Dependence of GAMA galaxy halo masses on the cosmic web environment from 100 deg<sup>2</sup>of KiDS weak lensing data

Brouwer, Margot M.; Cacciato, Marcello; Dvornik, Andrej; Eardley, Lizzie; Heymans, Catherine; Hoekstra, Henk; Kuijken, Konrad; McNaught-Roberts, Tamsyn; Sifón, Cristobál; Viola, Massimo; Alpaslan, Mehmet; Bilicki, Maciej; Bland-Hawthorn, Joss; Brough, Sarah; Choi, A.; Driver, Simon P.; Erben, T.; Grado, A.; Hildebrandt, Hendrik; Holwerda, Benne W.; Hopkins, A. M.; Jong, J. T. A. de; Liske, J.; McFarland, John; Nakajima, Reiko; Napolitano, N. R.; Norberg, Peder; Peacock, J. A.; Radovich, M.; Robotham, Aaron S. G.; Schneider, Peter; Sikkema, Gert; Uitert, Edo van; Kleijn, Gijs Verdoes; Valentijn, E. A.

doi:10.1093/mnras/stw1602

Cited by 34 publications

(19 citation statements)

References 69 publications

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“…Nonetheless, a similar implementation, the DISPERSE code of Sousbie (2011), has been used by Duckworth et al (2019) to connect MaNGA galaxy kinematics to assembly history. An implementation of the deformation tensor method we used was also recently used on a sample of ∼ 10 5 galaxies from the GAMA survey (Eardley et al 2015;Brouwer et al 2016). This analysis lead to the conclusion that the galaxy mass function does not depend on the deformation tensor, but only on the large-scale overdensity.…”

Section: Discussionmentioning

confidence: 99%

Baryons in the Cosmic Web of IllustrisTNG – II. The connection among galaxies, haloes, their formation time, and their location in the Cosmic Web

Martizzi

Vogelsberger

Torrey

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The connections among galaxies, the dark matter halos where they form and the properties of the large-scale Cosmic Web still need to be completely disentangled. We use the cosmological hydrodynamical simulation TNG100 of the IllustrisTNG suite to quantify the effects played by the large-scale density field and the Cosmic Web morphology on the relation between halo mass and galaxy stellar mass. We select objects with total dynamical mass in the range 6.3 × 10 10 h −1 M up to a few 10 14 h −1 M between redshift z = 4 and redshift z = 0. A Cosmic Web class (knot, filament, sheet, void) is assigned to each region of the volume using a density field deformation tensor-based method. We find that galaxy stellar mass strongly correlates with total dynamical mass and formation time, and more weakly with large-scale overdensity and Cosmic Web class. The latter two quantities correlate with each other, but are not entirely degenerate. Furthermore, we find that at fixed halo mass, galaxies with stellar mass lower than the median value are more likely to be found in voids and sheets, whereas galaxies with stellar mass higher than the median are more likely to be found in filaments and knots. The effect is stronger at redshift z 1, but it decreases at higher redshift. We predict that this effect should already be measurable from available galaxy surveys. Finally, we find that the dependence on environment is stronger for satellites than for centrals, and discuss the physical implications of these results.

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Section: Discussionmentioning

confidence: 99%

Baryons in the Cosmic Web of IllustrisTNG – II. The connection among galaxies, haloes, their formation time, and their location in the Cosmic Web

Martizzi

Vogelsberger

Torrey

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…For example, the "galactic conformity"-the observation that satellites are more likely to be quenched around quiescent centrals than star-forming (SF) ones-has been found on both small and larger megaparsec scales (Weinmann et al 2006;Kauffmann et al 2013;Hartley et al 2015;Hearin et al 2015;Berti et al 2017;Hatfield & Jarvis 2016;Kawinwanichakij et al 2016), suggesting the role of the large-scale gravitational tidal field on galaxy properties. Moreover, several observations have found that the star formation activity and other galaxy properties depend on the large-scale cosmic web (Fadda et al 2008;Porter et al 2008;Biviano et al 2011;Darvish et al 2014;Ricciardelli et al 2014;Chen et al 2016b;Darvish et al 2015a;Guo et al 2015;Alpaslan et al 2016;Pandey & Sarkar 2016), whereas others have seen no or at best a weak dependence between the properties of galaxies and the global cosmic web environments (Alpaslan et al 2015;Eardley et al 2015;Filho et al 2015;Penny et al 2015;Alonso et al 2016;Beygu et al 2016;Brouwer et al 2016;Vulcani et al 2016a).…”

Section: For Reviews)mentioning

confidence: 99%

Cosmic Web of Galaxies in the COSMOS Field: Public Catalog and Different Quenching for Centrals and Satellites

