Cosmic Voids: Structure, Dynamics and Galaxies

Weygaert, Rien van de; Platen, Erwin

doi:10.1142/s2010194511000092

Cited by 99 publications

(89 citation statements)

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“…Galaxies in low-redshift voids generally have smaller stellar masses, appear bluer, have a later morphological type, and have higher specific star formation rates than galaxies in average density environments (van de Weygaert & Platen 2011;Beygu et al 2015), although the latter properties might be solely due to their lower stellar mass (Hoyle et al 2005;Kreckel, Joung & Cen 2011). Extending similar studies to higher redshifts to see whether similar trends hold is a pressing observational challenge.…”

Section: Introductionmentioning

confidence: 99%

Finding high-redshift voids using Lyman α forest tomography

Stark

Font-Ribera

White

et al. 2015

Mon. Not. R. Astron. Soc.

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We present a new method of finding cosmic voids using tomographic maps of Lyα forest flux. We identify cosmological voids with radii of 2 -12 h −1 Mpc in a large N-body simulation at z = 2.5, and characterize the signal of the high-redshift voids in density and Lyα forest flux. The void properties are similar to what has been found at lower redshifts, but they are smaller and have steeper radial density profiles. Similarly to what has been found for low-redshift voids, the radial velocity profiles have little scatter and agree very well with the linear theory prediction. We run the same void finder on an ideal Lyα flux field and tomographic reconstructions at various spatial samplings. We compare the tomographic map void catalogs to the density void catalog and find good agreement even with modest-sized voids (r > 6 h −1 Mpc). Using our simple void-finding method, the configuration of the ongoing CLAMATO survey covering 1 deg 2 would provide a sample of about 100 high-redshift voids. We also provide void-finding forecasts for larger area surveys, and discuss how these void samples can be used to test modified gravity models, study high-redshift void galaxies, and to make an Alcock-Paczynski measurement. To aid future work in this area, we provide public access to our simulation products, catalogs, and sample tomographic flux maps.

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Section: Introductionmentioning

confidence: 99%

Finding high-redshift voids using Lyman α forest tomography

Stark

Font-Ribera

White

et al. 2015

Mon. Not. R. Astron. Soc.

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“…Shaded areas correspond to 68% uncertainty intervals. Figure from Ilbert et al (2013). al., 2015; Kodama and Bower, 2003;Vulcani et al, 2012;van der Burg et al, 2013). For example, Bolzonella et al (2010) studied the GSMF in different environments in the COSMOS field (using the zCOSMOS survey, see Lilly et al, 2007Lilly et al, , 2009) up to z = 1, finding a difference between the GSMF of high-and low-density environments, with the massive end of the GSMF being more enhanced in high-density environments (see Figure 7).…”

Section: The Galaxy Stellar Mass Function In Different Environmentsmentioning

confidence: 99%

“…In particular, galaxy groups and clusters have been extensively investigated, both with dedicated observations (see e. g. Gavazzi, 2006, 2014, for review) and by applying structure-finding algorithms to galaxy surveys (see Castignani et al, 2014a;Cucciati et al, 2010, for a review of methods for finding galaxy clusters). Together with voids (see Colberg et al 2008 for a review on void-finding algorithms, Beygu et al 2016;van de Weygaert and Platen 2011, and references therein for results on the study of properties of galaxies in voids), galaxy clusters have been by far the most-studied LSS features and have been recently detected also at very high redshift (see e. g. Toshikawa et al, 2016).…”

Section: Global Environmentmentioning

confidence: 99%

“…This result has been confirmed also by Davidzon et al (2016), by means of the VIPERS survey (Garilli et al, 2014;Guzzo et al, 2014). On the other hand, Vulcani et al (2012) find no difference for the GSMF of galaxies in clusters and in the field, while van der Burg et al (2013) reports a general difference in the GSMF for galaxies in clusters and in the field but the same shape for the GSMF of quiescent and star-forming galaxies in each environment. Although these differences could be due to the fact that both these works study a GSMF derived from a compilation of clusters and not from a single system, still the problem of determining whether local environment has an impact on the shape of the GSMF remains open.…”

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confidence: 97%

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The Role of the Environment on Galaxy Evolution

