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Forecasting cosmological bias due to local gravitational redshift

Haoting Xu

School of Physics and Astronomy, Sun Yat-sen University, 2 Daxue Road, Tangjia, Zhuhai, P. R. China

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Zhiqi Huang

http://orcid.org/0000-0002-1506-1063

School of Physics and Astronomy, Sun Yat-sen University, 2 Daxue Road, Tangjia, Zhuhai, P. R. China

E-mail Address: [email protected]

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Na Zhang

School of Physics and Astronomy, Sun Yat-sen University, 2 Daxue Road, Tangjia, Zhuhai, P. R. China

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, and

Yundong Jiang

School of Physics and Astronomy, Sun Yat-sen University, 2 Daxue Road, Tangjia, Zhuhai, P. R. China

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https://doi.org/10.1142/S0218271819501505Cited by:0 (Source: Crossref)

Abstract

When photons from distant galaxies and stars pass through our neighboring environment, the wavelengths of the photons would be shifted by our local gravitational potential. This local gravitational redshift effect can potentially have an impact on the measurement of cosmological distance–redshift relation. Using available supernovae data, Wojtak, Davis and Wiis [J. Cosmol. Astropart. Phys.2015 (2015) 025] found seemingly large biases of cosmological parameters for some extended models (nonflat $Λ$ CDM, $w$ CDM, etc.). Huang [Phys. Rev. D91 (2015) 121301] pointed out that, however, the biases can be reduced to a negligible level if cosmic microwave background (CMB) data are added to break the strong degeneracy between parameters in the extended models. In this paper, we forecast the cosmological bias due to local gravitational redshifts for a future WFIRST-like supernovae survey. We find that the local gravitational redshift effect remains negligible, provided that CMB data or some future redshift survey data are added to break the degeneracy between parameters.

Keywords:

References

1. R. Wojtak, T. M. Davis and J. Wiis, J. Cosmol. Astropart. Phys. 2015 (2015) 025. Web of Science, Google Scholar
2. Z. Huang, Phys. Rev. D 91 (2015) 121301. Web of Science, ADS, Google Scholar
3. J. Calcino and T. Davis, J. Cosmol. Astropart. Phys. 2017 (2017) 038. Google Scholar
4. M. Betoule et al., Astron. Astrophys. 568 (2014) A22. Web of Science, ADS, Google Scholar
5. D. Spergel et al., arXiv:1503.03757. Google Scholar
6. O. Doré et al., arXiv:1904.01174. Google Scholar
7. N. Aghanim et al., arXiv:1807.06209. Google Scholar
8. Y. Wang and P. Mukherjee, Phys. Rev. D 76 (2007) 103533. Web of Science, ADS, Google Scholar
9. Y. Wang and S. Wang, Phys. Rev. D 88 (2013) 043522. Web of Science, ADS, Google Scholar
10. Z. Zhai and Y. Wang, arXiv:1811.07425. Google Scholar
11. L. Amendola et al., Living Rev. Rel. 21 (2018) 1. Web of Science, Google Scholar
12. LSST Science Collab. (P. A. Abell et al.), LSST Science Book, Version 2.0 (2009). Google Scholar
13. M. Chevallier and D. Polarski, Int. J. Mod. Phys. D 10 (2001) 213. Link, Web of Science, ADS, Google Scholar
14. E. V. Linder, Phys. Rev. Lett. 90 (2003) 091301. Web of Science, ADS, Google Scholar
15. H. Xu, Z. Huang, Z. Liu and H. Miao, Astrophys. J. 877 (2019) 107. Web of Science, ADS, Google Scholar
16. N. Kaiser, Mon. Not. R. Astron. Soc. 227 (1987) 1. Web of Science, ADS, Google Scholar
17. A. Lewis, A. Challinor and A. Lasenby, Astrophys. J. 538 (2000) 473. Web of Science, ADS, Google Scholar
18. J. Carron, M. Wolk and I. Szapudi, Mon. Not. R. Astron. Soc. 453 (2015) 450. Web of Science, ADS, Google Scholar
19. J. Yoo, E. Mitsou, Y. Dirian and R. Durrer, arXiv:1905.09288. Google Scholar