STUDYING INTERCLUSTER GALAXY FILAMENTS THROUGH STACKING gmBCG GALAXY CLUSTER PAIRS

Zhang, Yuanyuan; McKay, Timothy A.; Sheldon, E.; Nguyen, A.-T.

doi:10.1088/0004-637x/773/2/115

Cited by 27 publications

(22 citation statements)

References 68 publications

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“…Pimbblet, Drinkwater & Hawkrigg 2004), or by stacking analysis from photometric galaxy surveys (e.g. Zhang et al 2013). While these studies confirm the strategy to focus on cluster pairs, they provide limited information into the nature of cosmic filaments; these luminous systems represent 10 per cent of the baryonic matter, their distribution and motions need not trace the majority of the gas, and they offer no insight into the presence of a WHIM.…”

Section: Introductionmentioning

confidence: 83%

Towards the statistical detection of the warm–hot intergalactic medium in intercluster filaments of the cosmic web

Tejos

Prochaska

Crighton

et al. 2015

Mon. Not. R. Astron. Soc.

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Modern analyses of structure formation predict a universe tangled in a 'cosmic web' of dark matter and diffuse baryons. These theories further predict that at low-z, a significant fraction of the baryons will be shock-heated to T ∼ 10 5 − 10 7 K yielding a warm-hot intergalactic medium (WHIM), but whose actual existence has eluded a firm observational confirmation. We present a novel experiment to detect the WHIM, by targeting the putative filaments connecting galaxy clusters. We use HST/COS to observe a remarkable QSO sightline that passes within ∆d = 3 Mpc from the 7 inter-cluster axes connecting 7 independent cluster-pairs at redshifts 0.1 z 0.5. We find tentative excesses of total H I, narrow H I (NLA; Doppler parameters b < 50 km s −1 ), broad H I (BLA; b 50 km s −1 ) and O VI absorption lines within rest-frame velocities of ∆v 1000 km s −1 from the cluster-pairs redshifts, corresponding to ∼ 2, ∼ 1.7, ∼ 6 and ∼ 4 times their field expectations, respectively. Although the excess of O VI likely comes from gas close to individual galaxies, we conclude that most of the excesses of NLAs and BLAs are truly intergalactic. We find the covering fractions, f c , of BLAs close to cluster-pairs are ∼ 4 − 7 times higher than the random expectation (at the ∼ 2σ c.l.), whereas the f c of NLAs and O VI are not significantly enhanced. We argue that a larger relative excess of BLAs compared to those of NLAs close to cluster-pairs may be a signature of the WHIM in inter-cluster filaments. By extending the present analysis to tens of sightlines our experiment offers a promising route to detect the WHIM.

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Section: Introductionmentioning

confidence: 83%

Towards the statistical detection of the warm–hot intergalactic medium in intercluster filaments of the cosmic web

Tejos

Prochaska

Crighton

et al. 2015

Mon. Not. R. Astron. Soc.

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“…The photometric properties of the galaxies in the inter-cluster filament, their star-formation evolution, their weak lensing properties, etc. were performed in many selected cluster (or group) pairs (e.g., Fadda et al 2008;Gallazzi et al 2009;Edwards et al 2010;Zhang et al 2013;Martínez et al 2016;Epps & Hudson 2017 A&A proofs: manuscript no. aa_new may show substructures or evidence of dynamical effect: they merge, interact, and accrete smaller groups.…”

