Dynamical properties of AMAZE and LSD galaxies from gas kinematics and the Tully-Fisher relation at<i>z</i>  ~  3

Gnerucci, Alessio; Marconi, A.; Cresci, G.; Maiolino, R.; Mannucci, F.; Calura, F.; Cimatti, A.; Cocchia, F.; Grazian, A.; Matteuccí, F.; Nagao, Tohru; Pozzetti, L.; Troncoso, P.

doi:10.1051/0004-6361/201015465

Cited by 160 publications

(292 citation statements)

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“…In the table, companions have the suffix "s". The model rotation curve only reproduces the velocity field and is not based on a gravitational potential model (as for instance in Förster Schreiber et al 2006;Cresci et al 2009;Gnerucci et al 2011) since the shape of the gravitational potential is unknown and can probably not be described by a stellar component only. Note that a gaseous thin disk in rotation is not incompatible with a spheroidal stellar distribution such as was observed in local ellipticals (e.g.…”

Section: Kinematics Modelingmentioning

confidence: 99%

“…From the IMAGES sample at 0.4 < z < 0.75 (Yang et al 2008;Neichel et al 2008;Puech et al 2008;Rodrigues et al 2008), it has been shown that regular rotating disks are quite similar to local rotators and that merging is playing a significant role in galaxy mass assembly. At higher redshift, the SINS sample at z ∼ 2.2 Shapiro et al 2008;Förster Schreiber et al 2009;Shapiro et al 2009;Cresci et al 2009), the LSD/AMAZE sample at z ∼ 3.3 (Gnerucci et al 2011) and the sample built by Law et al (2009) at 2 < z < 3 are all containing many galaxies with high gaseous turbulence. Based on numerical simulation results of unstable gas-rich disks (e.g.…”

Section: Introductionmentioning

confidence: 99%

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MASSIV: Mass Assembly Survey with SINFONI in VVDS

Divoy

Contini²,

Pérez-Montero³

et al. 2012

A&A

169

242

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Context. Processes driving mass assembly are expected to evolve on different timescales along cosmic time. A transition might happen around z ∼ 1 as the cosmic star formation rate starts its decrease. Aims. We aim to identify the dynamical nature of galaxies in a representative sample to be able to infer and compare the mass assembly mechanisms across cosmic time.Methods. We present an analysis of the kinematics properties of 50 galaxies with redshifts 0.9 < z < 1.6 from the MASSIV sample observed with SINFONI/VLT with a mass range from 4.5 × 10 9 M to 1.7 × 10 11 M and a star formation rate from 6 M yr −1 to 300 M yr −1 . This is the largest sample with 2D kinematics in this redshift range. We provide a classification based on kinematics as well as on close galaxy environment. Results. We find that a significant fraction of galaxies in our sample (29%) experience merging or have close companions that may be gravitationally linked. This places a lower limit on the fraction of interacting galaxies because ongoing mergers are probably also present but harder to identify. We find that at least 44% of the galaxies in our sample display ordered rotation, whereas at least 35% are non-rotating objects. All rotators except one are compatible with rotation-dominated (V max /σ > 1) systems. Non-rotating objects are mainly small objects (R e < 4 kpc). They show an anti-correlation of their velocity dispersion and their effective radius. These lowmass objects (log M star < 10.5) may be ongoing mergers in a transient state, galaxies with only one unresolved star-forming region, galaxies with an unstable gaseous phase or, less probably, spheroids. Combining our sample with other 3D-spectroscopy samples, we find that the local velocity dispersion of the ionized gas component decreases continuously from z ∼ 3 to z = 0. The proportion of disks also seems to be increasing in star-forming galaxies when the redshift decreases. The number of interacting galaxies seems to be at a maximum at z ∼ 1.2. Conclusions. These results draw a picture in which cold gas accretion may still be efficient at z ∼ 1.2 but in which mergers may play a much more significant role at z ∼ 1.2 than at higher redshift. From a dynamical point of view, the redshift range 1 < z < 2 therefore appears as a transition period in the galaxy mass assembly process .

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Section: Kinematics Modelingmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

MASSIV: Mass Assembly Survey with SINFONI in VVDS

Divoy

Contini²,

Pérez-Montero³

et al. 2012

A&A

169

242

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“…Many studies have taken advantage of this technique to study the gas dynamics of distant galaxies, from z ∼ 0.6 (Flores et al 2006) up to z 2 (Förster Schreiber et al 2009;Law et al 2009;Epinat et al 2009;Gnerucci et al 2011). Recently, the Mass Assembly Survey with SINFONI in VVDS (MASSIV; Contini et al 2012) has collected data of z ∼ 1−2 galaxies observed with the integral-field spectrograph SINFONI at the VLT (Eisenhauer et al 2003).…”

