Three-Point Correlation Functions of SDSS Galaxies: Constraining Galaxy-Mass Bias

McBride, Cameron K.; Connolly, Andrew J.; Gardner, J. P.; Scranton, Ryan; Berlind, Andreas A.; Marín, Felipe; Schneider, Donald P.

doi:10.1088/0004-637x/739/2/85

Cited by 66 publications

(76 citation statements)

References 65 publications

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“…We use the LasDamas 6 N-body simulations (McBride et al 2009(McBride et al , 2011, created with the publicly available code GADGET-II (Springel 2005). In particular we use the suite of realizations called Oriana; the Oriana suite, an ensemble of 40 independent realizations of the dark matter distribution in the Universe, studies the dark matter particles evolution in a box of 2.4 Gpc/h comoving filled with 1280 3 particles.…”

Section: N-body Simulationsmentioning

confidence: 99%

The importance of the cosmic web and halo substructure for power spectra

Pace

Manera

Bacon

et al. 2015

Mon. Not. R. Astron. Soc.

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In this work we study the relevance of the cosmic web and substructures on the matter and lensing power spectra measured from halo mock catalogues extracted from the N-body simulations. Since N-body simulations are computationally expensive, it is common to use faster methods that approximate the dark matter field as a set of halos. In this approximation, we replace mass concentrations in N-body simulations by a spherically symmetric Navarro-FrenkWhite halo density profile. We also consider the full mass field as the sum of two distinct fields: dark matter halos (M > 9 × 10 12 M ⊙ /h) and particles not included into halos. Mock halos reproduce well the matter power spectrum, but underestimate the lensing power spectrum on large and small scales. For sources at z s = 1 the lensing power spectrum is underestimated by up to 40% at ℓ ≈ 10 4 with respect to the simulated halos. The large scale effect can be alleviated by combining the mock catalogue with the dark matter distribution outside the halos. In addition, to evaluate the contribution of substructures we have smeared out the intra-halo substructures in a N-body simulation while keeping the halo density profiles unchanged. For the matter power spectrum the effect of this smoothing is only of the order of 5%, but for lensing substructures are much more important: for ℓ ≈ 10 4 the internal structures contribute 30% of the total spectrum. These findings have important implications in the way mock catalogues have to be created, suggesting that some approximate methods currently used for galaxy surveys will be inadequate for future weak lensing surveys.

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Section: N-body Simulationsmentioning

confidence: 99%

The importance of the cosmic web and halo substructure for power spectra

Pace

Manera

Bacon

et al. 2015

Mon. Not. R. Astron. Soc.

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“…Other examples of cosmological probes are the three-point correlation functions (e.g. McBride et al 2011;Marín et al 2013;Guo et al 2014a) and the power spectrum analysis (Hütsi 2006(Hütsi , 2010Blake et al 2010;Balaguera-Antolínez et al 2011).…”

Section: Introductionmentioning

confidence: 99%

Galaxy filaments as pearl necklaces

Tempel

Kipper

Saar

et al. 2014

A&A

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Context. Galaxies in the Universe form chains (filaments) that connect groups and clusters of galaxies. The filamentary network includes nearly half of the galaxies and is visually the most striking feature in cosmological maps. Aims. We study the distribution of galaxies along the filamentary network, trying to find specific patterns and regularities. Methods. Galaxy filaments are defined by the Bisous model, a marked point process with interactions. We use the two-point correlation function and the Rayleigh Z-squared statistic to study how galaxies and galaxy groups are distributed along the filaments. Results. We show that galaxies and groups are not uniformly distributed along filaments, but tend to form a regular pattern. The characteristic length of the pattern is around 7 h −1 Mpc. A slightly smaller characteristic length 4 h −1 Mpc can also be found, using the Z-squared statistic. Conclusions. We find that galaxy filaments in the Universe are like pearl necklaces, where the pearls are galaxy groups distributed more or less regularly along the filaments. We propose that this well-defined characteristic scale could be used to test various cosmological models and to probe environmental effects on the formation and evolution of galaxies.Key words. methods: numerical -methods: observational -large-scale structure of Universe IntroductionMany cosmological probes have been developed and used to estimate the parameters of the cosmological models describing our Universe. Most of them rely on some aspects of the large-scale structure. The most common probe used to quantify galaxy clustering is the two-point correlation function which was first used decades ago (Davis & Geller 1976;Groth & Peebles 1977;Davis et al. 1988;Hamilton 1988;White et al. 1988;Boerner et al. 1989;Einasto 1991) It is well known that galaxy filaments are visually the most dominant structures in the galaxy distribution, being part of the so-called cosmic network (Jõeveer et al. 1978;Bond et al. 1996). Presumably, nearly half (∼40%) of the galaxies (or mass in simulations) are located in filaments. This number is based on morphological or dynamical classification of the cosmic web (e.g. Jasche et al. 2010;Tempel et al. 2014b;Cautun et al. 2014). Properties of the three-point correlation function also indicate that galaxies tend to populate filamentary structures (Guo et al. 2014a) and, indeed, filaments have been found between galaxy clusters (e.g. Dietrich et al. 2012). Tempel et al. (2014a) show Appendices are available in electronic form at

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“…Other cosmological tests, such as the supernova Hubble diagram, will directly constrain H(a), while correlation functions will be measurable directly from the data set used. The linear clustering bias of host galaxies can be constrained in a number of ways; e.g., by direct comparison of galaxy correlation functions to the matter power spectrum derived from gravitational lensing; with galaxy three-point correlation functions [69] or angular bispectra [70]; or (if a large spectroscopic sample is available) by combining redshift-space distortions [19][20][21] with mean pairwise velocity statistics. Assuming these other quantities will be measured with errors which are small compared to our velocity errors, a measurement of v(r, a) will provide an estimate of d ln D/d ln a in several bins in a, which can then be used to constrain γ.…”

Section: Discussion and Future Prospectsmentioning

confidence: 99%

Galaxy peculiar velocities from large-scale supernova surveys as a dark energy probe

et al. 2011

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Upcoming imaging surveys such as the Large Synoptic Survey Telescope will repeatedly scan large areas of sky and have the potential to yield million-supernova catalogs. Type Ia supernovae are excellent standard candles and will provide distance measures that suffice to detect mean pairwise velocities of their host galaxies. We show that when combining these distance measures with photometric redshifts for either the supernovae or their host galaxies, the mean pairwise velocities of the host galaxies will provide a dark energy probe which is competitive with other widely discussed methods. Adding information from this test to type Ia supernova photometric luminosity distances from the same experiment, plus the cosmic microwave background power spectrum from the Planck satellite, improves the Dark Energy Task Force Figure of Merit by a factor of 1.8. Pairwise velocity measurements require no additional observational effort beyond that required to perform the traditional supernova luminosity distance test, but may provide complementary constraints on dark energy parameters and the nature of gravity. Incorporating additional spectroscopic redshift followup observations could provide important dark energy constraints from pairwise velocities alone. Mean pairwise velocities are much less sensitive to systematic redshift errors than the luminosity distance test or weak lensing techniques, and also are only mildly affected by systematic evolution of supernova luminosity.PACS numbers: 98.62. Py, 95.36.+x, 97.60.Bw

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Three-Point Correlation Functions of SDSS Galaxies: Constraining Galaxy-Mass Bias

Cited by 66 publications

References 65 publications

The importance of the cosmic web and halo substructure for power spectra

The importance of the cosmic web and halo substructure for power spectra

Galaxy filaments as pearl necklaces

Galaxy peculiar velocities from large-scale supernova surveys as a dark energy probe

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