The KMOS<sup>3D</sup> Survey: Demographics and Properties of Galactic Outflows at z = 0.6–2.7*

Schreiber, N. M. Förster; Übler, Hannah; Davies, R. L.; Genzel, R.; Wisnioski, Emily; Belli, Sirio; Shimizu, T.; Lutz, D.; Fossati, M.; Herrera-Camus, Rodrigo; Mendel, J. Trevor; Tacconi, L. J.; Wilman, David J.; Beifiori, A.; Brammer, Gabriel; Burkert, Andreas; Carollo, C. M.; Eisenhauer, F.; Fabricius, Maximilian; Lilly, S. J.; Momcheva, Ivelina; Naab, Thorsten; Nelson, Erica J.; Price, Sedona H.; Renzini, A.; Saglia, R.; Sternberg, A.; Dokkum, Pieter van; Wuyts, Stijn

doi:10.3847/1538-4357/ab0ca2

Cited by 176 publications

(150 citation statements)

References 271 publications

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“…Recent simulations start to reproduce the observed 'flickering' AGN accretion variations (e.g., Novak et al 2011;Gabor & Bournaud 2013). At high redshift, the smoothing of accretion rate variations provided by the observed outflow can explain the higher incidence of AGN-driven nuclear outflows, compared to direct AGN indicators such as Xrays (Genzel et al 2014;Förster Schreiber et al 2019).…”

Section: Evidence For a Role Of Intermittent Agn-drivingmentioning

confidence: 99%

Molecular outflows in local galaxies: Method comparison and a role of intermittent AGN driving

Lutz

Sturm

Janssen

et al. 2020

A&A

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143

137

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We report new detections and limits from a NOEMA and ALMA CO(1-0) search for molecular outflows in 13 local galaxies with high far-infrared surface brightness, and combine these with local universe CO outflow results from the literature. CO line ratios and spatial outflow structure of our targets provide some constraints on the conversion steps from observables to physical quantities such as molecular mass outflow rates. Where available, ratios between outflow emission in higher J CO transitions and in CO(1-0) typically are consistent with excitation R i1 1. For IRAS 13120-5453, however, R 31 = 2.10 ± 0.29 indicates optically thin CO in the outflow. Like much of the outflow literature, we use α CO(1−0) = 0.8, and we present arguments for using C=1 in deriving molecular mass outflow ratesṀ out = C Moutvout Rout . We compare the two main methods for molecular outflow detection: CO mm interferometry and Herschel OH-based spectroscopic outflow searches. For 26 sources studied with both methods, we find an 80% agreement in detecting v out 150 km s −1 outflows, and non-matches can be plausibly ascribed to outflow geometry and signal-to-noise ratio. For the González-Alfonso et al. (2017) sample of 12 bright ultraluminous infrared galaxies (ULIRGs) with detailed OH-based outflow modeling, CO outflows are detected in all but one. Outflow masses, velocities, and sizes for these 11 sources agree well between the two methods, and modest remaining differences may relate to the different but overlapping regions sampled by CO emission and OH absorption. Outflow properties correlate better with active galactic nucleus (AGN) luminosity and with bolometric luminosity than with far-infrared surface brightness. The most massive outflows are found for systems with current AGN activity, but significant outflows in non-AGN systems must relate to star formation or to AGN activity in the recent past. We report scaling relations for the increase of outflow mass, rate, momentum rate, and kinetic power with bolometric luminosity. Short ∼ 10 6 yr flow times and some sources with resolved multiple outflow episodes support a role of intermittent driving, likely by AGN.

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Section: Evidence For a Role Of Intermittent Agn-drivingmentioning

confidence: 99%

Molecular outflows in local galaxies: Method comparison and a role of intermittent AGN driving

Lutz

Sturm

Janssen

et al. 2020

A&A

Self Cite

143

137

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“…As highlighted by Veilleux et al (2005), it is hard to state whether a galactic wind is powered either by starburst and star formation activity only or by AGN activity alone. Recent observations have suggested correlations between outflow properties and ongoing AGN and star formation activity in systems with different mass: these relations can be exploited to distinguish between different mechanisms of outflow triggering (Förster Schreiber et al 2019). This topic represents a current challenge in cosmological simulations, too (e.g.…”

