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Puech, M.; Flores, H.; Hammer, F.; Yang, Yanbin; Neichel, Benoît; Lehnert, M. D.; Chemin, L.; Nesvadba, N. P. H.; Épinat, B.; Amram, P.; Balkowski, C.; Césarsky, C. J.; Dannerbauer, H.; Alighieri, S. di Serego; Fuentes-Carrera, I.; Guiderdoni, B.; Kembhavi, Ajit; Liang, Y. C.; Östlin, G.; Pozzetti, L.; Ravikumar, C.; Rawat, A.; Vergani, D.; Vernet, J.; Wozniak, H.

doi:10.1051/0004-6361:20079313

Cited by 126 publications

(249 citation statements)

References 67 publications

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“…Kassin et al (2012) and Puech et al (2008) than in that of Miller et al (2011) predominantly in objects with more disturbed morphologies. This scatter is considerably reduced in Kassin et al's use of the M-S 0.5 relation and is then brought on to the local Faber-Jackson relation (Gallazzi et al 2006).…”

Section: Evolution Of the Scaling Relations?mentioning

confidence: 83%

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

Glazebrook

2013

Publ. Astron. Soc. Aust.

136

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The last seven years have seen an explosion in the number of Integral Field galaxy surveys, obtaining resolved 2D spectroscopy, especially at high-redshift. These have taken advantage of the mature capabilities of 8-10 m class telescopes and the development of associated technology such as AO. Surveys have leveraged both high spectroscopic resolution enabling internal velocity measurements and high spatial resolution from AO techniques and sites with excellent natural seeing. For the first time, we have been able to glimpse the kinematic state of matter in young, assembling starforming galaxies and learn detailed astrophysical information about the physical processes and compare their kinematic scaling relations with those in the local Universe. Observers have measured disc galaxy rotation, merger signatures, and turbulence-enhanced velocity dispersions of gas-rich discs. Theorists have interpreted kinematic signatures of galaxies in a variety of ways (rotation, merging, outflows, and feedback) and attempted to discuss evolution vs. theoretical models and relate it to the evolution in galaxy morphology. A key point that has emerged from this activity is that substantial fractions of high-redshift galaxies have regular kinematic morphologies despite irregular photometric morphologies and this is likely due to the presence of a large number of highly gas-rich discs. There has not yet been a review of this burgeoning topic. In this first Dawes review, I will discuss the extensive kinematic surveys that have been done and the physical models that have arisen for young galaxies at high-redshift.

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Section: Evolution Of the Scaling Relations?mentioning

confidence: 83%

“…of Courteau (1997) which is an analytic form that expresses a profile initially rising smoothly with a 'kinematic scale radius' r p (Weiner et al 2006a;Puech et al 2008) and smoothly transitioning to a flat top; and (ii) the linear ramp function:…”

Section: Measuring Rotation Curvesmentioning

confidence: 99%

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

Glazebrook

2013

Publ. Astron. Soc. Aust.

136

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“…Table 1 summarizes its overall properties, including photometry, morphological parameters, and kinematical measurements (provided by the IMAGES data base that can be retrieved from Yang et al 2008;Neichel et al 2008;Puech et al 2008). This object has a stellar mass of 2.0 × 10 10 M , a K-band magnitude of M K = −20.94, and displays a peculiar morphology and kinematics.…”

Section: General Properties Of J03323972-2751547mentioning

confidence: 99%

“…Given the spatial resolution, it is not easy to derive a rotation curve. Nevertheless, thorough modelling of the velocity fields was completed by Puech et al (2008), who investigated the redshift evolution of the Tully-Fisher relation. Given its kinematical and morphological properties, it is thus unlikely that J033239.72-275154.7 can be a rotating disk hosting two giant HII regions because: (1) the two knots have a z-band luminosity corresponding to one third of the total z luminosity (the relative photometry was completed using apertures of diameter equal to the full width half maximum of the knot luminosity, using the IRAF/DAOPHOT/ package); (2) the dynamical axis is strongly off-center; (3) the value of σ is high and that of V rot is low.…”

Section: General Properties Of J03323972-2751547mentioning

confidence: 99%

A giant bar induced by a merger event at z = 0.4?