Section: Introductionmentioning

confidence: 99%

Gas and galaxies in filaments between clusters of galaxies

Bonjean

Aghanim

Salomé

et al. 2018

A&A

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We have performed a multi-wavelength analysis of two galaxy cluster systems selected with the thermal Sunyaev-Zel'dovich (tSZ) effect and composed of cluster pairs and an inter-cluster filament. We have focused on one pair of particular interest: A399-A401 at redshift z ∼ 0.073 seperated by 3 Mpc. We have also performed the first analysis of one lower significance newly associated pair: A21-PSZ2 G114.09-34.34 at z ∼ 0.094, separated by 4.2 Mpc. We have characterised the intra-cluster gas using the tSZ signal from Planck and, when this was possible, the galaxy optical and infra-red (IR) properties based on two photometric redshift catalogs: 2MPZ and WISExSCOS. From the tSZ data, we measured the gas pressure in the clusters and in the inter-cluster filaments. In the case of A399-A401, the results are in perfect agreement with previous studies and, using the temperature measured from the X-rays, we further estimate the gas density in the filament and find n 0 = (4.3 ± 0.7) × 10 −4 cm −3 . The optical and IR colour-colour and colour-magnitude analyses of the galaxies selected in the cluster system, together with their Star Formation Rate, show no segregation between galaxy populations, in the clusters and in the filament of A399-A401. Galaxies are all passive, early type, and red and dead. The gas and galaxy properties of this system suggest that the whole system formed at the same time and corresponds to a pre-merger, with a cosmic filament gas heated by the collapse. For the other cluster system, the tSZ analysis was performed and the pressure in the clusters and in the inter-cluster filament was constrained. However, the limited or nonexistent optical and IR data prevent us from concluding on the presence of an actual cosmic filament or from proposing a scenario.

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“…Colberg et al (2005) suggested that the probability of finding a fil-E-mail: julian@oac.unc.edu.ar ament between systems of galaxies is strongly dependent on their separation. Zhang et al (2013) used the SDSS Data Release 8 (Aihara et al 2011) and detected filaments using a sample of more than 50,000 clusters of galaxies. They selected cluster pairs separated by less than 35h −1 Mpc and found that richer clusters are connected to richer filaments.…”

Section: Introductionmentioning

confidence: 99%

“…The role of the filaments in this process has not been extensively studied. Zhang et al (2013) studied the colour and luminosity distribution of galaxies in filaments. They found that filament galaxies are bluer and fainter than cluster members.…”

Section: Introductionmentioning

confidence: 99%

Galaxies infalling into groups: filaments versus isotropic infall

Martínez

Muriel

Coenda

2015

Mon. Not. R. Astron. Soc.

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We perform a comparative analysis of the properties of galaxies infalling into groups classifying them accordingly to whether they are: falling along filamentary structures; or they are falling isotropically. For this purpose, we identify filamentary structures connecting massive groups of galaxies in the SDSS. We perform a comparative analysis of some properties of galaxies in filaments, in the isotropic infall region, in the field, and in groups. We study the luminosity functions (LF) and the dependence of the specific star formation rate (SSFR) on stellar mass, galaxy type, and projected distance to the groups that define the filaments. We find that the LF of galaxies in filaments and in the isotropic infalling region are basically indistinguishable between them, with the possible exception of late-type galaxies. On the other hard, regardless of galaxy type, their LFs are clearly different from that of field or group galaxies. Both of them have characteristic absolute magnitudes and faint end slopes in between the field and group values. More significant differences between galaxies in filaments and in the isotropic infall region are observed when we analyse the SSFR. We find that galaxies in filaments have a systematically higher fraction of galaxies with low SSFR as a function of both, stellar mass and distance to the groups, indicating a stronger quenching of the star formation in the filaments compared to both, the isotropic infalling region, and the field. Our results suggest that some physical mechanisms that determine the differences observed between field galaxies and galaxies in systems, affect galaxies even when they are not yet within the systems.

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STUDYING INTERCLUSTER GALAXY FILAMENTS THROUGH STACKING gmBCG GALAXY CLUSTER PAIRS

Cited by 27 publications

References 68 publications

Towards the statistical detection of the warm–hot intergalactic medium in intercluster filaments of the cosmic web

Towards the statistical detection of the warm–hot intergalactic medium in intercluster filaments of the cosmic web

Gas and galaxies in filaments between clusters of galaxies

Galaxies infalling into groups: filaments versus isotropic infall

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