THE DETECTION OF THE LARGE-SCALE ALIGNMENT OF MASSIVE GALAXIES AT
                    <i>z</i>
                    ∼ 0.6

Li, Cheng; Jing, Y. P.; Faltenbacher, A.; Wang, Jie

doi:10.1088/2041-8205/770/1/l12

Cited by 49 publications

(69 citation statements)

References 48 publications

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“…Lee & Erdogdu 2007;Faltenbacher et al 2009;Li et al 2013;Tempel & Libeskind 2013;Zhang et al 2013;Pahwa et al 2016). There is also agreement with Wang et al (2009) for main galaxies of groups.…”

Section: Early-type Galaxiessupporting

confidence: 65%

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Alignment of galaxies relative to their local environment in SDSS-DR8

Hirv

Pelt

Saar

et al. 2017

A&A

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Aims. We study the alignment of galaxies relative to their local environment in SDSS-DR8 and, using these data, we discuss evolution scenarios for different types of galaxies. Methods. We defined a vector field of the direction of anisotropy of the local environment of galaxies. We summed the unit direction vectors of all close neighbours of a given galaxy in a particular way to estimate this field. We found the alignment angles between the spin axes of disc galaxies, or the minor axes of elliptical galaxies, and the direction of anisotropy. The distributions of cosines of these angles are compared to the random distributions to analyse the alignment of galaxies. Results. Sab galaxies show perpendicular alignment relative to the direction of anisotropy in a sparse environment, for single galaxies and galaxies of low luminosity. Most of the parallel alignment of Scd galaxies comes from dense regions, from 2 . . . 3 member groups and from galaxies with low luminosity. The perpendicular alignment of S0 galaxies does not depend strongly on environmental density nor luminosity; it is detected for single and 2 . . . 3 member group galaxies, and for main galaxies of 4 . . . 10 member groups. The perpendicular alignment of elliptical galaxies is clearly detected for single galaxies and for members of ≤10 member groups; the alignment increases with environmental density and luminosity. Conclusions. We confirm the existence of fossil tidally induced alignment of Sab galaxies at low z. The alignment of Scd galaxies can be explained via the infall of matter to filaments. S0 galaxies may have encountered relatively massive mergers along the direction of anisotropy. Major mergers along this direction can explain the alignment of elliptical galaxies. Less massive, but repeated mergers are possibly responsible for the formation of elliptical galaxies in sparser areas and for less luminous elliptical galaxies.

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Section: Early-type Galaxiessupporting

confidence: 65%

“…For a straight isolated filament, DALE is equivalent to the direction of the spine. In principle, our approach is similar to the alignment correlation function method developed by Faltenbacher et al (2009) and Li et al (2013).…”

Section: Introductionmentioning

confidence: 99%

Alignment of galaxies relative to their local environment in SDSS-DR8

Hirv

Pelt

Saar

et al. 2017

A&A

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“…Mandelbaum et al 2006;Okumura et al 2009;Hirata et al ⋆ vuitert@ucl.ac.uk 2007; Joachimi et al 2011;Li et al 2013;Singh et al 2015), in N -body simulations (e.g. Croft & Metzler 2000;Hopkins et al 2005) and in hydrodynamical simulations (Codis et al 2015;Velliscig et al 2015;Chisari et al 2015Chisari et al , 2016Tenneti et al 2016;Hilbert et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Intrinsic alignment of redMaPPer clusters: cluster shape–matter density correlation

Uitert¹,

Joachimi²

2017

Monthly Notices of the Royal Astronomical Society

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We measure the alignment of the shapes of galaxy clusters, as traced by their satellite distributions, with the matter density field using the public redMaPPer catalogue based on SDSS-DR8, which contains 26 111 clusters up to z ∼ 0.6. The clusters are split into nine redshift and richness samples; in each of them we detect a positive alignment, showing that clusters point towards density peaks. We interpret the measurements within the tidal alignment paradigm, allowing for a richness and redshift dependence. The intrinsic alignment (IA) amplitude at the pivot redshift z = 0.3 and pivot richness λ = 30 is A gen IA = 12.6 +1.5 −1.2 . We obtain tentative evidence that the signal increases towards higher richness and lower redshift. Our measurements agree well with results of maxBCG clusters and with dark-matter-only simulations. Comparing our results to IA measurements of luminous red galaxies, we find that the IA amplitude of galaxy clusters forms a smooth extension towards higher mass. This suggests that these systems share a common alignment mechanism, which can be exploited to improve our physical understanding of IA.

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“…It is found that the major axes of LRGs at z∼ 0.3 are correlated up to 30 ∼70Mpc/h (Okumura et al 2009;Li et al 2013), as shown by the points in upper left panel of Fig.3. Okumura et al also found that if the major axis of LRG follows that of the dark matter perfectly, the predicted alignment from N-body simulation is higher than the data (red dashed line), but if there is an average misalignment about 35…”

Section: Resultsmentioning

confidence: 71%

“…(e.g., Yang et al 2006). On large scales, it is found that the shape of Luminous Red Galaxies (LRGs) are correlated up to scales of 30∼70Mpc/h (Okumura et al 2009;Li et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Galaxy alignment on large and small scales

et al. 2014

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Abstract. Galaxies are not randomly distributed across the universe but showing different kinds of alignment on different scales. On small scales satellite galaxies have a tendency to distribute along the major axis of the central galaxy, with dependence on galaxy properties that both red satellites and centrals have stronger alignment than their blue counterparts. On large scales, it is found that the major axes of Luminous Red Galaxies (LRGs) have correlation up to 30Mpc/h. Using hydro-dynamical simulation with star formation, we investigate the origin of galaxy alignment on different scales. It is found that most red satellite galaxies stay in the inner region of dark matter halo inside which the shape of central galaxy is well aligned with the dark matter distribution. Red centrals have stronger alignment than blue ones as they live in massive haloes and the central galaxy-halo alignment increases with halo mass. On large scales, the alignment of LRGs is also from the galaxy-halo shape correlation, but with some extent of mis-alignment. The massive haloes have stronger alignment than haloes in filament which connect massive haloes. This is contrary to the naive expectation that cosmic filament is the cause of halo alignment.

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THE DETECTION OF THE LARGE-SCALE ALIGNMENT OF MASSIVE GALAXIES AT z ∼ 0.6

Cited by 49 publications

References 48 publications

Alignment of galaxies relative to their local environment in SDSS-DR8

Alignment of galaxies relative to their local environment in SDSS-DR8

Intrinsic alignment of redMaPPer clusters: cluster shape–matter density correlation

Galaxy alignment on large and small scales

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