A Map of the Universe

Gott, J. Richard; Jurić, Mario; Schlegel, David J.; Hoyle, F.; Vogeley, Michael S.; Tegmark, Max; Bahcall, Neta A.; Brinkmann, J.

doi:10.1086/428890

Cited by 317 publications

(75 citation statements)

References 65 publications

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“…Observed luminous matter large-scale structures, most notably the >400 Mpc Sloan Great Wall (Gott et al 2005), demonstrate the existence of structure on larger scales than simulations predict (assuming luminous matter traces dark matter). It has also been shown that voids on scales similar to that of the Sloan Great Wall may explain the "cold spots" in the cosmic microwave background (Inoue & Silk 2006).…”

Section: Introductionmentioning

confidence: 75%

Testing for a Large Local Void by Investigating the Near-Infrared Galaxy Luminosity Function

Keenan

Barger

Cowie

et al. 2012

ApJ

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Recent cosmological modeling efforts have shown that a local underdensity on scales of a few hundred Mpc (out to z ∼ 0.1) could produce the apparent acceleration of the expansion of the universe observed via Type Ia supernovae. Several studies of galaxy counts in the near-infrared (NIR) have found that the local universe appears underdense by ∼25%-50% compared with regions a few hundred Mpc distant. Galaxy counts at low redshifts sample primarily L ∼ L * galaxies. Thus, if the local universe is underdense, then the normalization of the NIR galaxy luminosity function (LF) at z > 0.1 should be higher than that measured for z < 0.1. Here we present a highly complete (>90%) spectroscopic sample of 1436 galaxies selected in the H band (1.6 μm) to study the normalization of the NIR LF at 0.1 < z < 0.3 and address the question of whether or not we reside in a large local underdensity. Our survey sample consists of all galaxies brighter than 18th magnitude in the H band drawn from six widely separated fields at high Galactic latitudes, which cover a total of ∼2 deg 2 on the sky. We find that for the combination of our six fields, the product φ * L * at 0.1 < z < 0.3 is ∼30% higher than that measured at lower redshifts. While our statistical errors in this measurement are on the ∼10% level, we find the systematics due to cosmic variance may be larger still. We investigate the effects of cosmic variance on our measurement using the COSMOS cone mock catalogs from the Millennium Simulation and recent empirical estimates of cosmic variance. We find that our survey is subject to systematic uncertainties due to cosmic variance at the 15% level (1σ ), representing an improvement by a factor of ∼2 over previous studies in this redshift range. We conclude that observations cannot yet rule out the possibility that the local universe is underdense at z < 0.1. The fields studied in this work have a large amount of publicly available ancillary data and we make available the images and catalogs used here.

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Section: Introductionmentioning

confidence: 75%

Testing for a Large Local Void by Investigating the Near-Infrared Galaxy Luminosity Function

Keenan

Barger

Cowie

et al. 2012

ApJ

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“…The low-redshift limit of z 0.04 ensures that the sample is within the Hubble flow, and excludes the Coma and Virgo clusters. Since the SDSS "great wall" spans a redshift range of 0.065 z 0.09 (Gott et al 2005), it is fully contained within the low-redshift range. This allows us to isolate the effect of the "great wall" by comparing the low-redshift range to the high-redshift range.…”

Section: Catalog Datamentioning

confidence: 99%

The Galaxy Counts-in-Cells Distribution From the Sloan Digital Sky Survey

Yang

Saslaw

2011

ApJ

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We determine the galaxy counts-in-cells distribution from the Sloan Digital Sky Survey (SDSS) for threedimensional spherical cells in redshift space as well as for two-dimensional projected cells. We find that cosmic variance in the SDSS causes the counts-in-cells distributions in different quadrants to differ from each other by up to 20%. We also find that within this cosmic variance, the overall galaxy counts-in-cells distribution agrees with both the gravitational quasi-equilibrium distribution and the negative binomial distribution. We also find that brighter galaxies are more strongly clustered than if they were randomly selected from a larger complete sample that includes galaxies of all luminosities. The results suggest that bright galaxies could be in dark matter halos separated by less than ∼10 h −1 Mpc.

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“…Our numbers may not be precise, but they show the chronological orders and basic parameters of the various important landmarks of the cosmic history. A conformal map of the universe depicting the recent discoveries up to the beginning of this 21th century can be found in [242], which is largely for experts.…”

Section: A Cheat Sheet Of the Cosmo-history And A Map Of The Universementioning

confidence: 99%

“…The criterion for the existence of an event horizon is quite straightforward. From 242) The cosmic event horizon should not be confused with the black hole event horizon, although the two have some similarities. There is also an overall event horizon beyond which no light signal will be able to reach an observer.…”

Section: )mentioning

confidence: 99%

A survey of dark matter and related topics in cosmology

Young

2016

Front. Phys.

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A Map of the Universe

Cited by 317 publications

References 65 publications

Testing for a Large Local Void by Investigating the Near-Infrared Galaxy Luminosity Function

Testing for a Large Local Void by Investigating the Near-Infrared Galaxy Luminosity Function

The Galaxy Counts-in-Cells Distribution From the Sloan Digital Sky Survey

A survey of dark matter and related topics in cosmology

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