Boselli

2011

A Panchromatic View of Galaxies

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Esame finale anno 2016A Milena "Che fai tu, Luna, in ciel? Dimmi, che fai, silenziosa Luna?" -Giacomo Leopardi, Canto notturno di un pastore errante dell'Asia A B S T R A C TAlthough the general picture of how galaxies have formed and evolved through cosmic time is already in place, still many details are missing. An example is represented by a quantitative characterization of the role that environment plays during the evolution of galaxies in determining their observed properties in the local Universe. Local galaxy environment has been thoroughly explored through observations at low redshift and it has recently started to being investigated also in the distant Universe. Moreover, general attention has been increasingly focused on the relation between galaxy evolution and galaxy positions with respect to the large-scale structures of the cosmic web.This work explores how environment (defined both in terms of local overdensities on the Mpc scale around galaxies, as well as in terms of the distribution of galaxy distances from ∼ 10 2 Mpc long cosmic filaments) is observationally related to galaxy properties such as their stellar mass, their star-formation activity, or the presence of Active Galactic Nucleus phenomena. The analysis reported here is performed in a large redshift range, going from the local Universe (z 0.2) to intermediate (z ∼ 0.7) and high-redshifts (z 3). To perform this study, both spectroscopic redshift data sets as well as photometric redshift surveys have been deployed and (particularly for the photometric redshift data sets) a thorough analysis of the effect of their observational issues on the measurement of local and global environment has been executed.The picture that emerges is that high-density environments are favoured places for galaxy evolution, showing an enhanced fraction of massive galaxies which have stopped forming stars and belong to the quiescent population. Galaxies in high-density environments have an increased probability of hosting radio-AGNs (belonging to the ensemble of processes that turn off the star-formation in massive galaxies) and these effects are visible since the start of the decline in the cosmic star-formation history. Large-scale structures, such as the filaments of the cosmic web, have also a role in shaping galaxy evolution and they may represent key places for the pre-processing of galaxies before they enter higher density regions such as the cluster or group environment.As an increasing amount of observational evidence on the relation between the evolution of galaxies and their environment is gathered, a complete solution to the problem of how the local galaxy population has evolved approaches, and the history of galaxies from their formation at the dawn of time to the present day gets closer to being traced. Figure 2 Growth of structures . . . . . . . . . . . . . . . 7 Figure 3 Evolution of the global SFR density . . . . . . . 8 Figure 4 Colour-density relation for VVDS galaxies . . 11 Figure 5 Fraction of M * contained in galaxies as a function sSFR ....

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“…Voids are enormous regions with sizes in the range of 20 − 50h −1 Mpc that are practically devoid of any galaxy, usually roundish in shape and occupying the major share of space in the Universe [37]. Forming an essential ingredient of the Cosmic Web [4], they are surrounded by elongated filaments, sheetlike walls and dense compact clusters.…”

Section: Introduction: Voids and Void Galaxiesmentioning

confidence: 99%

The Void Galaxy Survey

Weygaert

Kreckel

Platen

et al. 2011

Astrophysics and Space Science Proceedings

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The Void Galaxy Survey (VGS) is a multi-wavelength program to study ∼60 void galaxies. Each has been selected from the deepest interior regions of identified voids in the SDSS redshift survey on the basis of a unique geometric technique, with no a prior selection of intrinsic properties of the void galaxies. The project intends to study in detail the gas content, star formation history and stellar content, as well as kinematics and dynamics of void galaxies and their companions in a broad sample of void environments. It involves the HI imaging of the gas distribution in each of the VGS galaxies. Amongst its most tantalizing findings is the possible evidence for cold gas accretion in some of the most interesting objects, amongst which are a polar ring galaxy and a filamentary configuration of void galaxies. Here we shortly describe the scope of the VGS and the results of the full analysis of the pilot sample of 15 void galaxies.

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Cosmic Voids: Structure, Dynamics and Galaxies

Cited by 99 publications

References 95 publications

Finding high-redshift voids using Lyman α forest tomography

Finding high-redshift voids using Lyman α forest tomography

The Role of the Environment on Galaxy Evolution

The Void Galaxy Survey

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