The BigBOSS Experiment

Schlegel, David J.; Abdalla, F. B.; Abraham, Tara H.; Ahn, Christopher; Prieto, C. Allende; Annis, J.; Aubourg, É.; Azzaro, M.; Bailey, S.; Baltay, C.; Baugh, Carlton M.; Bebek, C.; Becerril, S.; Blanton, Michael R.; Bolton, A.; Bromley, Benjamin C.; Cahn, Robert W.; Carton, Pierre-Henri; Cervantes-Cota, Jorge L.; Chu, Youqun; Cortês, Marina; Dawson, Kyle; Dey, Arjun; Dickinson, M.; Diehl, H. T.; Doel, P.; Ealet, A.; Edelstein, Jerry; Eppelle, Dominique; Escoffier, S.; Evrard, A.; Faccioli, L.; Frenk, Carlos S.; Geha, Marla; Gerdes, D. W.; Gondolo, Paolo; González-Arroyo, Antonio; Grossan, B.; Heckman, Timothy M.; Heetderks, H.; Ho, Shirley; Honscheid, K.; Huterer, Dragan; Ilbert, O.; Ivans, Inese I.; Jelinsky, Patrick; Jing, Yingjie; Joyce, D.; Kennedy, Rebecca; Kent, S.; Kieda, D.; Kim, A.; Kim, C.; Kneib, J.-P.; Kong, Xu; Kosowsky, Arthur; Krishnan, Krish; Lahav, O.; Lampton, M.; LeBohec, S.; Brun, V. Le; Levi, Mark; Li, C.; Liang, Ming; Lim, H.; Lin, Weipeng; Linder, Eric V.; Lorenzon, W.; Macorra, Axel de la; Magneville, C.; Malina, Roger F.; Marinoni, C.; Martinez, V.; Majewski, Steven R.; Matheson, T.; McCloskey, R.; McDonald, Patrick; McKay, T. A.; McMahon, Janice; Ménard, Brice; Miralda-Escudé, Jordi; Modjaz, M.; Montero-Dorta, Antonio D.; Morales, Irma Fuentes; Mostek, N.; Newman, Jeffrey A.; Nichol, R.; Nugent, P.; Olsen, Knut; Padmanabhan, Nikhil; Palanque-Delabrouille, N.; Park, I.; Peacock, J. A.; Percival, W.; Perlmutter, S.; Péroux, Céline; Petitjean, P.; Prada, Francisco; Prieto, Éric; Prochaska, J. X.; Reil, K.; Rockosi, Constance M.; Roe, Natalie A.; Rollinde, Emmanuel; Roodman, A.; Ross, N. P.; Rudnick, Gregory; Ruhlmann-Kleider, V.; Sanchez, Jorge Abril; Sawyer, David; Schimd, C.; Schubnell, M.; Scoccimaro, R.; Seljak, U.; Seo, Hee-Jong; Sheldon, E.; Sholl, Michael; Shulte-Ladbeck, R.; Slosar, A.; Smith, D.; Smoot, George F.; Springer, R. W.; Stril, A.; Szalay, A. S.; Tao, C.; Tarlè, G.; Taylor, Edward N.; Tilquin, A.; Tinker, Jeremy L.; Valdés, F.; Wang, J.; Wang, T.; Weaver, B. A.; Weinberg, David H.; White, M. J.; Wood-Vasey, Michael; Yang, Jinyi; Yang, Xiaohong; Zakamska, Nadia L.; Zentner, Andrew R.; Zhai, Chengxing; Zhang, P.; Yéche, C.

doi:10.2172/1027233

Cited by 47 publications

(50 citation statements)

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“…BigBOSS plans to survey 14, 000 deg 2 in the northern hemisphere, and a southern hemisphere equivalent could increase the area to 24, 000 deg 2 (limited in the end by Galactic extinction). Sampling density forecasts are more uncertain for BigBOSS than for Euclid; Schlegel et al (2011) predict nP > 2 out to z ≈ 1.05 and nP > 0.5 out to z ≈ 1.35, falling to nP = 0.35 by z = 1.65. 81 The WFIRST DRM1 of Green et al (2012), with 2.4 years devoted to high-latitude imaging and spectroscopy, is projected to achieve nP 1 from 1.3 < z < 2.0, declining to nP ≈ 0.5 at z = 2.7.…”

Section: Observables and Aggregate Precisionmentioning

confidence: 97%

“…81 Schlegel et al (2011) use a different convention, quoting nP for the redshift-space power spectrum at k = 0.14 h Mpc −1 and µ = 0.6 instead of the real-space power spectrum at k = 0.2 h Mpc −1 . We have quoted the numbers from their Table 2.3 as is, with no conversion to our nP convention and no independent assessment of the sampling density the instrument is likely to achieve.…”

