| Full text | |
| Author(s): |
Moreira, Maria G.
[1, 2]
;
Andrade-Oliveira, Felipe
[1, 2]
;
Fang, Xiao
[3]
;
Huang, Hung-Jin
[3]
;
Krause, Elisabeth
[3, 4]
;
Miranda, Vivian
[3]
;
Rosenfeld, Rogerio
[1, 5, 2]
;
Simonovic, Marko
[6]
Total Authors: 8
|
| Affiliation: | [1] Univ Estadual Paulista, Inst Fis Teor, BR-01140070 Sao Paulo, SP - Brazil
[2] Lab Interinst E Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ - Brazil
[3] Univ Arizona, Steward Observ, Dept Astron, 933 North Cherry Ave, Tucson, AZ 85721 - USA
[4] Univ Arizona, Dept Phys, 1118 E Fourth St, Tucson, AZ 85721 - USA
[5] ICTP South Amer Inst Fundamental Res, BR-01140070 Sao Paulo, SP - Brazil
[6] CERN, Theoret Phys Dept, 1 Esplanade Particules, CH-1211 Geneva 23 - Switzerland
Total Affiliations: 6
|
| Document type: | Journal article |
| Source: | Monthly Notices of the Royal Astronomical Society; v. 507, n. 4, p. 5592-5601, NOV 2021. |
| Web of Science Citations: | 0 |
| Abstract | |
One of the primary sources of uncertainties in modelling the cosmic-shear power spectrum on small scales is the effect of baryonic physics. Accurate cosmology for stage-IV surveys requires knowledge of the matter power spectrum deep in the non-linear regime at the percent level. Therefore, it is important to develop reliable mitigation techniques to take into account baryonic uncertainties if information from small scales is to be considered in the cosmological analysis. In this work, we develop a new mitigation method for dealing with baryonic physics for the case of the shear angular power spectrum. The method is based on an augmented covariance matrix that incorporates baryonic uncertainties informed by hydrodynamical simulations. We use the results from 13 hydrodynamical simulations and the residual errors arising from a fit to a Lambda CDM model using the extended halo model code HMCODE to account for baryonic physics. These residual errors are used to model a so-called theoretical error covariance matrix that is added to the original covariance matrix. In order to assess the performance of the method, we use the 2D tomographic shear from four hydrodynamical simulations that have different extremes of baryonic parameters as mock data and run a likelihood analysis comparing the residual bias on Omega(m) and sigma(8) of our method and the HMCODE for an LSST-like survey. We use different modelling of the theoretical error covariance matrix to test the robustness of the method. We show that it is possible to reduce the bias in the determination of the tested cosmological parameters at the price of a modest decrease in the precision. (AU) | |
| FAPESP's process: | 16/01343-7 - ICTP South American Institute for Fundamental Research: a regional center for theoretical physics |
| Grantee: | Nathan Jacob Berkovits |
| Support Opportunities: | Special Projects |