2D kinematics and physical properties of<i>z ∼ 3</i>star-forming galaxies

Lemoine-Busserolle, Marie; Bunker, Andrew J.; Lamareille, F.; Kissler-Patig, M.

doi:10.1111/j.1365-2966.2009.15807.x

Cited by 43 publications

(48 citation statements)

References 63 publications

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“…By combining samples spanning a range of star-formation rates and redshifts (Law et al , 2007Yang et al 2008;Garrido et al 2002;Epinat et al 2008b;Epinat, Amram, & Marcelin 2008a;Epinat et al 2009;Lemoine-Busserolle et al 2010;Cresci et al 2009;Contini et al, 2012;Wisnioski et al 2011;Jones et al 2010;Swinbank et al 2012;Green et al 2014), Green et al (2010Green et al ( , 2014 found that velocity dispersion did correlate with the star-formation rate. From this, they suggested that star formation is the energetic driver of galaxy disc turbulence at both high and low redshift.…”

Section: Introductionmentioning

confidence: 96%

Resolved Gas Kinematics in a Sample of Low-Redshift High Star-Formation Rate Galaxies

Varidel

Pracy

Croom

et al. 2016

Publ. Astron. Soc. Aust.

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We have used integral field spectroscopy of a sample of six nearby (z ∼ 0.01-0.04) high star-formation rate (SFR ∼ 10-40 M yr −1 ) galaxies to investigate the relationship between local velocity dispersion and star-formation rate on sub-galactic scales. The low-redshift mitigates, to some extent, the effect of beam smearing which artificially inflates the measured dispersion as it combines regions with different line-of-sight velocities into a single spatial pixel. We compare the parametric maps of the velocity dispersion with the Hα flux (a proxy for local star-formation rate), and the velocity gradient (a proxy for the local effect of beam smearing). We find, even for these very nearby galaxies, the Hα velocity dispersion correlates more strongly with velocity gradient than with Hα flux-implying that beam smearing is still having a significant effect on the velocity dispersion measurements. We obtain a first-order non parametric correction for the unweighted and flux weighted mean velocity dispersion by fitting a 2D linear regression model to the spaxel-byspaxel data where the velocity gradient and the Hα flux are the independent variables and the velocity dispersion is the dependent variable; and then extrapolating to zero velocity gradient. The corrected velocity dispersions are a factor of ∼1.3-4.5 and ∼1.3-2.7 lower than the uncorrected flux-weighted and unweighted mean line-of-sight velocity dispersion values, respectively. These corrections are larger than has been previously cited using disc models of the velocity and velocity dispersion field to correct for beam smearing. The corrected flux-weighted velocity dispersion values are σ m ∼ 20-50 km s −1 .

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Section: Introductionmentioning

confidence: 96%

Resolved Gas Kinematics in a Sample of Low-Redshift High Star-Formation Rate Galaxies

Varidel

Pracy

Croom

et al. 2016

Publ. Astron. Soc. Aust.

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“…Several active processes, including minor and major mergers, smooth accretion, feedback from star formation, and violent disk instabilities, can disrupt or stall disk formation. Indeed, observations indicate that the internal kinematics of star-forming galaxies at this time have large amounts of disordered motions (as measured by the velocity dispersion of the gas s g ) in addition to ordered rotation (V rot ) (e.g., Förster Schreiber et al 2006Schreiber et al , 2009Genzel et al 2006Genzel et al , 2008Law et al 2007Law et al , 2009Law et al , 2012Wright et al 2007;Wright et al 2009;Shapiro et al 2008;Lemoine-Busserolle et al 2010;Jones et al 2010;Swinbank et al 2011;Glazebrook 2013;Newman et al 2013b;Wisnioski et al 2015;Price et al 2016;Simons et al 2016;Mason et al 2017;Straatman et al 2017). Regardless, the majority of massive star-forming galaxies, * >  M M log 10, at this redshift are rotation-dominated ( s > V g rot ), with at least 70% showing disk-like kinematic signatures (Wisnioski et al 2015).…”

