The Dawes Review 1: Kinematic Studies of Star-Forming Galaxies Across Cosmic Time

Glazebrook, Karl

doi:10.1017/pasa.2013.34

Cited by 134 publications

(42 citation statements)

References 366 publications

(806 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The height of the ionised (present work) and warm molecular (Hicks et al 2009) discs are well below the measurements of h z for the thin stellar disc of our Galaxy. As a reference, the stellar thin (thick) disc in the Milky Way has a scale height of ∼ 200-300 pc (∼ 1.4 kpc) but with a (much) lower vertical velocity dispersion ∼ 20 km s −1 (∼ 40 km s −1 ), as reported by Glazebrook (2013). We would like to note that the thickness of the very-thin disc in NGC 7469 is comparable to that of the 'nuclear stellar disc' of the Milky Way which have a scale height of 45 ± 5 pc (see Nishiyama et al 2013 andSchödel et al 2014 for details).…”

Section: Dynamical Support and Disc Height Of The Narrow Componentssupporting

confidence: 53%

NGC 7469 as seen by MEGARA: new results from high-resolution IFU spectroscopy

Cazzoli

Paz

Márquez

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present our analysis of high-resolution (R ∼ 20 000) GTC/MEGARA integral-field unit spectroscopic observations, obtained during the commissioning run, in the inner region (12.5 arcsec × 11.3 arcsec) of the active galaxy NGC 7469, at spatial scales of 0.62 arcsec. We explore the kinematics, dynamics, ionisation mechanisms and oxygen abundances of the ionised gas, by modelling the Hα-[N II] emission lines at high signal-to-noise (> 15) with multiple Gaussian components. MEGARA observations reveal, for the first time for NGC 7469, the presence of a very thin (20 pc) ionised gas disc supported by rotation (V/σ = 4.3), embedded in a thicker (222 pc), dynamically hotter (V/σ = 1.3) one. These discs nearly co-rotate with similar peak-to-peak velocities (163 vs. 137 km s −1 ), but with different average velocity dispersion (38 ± 1 vs. 108 ± 4 km s −1 ). The kinematics of both discs could be possibly perturbed by star-forming regions. We interpret the morphology and the kinematics of a third (broader) component (σ > 250 km s −1 ) as suggestive of the presence of non-rotational turbulent motions possibly associated either to an outflow or to the lense. For the narrow component, the [N II]/Hα ratios point to the star-formation as the dominant mechanism of ionisation, being consistent with ionisation from shocks in the case of the intermediate component. All components have roughly solar metallicity. In the nuclear region of NGC 7469, at r ≤ 1.85 arcsec, a very broad (FWHM = 2590 km s −1 ) Hα component is contributing (41 per cent) to the global Hα-[N II] profile, being originated in the (unresolved) broad line region of the Seyfert 1.5 nucleus of NGC 7469.

show abstract

Section: Dynamical Support and Disc Height Of The Narrow Componentssupporting

confidence: 53%

NGC 7469 as seen by MEGARA: new results from high-resolution IFU spectroscopy

Cazzoli

Paz

Márquez

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…These studies resulted in contrary estimates of a potential evolution of the stellar mass zero-point of the TullyFisher relation with redshift (Glazebrook 2013). For example, studies by Puech et al (2008), Vergani et al (2012), Cresci et al (2009), Gnerucci et al (2011), and Simons et al (2016) indicate evolution already at  z 0.6.…”

Section: Introductionmentioning

confidence: 97%

“…In the framework of hierarchical clustering at fixed velocity, the mass of a disk that is a fixed fraction of the total mass of an isothermal halo is predicted to change proportionately to the inverse of the Hubble constant (Mo et al 1998;Glazebrook 2013). The average properties of galaxies also evolve strongly with redshift.…”

Section: Introductionmentioning

confidence: 99%

ZFIRE: The Evolution of the Stellar Mass Tully–Fisher Relation to Redshift ∼2.2

Straatman

Glazebrook

Kacprzak

et al. 2017

ApJ

Self Cite

View full text Add to dashboard Cite

Using observations made with MOSFIRE on Keck I as part of the ZFIRE survey, we present the stellar mass Tully-Fisher relation at < < z 2.0 2.5. The sample was drawn from a stellar-mass-limited, K s -band-selected catalog from ZFOURGE over the CANDELS area in the COSMOS field. We model the shear of the Hα emission line to derive rotational velocities at2.2 the scale radius of an exponential disk (V 2.2 ). We correct for the blurring effect of a 2D point-spread function (PSF) and the fact that the MOSFIRE PSF is better approximated by a Moffat than a Gaussian, which is more typically assumed for natural seeing. We find for the Tully-Fisher relation at 10 , and infer an evolution of D =  M M - 0.45 0.13 dex compared to < z 1.2 if we adopt a fixed slope. We investigate and review various systematics, such as PSF effects, projection effects, systematics related to stellar mass derivation, selection biases, and slope. We find that discrepancies between the various literature values are reduced when taking these into account. Our observations correspond well with the gradual evolution predicted by semianalytic models.

