We present Fisher matrix projections for future cosmological parameter measurements, including neutrino masses, Dark Energy, curvature, modified gravity, the inflationary perturbation spectrum, non-Gaussianity, and dark radiation. We focus on DESI and generally redshift surveys (BOSS, HETDEX, eBOSS, Euclid, and WFIRST), but also include CMB (Planck) and weak gravitational lensing (DES and LSST) constraints. The goal is to present a consistent set of projections, for concrete experiments, which are otherwise scattered throughout many papers and proposals. We include neutrino mass as a free parameter in most projections, as it will inevitably be relevant -DESI and other experiments can measure the sum of neutrino masses to ∼ 0.02 eV or better, while the minimum possible sum is ∼ 0.06 eV. We note that constraints on Dark Energy are significantly degraded by the presence of neutrino mass uncertainty, especially when using galaxy clustering only as a probe of the BAO distance scale (because this introduces additional uncertainty in the background evolution after the CMB epoch). Using broadband galaxy power becomes relatively more powerful, and bigger gains are achieved by combining lensing survey constraints with redshift survey constraints. We do not try to be especially innovative, e.g., with complex treatments of potential systematic errors -these projections are intended as a straightforward baseline for comparison to more detailed analyses.

Mapping the recent expansion history of the Universe offers the best hope for uncovering the characteristics of the dark energy believed to be responsible for the acceleration of the expansion. In determining cosmological and dark-energy parameters to the percentage level, systematic uncertainties impose a more severe floor on the accuracy than the statistical measurement precision. We delineate the categorization, simulation and understanding required to bound systematics for the specific case of the Type Ia supernova method. Using the simulated data of the forthcoming ground-based surveys and the proposed space-based Supernova/Acceleration Probe (SNAP) mission we present Monte Carlo results for the residual uncertainties on the cosmological parameter determination. The tight systematics control with optical and near-infrared observations and the extended redshift reach allow a space survey to bound the systematics below 0.02 mag at z = 1.7. For a typical SNAP-like supernova survey, this keeps total errors within 15 per cent of the statistical values and provides estimation of m to 0.03, w 0 to 0.07 and w to 0.3; these can be further improved by incorporating complementary data. I N T RO D U C T I O NWith the great increase in observational capabilities in the past and next few years, we can look forward to cosmological data of unprecedented volume and quality. These will be brought to bear on the outstanding questions of our 'preposterous Universe' (Carroll 2001). What new forms of matter and energy constitute 95 per cent of the Universe? What is the underlying nature of the mysterious dark energy causing the observed acceleration of the expansion of the Universe yet without an explanation within the standard model of particle physics? However, more photons of any given observational method will not teach us the properties of the cosmological model before we understand the sources and the intervening medium. Systematic uncertainties, rather than statistical errors, will bound our progress at the level where we fail to correct for astrophysical interference to our inference.This applies to each one of the promising cosmological probes. Use of cosmic microwave background radiation has been dramatically successful in fitting certain cosmological properties (Spergel et al. 2003), but others are tied up in degeneracies, insensitivities (e.g. to the dark energy equation of state (EOS) behaviour) and astrophysical foregrounds. Structure growth and evolution measures such as cluster counts by the Sunyaev-Zel'dovich effect or X-ray

We present DEEP2 galaxy clustering measurements at z ∼ 1 as a function of stellar mass, star formation rate (SFR), and specific SFR (sSFR). We find a strong positive correlation between stellar mass and clustering amplitude on 1-10 h −1 Mpc scales for blue, star-forming galaxies with 9.5

BigBOSS: The Ground-Based Stage IV BAO ExperimentThis Response to the Decadal Survey is submitted by:The Lawrence Berkeley National Laboratory 1 Cyclotron Rd MS 50R-5032, Berkeley, CA 94720 David Schlegel, DJSchlegel@lbl.gov, 510-495-2595 Chris EXECUTIVE SUMMARYThe BigBOSS experiment is a proposed DOE-NSF Stage IV ground-based dark energy experiment to study baryon acoustic oscillations (BAO) and the growth of structure with an allsky galaxy redshift survey. The project is designed to unlock the mystery of dark energy using existing ground-based facilities operated by NOAO. A new 4000-fiber R=5000 spectrograph covering a 3-degree diameter field will measure BAO and redshift space distortions in the distribution of galaxies and hydrogen gas spanning redshifts from 0.2 < z < 3.5. The Dark Energy Task Force figure of merit (DETF FoM) for this experiment is expected to be equal to that of a JDEM mission for BAO with the lower risk and cost typical of a ground-based experiment. This project will enable an unprecedented multi-object spectroscopic capability for the U.S. community through an existing NOAO facility. The U.S. community would have access directly to this instrument/telescope combination, as well as access to the legacy archives that will be created by the BAO key project.The BigBOSS survey will target luminous red galaxies, emission line galaxies, and QSOs. This experiment builds upon the SDSS-III/BOSS project, reusing many aspects of the BOSS spectrograph and computing pipeline designs. The BigBOSS project is enabled by the impressive 3 degree diameter field of view of the 4-m Mayall telescope at KPNO. The focal plane of this telescope will be filled with an automated fiber-positioner capable of targeting 4000 objects simultaneously over a wavelength range from 340 nm to 1130 nm with resolution R=2300-6100. This carefully-designed instrument is capable of measuring redshifts to the brightest [OII] emitters to z=2 with a 4-m aperture. Assuming a majority allocation of the dark time and optimal observing conditions during 30% of all nights, and with approximately onehour exposures, over 5 million targets will be visited per year. We propose to operate for six years at KPNO and then move the instrument to CTIO, the Mayall sister telescope in the southern hemisphere, for a four year run commencing after the Dark Energy Survey (DES) program.The 30-million galaxy sample of BigBOSS-North provides precision baryon acoustic oscillation measurements over 14000 square degrees from 0.2 < z < 2.0 and a million QSOs from 1.8< z <3.5. A continuation with BigBOSS-South completes the survey, bringing the total to 50 million galaxies over 24000 square degrees. BigBOSS will sculpt the redshift distribution to maximize the statistical significance of the dark energy measurement. The target selection will be done using existing and planned imaging surveys. A summary of experiment goals is shown in Table 1.BigBOSS is proposed as a partnership between NSF/NOAO and DOE/OHEP. Details of this partnership will be determined w...

No abstract