Section: Galactic Outflowsmentioning

confidence: 99%

Impact of AGN feedback on galaxies and their multiphase ISM across cosmic time

Valentini

Murante

Borgani

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present simulations of galaxy formation, based on the GADGET-3 code, in which a sub-resolution model for star formation and stellar feedback is interfaced with a new model for AGN feedback. Our sub-resolution model describes a multiphase ISM, accounting for hot and cold gas within the same resolution element: we exploit this feature to investigate the impact of coupling AGN feedback energy to the different phases of the ISM over cosmic time. Our fiducial model considers that AGN feedback energy coupling is driven by the covering factors of the hot and cold phases. We perform a suite of cosmological hydrodynamical simulations of disc galaxies (M halo, DM 2 · 10 12 M , at z = 0), to investigate: (i) the effect of different ways of coupling AGN feedback energy to the multiphase ISM; (ii) the impact of different prescriptions for gas accretion (i.e. only cold gas, both cold and hot gas, with the additional possibility of limiting gas accretion from cold gas with high angular momentum); (iii) how different models of gas accretion and coupling of AGN feedback energy affect the coevolution of supermassive BHs and their host galaxy. We find that at least a share of the AGN feedback energy has to couple with the diffuse gas, in order to avoid an excessive growth of the BH mass. When the BH only accretes cold gas, it experiences a growth that is faster than in the case in which both cold and hot gas are accreted. If the accretion of cold gas with high angular momentum is reduced, the BH mass growth is delayed, the BH mass at z = 0 is reduced by up to an order of magnitude, and the BH is prevented from accreting below z 2, when the galaxy disc forms.

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“…• established the trends with stellar mass and SFR of the incidence, strength, velocity, electron density, and mass ejection rate of ionized gas outflows, and the high duty cycle > 50% of nuclear, AGN-driven winds at log(M /M ) 11 Förster Schreiber et al 2019);…”

Section: Introductionmentioning

confidence: 99%

The KMOS^3D Survey: Data Release and Final Survey Paper*

Wisnioski

Schreiber

Fossati

et al. 2019

ApJ

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We present the completed KMOS 3D survey − an integral field spectroscopic survey of 739, log(M /M ) > 9, galaxies at 0.6 < z < 2.7 using the K-band Multi Object Spectrograph (KMOS) at the Very Large Telescope (VLT). KMOS 3D provides a population-wide census of kinematics, star formation, outflows, and nebular gas conditions both on and off the star-forming galaxy main sequence through the spatially resolved and integrated properties of Hα, [NII], and [SII] emission lines. We detect Hα emission for 91% of galaxies on the main sequence of star-formation and 79% overall. The depth of the survey has allowed us to detect galaxies with star-formation rates below 1 M yr −1 , as well as to resolve 81% of detected galaxies with ≥ 3 resolution elements along the kinematic major axis. The detection fraction of Hα is a strong function of both color and offset from the main sequence, with the detected and non-detected samples exhibiting different SED shapes. Comparison of Hα and UV+IR star formation rates (SFRs) reveal that dust attenuation corrections may be underestimated by 0.5 dex at the highest masses (log(M /M ) > 10.5). We confirm our first year results of a high rotation dominated fraction (monotonic velocity gradient and v rot /σ 0 > √ 3.36) of 77% for the full KMOS 3D sample. The rotation-dominated fraction is a function of both stellar mass and redshift with the strongest evolution measured over the redshift range of the survey for galaxies with log(M /M ) < 10.5. With this paper we include a final data release of all 739observed objects § .

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The KMOS^3D Survey: Demographics and Properties of Galactic Outflows at z = 0.6–2.7*

Cited by 176 publications

References 271 publications

Molecular outflows in local galaxies: Method comparison and a role of intermittent AGN driving

Molecular outflows in local galaxies: Method comparison and a role of intermittent AGN driving

Impact of AGN feedback on galaxies and their multiphase ISM across cosmic time

The KMOS^3D Survey: Data Release and Final Survey Paper*

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The KMOS3D Survey: Demographics and Properties of Galactic Outflows at z = 0.6–2.7*

Cited by 176 publications

References 271 publications

Molecular outflows in local galaxies: Method comparison and a role of intermittent AGN driving

Molecular outflows in local galaxies: Method comparison and a role of intermittent AGN driving

Impact of AGN feedback on galaxies and their multiphase ISM across cosmic time

The KMOS3D Survey: Data Release and Final Survey Paper*

Contact Info

Product

Resources

About

The KMOS^3D Survey: Demographics and Properties of Galactic Outflows at z = 0.6–2.7*

The KMOS^3D Survey: Data Release and Final Survey Paper*