Modeling biased tracers at the field level

Schmittfull, Marcel; Simonović, Marko; Assassi, Valentin; Zaldarriaga, Matías

doi:10.1103/physrevd.100.043514

Cited by 113 publications

(173 citation statements)

References 114 publications

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“…This is supported by the results of Ref. [78]. This study also showed that the amplitude of the shot noise can be super-or sub-Poissonian for very light or massive halos, respectively.…”

Section: )supporting

confidence: 87%

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Measuring neutrino masses with large-scale structure: Euclid forecast with controlled theoretical error

Chudaykin

Ivanov

2019

J. Cosmol. Astropart. Phys.

144

171

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We present a Markov-Chain Monte-Carlo (MCMC) forecast for the precision of neutrino mass and cosmological parameter measurements with a Euclidlike galaxy clustering survey. We use a complete perturbation theory model for the galaxy one-loop power spectrum and tree-level bispectrum, which includes bias, redshift space distortions, IR resummation for baryon acoustic oscillations and UV counterterms. The latter encapsulate various effects of short-scale dynamics which cannot be modeled within perturbation theory. Our MCMC procedure consistently computes the non-linear power spectra and bispectra as we scan over different cosmologies. The second ingredient of our approach is the theoretical error covariance which captures uncertainties due to higher-order non-linear corrections omitted in our model. Having specified characteristics of a Euclid-like spectroscopic survey, we generate and fit mock galaxy power spectrum and bispectrum likelihoods. Our results suggest that even under very agnostic assumptions about non-linearities and short-scale physics a future Euclid-like survey will be able to measure the sum of neutrino masses with a standard deviation of 28 meV. When combined with the most recent Planck likelihood, this uncertainty decreases to 19 meV. Reducing the theoretical error on the bispectrum down to the two-loop level marginally tightens the bound to 17 meV. 1 chudy@ms2.inr.ac.ru 2 mi1271@nyu.edu arXiv:1907.06666v1 [astro-ph.CO] 15 Jul 2019 exploit the potential of upcoming surveys will strongly depend on the understanding on these effects, which is not yet complete.Fortunately, the bulk of information about the neutrino free-streaming is encoded in mildly non-linear scales which can be robustly and systematically described within perturbation theory. One of the most popular approaches is Eulerian standard cosmological perturbation theory (SPT) [14]. The basic formulation of SPT, however, does not correctly capture the non-linear evolution of baryon acoustic oscillations (BAO) [15] and short-scale physics beyond the single-stream pressureless perfect fluid hydrodynamics [16][17][18]. These problems have been intensely studied in the recent years.First, it has been shown that the non-linear suppression and distortion of the BAO can be captured by a resummation of contributions describing the tidal effects of large-scale bulk flows. This procedure, called infrared (IR) resummation, is essential for an accurate description of the BAO and has been formulated within various theoretical frameworks [19][20][21][22][23][24][25]. We will adopt a systematic approach of [22,24] streamlined in the context of time-sliced perturbation theory [26].Second, we will use the effective field theory of large-scale structure (EFT) to account for the back-reaction of small scale nonlinearities on larger scales [17,27,28]. This approach removes the unphysical UV sensitivity of perturbation theory loop integrals and parameterizes the ignorance about short scale-dynamics by various effective operators in the equations of motion for ...

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“…This is supported by the results of Ref. [78]. This study also showed that the amplitude of the shot noise can be super-or sub-Poissonian for very light or massive halos, respectively.…”

Section: )supporting

confidence: 87%

“…As for the higher-derivative bias coefficient, the measurements from N-body simulations [34,78,101] suggest that it is an order-one quantity in units of [Mpc/h] 2 . Thus, we adopt the following fiducial value along with the time-dependence that corresponds to the one-loop contribution,…”

Section: Parameter Definition Fiducial Value Hmentioning

confidence: 99%

Measuring neutrino masses with large-scale structure: Euclid forecast with controlled theoretical error

