.

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“…The mechanical power of these winds can reach a significant fraction of the Eddington limit, which may be more than sufficient to provide the mechanical feedback required by models of black hole and host galaxy coevolution (Silk & Rees 1998;Fabian 1999;King 2003;Di Matteo et al 2005;Hopkins & Elvis 2010). Such black hole winds may play a crucial part in regulating the growth of supermassive black holes and the bulges of their host galaxies in luminous QSOs (Ferrarese & Merritt 2000;Gebhardt 2000;Tremaine et al 2002).…”

Section: Introductionmentioning

confidence: 99%

Rapid Variability of the Accretion Disk Wind in the Narrow-line Seyfert 1, PG 1448+273

Reeves

Braito

Porquet

et al. 2023

ApJ

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PG 1448+273 is a luminous, nearby (z = 0.0645), narrow-line Seyfert 1 galaxy, which likely accretes close to the Eddington limit. XMM-Newton observations of PG 1448+273 in 2017 revealed the presence of an ultrafast outflow, as seen through its blueshifted iron K absorption profile, with an outflow velocity of about 0.1 c. Here, the first NuSTAR observation of PG 1448+273, performed in 2022 and coordinated with XMM-Newton, is presented, which shows remarkable variability of its ultrafast outflow. The average count rate is a factor of 2 lower during the last 60 ks of the NuSTAR observation, where a much faster component of the ultrafast outflow was detected with a terminal velocity of 0.26 ± 0.04 c. This is significantly faster than the outflow component that was initially detected in 2017, when overall PG 1448+273 was observed at a lower X-ray flux, and which implies an order of magnitude increase in the wind kinetic power between the 2017 and 2022 epochs. Furthermore, the rapid variability of the ultrafast outflow in 2022, on timescales down to 10 ks, suggests we are viewing through a highly inhomogeneous disk wind in PG 1448+273, where the passage of a denser wind clump could account for the increase in obscuration in the last 60 ks of the NuSTAR observation.

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Cited by 13 publications

References 0 publications

Large-scale Dynamics of Line-driven Winds with the Re-radiation Effect

Large-scale Dynamics of Line-driven Winds with the Re-radiation Effect

Gemini Near Infrared Spectrograph–Distant Quasar Survey: Augmented Spectroscopic Catalog and a Prescription for Correcting UV-based Quasar Redshifts

Rapid Variability of the Accretion Disk Wind in the Narrow-line Seyfert 1, PG 1448+273

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