Tracing the filamentary structure of the galaxy distribution at z∼0.8

Choi, Ena; Bond, Nicholas A.; Strauss, Michael A.; Coil, Alison L.; Davis, Marc; Willmer, Christopher N. A.

doi:10.1111/j.1365-2966.2010.16707.x

Cited by 30 publications

(28 citation statements)

References 57 publications

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“…The typical width of the three filaments is (1.5−2.0) h −1 70 Mpc with local variations up to 3 Mpc. Choi et al (2010) observed similar values for a sample of high and low redshift filaments (z ∼ 0.8 and z ∼ 0.1, respectively) taken from the DEEP2 (Davis et al 2003) …”

Section: Width and Length Of The Filaments In Scl2243supporting

confidence: 50%

Mass, light and colour of the cosmic web in the supercluster SCL2243-0935 (z = 0.447)

Schirmer

Hildebrandt

Kuijken

et al. 2011

A&A

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AstrophysicsMass, light and colour of the cosmic web in the supercluster SCL2243-0935 (z = 0.447) , ABSTRACTAims. In archival 2.2 m MPG-ESO/WFI data we discovered several mass peaks through weak gravitational lensing, forming a possible supercluster at redshift 0.45. Through wide-field imaging and spectroscopy we aim to identify the supercluster centre, confirm individual member clusters, and detect possible connecting filaments. Methods. Through multi-colour imaging with CFHT/Megaprime and INT/WFC we identify a population of early-type galaxies and use it to trace the supercluster network. EMMI/NTT multi-object spectroscopy is used to verify the initial shear-selected cluster candidates. We use weak gravitational lensing to obtain mass estimates for the supercluster centre and the filaments. Results. We identified the centre of the SCL2243-0935 supercluster, MACS J2243-0935, which was found independently by Ebeling et al. (2001Ebeling et al. ( , 2010. We found 13 more clusters or overdensities embedded in a large filamentary network. Spectroscopic confirmation for about half of them is still pending. Three Integrating the weak lensing surface mass density over the supercluster network (defined by increased i-band luminosity or g − i colours), we find (1.53 ± 1.01) × 10 15 M and M/L = 305 ± 201 for the three main filaments, consistant with theoretical predictions. The filaments' projected dimensionless surface mass density κ varies between 0.007−0.012, corresponding to ρ/ρ crit = 10−100 depending on location and de-projection. The greatly varying density of the cosmic web is also reflected in the mean colour of galaxies, e.g. g − i = 2.27 mag for the supercluster centre and 1.80 mag for the filaments. Conclusions. SCL2243 is significantly larger and much more richly structured than other known superclusters such as A901/902 or MS0302 studied with weak lensing before. It is a text-book supercluster with little contamination along the line of sight, making it a perfect sandbox for testing new techniques probing the cosmic web.

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Section: Width and Length Of The Filaments In Scl2243supporting

confidence: 50%

Mass, light and colour of the cosmic web in the supercluster SCL2243-0935 (z = 0.447)

Schirmer

Hildebrandt

Kuijken

et al. 2011

A&A

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“…Bond et al (2010b);Choi et al (2010); Eardley et al (2015)), where three-dimensional positions can be accurately determined for all galaxies (at least up to the effect of peculiar velocities). However, determining accurate spectroscopic redshifts for individual galaxies is a very time-consuming operation, and often in astronomy we are forced to make do with datasets for which radial positions are very poorly measured, as is the case for photometric redshift surveys, or even completely unknown.…”

Section: Definitionmentioning

confidence: 99%

Recovering the tidal field in the projected galaxy distribution

Alonso

Hadzhiyska

Strauss

2016

Mon. Not. R. Astron. Soc.

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We present a method to recover and study the projected gravitational tidal forces from a galaxy survey containing little or no redshift information. The method and the physical interpretation of the recovered tidal maps as a tracer of the cosmic web are described in detail. We first apply the method to a simulated galaxy survey and study the accuracy with which the cosmic web can be recovered in the presence of different observational effects, showing that the projected tidal field can be estimated with reasonable precision over large regions of the sky. We then apply our method to the 2MASS survey and present a publicly available full-sky map of the projected tidal forces in the local Universe. As an example of an application of these data we further study the distribution of galaxy luminosities across the different elements of the cosmic web, finding that, while more luminous objects are found preferentially in the most dense environments, there is no further segregation by tidal environment.

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“…If the standard deviation of the fit to a candidate structure was less than 1.5 h −1 Mpc (comparable to or less than the typical thickness of filaments in simulations and observations; e.g. Colberg et al 2005;Akahori & Ryu 2010;Choi et al 2010;Vazza et al 2014), the structure was retained and classified as a filament. If not, the candidate structure was rejected.…”

Section: Data and Analysismentioning

confidence: 99%

Large-Scale Filamentary Structures Around the Virgo Cluster Revisited

Kim

Rey

Bureau

et al. 2016

ApJ

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We revisit the filamentary structures of galaxies around the Virgo cluster, exploiting a larger dataset based on the HyperLeda database than previous studies. In particular, this includes a large number of low-luminosity galaxies, resulting in better sampled individual structures. We confirm seven known structures in the distance range 4 h −1 Mpc < SGY < 16 h −1 Mpc, now identified as filaments, where SGY is the axis of the supergalactic coordinate system roughly along the line of sight. The Hubble diagram of the filament galaxies suggests they are infalling toward the main-body of the Virgo cluster. We propose that the collinear distribution of giant elliptical galaxies along the fundamental axis of the Virgo cluster is smoothly connected to two of these filaments (Leo II A and B). Behind the Virgo cluster (16 h −1 Mpc < SGY < 27 h −1 Mpc), we also identify a new filament elongated toward the NGC 5353/4 group ("NGC 5353/4 filament") and confirm a sheet that includes galaxies from the W and M clouds of the Virgo cluster ("W-M sheet"). In the Hubble diagram, the NGC 5353/4 filament galaxies show infall toward the NGC 5353/4 group, whereas the W-M sheet galaxies do not show hints of gravitational influence from the Virgo cluster. The filamentary structures identified can now be used to better understand the generic role of filaments in the build-up of galaxy clusters at z ≈ 0.

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Tracing the filamentary structure of the galaxy distribution at z∼0.8

Cited by 30 publications

References 57 publications

Mass, light and colour of the cosmic web in the supercluster SCL2243-0935 (z = 0.447)

Mass, light and colour of the cosmic web in the supercluster SCL2243-0935 (z = 0.447)

Recovering the tidal field in the projected galaxy distribution

Large-Scale Filamentary Structures Around the Virgo Cluster Revisited

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