Exploring Large‐Scale Structure with Billions of Galaxies

Zhan, Hongbing; Knox, L.; Margoniner, V. E.

doi:10.1086/500077

Cited by 32 publications

(41 citation statements)

References 87 publications

(147 reference statements)

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“…Our study complements previous work [29,30,31] on the observable predictions of classes of dark energy models, and follows a long history of studies concerning the best way to probe dark energy using cosmological observations [32,33,34,35,36,37,38,39,40,41,42,43,44,45,46,47,48,49,50,51,52,53,54,55,56,57,58,59,60,61,62,63,64,65,66,67,68,69,70]. To our knowledge this is the first time that consistency between growth, distance, and other expansion observables has been studied in such a general and quantitative way.…”

Section: Introductionsupporting

confidence: 66%

Falsifying Paradigms for Cosmic Acceleration

Huterer

2009

Nuclear Physics B - Proceedings Supplements

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Consistency relations between growth of structure and expansion history observables exist for any physical explanation of cosmic acceleration, be it a cosmological constant, scalar field quintessence, or a general component of dark energy that is smooth relative to dark matter on small scales. The high-quality supernova sample anticipated from an experiment like SNAP and CMB data expected from Planck thus make strong predictions for growth and expansion observables that additional observations can test and potentially falsify. We perform an MCMC likelihood exploration of the strength of these consistency relations based on a complete parametrization of dark energy behavior by principal components. For ΛCDM, future SN and CMB data make percent level predictions for growth and expansion observables. For quintessence, many of the predictions are still at a level of a few percent with most of the additional freedom coming from curvature and early dark energy. While such freedom is limited for quintessence where phantom equations of state are forbidden, it is larger in the smooth dark energy class. Nevertheless, even in this general class predictions relating growth measurements at different redshifts remain robust, although predictions for the instantaneous growth rate do not. Finally, if observations falsify the whole smooth dark energy class, new paradigms for cosmic acceleration such as modified gravity or interacting dark matter and dark energy would be required.

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Section: Introductionsupporting

confidence: 66%

Falsifying Paradigms for Cosmic Acceleration

Huterer

2009

Nuclear Physics B - Proceedings Supplements

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“…Future instruments, such as the Large Synoptic Survey Telescope (LSST), will measure the matter power spectrum with unprecedented precision ( P=P 0:01) [76,77]. This order of magnitude improvement over past work [78,79] will improve the constraint to a h 2 by an order of magnitude, resulting in the improved sensitivity to axion masses and reheating temperatures shown by the dotted line in Fig.…”

Section: B Constraints To the Axion Mass From Cmb/lss Datamentioning

confidence: 95%

“…6. Estimated improvement in the accessible axion parameter space from including more precise measurements of the matter power spectrum (region bounded by the dotted line), corresponding to LSST [76,77], or from measurements of clustering on smaller length scales, corresponding to Lyman-forest measurements (region bounded by the dashed line) [80]. The hatched region indicates the parameter space excluded by WMAP1/SDSS measurements.…”

Section: Axions As Relativistic Degrees Of Freedom At Early Timesmentioning

confidence: 99%

Axion constraints in nonstandard thermal histories

2008

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It is usually assumed that dark matter is produced during the radiation-dominated era. There is, however, no direct evidence for radiation domination prior to big-bang nucleosynthesis. Two nonstandard thermal histories are considered. In one, the low-temperature-reheating scenario, radiation domination begins as late as 1 MeV, and is preceded by significant entropy generation. Thermal axion relic abundances are then suppressed, and cosmological limits to axions are loosened. For reheating temperatures T rh & 35 MeV, the large-scale structure limit to the axion mass is lifted. The remaining constraint from the total density of matter is significantly relaxed. Constraints are also relaxed for higher reheating temperatures. In a kination scenario, a more modest change to cosmological axion constraints is obtained. Future possible constraints to axions and low-temperature reheating from the helium abundance and nextgeneration large-scale-structure surveys are discussed.

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“…The cosmological parameter constraints resulting from future photometric redshift imaging surveys have been simulated by several authors (e.g. Seo & Eisenstein 2003; Dolney, Jain & Takada 2004; Zhan et al 2006). Application to data such as the SDSS LRG samples were given by Blake et al (2007) and Padmanabhan et al (2007).…”

Section: Introductionmentioning

confidence: 99%

Forecasting neutrino masses from galaxy clustering in the Dark Energy Survey combined with thePlanckmeasurements

Lahav

Kiakotou

Abdalla

2010

Monthly Notices of the Royal Astronomical Society

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We study the prospects for detecting neutrino masses from the galaxy angular power spectrum in photometric redshift shells of the Dark Energy Survey (DES) over a volume of ∼20 h−3 Gpc3, combined with the cosmic microwave background (CMB) angular fluctuations expected to be measured from the Planck satellite. We find that for a Λ cold dark matter concordance model with seven free parameters in addition to a fiducial neutrino mass of Mν= 0.24 eV, we recover from DES and Planck the correct value with uncertainty of ±0.12 eV (95 per cent confidence level; CL), assuming perfect knowledge of the galaxy biasing. If the fiducial total mass is close to zero, then the upper limit is 0.11 eV (95 per cent CL). This upper limit from DES and Planck is over three times tighter than using Planck alone, as DES breaks the parameter degeneracies in a CMB‐only analysis. The analysis utlilizes spherical harmonics up to 300, averaged in bin of 10 to mimic the DES sky coverage. The results are similar if we supplement DES bands (grizY) with the Visible and Infra‐Red Survey Telescope for Astronomy Hemisphere Survey (VHS) near‐infrared band (JHK). The result is robust to uncertainties in non‐linear fluctuations and redshift distortions. However, the result is sensitive to the assumed galaxy biasing schemes and it requires accurate prior knowledge of the biasing. To summarize, if the total neutrino mass in nature is greater than 0.1 eV, we should be able to detect it with DES and Planck, a result with great importance to fundamental physics.

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Exploring Large‐Scale Structure with Billions of Galaxies

Cited by 32 publications

References 87 publications

Falsifying Paradigms for Cosmic Acceleration

Falsifying Paradigms for Cosmic Acceleration

Axion constraints in nonstandard thermal histories

Forecasting neutrino masses from galaxy clustering in the Dark Energy Survey combined with thePlanckmeasurements

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