Total Acidity and pH

Gould, Wilbur A.

doi:10.1533/9781845696153.2.383

Cited by 17 publications

(32 citation statements)

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“…Consequently the reduced χ 2 of our chains is 28.0/24 = 1.17 for true cosmic environments, and 34.2/24 = 1.43 for shuffled environments. In the Gaussian case the uncertainty on χ 2 is σ χ 2 = √ 2(N dof ) = 6.93 Gould (2003). This indicates that the minimum χ 2 value lies well within 1σ of the expected minimum χ 2 for true environments, and just outside for shuffled environments.…”

Section: Surface Density Modelmentioning

confidence: 71%

Dependence of GAMA galaxy halo masses on the cosmic web environment from 100 deg²of KiDS weak lensing data

Brouwer¹,

Cacciato²,

Dvornik³

et al. 2016

Mon. Not. R. Astron. Soc.

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Galaxies and their dark matter haloes are part of a complex network of mass structures, collectively called the cosmic web. Using the tidal tensor prescription these structures can be classified into four cosmic environments: voids, sheets, filaments and knots. As the cosmic web may influence the formation and evolution of dark matter haloes and the galaxies they host, we aim to study the effect of these cosmic environments on the average mass of galactic haloes. To this end we measure the galaxy-galaxy lensing profile of 91, 195 galaxies, within 0.039 < z < 0.263, from the spectroscopic Galaxy And Mass Assembly (GAMA) survey, using ∼ 100 deg 2 of overlapping data from the Kilo-Degree Survey (KiDS). In each of the four cosmic environments we model the contributions from group centrals, satellites and neighbouring groups to the stacked galaxy-galaxy lensing profiles. After correcting the lens samples for differences in the stellar mass distribution, we find no dependence of the average halo mass of central galaxies on their cosmic environment. We do find a significant increase in the average contribution of neighbouring groups to the lensing profile in increasingly dense cosmic environments. We show, however, that the observed effect can be entirely attributed to the galaxy density at much smaller scales (within 4 h −1 Mpc), which is correlated with the density of the cosmic environments. Within our current uncertainties we find no direct dependence of galaxy halo mass on their cosmic environment.

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Section: Surface Density Modelmentioning

confidence: 71%

Dependence of GAMA galaxy halo masses on the cosmic web environment from 100 deg²of KiDS weak lensing data

Brouwer¹,

Cacciato²,

Dvornik³

et al. 2016

Mon. Not. R. Astron. Soc.

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“…On the other side, Gould and Alam [28], using arguments based on calculations of asteroids trajectories [41], have pointed out that solar-bound WIMPs could evolve in a way quite different from the one derived in Ref. [27], with an ensuing suppression of the up-going muon flux usually expected from the center of the Earth for a standard halo population.…”

Section: Constraints From Neutralino-neutralino Annihilation Insmentioning

confidence: 93%

“…However, in the implementation of constraints from up-going muons at neutrino telescopes, we have also considered recent theoretical developments which may have quite contrasting effects on the expected signals [27,28]. These different instances are examined in Sect.…”

Section: Introductionmentioning

confidence: 99%

Further investigation of a relic neutralino as a possible origin of an annual-modulation effect in weakly interacting massive particle direct search

et al. 2000

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We analyze the annual-modulation effect, measured by the DAMA Collaboration with the new implementation of a further two-years running, in the context of a possible interpretation in terms of relic neutralinos. We impose over the set of supersymmetric configurations, selected by the annualmodulation data, the constraints derived from WIMP indirect measurements, and discuss the features of the ensuing relic neutralinos. We critically discuss the sources of the main theoretical uncertainties in the analysis of event rates for direct and indirect WIMP searches.

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“…measuring the photocentre motion during microlensing) will be feasible quite soon, especially with the foreseen fame, gaia and sim astrometric satellites. I do not discuss it further and refer the reader to the review of Gould (2001); let me mention only that astrometric microlensing has a shallower dependence on the impact parameter, and that it provides information complementary to that of photometric microlensing; this will help in breaking the timescale degeneracy. Apart from microlensing timescale, the other important observable is its rate.…”

Section: Simple Microlensingmentioning

confidence: 99%

“…As the present review is short and contains no calculations, I refer the interested reader to other sources (Paczyński, 1996;Roulet and Möllerach, 1997;Gould, 2000;Gould, 2001). …”

Section: Introductionmentioning

confidence: 99%

The Galactic Halo from Microlensing

Milsztajn

2002

Space Sciences Series of ISSI

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Total Acidity and pH

Cited by 17 publications

References 0 publications

Dependence of GAMA galaxy halo masses on the cosmic web environment from 100 deg²of KiDS weak lensing data

Dependence of GAMA galaxy halo masses on the cosmic web environment from 100 deg²of KiDS weak lensing data

Further investigation of a relic neutralino as a possible origin of an annual-modulation effect in weakly interacting massive particle direct search

The Galactic Halo from Microlensing

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Total Acidity and pH

Cited by 17 publications

References 0 publications

Dependence of GAMA galaxy halo masses on the cosmic web environment from 100 deg2of KiDS weak lensing data

Dependence of GAMA galaxy halo masses on the cosmic web environment from 100 deg2of KiDS weak lensing data

Further investigation of a relic neutralino as a possible origin of an annual-modulation effect in weakly interacting massive particle direct search

The Galactic Halo from Microlensing

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Dependence of GAMA galaxy halo masses on the cosmic web environment from 100 deg²of KiDS weak lensing data

Dependence of GAMA galaxy halo masses on the cosmic web environment from 100 deg²of KiDS weak lensing data