Section: Observables and Aggregate Precisionmentioning

confidence: 99%

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Observational probes of cosmic acceleration

et al. 2013

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The accelerating expansion of the universe is the most surprising cosmological discovery in many decades, implying that the universe is dominated by some form of "dark energy" with exotic physical properties, or that Einstein's theory of gravity breaks down on cosmological scales. The profound implications of cosmic acceleration have inspired ambitious efforts to understand its origin, with experiments that aim to measure the history of expansion and growth of structure with percent-level precision or higher. We review in detail the four most well established methods for making such measurements: Type Ia supernovae, baryon acoustic oscillations (BAO), weak gravitational lensing, and the abundance of galaxy clusters. We pay particular attention to the systematic uncertainties in these techniques and to strategies for controlling them at the level needed to exploit "Stage IV" dark energy facilities such as BigBOSS, LSST, Euclid, and WFIRST. We briefly review a number of other approaches including redshift-space distortions, the Alcock-Paczynski effect, and direct measurements of the Hubble constant H 0 . We present extensive forecasts for constraints on the dark energy equation of state and parameterized deviations from General Relativity, achievable with Stage III and Stage IV experimental programs that incorporate supernovae, BAO, weak lensing, and cosmic microwave background data. We also show the level of precision required for clusters or other methods to provide constraints competitive with those of these fiducial programs. We emphasize the value of a balanced program that employs several of the most powerful methods in combination, both to cross-check systematic uncertainties and to take advantage of complementary information. Surveys to probe cosmic acceleration produce data sets that support a wide range of scientific investigations, and they continue the longstanding astronomical tradition of mapping the universe in ever greater detail over ever larger scales.

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Section: Observables and Aggregate Precisionmentioning

confidence: 97%

Section: Observables and Aggregate Precisionmentioning

confidence: 99%

Observational probes of cosmic acceleration

et al. 2013

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“…One can infer the features generated by constructing the potential (22). It is straightforward to check that to leading order in slow roll parameters, this is simply…”

Section: Light Particle Content and Particle Productionmentioning

confidence: 99%

“…It thus remains a pertinent question to ask whether or not we have exhausted all the information content that is potentially available in the primordial two-point correlation functions. Even if primordial non-Gaussianity is ever detected, the question takes on added significance in light of the vast amount of data due to become available in the near to long term through large-scale structure [21][22][23], 21 cm observations [24][25][26][27] and observations of the spectral distortion of the CMB [28,29]. In partici Although interesting deviations from its predictions might be present at longer wavelengths with marginal significance [5].…”

Section: Introductionmentioning

confidence: 99%

Features and new physical scales in primordial observables: Theory and observation

Chluba

Hamann

Patil

2015

Int. J. Mod. Phys. D

212

233

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June 22, 20152 All cosmological observations to date are consistent with adiabatic, Gaussian and nearly scale invariant initial conditions. These findings provide strong evidence for a particular symmetry breaking pattern in the very early universe (with a close to vanishing order parameter, ), widely accepted as conforming to the predictions of the simplest realizations of the inflationary paradigm. However, given that our observations are only privy to perturbations, in inferring something about the background that gave rise to them, it should be clear that many different underlying constructions project onto the same set of cosmological observables. Features in the primordial correlation functions, if present, would offer a unique and discriminating window onto the parent theory in which the mechanism that generated the initial conditions is embedded. In certain contexts, simple linear response theory allows us to infer new characteristic scales from the presence of features that can break the aforementioned degeneracies among different background models, and in some cases can even offer a limited spectroscopy of the heavier degrees of freedom that couple to the inflaton. In this review, we offer a pedagogical survey of the diverse, theoretically well grounded mechanisms which can imprint features into primordial correlation functions in addition to reviewing the techniques one can employ to probe observations. These observations include cosmic microwave background anisotropies and spectral distortions as well as the matter two and three point functions as inferred from large-scale structure and potentially, 21 cm surveys.

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“…At intermediate z, Terlevich et al (2015) used 25 HII galaxies at z ∼ 2.3 to constrain M , however the dispersion obtained is larger than the one using supernovae. Another method to reach higher z (∼3.5) involves the use of baryonic acoustic oscillations (BAOs) obtained from the database BigBOSS/DESI (Schlegel et al, 2011). Major surveys are tracking the BAOs as standard rulers.…”

Section: Introductionmentioning

confidence: 99%

Quasars as Cosmological Standard Candles

Negrete

Dultzin²,

Marziani

et al. 2017

Front. Astron. Space Sci.

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We propose the use of quasars with accretion rate near the Eddington ratio (extreme quasars) as standard candles. The selection criteria are based on the Eigenvector 1 (E1) formalism. Our first sample is a selection of 334 optical quasar spectra from the SDSS DR7 database with a S/N > 20. Using the E1, we define primary and secondary selection criteria in the optical spectral range. We show that it is possible to derive a redshift-independent estimate of luminosity for extreme Eddington ratio sources. Our results are consistent with concordance cosmology but we need to work with other spectral ranges to take into account the quasar orientation, among other constrains.

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The BigBOSS Experiment

Cited by 47 publications

References 0 publications

Observational probes of cosmic acceleration

Observational probes of cosmic acceleration

Features and new physical scales in primordial observables: Theory and observation

Quasars as Cosmological Standard Candles

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