Cosmic voids in Sloan Digital Sky Survey Data Release 7

Pan, Danny; Vogeley, Michael S.; Hoyle, F.; Choi, Yun‐Young; Park, Changbom

doi:10.1111/j.1365-2966.2011.20197.x

Cited by 221 publications

(333 citation statements)

References 101 publications

Supporting

Mentioning

316

Contrasting

Order By: Relevance

“…We therefore turned to other samples, for example, to the catalogue of Pan et al (2012) 1054 statistically significant voids it contains are larger than 10 h −1 Mpc in radius and, with redshifts lower than 0.1, they are much closer to us than the structures of GR08. Direct stacking gives only a weak signal at about the 1σ level, which is difficult to reconcile with the previous results.…”

Section: Discussion and Alternative Cataloguesmentioning

confidence: 99%

“…This may be due to the inclusion of a large number of small voids that may dilute the signal. Moreover, unlike the voids of GR08, the voids of Pan et al (2012) have a large scatter in angular sizes on the sky, from about 2 • to 20 • (e.g., Ilić et al 2013). To try to enhance the signal, we repeated the stacking after rescaling the voids to their effective sizes.…”

Section: Discussion and Alternative Cataloguesmentioning

confidence: 99%

“…We concentrated here on using the supervoid catalogue by Granett et al (2008b) because it can be compared with two other, more recent catalogues of voids. The second catalogue of cosmic voids that we considered here was published by Pan et al (2012) 4 . It has been built from the seventh data release (DR7) of the SDSS.…”

Section: Main Photometric Sdss Galaxy Samplementioning

confidence: 99%

See 2 more Smart Citations

Planck2013 results. XIX. The integrated Sachs-Wolfe effect

Ade¹,

Aghanim²,

Armitage-Caplan³

et al. 2014

A&A

135

View full text Add to dashboard Cite

Based on cosmic microwave background (CMB) maps from the 2013 Planck Mission data release, this paper presents the detection of the integrated Sachs-Wolfe (ISW) effect, that is, the correlation between the CMB and large-scale evolving gravitational potentials. The significance of detection ranges from 2 to 4σ, depending on which method is used. We investigated three separate approaches, which essentially cover all previous studies, and also break new ground. (i) We correlated the CMB with the Planck reconstructed gravitational lensing potential (for the first time). This detection was made using the lensing-induced bispectrum between the low-and high-temperature anisotropies; the correlation between lensing and the ISW effect has a significance close to 2.5σ. (ii) We cross-correlated with tracers of large-scale structure, which yielded a significance of about 3σ, based on a combination of radio (NVSS) and optical (SDSS) data. (iii) We used aperture photometry on stacked CMB fields at the locations of known large-scale structures, which yielded and confirms a 4σ signal, over a broader spectral range, when using a previously explored catalogue, but shows strong discrepancies in amplitude and scale when compared with expectations. More recent catalogues give more moderate results that range from negligible to 2.5σ at most, but have a more consistent scale and amplitude, the latter being still slightly higher than what is expected from numerical simulations within ΛCMD. Where they can be compared, these measurements are compatible with previous work using data from WMAP, where these scales have been mapped to the limits of cosmic variance. Planck's broader frequency coverage allows for better foreground cleaning and confirms that the signal is achromatic, which makes it preferable for ISW detection. As a final step we used tracers of large-scale structure to filter the CMB data, from which we present maps of the ISW temperature perturbation. These results provide complementary and independent evidence for the existence of a dark energy component that governs the currently accelerated expansion of the Universe.

show abstract

Section: Discussion and Alternative Cataloguesmentioning

confidence: 99%

Section: Discussion and Alternative Cataloguesmentioning

confidence: 99%

Section: Main Photometric Sdss Galaxy Samplementioning

confidence: 99%

See 1 more Smart Citation

Planck2013 results. XIX. The integrated Sachs-Wolfe effect

Ade¹,

Aghanim²,

Armitage-Caplan³

et al. 2014

A&A

135

View full text Add to dashboard Cite

show abstract

“…Nowadays, there is a general consensus in that voids occupy most of the volume of the Universe (Sheth & van de Weygaert 2004;van de Weygaert & Platen 2011;Pan et al 2012) and that they are far from being simple structures. As shown by nu-⋆ E-mail: elena.ricciardelli@uv.es merical simulations (van de Weygaert & van Kampen 1993;Sheth & van de Weygaert 2004;Aragon-Calvo & Szalay 2013;Ricciardelli, Quilis, & Planelles 2013), voids host a rich infrastructure, made of subvoids, sheet-like structures and tenuous filaments.…”

