Detection of the Effect of Cosmological Large-Scale Structure on the Orientation of Galaxies

Trujillo, Ignacio; Carretero, C.; Patiri, Santiago G.

doi:10.1086/503548

Cited by 120 publications

(170 citation statements)

References 25 publications

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“…Each spin vector is normalized to unity. Other authors chose to use just one (Lee & Erdogdu 2007) or both (Kashikawa & Okamura 1992;Varela et al 2012) spin vector simultaneously (as we do) or use some other approach to deal with this indeterminacy of the spin vectors of galaxies (Trujillo et al 2006;Slosar & White 2009). …”

Section: Observational Samples and Galaxy Spin Vectorsmentioning

confidence: 99%

“…Navarro et al (2004) found that (spiral) galaxies in the supergalactic plane tend to spin with their spin axis in the supergalactic plane. Trujillo et al (2006) also found that spin axes of spiral galaxies are preferentially in the plane of the walls of cosmic voids, although this signal appears to be disputed by Slosar & White (2009) who found no alignment between spiral galaxies and void walls. If sitting in a cosmic filament, and Tempel & Libeskind (2013) used the SDSS to show that the short axes of elliptical galaxies tend to be perpendicular to the filament axis.…”

Section: Introductionmentioning

confidence: 99%

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The alignment of galaxy spin with the shear field in observations

Pahwa

Libeskind

Tempel

et al. 2016

Mon. Not. R. Astron. Soc.

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Tidal torque theory suggests that galaxies gain angular momentum in the linear stage of structure formation. Such a theory predicts alignments between the spin of haloes and tidal shear field. However, non-linear evolution and angular momentum acquisition may alter this prediction significantly. In this paper, we use a reconstruction of the cosmic shear field from observed peculiar velocities combined with spin axes extracted from galaxies within 115 Mpc (∼ 8000 kms −1 ) from 2MRS catalog, to test whether or not galaxies appear aligned with principal axes of shear field. Although linear reconstructions of the tidal field have looked at similar issues, this is the first such study to examine galaxy alignments with velocity-shear field. Ellipticals in the 2MRS sample, show a statistically significant alignment with two of the principal axes of the shear field. In general, elliptical galaxies have their short axis aligned with the axis of greatest compression and perpendicular to the axis of slowest compression. Spiral galaxies show no signal. Such an alignment is significantly strengthened when considering only those galaxies that are used in velocity field reconstruction. When examining such a subsample, a weak alignment with the axis of greatest compression emerges for spiral galaxies as well. This result indicates that although velocity field reconstructions still rely on fairly noisy and sparse data, the underlying alignment with shear field is strong enough to be visible even when small numbers of galaxies are considered -especially if those galaxies are used as constraints in the reconstruction.

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Section: Observational Samples and Galaxy Spin Vectorsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The alignment of galaxy spin with the shear field in observations

Pahwa

Libeskind

Tempel

et al. 2016

Mon. Not. R. Astron. Soc.

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“…This has resulted in robust detections of various alignments: Brainerd (2005), Yang et al (2006), and Azzaro et al (2007) all found that satellite galaxies are preferentially distributed along the major axes of their host galaxies, Trujillo et al (2006) found that spiral galaxies located on the shells of large voids have rotation axes that lie preferentially on the void surface, and Pereira & Kuhn (2005) and Agustsson & Brainerd (2006a) noticed that satellite galaxies tend to be preferentially oriented toward the galaxy at the center of the halo.…”

Section: Introductionmentioning

confidence: 99%

Three Different Types of Galaxy Alignment within Dark Matter Halos

Faltenbacher

Mao

et al. 2007

ApJ

101

125

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Using a large galaxy group catalog based on the Sloan Digital Sky Survey Data Release 4, we measure three different types of intrinsic galaxy alignment within groups: halo alignment between the orientation of the brightest group galaxies (BGG) and the distribution of its satellite galaxies, radial alignment between the orientation of a satellite galaxy and the direction toward its BGG, and direct alignment between the orientation of the BGG and that of its satellites. In agreement with previous studies, we find that satellite galaxies are preferentially located along the major axis. In addition, on scales we find that red satellites are preferentially aligned radially r ! 0.7R vir with the direction to the BGG. The orientations of blue satellites, however, are perfectly consistent with being isotropic. Finally, on scales , we find a weak but significant indication for direct alignment between r ! 0.1R vir satellites and BGGs. We briefly discuss the implications for weak-lensing measurements.