Chudaykin

Ivanov

2019

J. Cosmol. Astropart. Phys.

144

171

View full text Add to dashboard Cite

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“…To fit for the bias parameters, we use the approach developed by ref. [23], specifically we match the model with the observations at the level of the field instead of only matching the two-point functions. The component biased fields are 'shifted' to their Eulerian position with the non-linear dynamics of choice and then binned onto the grid with cloud-in-cloud (CIC) interpolation to get the corresponding Eulerian (shifted) fields (δ L (x), ...).…”

Section: Forward Modelmentioning

confidence: 99%

“…where the sum is over half of the k plane since δ (k) = δ(−k) for the Fourier transform of a real field. In principle the bias parameters can be made scale dependent, b(k), and treated as transfer functions [23]. To get these transfer functions, we simply minimize Eq.…”

Section: Forward Modelmentioning

confidence: 99%

Reconstructing large-scale structure with neutral hydrogen surveys

Modi

White

Slosar

et al. 2019

J. Cosmol. Astropart. Phys.

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Upcoming 21-cm intensity surveys will use the hyperfine transition in emission to map out neutral hydrogen in large volumes of the universe. Unfortunately, large spatial scales are completely contaminated with spectrally smooth astrophysical foregrounds which are orders of magnitude brighter than the signal. This contamination also leaks into smaller radial and angular modes to form a foreground wedge, further limiting the usefulness of 21-cm observations for different science cases, especially cross-correlations with tracers that have wide kernels in the radial direction. In this paper, we investigate reconstructing these modes within a forward modeling framework. Starting with an initial density field, a suitable bias parameterization and non-linear dynamics to model the observed 21-cm field, our reconstruction proceeds by maximizing the likelihood of a forward simulation to match the observations, under given modeling error and a data noise model. For redshifts z = 2 and 4, we are able to reconstruct 21cm field with cross correlation, r c > 0.8 on all scales for both our optimistic and pessimistic assumptions about foreground contamination and for different levels of thermal noise. The performance deteriorates slightly at z = 6. The large-scale line-of-sight modes are reconstructed almost perfectly. We demonstrate how our method also provides a technique for density field reconstruction for baryon acoustic oscillations, outperforming standard methods on all scales. We also describe how our reconstructed field can provide superb clustering redshift estimation at high redshifts, where it is otherwise extremely difficult to obtain dense spectroscopic samples, as well as open up a wealth of cross-correlation opportunities with projected fields (e.g. lensing) which are restricted to modes transverse to the line of sight.

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“…Nonetheless, clustering and halo exclusion may introduce deviations from a Poissonian shot noise. This non-Poissonian contribution can change the amplitude of the shot noise and even induces a small scale dependence [133,134].…”

Section: Cross-correlation With Galaxy Surveysmentioning

confidence: 99%

User’s guide to extracting cosmological information from line-intensity maps

et al. 2019

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Line-intensity mapping (LIM) provides a promising way to probe cosmology, reionization and galaxy evolution. However, its sensitivity to cosmology and astrophysics at the same time is also a nuisance. Here we develop a comprehensive framework for modelling the LIM power spectrum, which includes redshift space distortions and the Alcock-Paczynski effect. We then identify and isolate degeneracies with astrophysics so that they can be marginalized over. We study the gains of using the multipole expansion of the anisotropic power spectrum, providing an accurate analytic expression for their covariance, and find a 10%-60% increase in the precision of the baryon acoustic oscillation scale measurements when including the hexadecapole in the analysis. We discuss different observational strategies when targeting other cosmological parameters, such as the sum of neutrino masses or primordial non-Gaussianity, finding that fewer and wider bins are typically more optimal. Overall, our formalism facilitates an optimal extraction of cosmological constraints robust to astrophysics.PACS numbers:

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Modeling biased tracers at the field level

Cited by 113 publications

References 114 publications

Measuring neutrino masses with large-scale structure: Euclid forecast with controlled theoretical error

Measuring neutrino masses with large-scale structure: Euclid forecast with controlled theoretical error

Reconstructing large-scale structure with neutral hydrogen surveys

User’s guide to extracting cosmological information from line-intensity maps

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