The Sami Galaxy Survey: Galaxy Interactions and Kinematic Anomalies in Abell 119

Oh, Sree; Yi, Sukyoung K.; Cortese, Luca; Sande, Jesse van de; Mahajan, Smriti; Jeong, Hyunjin; Sheen, Yun-Kyeong; Allen, J. T.; Bekki, Kenji; Bland-Hawthorn, Joss; Bloom, J. V.; Brough, Sarah; Bryant, Julia J.; Colless, Matthew; Croom, S. M.; Fogarty, L. M. R.; Goodwin, Michael; Green, Andrew W.; Konstantopoulos, I. S.; Lawrence, Jon; López-Sánchez, Á. R.; Lorente, Nuria P. F.; Medling, Anne M.; Owers, Matt S.; Richards, Samuel N.; Scott, Nicholas; Sharp, Robert; Sweet, Sarah M.

doi:10.3847/0004-637x/832/1/69

Cited by 23 publications

(21 citation statements)

References 93 publications

(99 reference statements)

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“…effective in reducing galaxy spin over a long period of time because only a small parameter space of a merger results in a spin-up during minor merger. Supporting our findings, recent observational studies have also found no clear correlation between post-merger features and spin properties (Duc et al 2015;Oh et al 2016). …”

Section: Resultssupporting

confidence: 81%

On the Evolution of Galaxy Spin in a Cosmological Hydrodynamic Simulation of Galaxy Clusters

Choi

2017

ApJ

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The traditional view of the morphology-spin connection is being challenged by recent integral field unit observations, as the majority of early-type galaxies are found to have a rotational component that is often as large as a dispersion component. Mergers are often suspected to be critical in galaxy spin evolution, yet the details of their roles are still unclear. We present the first results on the spin evolution of galaxies in cluster environments through a cosmological hydrodynamic simulation. Galaxies spin down globally with cosmic evolution. Major (mass ratios > 1/4) and minor (1/4  mass ratios > 1/50) mergers are important contributors to the spin-down in particular in massive galaxies. Minor mergers appear to have stronger cumulative effects than major mergers. Surprisingly, the dominant driver of galaxy spin-down seems to be environmental effects rather than mergers. However, since multiple processes act in combination, it is difficult to separate their individual roles. We briefly discuss the caveats and future studies that are called for.

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Section: Resultssupporting

confidence: 81%

On the Evolution of Galaxy Spin in a Cosmological Hydrodynamic Simulation of Galaxy Clusters

Choi

2017

ApJ

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“…There is more negative scatter in the low than higher mass cases: 25 ± 3% of galaxies with log(M * /M ) < 9.5 lie below the RMS line, compared to 10% ± 1 of galaxies with log(M * /M ) > 9.5. This result is in agreement with Krajnović et al (2011), Oh et al (2016 and others.…”

Section: D Spatially Resolved Tfrsupporting

confidence: 94%

“…However, that the degree to which scatter depends on stellar mass changes between the presented TFRs (see Table 2) is indicative that it is more than a purely physical relationship, and could be at least partly a function of measurement. Oh et al (2016) demonstrated an inverse relationship between asymmetry and rotation velocity from stellar kinematics.…”

Section: Kinematic Asymmetrymentioning

confidence: 97%

The SAMI Galaxy Survey: the low-redshift stellar mass Tully–Fisher relation

Bloom

Croom

Bryant

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We investigate the Tully-Fisher Relation (TFR) for a morphologically and kinematically diverse sample of galaxies from the SAMI Galaxy Survey using 2 dimensional spatially resolved Hα velocity maps and find a well defined relation across the stellar mass range of 8.0 < log(M * /M ) < 11.5.We use an adaptation of kinemetry to parametrise the kinematic Hα asymmetry of all galaxies in the sample, and find a correlation between scatter (i.e. residuals off the TFR) and asymmetry. This effect is pronounced at low stellar mass, corresponding to the inverse relationship between stellar mass and kinematic asymmetry found in previous work. For galaxies with log(M * /M ) < 9.5, 25 ± 3% are scattered below the root mean square (RMS) of the TFR, whereas for galaxies with log(M * /M ) > 9.5 the fraction is 10 ± 1%We use 'simulated slits' to directly compare our results with those from long slit spectroscopy and find that aligning slits with the photometric, rather than the kinematic, position angle, increases global scatter below the TFR. Further, kinematic asymmetry is correlated with misalignment between the photometric and kinematic position angles. This work demonstrates the value of 2D spatially resolved kinematics for accurate TFR studies; integral field spectroscopy reduces the underestimation of rotation velocity that can occur from slit positioning off the kinematic axis.

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“…Owing to several large IFS surveys, now it is known that even early-type galaxies mostly rotate and such rotation is tightly related to environmental density (Cappellari et al 2006;Cappellari et al 2011;Krajnović et al 2011, and many other studies). It was also revealed that direct interactions or mergers between galaxies significantly affect the position angle of galaxy rotation axis, which may result in prolate rotation (Tsatsi et al 2017;Krajnović et al 2018;Weaver et al 2018), morpho-kinematic misalignment (Barrera-Ballesteros et al 2015;Oh et al 2016), or kinematically distinct cores (Emsellem et al 2014;Krajnović et al 2015;Taylor et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Mysterious Coherence in Several-megaparsec Scales between Galaxy Rotation and Neighbor Motion

Lee

Pak

Song

et al. 2019

ApJ

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In our recent report, observational evidence supports that the rotational direction of a galaxy tends to be coherent with the average motion of its nearby neighbors within 1 Mpc. We extend the investigation to neighbors at farther distances, in order to examine if such dynamical coherence is found even in large scales. The Calar Alto Legacy Integral Field Area (CALIFA) survey data and the NASA-Sloan Atlas (NSA) catalog are used. From the composite map of velocity distribution of 'neighbor' galaxies within 15 Mpc from the CALIFA galaxies, the composite radial profiles of the luminosity-weighted mean velocity of neighbors are derived. These profiles show unexpectedly strong evidence of the dynamical coherence between the rotation of the CALIFA galaxies and the average line-of-sight motion of their neighbors within several Mpc distances. Such a signal is particularly strong when the neighbors are limited to red ones: the luminosity-weighted mean velocity at 1 < D ≤ 6 Mpc is as large as 30.6 ± 10.9 km s −1 (2.8σ significance to random spin-axis uncertainty) for central rotation (R ≤ R e ). In the comparison of several subsamples, the dynamical coherence tends to be marginally stronger for the diffuse or kinematically-well-aligned CALIFA galaxies. For this mysterious coherence in large scales, we cautiously suggest a scenario that it results from a possible relationship between the long-term motion of a large-scale structure and the rotations of galaxies in it.

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The Sami Galaxy Survey: Galaxy Interactions and Kinematic Anomalies in Abell 119

Cited by 23 publications

References 93 publications

On the Evolution of Galaxy Spin in a Cosmological Hydrodynamic Simulation of Galaxy Clusters

On the Evolution of Galaxy Spin in a Cosmological Hydrodynamic Simulation of Galaxy Clusters

The SAMI Galaxy Survey: the low-redshift stellar mass Tully–Fisher relation

Mysterious Coherence in Several-megaparsec Scales between Galaxy Rotation and Neighbor Motion

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