Precision Studies of Dark Energy with LSST

Tyson, J. Anthony; ,

doi:10.1063/1.2402596

Cited by 16 publications

(14 citation statements)

References 16 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…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: 87%

“…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%

See 1 more Smart Citation

Axion constraints in nonstandard thermal histories

2008

View full text Add to dashboard Cite

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.

show abstract

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

confidence: 87%

Section: Axions As Relativistic Degrees Of Freedom At Early Timesmentioning

confidence: 99%

Axion constraints in nonstandard thermal histories

2008

View full text Add to dashboard Cite

show abstract

“…There are various ongoing and planned cosmic shear surveys, like for instance the Canada-France-Hawaii Telescope Legacy Survey 20 (CFHTLS) [162]; the Dark Energy Survey 21 (DES) [212,213,214]; the SuperNova Acceleration Probe 22 (SNAP); the Panoramic Survey Telescope And Rapid Response System 23 (Pan-STARRS); or the Large Synoptic Survey Telescope 24 (LSST) [234,235]. The sensitivity of this type of observation to neutrino masses has been addressed first in [236], and later in [237,206,238].…”

Section: Neutrino Mass From Cosmic Shear Surveysmentioning

confidence: 99%

Massive neutrinos and cosmology

2006

View full text Add to dashboard Cite

The present experimental results on neutrino flavour oscillations provide evidence for non-zero neutrino masses, but give no hint on their absolute mass scale, which is the target of beta decay and neutrinoless double-beta decay experiments. Crucial complementary information on neutrino masses can be obtained from the analysis of data on cosmological observables, such as the anisotropies of the cosmic microwave background or the distribution of large-scale structure. In this review we describe in detail how free-streaming massive neutrinos affect the evolution of cosmological perturbations. We summarize the current bounds on the sum of neutrino masses that can be derived from various combinations of cosmological data, including the most recent analysis by the WMAP team. We also discuss how future cosmological experiments are expected to be sensitive to neutrino masses well into the sub-eV range.Comment: 122 pages, 23 figures, misprints corrected and references added. Review article to be published in Physics Report

show abstract

“…The situation will be quite different for future weak lensing surveys, like LSST [36] or DUNE (now EUCLID) [37]; indeed, these surveys will obtain precise photometric redshifts up to very high redshifts z ∼ 3, and therefore the magnification bias correction will not be a priori negligible. In particular, for high lens redshift z f 1, if the foreground number slope s f is not such that the magnification is small, the correction can be of order one.…”

Section: Correction Due To Magnification Biasmentioning

confidence: 99%

Magnification bias corrections to galaxy-lensing cross-correlations

Ziour

Hui

2008

Phys. Rev. D

View full text Add to dashboard Cite

Galaxy-galaxy or galaxy-quasar lensing can provide important information on the mass distribution in the universe. It consists of correlating the lensing signal (either shear or magnification) of a background galaxy/quasar sample with the number density of a foreground galaxy sample. However, the foreground galaxy density is inevitably altered by the magnification bias due to the mass between the foreground and the observer, leading to a correction to the observed galaxy-lensing signal. The aim of this paper is to quantify this correction. The single most important determining factor is the foreground redshift z f : the correction is small if the foreground galaxies are at low redshifts but can become non-negligible for sufficiently high redshifts. For instance, we find that for the multipole ℓ = 1000, the correction is above 1% × (5s f − 2)/b f for z f 0.37, and above 5% × (5s f − 2)/b f for z f 0.67, where s f is the number count slope of the foreground sample, and b f its galaxy bias. These considerations are particularly important for geometrical measures, such as the Jain and Taylor ratio or its generalization by Zhang et al. Assuming (5s f − 2)/b f = 1, we find that the foreground redshift should be limited to z f 0.45 in order to avoid biasing the inferred dark energy equation of state w by more than 5%, and that even for a low foreground redshift (< 0.45), the background samples must be well separated from the foreground to avoid incurring a bias of similar magnitude. Lastly, we briefly comment on the possibility of obtaining these geometrical measures without using galaxy shapes, using instead magnification bias itself.PACS numbers: 98.80.Es; 98.65.Dx; 95.35.+d

show abstract

Precision Studies of Dark Energy with LSST

Cited by 16 publications

References 16 publications

Axion constraints in nonstandard thermal histories

Axion constraints in nonstandard thermal histories

Massive neutrinos and cosmology

Magnification bias corrections to galaxy-lensing cross-correlations

Contact Info

Product

Resources

About