Section: Introductionmentioning

confidence: 99%

z ∼ 2: An Epoch of Disk Assembly

Simons

Kassin

Weiner

et al. 2017

ApJ

131

123

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We explore the evolution of the internal gas kinematics of star-forming galaxies from the peak of cosmic star formation atz 2 to today. Measurements of galaxy rotation velocity V rot , which quantify ordered motions, and gas velocity dispersion s g , which quantify disordered motions, are adopted from the DEEP2 and SIGMA surveys. This sample covers a continuous baseline in redshift over < < z 0.1 2.5, spanning 10 Gyr. At low redshift, nearly all sufficiently massive star-forming galaxies are rotationally supported (By z=2, 50% and 70% of galaxies are rotationally supported at low ( ) stellar mass, respectively. For, the percentage drops below 35% for all masses. From z=2 to now, galaxies exhibit remarkably smooth kinematic evolution on average. All galaxies tend toward rotational support with time, and higher-mass systems reach it earlier. This is largely due to a mass-independent decline in s g by a factor of 3 since z=2. Over the same time period, V rot increases by a factor of 1.5 in low-mass systems but does not evolve at high mass. These trends in V rot and s g are at a fixed stellar mass and therefore should not be interpreted as evolutionary tracks for galaxy populations. When populations are linked in time via abundance matching, s g declines as before and V rot strongly increases with time for all galaxy populations, enhancing the evolution in s V g rot . These results indicate that = z 2 is a period of disk assembly, during which strong rotational support is only just beginning to emerge.

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“…Many dynamical studies have been performed on extended samples of z ∼ 1−2.5 objects Förster Schreiber et al 2006Cresci et al 2009;Erb et al 2006;Law et al 2007Law et al , 2009Epinat et al 2009;Wright et al 2007Wright et al , 2009). However, little is known on the dynamics of galaxies at z > ∼ 2.5, where only a few particular objects have been investigated (Nesvadba et al 2006(Nesvadba et al , 2007(Nesvadba et al , 2008Jones et al 2010;Law et al 2009;Lemoine-Busserolle et al 2010;Swinbank et al 2007Swinbank et al , 2009.…”

Section: Introductionmentioning

confidence: 99%

Dynamical properties of AMAZE and LSD galaxies from gas kinematics and the Tully-Fisher relation atz ~ 3

Gnerucci

Marconi

Cresci

et al. 2011

A&A

158

264

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We present a SINFONI integral-field kinematical study of 33 galaxies at z ∼ 3 from the AMAZE and LSD projects, which are aimed at studying metallicity and dynamics of high-redshift galaxies. The number of galaxies analyzed in this paper constitutes a significant improvement over existing data in the literature, and this is the first time that a dynamical analysis is obtained for a relatively large sample of galaxies at z ∼ 3. Eleven galaxies show ordered rotational motions (∼30% of the sample). In these cases we estimate dynamical masses by modeling the gas kinematics with rotating disks and exponential mass distributions. We find dynamical masses in the range 2 × 10 9 M −2 × 10 11 M with a mean value of ∼2 × 10 10 M . By comparing observed gas velocity dispersion with what is expected from models, we find that most rotating objects are dynamically "hot", with intrinsic velocity dispersions of ∼90 km s −1 . The median value of the ratio between the maximum disk rotational velocity and the intrinsic velocity dispersion for the rotating objects is 1.6, much lower than observed in local galaxies value (∼10) and slightly lower than the z ∼ 2 value (2-4). Finally we use the maximum rotational velocity from our modeling to build a baryonic Tully-Fisher relation at z ∼ 3. Our measurements indicate that z ∼ 3 galaxies have lower stellar masses (by a factor of ten on average) compared to local galaxies with the same dynamical mass. However, the large observed scatter suggests that the Tully-Fisher relation is not yet "in place" at these early cosmic ages, possibly owing to the young age of galaxies. A smaller dispersion of the Tully-Fisher relation is obtained by taking the velocity dispersion into account with the use of the S 0.5 indicator, suggesting that turbulent motions might play an important dynamical role.

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2D kinematics and physical properties ofz ∼ 3star-forming galaxies

Cited by 43 publications

References 63 publications

Resolved Gas Kinematics in a Sample of Low-Redshift High Star-Formation Rate Galaxies

Resolved Gas Kinematics in a Sample of Low-Redshift High Star-Formation Rate Galaxies

z ∼ 2: An Epoch of Disk Assembly

Dynamical properties of AMAZE and LSD galaxies from gas kinematics and the Tully-Fisher relation atz ~ 3

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