The MOSDEF Survey: A Census of AGN-driven Ionized Outflows at z = 1.4–3.8

Leung, Gene C. K.; Coil, Alison L.; Aird, James; Azadi, Mojegan; Kriek, Mariska; Mobasher, Bahram; Reddy, Naveen A.; Shapley, Alice E.; Siana, Brian; Fetherolf, Tara; Fornasini, Francesca M.; Freeman, William R.; Price, Sedona H.; Sanders, Ryan L.; Shivaei, Irene; Zick, Tom

doi:10.3847/1538-4357/ab4a7c

Cited by 84 publications

(58 citation statements)

References 122 publications

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“…Errors in line fluxes were derived by allowing the spectra to vary 500 times according to the error spectra and remeasuring the line fluxes from these realizations. For this study, active galactic nuclei (AGNs) were excluded based on the IR, X-ray, and rest-frame optical line flux criteria as described in Coil et al (2015), Azadi et al (2017Azadi et al ( , 2018, and Leung et al (2019). Further details on target selection, observations, spectroscopic data reduction, slit loss corrections, and line flux measurements are provided in several papers discussing results from the MOSDEF survey (e.g., Kriek et al 2015;Reddy et al 2015).…”

Section: Line Flux Measurementsmentioning

confidence: 99%

The MOSDEF Survey: The First Direct Measurements of the Nebular Dust Attenuation Curve at High Redshift*

Reddy

Shapley

Kriek

et al. 2020

ApJ

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We use a sample of 532 star-forming galaxies at redshifts z ; 1.4-2.6 with deep rest-frame optical spectra from the MOSFIRE Deep Evolution Field (MOSDEF) survey to place the first constraints on the nebular attenuation curve at high redshift. Based on the first five low-order Balmer emission lines detected in the composite spectra of these galaxies (Hα through  H), we derive a nebular attenuation curve that is similar in shape to that of the Galactic extinction curve, suggesting that the dust covering fraction and absorption/scattering properties along the lines of sight to massive stars at high redshift are similar to those of the average Milky Way sight line. The curve derived here implies nebular reddening values that are, on average, systematically larger than those derived for the stellar continuum. In the context of stellar population synthesis models that include the effects of stellar multiplicity, the difference in reddening of the nebular lines and stellar continuum may imply molecular cloud crossing timescales that are a factor of3 longer than those inferred for local molecular clouds, star formation rates that are constant or increasing with time such that newly formed and dustier OB associations always dominate the ionizing flux, and/or that the dust responsible for reddening the nebular emission may be associated with nonmolecular (i.e., ionized and neutral) phases of the interstellar medium. Our analysis points to a variety of investigations of the nebular attenuation curve that will be enabled with the next generation of ground-and space-based facilities.

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Section: Line Flux Measurementsmentioning

confidence: 99%

The MOSDEF Survey: The First Direct Measurements of the Nebular Dust Attenuation Curve at High Redshift*

Reddy

Shapley

Kriek

et al. 2020

ApJ

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“…Among AGN surveys, Leung et al (2019) target opticallyselected AGN using single-slit spectroscopy from the MOS-DEF survey with bolometric luminosities in the range 10 44 −10 47 erg s −1 at z ∼ 1.4-3.8 and find outflows in 17% of their sample of ∼160 AGN. Moreover, it is claimed that the ionised gas mass outflow rates correlate positively with the luminosity of the AGN, but do not depend on the galaxy stellar mass, which is in contrast with the findings of Förster Schreiber et al (2018) concerning star forming galaxies.…”

Section: Introductionmentioning

confidence: 99%

Super

Kakkad

Mainieri

Vietri

et al. 2020

A&A

109

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Aims. The SINFONI survey for Unveiling the Physics and Effect of Radiative feedback (SUPER) aims to trace and characterise ionised gas outflows and their impact on star formation in a statistical sample of X-ray selected active galactic nuclei (AGN) at z ∼ 2. We present the first SINFONI results for a sample of 21 Type 1 AGN spanning a wide range in bolometric luminosity (log Lbol = 45.4–47.9 erg s−1). The main aims of this paper are to determine the extension of the ionised gas, characterise the occurrence of AGN-driven outflows, and link the properties of such outflows with those of the AGN. Methods. We used adaptive optics-assisted SINFONI observations to trace ionised gas in the extended narrow line region using the [O III] λ5007 line. We classified a target as hosting an outflow if its non-parametric velocity of the [O III] line, w80, was larger than 600 km s−1. We studied the presence of extended emission using dedicated point-spread function (PSF) observations, after modelling the PSF from the Balmer lines originating from the broad line region. Results. We detect outflows in all the Type 1 AGN sample based on the w80 value from the integrated spectrum, which is in the range ∼650–2700 km s−1. There is a clear positive correlation between w80 and the AGN bolometric luminosity (> 99% correlation probability), and the black hole mass (98% correlation probability). A comparison of the PSF and the [O III] radial profile shows that the [O III] emission is spatially resolved for ∼35% of the Type 1 sample and the outflows show an extension up to ∼6 kpc. The relation between maximum velocity and the bolometric luminosity is consistent with model predictions for shocks from an AGN-driven outflow. The escape fraction of the outflowing gas increases with the AGN luminosity, although for most galaxies, this fraction is less than 10%.

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“…A number of observational campaigns such as the WISSH survey of hyper-luminous QSOs (Bischetti et al 2017), the SUPER survey (Circosta et al 2018), the KASH-z survey of X-ray selected AGN (Harrison et al 2016), found ubiquitous ionised outflows at these redshifts. Moreover, the SINS zC-SINF plus KMOS3D (Förster Schreiber et al 2018 and the MOSDEF (Leung et al 2019) surveys found that the incidence of fast ionised outflows increases with stellar mass jointly with AGN fraction, and so their incidence in AGN is independent on stellar mass.…”

Section: Outflows From High To Low Redshiftmentioning

confidence: 99%

The physical properties and impact of AGN outflows from high to low redshift

Venturi

Marconi

2019

Proc. IAU

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Feedback from active galactic nuclei (AGN) on their host galaxies, in the form of gas outflows capable of quenching star formation, is considered a major player in galaxy evolution. However, clear observational evidence of such major impact is still missing; uncertainties in measuring outflow properties might be partly responsible because of their critical role in comparisons with models and in constraining the impact of outflows on galaxies. Here we briefly review the challenges in measuring outflow physical properties and present an overview of outflow studies from high to low redshift. Finally, we present highlights from our MAGNUM survey of nearby AGN with VLT/MUSE, where the high intrinsic spatial resolution (down to ˜ 10 pc) allows us to accurately measure the physical and kinematic properties of ionised gas outflows.

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The MOSDEF Survey: A Census of AGN-driven Ionized Outflows at z = 1.4–3.8

Cited by 84 publications

References 122 publications

The MOSDEF Survey: The First Direct Measurements of the Nebular Dust Attenuation Curve at High Redshift*

The MOSDEF Survey: The First Direct Measurements of the Nebular Dust Attenuation Curve at High Redshift*

Super

The physical properties and impact of AGN outflows from high to low redshift

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