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“…An important aspect of galaxy evolution with respect to CW features is the correlation between the spin of galaxies and their filaments, as recently detected in the SDSS (Tempel, Stoica, and Saar, 2013;Trujillo, Carretero, and Patiri, 2006;Zhang et al, 2013). This result confirms the role played by the large scale dynamical environment in the evolution of galaxies.…”

Section: Galaxy Properties and Large Scale Structure Of The Universementioning

confidence: 86%

“…On the other hand, Darvish et al (2014) and Fadda et al (2008) found an increased SFR for galaxies in filaments compared to clusters. In recent years, a few studies have also started to investigate the CW in great detail, considering all the possible structures (clusters, filaments, walls, and voids) and studying the statistical distribution of galaxy properties with respect to the CW (Brouwer et al, 2016;Eardley et al, 2015;Martínez, Muriel, and Coenda, 2016).An important aspect of galaxy evolution with respect to CW features is the correlation between the spin of galaxies and their filaments, as recently detected in the SDSS (Tempel, Stoica, and Saar, 2013;Trujillo, Carretero, and Patiri, 2006;Zhang et al, 2013). This result confirms the role played by the large scale dynamical environment in the evolution of galaxies.…”

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confidence: 99%

The Role of the Environment on Galaxy Evolution

Boselli

2011

A Panchromatic View of Galaxies

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Esame finale anno 2016A Milena "Che fai tu, Luna, in ciel? Dimmi, che fai, silenziosa Luna?" -Giacomo Leopardi, Canto notturno di un pastore errante dell'Asia A B S T R A C TAlthough the general picture of how galaxies have formed and evolved through cosmic time is already in place, still many details are missing. An example is represented by a quantitative characterization of the role that environment plays during the evolution of galaxies in determining their observed properties in the local Universe. Local galaxy environment has been thoroughly explored through observations at low redshift and it has recently started to being investigated also in the distant Universe. Moreover, general attention has been increasingly focused on the relation between galaxy evolution and galaxy positions with respect to the large-scale structures of the cosmic web.This work explores how environment (defined both in terms of local overdensities on the Mpc scale around galaxies, as well as in terms of the distribution of galaxy distances from ∼ 10 2 Mpc long cosmic filaments) is observationally related to galaxy properties such as their stellar mass, their star-formation activity, or the presence of Active Galactic Nucleus phenomena. The analysis reported here is performed in a large redshift range, going from the local Universe (z 0.2) to intermediate (z ∼ 0.7) and high-redshifts (z 3). To perform this study, both spectroscopic redshift data sets as well as photometric redshift surveys have been deployed and (particularly for the photometric redshift data sets) a thorough analysis of the effect of their observational issues on the measurement of local and global environment has been executed.The picture that emerges is that high-density environments are favoured places for galaxy evolution, showing an enhanced fraction of massive galaxies which have stopped forming stars and belong to the quiescent population. Galaxies in high-density environments have an increased probability of hosting radio-AGNs (belonging to the ensemble of processes that turn off the star-formation in massive galaxies) and these effects are visible since the start of the decline in the cosmic star-formation history. Large-scale structures, such as the filaments of the cosmic web, have also a role in shaping galaxy evolution and they may represent key places for the pre-processing of galaxies before they enter higher density regions such as the cluster or group environment.As an increasing amount of observational evidence on the relation between the evolution of galaxies and their environment is gathered, a complete solution to the problem of how the local galaxy population has evolved approaches, and the history of galaxies from their formation at the dawn of time to the present day gets closer to being traced. Figure 2 Growth of structures . . . . . . . . . . . . . . . 7 Figure 3 Evolution of the global SFR density . . . . . . . 8 Figure 4 Colour-density relation for VVDS galaxies . . 11 Figure 5 Fraction of M * contained in galaxies as a function sSFR ....

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Detection of the Effect of Cosmological Large-Scale Structure on the Orientation of Galaxies

Cited by 120 publications

References 25 publications

The alignment of galaxy spin with the shear field in observations

The alignment of galaxy spin with the shear field in observations

Three Different Types of Galaxy Alignment within Dark Matter Halos

The Role of the Environment on Galaxy Evolution

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