show abstract

“…By revealing the kinematic nature and prevalence of rotating disks among luminous SFGs at z ∼ 1-4, these surveys have contributed key evidence in support of "smoother" mass accretion and for the importance of internal dynamical processes in the early evolution of massive galaxies (e.g., Genzel et al 2006Genzel et al , 2008Förster Schreiber et al 2006;Wright et al 2009;Law et al 2009;Förster Schreiber et al 2009;Epinat et al 2009Epinat et al , 2012Wisnioski et al 2011;Contini et al 2012;Swinbank et al 2012;Sobral et al 2013;Stott et al 2014). However, due to practical limitations of sample selection and telescope time, large statistical and cohesive data sets at z 1 have been unattainable especially at the depth required to measure subtle kinematic and emission line features (see Glazebrook 2013 for a review of IFS results). Currently, a new multiplexed generation has begun for high-redshift galaxy studies of dynamics and chemical evolution with the advent of deployable integral field unit (IFU) systems and multi-object spectrographs operating in the near-infrared where key emission lines are redshifted at 0.5 z 3.…”

Section: Introductionmentioning

confidence: 99%

THE KMOS^3DSURVEY: DESIGN, FIRST RESULTS, AND THE EVOLUTION OF GALAXY KINEMATICS FROM 0.7 ⩽z⩽ 2.7

Wisnioski

Schreiber

Wuyts

et al. 2015

ApJ

527

110

840

View full text Add to dashboard Cite

We present the KMOS 3D survey, a new integral field survey of over 600 galaxies at 0.7 < z < 2.7 using KMOS at the Very Large Telescope. The KMOS 3D survey utilizes synergies with multi-wavelength ground-and spacebased surveys to trace the evolution of spatially resolved kinematics and star formation from a homogeneous sample over 5 Gyr of cosmic history. Targets, drawn from a mass-selected parent sample from the 3D-HST survey, cover the star formation-stellar mass (M * ) and rest-frame (U − V ) − M * planes uniformly. We describe the selection of targets, the observations, and the data reduction. In the first-year of data we detect Hα emission in 191 M * = 3 × 10 9 -7 × 10 11 M galaxies at z = 0.7-1.1 and z = 1.9-2.7. In the current sample 83% of the resolved galaxies are rotation dominated, determined from a continuous velocity gradient and v rot /σ 0 > 1, implying that the star-forming "main sequence" is primarily composed of rotating galaxies at both redshift regimes. When considering additional stricter criteria, the Hα kinematic maps indicate that at least ∼70% of the resolved galaxies are disk-like systems. Our high-quality KMOS data confirm the elevated velocity dispersions reported in previous integral field spectroscopy studies at z 0.7. For rotation-dominated disks, the average intrinsic velocity dispersion decreases by a factor of two from 50 km s −1 at z ∼ 2.3 to 25 km s −1 at z ∼ 0.9. Combined with existing results spanning z ∼ 0-3, we show that disk velocity dispersions follow an evolution that is consistent with the dependence of velocity dispersion on gas fractions predicted by marginally stable disk theory.

show abstract

The Dawes Review 1: Kinematic Studies of Star-Forming Galaxies Across Cosmic Time

Cited by 134 publications

References 366 publications

NGC 7469 as seen by MEGARA: new results from high-resolution IFU spectroscopy

NGC 7469 as seen by MEGARA: new results from high-resolution IFU spectroscopy

ZFIRE: The Evolution of the Stellar Mass Tully–Fisher Relation to Redshift ∼2.2

THE KMOS^3DSURVEY: DESIGN, FIRST RESULTS, AND THE EVOLUTION OF GALAXY KINEMATICS FROM 0.7 ⩽z⩽ 2.7

Contact Info

Product

Resources

About

The Dawes Review 1: Kinematic Studies of Star-Forming Galaxies Across Cosmic Time

Cited by 134 publications

References 366 publications

NGC 7469 as seen by MEGARA: new results from high-resolution IFU spectroscopy

NGC 7469 as seen by MEGARA: new results from high-resolution IFU spectroscopy

ZFIRE: The Evolution of the Stellar Mass Tully–Fisher Relation to Redshift ∼2.2

THE KMOS3DSURVEY: DESIGN, FIRST RESULTS, AND THE EVOLUTION OF GALAXY KINEMATICS FROM 0.7 ⩽z⩽ 2.7

Contact Info

Product

Resources

About

THE KMOS^3DSURVEY: DESIGN, FIRST RESULTS, AND THE EVOLUTION OF GALAXY KINEMATICS FROM 0.7 ⩽z⩽ 2.7