Darvish

Mobasher

Martin

et al. 2017

ApJ

105

170

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We use a mass complete (log(  M M )  9.6) sample of galaxies with accurate photometric redshifts in the COSMOS field to construct the density field and the cosmic web to z=1.2. The comic web extraction relies on the density field Hessian matrix and breaks the density field into clusters, filaments, and the field. We provide the density field and cosmic web measures to the community. We show that at z0.8, the median star formation rate (SFR) in the cosmic web gradually declines from the field to clusters and this decline is especially sharp for satellites (∼1 dex versus ∼0.5 dex for centrals). However, at z0.8, the trend flattens out for the overall galaxy population and satellites. For star-forming (SF) galaxies only, the median SFR is constant at z0.5 but declines by ∼0.3-0.4 dex from the field to clusters for satellites and centrals at z0.5. We argue that for satellites, the main role of the cosmic web environment is to control their SF fraction, whereas for centrals, it is mainly to control their overall SFR at z0.5 and to set their fraction at z0.5. We suggest that most satellites experience a rapid quenching mechanism as they fall from the field into clusters through filaments, whereas centrals mostly undergo a slow environmental quenching at z0.5 and a fast mechanism at higher redshifts. Our preliminary results highlight the importance of the large-scale cosmic web on galaxy evolution.

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“…The first two data releases from KiDS (de Jong et al 2015) became public in 2013 and 2015, containing reduced image data, source lists and a multi-band catalogue for a total of 148 survey tiles ( 160 deg 2 ). Based on this data set, the first scientific results focused on weak lensing studies of galaxies and galaxy A134, page 2 of 26 groups in the Galaxy And Mass Assembly (GAMA, Driver et al 2011) fields (Kuijken et al 2015;Sifón et al 2015;Viola et al 2015;Brouwer et al 2016;van Uitert et al 2016). Furthermore, these data releases were the basis for the first results from a z ∼ 6 quasar search (Venemans et al 2015), a catalogue of photometric redshifts from machine-learning (Cavuoti et al 2015(Cavuoti et al , 2017, preliminary results on super-compact massive galaxies (Tortora et al 2016), and a catalogue of galaxy clusters (Radovich et al 2017).…”

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confidence: 99%

The third data release of the Kilo-Degree Survey and associated data products

Jong

Kleijn

Erben³

et al. 2017

A&A

Self Cite

186

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Context. The Kilo-Degree Survey (KiDS) is an ongoing optical wide-field imaging survey with the OmegaCAM camera at the VLT Survey Telescope. It aims to image 1500 square degrees in four filters (ugri). The core science driver is mapping the large-scale matter distribution in the Universe, using weak lensing shear and photometric redshift measurements. Further science cases include galaxy evolution, Milky Way structure, detection of high-redshift clusters, and finding rare sources such as strong lenses and quasars. Aims. Here we present the third public data release and several associated data products, adding further area, homogenized photometric calibration, photometric redshifts and weak lensing shear measurements to the first two releases. Methods. A dedicated pipeline embedded in the Astro-WISE information system is used for the production of the main release. Modifications with respect to earlier releases are described in detail. Photometric redshifts have been derived using both Bayesian template fitting, and machine-learning techniques. For the weak lensing measurements, optimized procedures based on the THELI data reduction and lensfit shear measurement packages are used. Results. In this third data release an additional 292 new survey tiles (≈300 deg 2 ) stacked ugri images are made available, accompanied by weight maps, masks, and source lists. The multi-band catalogue, including homogenized photometry and photometric redshifts, covers the combined DR1, DR2 and DR3 footprint of 440 survey tiles (44 deg 2 ). Limiting magnitudes are typically 24.3, 25.1, 24.9, 23.8 (5σ in a 2 aperture) in ugri, respectively, and the typical r-band PSF size is less than 0.7 . The photometric homogenization scheme ensures accurate colours and an absolute calibration stable to ≈2% for gri and ≈3% in u. Separately released for the combined area of all KiDS releases to date are a weak lensing shear catalogue and photometric redshifts based on two different machine-learning techniques.

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Dependence of GAMA galaxy halo masses on the cosmic web environment from 100 deg²of KiDS weak lensing data

Cited by 34 publications

References 69 publications

Baryons in the Cosmic Web of IllustrisTNG – II. The connection among galaxies, haloes, their formation time, and their location in the Cosmic Web

Baryons in the Cosmic Web of IllustrisTNG – II. The connection among galaxies, haloes, their formation time, and their location in the Cosmic Web

Cosmic Web of Galaxies in the COSMOS Field: Public Catalog and Different Quenching for Centrals and Satellites

The third data release of the Kilo-Degree Survey and associated data products

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Dependence of GAMA galaxy halo masses on the cosmic web environment from 100 deg2of KiDS weak lensing data

Cited by 34 publications

References 69 publications

Baryons in the Cosmic Web of IllustrisTNG – II. The connection among galaxies, haloes, their formation time, and their location in the Cosmic Web

Baryons in the Cosmic Web of IllustrisTNG – II. The connection among galaxies, haloes, their formation time, and their location in the Cosmic Web

Cosmic Web of Galaxies in the COSMOS Field: Public Catalog and Different Quenching for Centrals and Satellites

The third data release of the Kilo-Degree Survey and associated data products

Contact Info

Product

Resources

About

Dependence of GAMA galaxy halo masses on the cosmic web environment from 100 deg²of KiDS weak lensing data