Section: Introductionmentioning

confidence: 99%

The star formation activity in cosmic voids

Ricciardelli¹,

Cava²,

Varela³

et al. 2014

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Using a sample of cosmic voids identified in the Sloan Digital Sky Survey Data Release 7, we study the star formation activity of void galaxies. The properties of galaxies living in voids are compared with those of galaxies living in the void shells and with a control sample, representing the general galaxy population. Void galaxies appear to form stars more efficiently than shell galaxies and the control sample. This result can not be interpreted as a consequence of the bias towards low masses in underdense regions, as void galaxy subsamples with the same mass distribution as the control sample also show statistically different specific star formation rates. This highlights the fact that galaxy evolution in voids is slower with respect to the evolution of the general population. Nevertheless, when only the star forming galaxies are considered, we find that the star formation rate is insensitive to the environment, as the main sequence is remarkably constant in the three samples under consideration. This fact implies that environmental effects manifest themselves as fast quenching mechanisms, while leaving the non-quenched galaxies almost unaffected, as their star formation activity is largely regulated by the mass of their halo. We also analyse galaxy properties as a function of void-centric distance and find that the enhancement in the star formation activity with respect to the control sample is observable up to a radial distance 1.5 · R void . This result can be used as a suitable definition of void shells. Finally, we find that larger voids show an enhanced star formation activity in the shells with respect to their smaller counterparts, that could be related to the different dynamical evolution experienced by voids of different sizes.

show abstract

“…The modern catalogues of voids (Pan et al 2012;Sutter et al 2012;Nadathur & Hotchkiss 2014;Mao et al 2016), which have been created on the basis of the Sloan Digital Sky Survey (SDSS) data releases, contain the main data for about ten thousand of voids with radii spanning the range ∼ 10 − 150 Mpc located at redshifts up to z ∼ 0.7. The various aspects of their formation and distribution of sizes and amplitudes have been developed by Sheth & van de Weygaert (2004) in the context of hierarchical scenarios of the large-scale structure formation.…”

Section: Introductionmentioning

confidence: 99%

Evolution of density and velocity profiles of dark matter and dark energy in spherical voids

Novosyadlyj¹,

Tsizh²,

Kulinich³

2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

We analyse the evolution of cosmological perturbations which leads to the formation of large isolated voids in the Universe. We assume that initial perturbations are spherical and all components of the Universe (radiation, matter and dark energy) are continuous media with perfect fluid energy-momentum tensors, which interact only gravitationally. Equations of the evolution of perturbations for every component in the comoving to cosmological background reference frame are obtained from equations of energy and momentum conservation and Einstein's ones and are integrated numerically. Initial conditions are set at the early stage of evolution in the radiation-dominated epoch, when the scale of perturbation is much larger than the particle horizon. Results show how the profiles of density and velocity of matter and dark energy are formed and how they depend on parameters of dark energy and initial conditions. In particular, it is shown that final matter density and velocity amplitudes change within range ∼4-7% when the value of equation-of-state parameter of dark energy w vary in the range from -0.8 to -1.2, and change within ∼1% only when the value of effective sound speed of dark energy vary over all allowable range of its values.

show abstract

Cosmic voids in Sloan Digital Sky Survey Data Release 7

Cited by 221 publications

References 101 publications

Planck2013 results. XIX. The integrated Sachs-Wolfe effect

Planck2013 results. XIX. The integrated Sachs-Wolfe effect

The star formation activity in cosmic voids

Evolution of density and velocity profiles of dark matter and dark energy in spherical voids

Contact Info

Product

Resources

About