The Void Galaxy Survey

Weygaert, Rien van de; Kreckel, Kathryn; Platen, Erwin; Beygu, B.; Gorkom, J. H. van; Hulst, J. M. van der; Aragón-Calvo, M. A.; Peebles, P. J. E.; Jarrett, T. H.; Rhee, G.; Kovač, K.; Yip, Ching-Wa

doi:10.1007/978-3-642-20285-8_3

Cited by 16 publications

(7 citation statements)

References 36 publications

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“…Statistically, it has been found that galaxies embedded in cosmic voids are bluer (Grogin & Geller 1999;Rojas et al 2004), and tend to have later morphological type (Grogin & Geller 1999;Rojas et al 2004). From observations, it seems that these void galaxies also have stellar disks with smaller radii compared to a control sample of late-type galaxies (van de Weygaert et al 2011). Using galaxy samples from SDSS, Rojas et al (2005) compare the equivalent width (Hα, [OII], [NII], Hβ, [OIII]) of galaxies located in voids or walls.…”

Section: Introductionmentioning

confidence: 99%

Properties of simulated galaxies and supermassive black holes in cosmic voids

Habouzit

Pisani

Goulding

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Cosmic voids, the under-dense regions of the cosmic web, are widely used to constrain cosmology. Voids contain few, isolated galaxies, presumably expected to be less evolved and preserving memory of the pristine Universe. We use the cosmological hydrodynamical simulation Horizon-AGN coupled to the void finder VIDE to investigate properties of galaxies in voids at z = 0. We find that, closer to void centers, low-mass galaxies are more common than their massive counterparts. At fixed dark matter halo mass, they have smaller stellar masses than in denser regions. The star formation rate of void galaxies diminishes when approaching void centers, but their sSFR slightly increases, suggesting that void galaxies form stars more efficiently with respect to their stellar mass. We find that this can not only be attributed to the prevalence of low-mass galaxies. The inner region of voids also predominantly host low-mass BHs. However, the BH mass to galaxy mass ratios resemble those of the whole simulation at z = 0. Our results suggest that even if the growth channels in cosmic voids are different than in denser environments, voids grow their galaxies and BHs in a similar way. While a large fraction of the BHs have low Eddington ratios, we find that ∼ 20% could be observed as AGN with log 10 L 2−10 keV = 41.5 − 42.5 erg/s. These results pave the way to future work with larger next-generation hydro simulations, aiming to confirm our findings and prepare the application on data from upcoming large surveys such as PFS, Euclid and WFIRST.

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Section: Introductionmentioning

confidence: 99%

Properties of simulated galaxies and supermassive black holes in cosmic voids

Habouzit

Pisani

Goulding

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…The underdense environment in voids can be used as a laboratory to study the environmental dependence of galaxy evolution (e.g. [25][26][27]) and they are also particularly sensitive to warm dark matter and neutrinos [28][29][30][31]. While most of the matter of the Universe ends up in collapsed objects at late times, voids account for the majority of the late-time volume of the universe.…”

Section: Introductionmentioning

confidence: 99%

Separate universe void bias

Jamieson¹,

Loverde²

2019

Phys. Rev. D

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Voids have emerged as a novel probe of cosmology and large-scale structure. These regions of extreme underdensity are sensitive to physics beyond the standard model of cosmology, and can potentially be used as a testing ground to constrain new physics. We present the first determination of the linear void bias measured in separate universe simulations. Our methods are validated by comparing the separate universe response bias with the clustering bias of voids. We find excellent agreement between the two methods for voids identified in the halo field and the down-sampled dark matter field. For voids traced by halos, we identify two different contributions to the bias. The first is due to the bias of the underlying halo field used to identify voids, while the second we attribute to the dynamical impact of long-wavelength density perturbations on void formation and expansion. By measuring these contributions individually, we demonstrate that their sum is consistent with the total void bias. We also measure the void profiles in our simulations, and determine their separate universe response. These can be interpreted as the sensitivity of the profiles to the background density of the Universe.

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“…Another issue of interest is whether we can observe the intricate filigree of substructure in voids, expected as the remaining debris of the merging of voids and filaments in the hierarchical formation process (van de Weygaert & van Kampen 1993;Sheth & van de Weygaert 2004;van de Weygaert & Platen 2011;Aragon-Calvo 2012). Evidence for such substructure, three interacting galaxies embedded in a common HI envelope, has been reported by Beygu et al (2013), who hypothesised it to be an assembly of a filament in a void.…”

Section: Introductionmentioning

confidence: 99%

The void galaxy survey: photometry, structure and identity of void galaxies

Beygu

Peletier

Hulst

et al. 2016

Mon. Not. R. Astron. Soc.

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We analyze photometry from deep B-band images of 59 void galaxies in the Void Galaxy Survey (VGS), together with their near-infrared 3.6µm and 4.5µm Spitzer photometry. The VGS galaxies constitute a sample of void galaxies that were selected by a geometric-topological procedure from the SDSS DR7 data release, and which populate the deep interior of voids. Our void galaxies span a range of absolute Bmagnitude from M B = −15.5 to M B = −20, while at the 3.6µm band their magnitudes range from M 3.6 = −18 to M 3.6 = −24. Their B-[3.6] colour and structural parameters indicate these are star forming galaxies. A good reflection of the old stellar population, the near-infrared band photometry also provide a robust estimate of the stellar mass, which for the VGS galaxies we confirm to be smaller than 3 × 10 10 M . In terms of the structural parameters and morphology, our findings align with other studies in that our VGS galaxy sample consists mostly of small late-type galaxies. Most of them are similar to Sd-Sm galaxies, although a few are irregularly shaped galaxies. The sample even includes two early-type galaxies, one of which is an AGN. Their Sérsic indices are nearly all smaller than n = 2 in both bands and they also have small half-light radii. In all, we conclude that the principal impact of the void environment on the galaxies populating them mostly concerns their low stellar mass and small size.

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The Void Galaxy Survey

Cited by 16 publications

References 36 publications

Properties of simulated galaxies and supermassive black holes in cosmic voids

Properties of simulated galaxies and supermassive black holes in cosmic voids

Separate universe void bias

The void galaxy survey: photometry, structure and identity of void galaxies

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