Section: Introductionmentioning

confidence: 99%

MASSIV: Mass Assembly Survey with SINFONI in VVDS

Contini

Kissler-Patig

Épinat³

et al. 2012

A&A

137

166

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Aims. The estimate of radial abundance gradients in high-redshift galaxies allows to constrain their star formation history and their interplay with the surrounding intergalactic medium. Methods. We present VLT/SINFONI integral-field spectroscopy of a first sample of 50 galaxies at z ∼ 1.2 in the MASSIV survey. Using the N2 ratio between the [N ii]6584 and Hα rest-frame optical emission lines as a proxy for oxygen abundance in the interstellar medium, we measured the metallicity of the sample galaxies. We developed a tool to extract spectra in annular regions, leading to a spatially resolved estimate of the oxygen abundance in each galaxy. We were able to derive a metallicity gradient for 26 galaxies in our sample and discovered a significant fraction of galaxies with a "positive" gradient. Using a simple chemical evolution model, we derived infall rates of pristine gas onto the disks. Results. Seven galaxies display a positive gradient at a high confidence level. Four out of these are interacting, and one is a chain galaxy. We suggest that interactions might be responsible for shallowing and even inverting the abundance gradient. We also identify two interesting correlations in our sample: a) galaxies with higher gas velocity dispersion have shallower/positive gradients; and b) metal-poor galaxies tend to show a positive gradient, whereas metal-rich ones tend to show a negative one. This last observation can be explained by the infall of metal-poor gas into the center of the disks. We address the question of the origin of this infall under the influence of gas flows triggered by interactions and/or cold gas accretion. All the data published in this paper are publicly available at the time of publication following this link: http://cosmosdb.lambrate.inaf.it/VVDS-SINFONI.

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“…Bell & de Jong 2001;Pizagno et al 2007;Meyer et al 2008;Gurovich et al 2010) and intermediate and high redshifts (e.g. Conselice et al 2005;Flores et al 2006;Atkinson et al 2007;Kassin et al 2007;Puech et al 2008;Cresci et al 2009;Gnerucci et al 2011) has been the subject of numerous works. Although many authors suggest the existence of evolution, observational results have not converged yet, and it is also unclear if the evolution is present in the zero point, the slope, or in both (Vogt et al 1996(Vogt et al , 1997Nakamura et al 2006).…”

Section: Introductionmentioning

confidence: 99%

Fingerprints of the hierarchical building-up of the structure on the gas kinematics of galaxies

Rossi

Tissera

Pedrosa

2012

A&A

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Context. Recent observational and theoretical works have suggested that the Tully-Fisher relation might be generalised to include dispersion-dominated systems by combining the rotation and dispersion velocity in the definition of the kinematical indicator. Mergers and interactions have been pointed out as responsible of driving turbulent and disordered gas kinematics, which could generate TullyFisher relation outliers. Aims. We investigated the gas kinematics of galaxies by using a simulated sample that includes gas-disc-dominated as well as spheroid-dominated systems. We paid particular attention to the scatter evolution of the Tully-Fisher relation. We also determined the gas-phase velocity indicator, which traces the potential well of the galaxy better. Methods. Cosmological hydrodynamical simulations that include a multiphase model and physically motivated supernova feedback were performed to follow the evolution of galaxies as they are assembled. We analysed the gas kinematics of the surviving gas discs to estimate all velocity indicators. Results. Both the baryonic and stellar Tully-Fisher relations for gas-disc-dominated systems are tight while, as more dispersiondominated systems are included, the scatter increases. We found a clear correlation between σ/V rot and morphology, with dispersiondominated systems exhibiting higher values (>0.7). Mergers and interactions can affect the rotation curves directly or indirectly, inducing a scatter in the Tully-Fisher relation larger than the simulated evolution since z ∼ 3. Kinematical indicators, which combine rotation velocity and dispersion velocity, can reduce the scatter in the baryonic and the stellar mass-velocity relations. In particular, s 1.0 = (V 2 rot + σ 2 ) 0.5 seems to be the best tracer of the circular velocity at larger radii. Our findings also show that the lowest scatter in both relations is obtained if the velocity indicators are measured at the maximum of the rotation curve. Conclusions. In agreement with previous works, we found that the gas kinematics of galaxies is significantly regulated by mergers and interactions, which play a key role in inducing gas accretion, outflows and starbursts. The joint action of these processes within a hierarchical ΛCDM Universe generates a mean simulated Tully-Fisher relation in good agreement with observations since z ∼ 3 but with a scatter depending on morphology. The rotation velocity estimated at the maximum of the gas rotation curve is found to be the best proxy for the potential well regardless of morphology.

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

Cited by 160 publications

References 56 publications

MASSIV: Mass Assembly Survey with SINFONI in VVDS

MASSIV: Mass Assembly Survey with SINFONI in VVDS

MASSIV: Mass Assembly Survey with SINFONI in VVDS

Fingerprints of the hierarchical building-up of the structure on the gas kinematics of galaxies

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