Warmth elevating the depths: shallower voids with warm dark matter

Yang, Lin F.; Neyrinck, Mark C.; Aragón-Calvo, M. A.; Falck, Bridget; Silk, Joseph

doi:10.1093/mnras/stv1087

Cited by 50 publications

(49 citation statements)

References 52 publications

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“…In addition to constraining standard cosmological parameters, voids have been used to investigate alternative dark matter scenarios like warm dark matter (Yang et al 2015), or the effects of neutrinos on void lensing (Massara et al 2015). Especially numerous are the studies on void abundance (Li 2011;Clampitt, Cai & Li 2013;Cai et al 2015;Lam et al 2015;Zivick et al 2015;Pollina et al 2016) and lensing (Cai et al 2014;Barreira et al 2015) as promising probes of alternatives to general relativity (GR).…”

Section: Discussionmentioning

confidence: 99%

Cosmic voids and void lensing in the Dark Energy Survey Science Verification data

Sánchez

Clampitt

Kovács

et al. 2016

Mon. Not. R. Astron. Soc.

111

121

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Cosmic voids are usually identified in spectroscopic galaxy surveys, where 3D information about the large-scale structure of the Universe is available. Although an increasing amount of photometric data is being produced, its potential for void studies is limited since photometric redshifts induce line-of-sight position errors of ≥50 Mpc h −1 which can render many voids undetectable. We present a new void finder designed for photometric surveys, validate it using simulations, and apply it to the high-quality photo-z redMaGiC galaxy sample of the DES Science Verification data. The algorithm works by projecting galaxies into 2D slices and finding voids in the smoothed 2D galaxy density field of the slice. Fixing the line-of-sight size of the slices to be at least twice the photo-z scatter, the number of voids found in simulated spectroscopic and photometric galaxy catalogues is within 20 per cent for all transverse void sizes, and indistinguishable for the largest voids (R v ≥ 70 Mpc h −1 ). The positions, radii, and projected galaxy profiles of photometric voids also accurately match the spectroscopic void sample. Applying the algorithm to the DES-SV data in the redshift range 0.2 < z < 0.8, we identify 87 voids with comoving radii spanning the range 18-120 Mpc h −1 , and carry out a stacked weak lensing measurement. With a significance of 4.4σ , the lensing measurement confirms that the voids are truly underdense in the matter field and hence not a product of

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Section: Discussionmentioning

confidence: 99%

Cosmic voids and void lensing in the Dark Energy Survey Science Verification data

Sánchez

Clampitt

Kovács

et al. 2016

Mon. Not. R. Astron. Soc.

111

121

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“…Ceccarelli et al 2013). Voids in WDM cosmology have been investigated in the recent works of Reed et al (2015) who studied galaxy clustering and void volume fraction, and Yang et al (2015), who measured the statistics and density profiles of voids in CDM cosmology and three WDM cosmologies with mx = 1.4, 0.8 and 0.4kev. For our purposes, we define voids in our z=0 galaxy catalogue as under-dense spheres of a fixed radius 10 −1 hMpc; we choose this value because it is a typical scale of voids probed by galaxy redshift surveys (Ceccarelli et al 2013).…”

Section: Galaxy Population In Voidsmentioning

confidence: 99%

The galaxy population in cold and warm dark matter cosmologies

Wang

González-Pérez²,

Xie

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We use a pair of high resolution N-body simulations implementing two dark matter models, namely the standard cold dark matter (CDM) cosmogony and a warm dark matter (WDM) alternative where the dark matter particle is a 1.5 keV thermal relic. We combine these simulations with the GALFORM semi-analytical galaxy formation model in order to explore differences between the resulting galaxy populations. We use GALFORM model variants for CDM and WDM that result in the same z = 0 galaxy stellar mass function by construction. We find that most of the studied galaxy properties have the same values in these two models, indicating that both dark matter scenarios match current observational data equally well. Even in under-dense regions, where discrepancies in structure formation between CDM and WDM are expected to be most pronounced, the galaxy properties are only slightly different. The only significant difference in the local universe we find is in the galaxy populations of "Local Volumes", regions of radius 1 to 8Mpc around simulated Milky Way analogues. In such regions our WDM model provides a better match to observed local galaxy number counts and is five times more likely than the CDM model to predict subregions within them that are as empty as the observed Local Void. Thus, a highly complete census of the Local Volume and future surveys of void regions could provide constraints on the nature of dark matter.

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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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Warmth elevating the depths: shallower voids with warm dark matter

Cited by 50 publications

References 52 publications

Cosmic voids and void lensing in the Dark Energy Survey Science Verification data

Cosmic voids and void lensing in the Dark Energy Survey Science Verification data

The galaxy population in cold and warm dark matter cosmologies

Separate universe void bias

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