The LSST Dark Energy Science Collaboration (DESC) Science Requirements Document

Mandelbaum, Rachel; Eifler, T. F.; Hložek, Renée; Collett, Thomas E.; Gawiser, Eric; Scolnic, D.; Alonso, David; Awan, Humna; Biswas, Rahul; Blazek, Jonathan; Burchat, P. R.; Chisari, Nora Elisa; Dell’Antonio, Ian; Digel, S. W.; Frieman, J.; Goldstein, Daniel A.; Hook, I.; Ivezić, Željko; Kahn, S. M.; Kamath, S. Sowmya; Kirkby, D.; Kitching, Thomas D.; Krause, E.; Léget, P. F.; Marshall, Philip J.; Meyers, J.; Miyatake, Hironao; Newman, Jeffrey A.; Nichol, R. C.; Rykoff, E. S.; Sánchez, Francisco Javier Martín; Slosar, Anže; Sullivan, M.; Troxel, M. A.

doi:10.2172/1471560

Cited by 52 publications

(74 citation statements)

References 6 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Since there is no evidence for a spatiotemporal variation of such a dark component [6,7,11,12], the cosmological constant seems to be the simplest and most favored explanation for the phenomenon 1 . In the next few years, substantial efforts will be made to determine if a more sophisticated dynamical scenario is required [18][19][20].…”

Section: Introductionmentioning

confidence: 99%

Can the quantum vacuum fluctuations really solve the cosmological constant problem?

et al. 2020

View full text Add to dashboard Cite

Recently it has been argued that a correct reading of the quantum fluctuations of the vacuum could lead to a solution to the cosmological constant problem. In this work we critically examine such a proposal, finding it questionable due to conceptual and self-consistency problems, as well as issues with the actual calculations. We conclude that the proposal is inadequate as a solution to the cosmological constant problem.

show abstract

Section: Introductionmentioning

confidence: 99%

Can the quantum vacuum fluctuations really solve the cosmological constant problem?

et al. 2020

View full text Add to dashboard Cite

show abstract

“…Additionally, with a survey instrument examining the sky every day, additional dSphs that haven't been discovered yet will have already been observed with the instrument's full sensitivity. The Rubin Observatory [33] will survey the Southern Hemisphere sky with unprecedented sensitivity and is expected to find hundreds of new dSphs [34]. Legacy data from SWGO at these locations could easily and immediately be analysed when new dSphs are found.…”

Section: Pos(icrc2021)555mentioning

confidence: 99%

Searching for Dark Matter with the Southern Wide-field Gamma-ray Observatory (SWGO)

Viana¹,

Albert²,

Harding³

et al. 2021

Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)

View full text Add to dashboard Cite

Despite mounting evidence that dark matter (DM) exists in the Universe, its fundamental nature remains unknown. We present sensitivity estimates to detect DM particles with a future very-highenergy ( TeV) wide field-of-view gamma-ray observatory in the Southern Hemisphere, currently in its research and development phase under the name Southern Wide field-of-view Gamma-ray Observatory (SWGO). This observatory would search for gamma rays from the annihilation or decay of DM particles in many key targets in the Southern sky, such as the Galactic halo, several dwarf galaxies, including the promising Reticulum II, and the Large Magellanic Cloud. With a wide field of view and long exposures, such observatory will have unprecedented sensitivity to DM in the mass range of ∼100 GeV to a few PeV from observations of a large fraction of the Galactic halo around the Galactic Center and from Galactic subhalos targets. These results, combined with those from other present and future gamma-ray observatories, will likely probe the thermal relic annihilation cross section of Weakly Interacting Massive Particles for all masses from ∼80 TeV down to the GeV range in most annihilation channels.

show abstract

“…The Vera C. Rubin Observatory, previously LSST, will be a 8.4 meter ground-based telescope in Chile that will measure the galaxy clustering and weak lensing with a photometric survey that will cover a 13800 deg 2 area. This survey is expected to observen g ¼ 48 sources per arcmin 2 , with a linear galaxy bias, which evolves with redshift following the equation b G ðzÞ ¼ 0.95=DðzÞ [79], where DðzÞ is the linear growth factor. The number density redshift distribution is parametrized using Eq.…”

Section: Vera C Rubin Observatorymentioning

confidence: 99%

Cosmological parameter forecasts by a joint 2D tomographic approach to CMB and galaxy clustering

et al. 2021

View full text Add to dashboard Cite

The cross-correlation between the cosmic microwave background (CMB) fields and matter tracers carries important cosmological information. In this paper, we forecast by a signal-to-noise ratio analysis the information contained in the cross-correlation of the CMB anisotropy fields with source counts for future cosmological observations and its impact on cosmological parameters uncertainties, using a joint tomographic analysis. We include temperature, polarization, and lensing for the CMB fields and galaxy number counts for the matter tracers. We consider Planck-like, the Simons Observatory, LiteBIRD, and CMB-S4 specifications for CMB, and Euclid-like, Vera C. Rubin Observatory, SPHEREx, EMU, and SKA1 for future galaxy surveys. We restrict ourselves to quasilinear scales in order to deliver results that are free as much as possible from the uncertainties in modeling nonlinearities. We forecast by a Fisher matrix formalism the relative importance of the cross-correlation of source counts with the CMB in the constraints on the parameters for several cosmological models. We obtain that the CMB-number counts cross-correlation can improve the dark energy figure of merit (FOM) at most up to a factor ∼2 for LiteBIRD þ CMB-S4 × SKA1 compared to the uncorrelated combination of both probes and will enable the Euclid-like photometric survey to reach the highest FOM among those considered here. We also forecast how CMB-galaxy clustering cross-correlation could increase the FOM of the neutrino sector, also enabling a statistically significant (≳3σ for LiteBIRD þ CMB-S4 × SPHEREx) detection of the minimal neutrino mass allowed in a normal hierarchy by using quasilinear scales only. Analogously, we find that the uncertainty in the local primordial non-Gaussianity could be as low as σðf NL Þ ∼ 1.5-2 by using two-point statistics only with the combination of CMB and radio surveys, such as EMU and SKA1. Further, we quantify how cross-correlation will help characterizing the galaxy bias. Our results highlight the additional constraining power of the cross-correlation between CMB and galaxy clustering from future surveys, which is mainly based on quasilinear scales and therefore, sufficiently robust to nonlinear effects.

show abstract

The LSST Dark Energy Science Collaboration (DESC) Science Requirements Document

Cited by 52 publications

References 6 publications

Can the quantum vacuum fluctuations really solve the cosmological constant problem?

Can the quantum vacuum fluctuations really solve the cosmological constant problem?

Searching for Dark Matter with the Southern Wide-field Gamma-ray Observatory (SWGO)

Cosmological parameter forecasts by a joint 2D tomographic approach to CMB and galaxy clustering

Contact Info

Product

Resources

About