Peirani¹,

Hammer

Flores

et al. 2009

A&A

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Context. Disk galaxies are the most common galaxy population in the local universe. However, the formation of their disks and structures -in particular their bars -is still a matter of debate. Aims. We present a physical model of the formation of J033239.72-275154.7, a galaxy observed at z = 0.41 that contains a large, young bar of size 6 kpc. The study of this system is particularly interesting to the understanding of the connection between mergers and bars, as well as the properties and fate of this system in relation to disk galaxy formation. Methods. We compare the morphological and kinematic properties of J033239.72-275154.7, the latter obtained by the GIRAFFE spectrograph, to those derived from the merger of two spiral galaxies described by idealized N-body simulations, including a star formation prescription. Results. We found that the general morphological shape and most of the dynamical properties of the object can be well reproduced by a model in which the satellite is initially placed in a retrograde orbit and the mass ratio of the system is 1:3. In this scenario, a bar forms in the host galaxy after the first passage of the satellite, where a significant fraction of the available gas is consumed in an induced burst. In its later evolution, however, we find that J033239.72-275154.7, whose major progenitor was an Sab galaxy, will probably become a S0 galaxy. This is mainly due to the violent relaxation and the angular momentum loss experienced by the host galaxy during the merger process, which is caused by the adopted orbital parameters. This result suggests that the building of the Hubble sequence is influenced significantly by the last major collision. In the present case, the merger leads to a severe damage of the disk of the progenitor, leading to an evolution towards a more bulge-dominated galaxy. Conclusions.

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“…When the infrared TFR was recently applied to evolutionary studies, Conselice et al (2005) and Flores et al (2006) did not find a K-band TFR evolution. However, in a recent work, Puech et al (2008) do find evolution in the sense that galaxies had been fainter in the past, a result opposite to what is found in the optical bands (for example, Böhm et al 2004). These results suggest that the TFR could be dependent on the observed photometric band.…”

Section: Introductionmentioning

confidence: 62%

Evolution of the optical Tully-Fisher relation up to z = 1.3

Lorenzo¹,

Cepa

Bongiovanni³

et al. 2009

A&A

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Context. The study of the evolution of the Tully-Fisher relation has been controversial in the past years. The main difficulty is in determining the required parameters for intermediate and high redshift galaxies, given the cosmological corrections and biases involved. Aims. This work aims to identify the main problems of the study of the Tully-Fisher relation at high redshift using optical emission lines, in order to draw conclusions about the possible evolution of this relation in the B, R, and I-bands. Methods. With this aim, the rotational velocities obtained from the widths of different optical lines using DEEP2 spectra are compared. This method allows reaching higher redshifts against the rotation curve one, due to spatial resolution limitations. Morphology has been determined via HST images, using and comparing different methodologies. Instrumental magnitudes are then corrected for K and extinction and the absolute magnitudes derived for the concordance cosmological model. Finally, the optical Tully-Fisher relations in B, R, and I-bands at different redshifts up to z = 1.3 are derived. Results. Although most studies (this one included) find evidence of evolution, the results are not conclusive enough, since the possible luminosity evolution is within the scattering of the relation, and the evolution in slope is difficult to determine because at high redshift only the brightest galaxies can be measured. Nevertheless, our study shows a clear tendency, which is the same for all bands studied, that favours a luminosity evolution where galaxies were brighter in the past for the same rotation velocity. This result also implies that the colour of the Tully-Fisher relation does not change with redshift, supporting the collapse model versus the accretion model of disc galaxy formation.

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Cited by 126 publications

References 67 publications

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

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

A giant bar induced by a merger event at z = 0.4?

Evolution of the optical Tully-Fisher relation up to z = 1.3

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