The KMOS<sup>3D</sup> Survey: Data Release and Final Survey Paper*

Wisnioski, Emily; Schreiber, N. M. Förster; Fossati, M.; Mendel, J. Trevor; Wilman, David J.; Genzel, R.; Bender, R.; Wuyts, Stijn; Davies, R. L.; Übler, Hannah; Bandara, K.; Beifiori, A.; Belli, Sirio; Brammer, Gabriel; Chan, J.; Davies, R. I.; Fabricius, Maximilian; Galametz, A.; Lang, P.; Lutz, D.; Nelson, Erica J.; Momcheva, Ivelina; Price, Sedona H.; Rosario, D. J.; Saglia, R.; Seitz, S.; Shimizu, T.; Tacconi, L. J.; Tadaki, Ken-ichi; Dokkum, Pieter van; Wuyts, Eva

doi:10.3847/1538-4357/ab4db8

Cited by 111 publications

(98 citation statements)

References 147 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…At all redshifts up to the (z ∼ 2) peak of the galaxy or SFR, MS SFGs have disky, exponential rest-frame optical-light distributions with Sersic indices, n Sersic ∼ 1-2 (Wuyts et al 2011b), despite the often clumpy and irregular appearance of z > 1 SFGs in the rest-frame UV. The majority of massive [log(M * /M ) > 10] SFGs are rotationally supported disks (e.g., Wisnioski et al 2015Wisnioski et al , 2019Simons et al 2017). With increasing redshift, the fraction of lower-mass SFGs with dispersiondominated kinematics increases, suggesting that these systems are not settled, equilibrium disks (Kassin et al 2012, Newman et al 2013, Simons et al 2017.…”

Section: Structure Of Main Sequence Galaxiesmentioning

confidence: 99%

The Evolution of the Star-Forming Interstellar Medium Across Cosmic Time

Tacconi

Genzel

Sternberg

2020

Annu. Rev. Astron. Astrophys.

340

327

View full text Add to dashboard Cite

Over the past decade, increasingly robust estimates of the dense molecular gas content in galaxy populations between redshift z = 0 and the peak of cosmic galaxy/star formation ( z ∼ 1–3) have become available. This rapid progress has been possible due to the advent of powerful ground- and space-based telescopes for the combined study of several millimeter to far-IR, line or continuum tracers of the molecular gas and dust components. The main conclusions of this review are as follows: ▪ Star-forming galaxies contained much more molecular gas at earlier cosmic epochs than at the present time. ▪ The galaxy-integrated depletion timescale for converting the gas into stars depends primarily on z or Hubble time and, at a given z, on the vertical location of a galaxy along the star-formation rate versus stellar mass main sequence (MS) correlation. ▪ Global rates of galaxy gas accretion primarily control the evolution of the cold molecular gas content and star-formation rates of the dominant MS galaxy population, which in turn vary with cosmological expansion. Another key driver may be global disk fragmentation in high- z, gas-rich galaxies, which ties local free-fall timescales to galactic orbital times and leads to rapid radial matter transport and bulge growth. The low star-formation efficiency inside molecular clouds is plausibly set by supersonic streaming motions and internal turbulence, which in turn may be driven by conversion of gravitational energy at high z and/or by local feedback from massive stars at low z. ▪ A simple gas regulator model is remarkably successful in predicting the combined evolution of molecular gas fractions, star-formation rates, galactic winds, and gas-phase metallicities. Expected final online publication date for the Annual Review of Astronomy, Volume 58 is August 18, 2020. Please see http://www.annualreviews.org/page/journal/pubdates for revised estimates.

show abstract

Section: Structure Of Main Sequence Galaxiesmentioning

confidence: 99%

The Evolution of the Star-Forming Interstellar Medium Across Cosmic Time

Tacconi

Genzel

Sternberg

2020

Annu. Rev. Astron. Astrophys.

340

327

View full text Add to dashboard Cite

show abstract

“…We are currently in an era of large IFU surveys of galaxies (Sánchez et al 2012;Bundy et al 2015;Bryant et al 2015;Stott et al 2016;Förster Schreiber et al 2018;Wisnioski et al 2019;den Brok et al 2020). Such statistical samples are now able to eliminate the selection biases from previous studies and give an overall picture of the ISM dynamics in the presence of both star formation and AGN processes.…”

Section: Introductionmentioning

confidence: 99%

Super

Kakkad

Mainieri

Vietri

et al. 2020

A&A

109

View full text Add to dashboard Cite

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%.

show abstract

“…Disk galaxies are increasingly clumpy and irregular at high redshift (e.g., Cowie et al 1995;van den Bergh et al 1996;Elmegreen & Elmegreen 2005;Elmegreen et al 2007aElmegreen et al , 2007bGuo et al 2018), and the gas velocity dispersions are several times higher than in local disk galaxies (e.g., Tacconi et al 2010;Wisnioski et al 2015Wisnioski et al , 2019Simons et al 2017). Starforming clumps (often referred to in local galaxies as "complexes" or "star-forming complexes;" "clumps" will be used throughout this paper) of kiloparsec size can be resolved out to redshifts z = 4-5 (Elmegreen & Elmegreen 2005;Elmegreen et al 2007aElmegreen et al , 2007bElmegreen et al , 2009bGuo et al 2015Guo et al , 2018, but their substructure is not resolved.…”

Section: Introductionmentioning

confidence: 99%

A Comparison of Star-forming Clumps and Tidal Tails in Local Mergers and High-redshift Galaxies

Elmegreen

Whitmore

et al. 2021

ApJ

View full text Add to dashboard Cite

The Clusters, Clumps, Dust, and Gas in Extreme Star-forming Galaxies (CCDG) survey with the Hubble Space Telescope includes multiwavelength imaging of 13 galaxies less than 100 Mpc away, spanning a range of morphologies and sizes, from blue compact dwarfs to luminous infrared galaxies, all with star formation rates in excess of hundreds of solar masses per year. Images of seven merging galaxies in the CCDG survey were artificially redshifted to compare with galaxies at z = 0.5, 1, and 2. Most redshifted tails have surface brightnesses that would be visible at z = 0.5 or 1 but not at z = 2 due to cosmological dimming. Giant star clumps are apparent in these galaxies; the 51 measured have similar sizes, masses, and colors to clumps in observed high-z systems in the UDF, GEMS, GOODS, and CANDELS surveys. These results suggest that some clumpy high-z galaxies without observable tidal features could be the result of mergers. The local clumps also have the same star formation rate per unit area and stellar surface density as clumps observed at intermediate and high redshift, so they provide insight into the substructure of distant clumps. A total of 1596 star clusters brighter than M V = −9 were identified within the boundaries of the local clumps. The cluster magnitude distribution function is a power law with approximately the same slope (∼−1 for a plot of number versus log luminosity) for all the galaxies both inside and outside the clumps and independently of clump surface brightness.

show abstract

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

Cited by 111 publications

References 147 publications

The Evolution of the Star-Forming Interstellar Medium Across Cosmic Time

The Evolution of the Star-Forming Interstellar Medium Across Cosmic Time

Super

A Comparison of Star-forming Clumps and Tidal Tails in Local Mergers and High-redshift Galaxies

Contact Info

Product

Resources

About

The KMOS3D Survey: Data Release and Final Survey Paper*

Cited by 111 publications

References 147 publications

The Evolution of the Star-Forming Interstellar Medium Across Cosmic Time

The Evolution of the Star-Forming Interstellar Medium Across Cosmic Time

Super

A Comparison of Star-forming Clumps and Tidal Tails in Local Mergers and High-redshift Galaxies

Contact Info

Product

Resources

About

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