Skip to content

Opening book details…

Can I read It's not $\sigma_8$ : constraining the non-linear matter power spectrum with the Dark Energy Survey Year-5 supernova sample on EtoBox?

It's not $\sigma_8$ : constraining the non-linear matter power spectrum with the Dark Energy Survey Year-5 supernova sample by Shah, Paul; Davis, T. M.; Vincenzi, M.; Armstrong, P.; Brout, D.; Camilleri, R.; Galbany, L.; Gill, M. S. S.; Huterer, D.; Jeffrey, N.; Lahav, O.; Lee, J.; Lidman, C.; Möller, A.; Sullivan, M.; Whiteway, L.; Wiseman, P.; Allam, S.; Aguena, M.; Annis, J.; Blazek, J.; Brooks, D.; Rosell, A. Carnero; Carretero, J.; Conselice, C.; da Costa, L. N.; Pereira, M. E. S.; Desai, S.; Diehl, H. T.; Doel, P.; Everett, S.; Ferrero, I.; Flaugher, B.; Frieman, J.; García-Bellido, J.; Gaztanaga, E.; Giannini, G.; Gruen, D.; Gruendl, R. A.; Gutierrez, G.; Hinton, S. R.; Hollowood, D. L.; Honscheid, K.; James, D. J.; Lee, S.; Marshall, J. L.; Mena-Fernández, J.; Miquel, R.; Palmese, A.; Pieres, A.; Malagón, A. A. Plazas; Porredon, A.; Samuroff, S.; Sanchez, E.; Sevilla-Noarbe, I.; Smith, M.; Suchyta, E.; Swanson, M. E. C.; Tarle, G.; Tucker, D. L.; Weaverdyck, N. is a scholarly article available to read on EtoBox.

What is It's not $\sigma_8$ : constraining the non-linear matter power spectrum with the Dark Energy Survey Year-5 supernova sample about?

The weak gravitational lensing magnification of Type Ia supernovae (SNe Ia) is sensitive to the matter power spectrum on scales $k>1 h$ Mpc$^{-1}$, making it unwise to interpret SNe Ia lensing in terms of power on linear scales. We compute the probability density function of SNe Ia magnification as a function of standard cosmological parameters, plus an empirical parameter $A_{\rm mod}$ which describes the suppression or enhancement of matter power on non-linear scales compared to a cold dark matter only model. While baryons are expected to enhance power on the scales relevant to SN Ia lensing, other physics such as neutrino masses or non-standard dark matter may suppress power. Using the Dark Energy Survey Year-5 sample, we find $A_{\rm mod} = 0.77^{+0.69}_{-0.40}$ (68\% credible interval around the median). Although the median is consistent with unity there are hints of power suppression, with $A_{\rm mod} < 1.09$ at 68\% credibility.

Author
Shah, Paul; Davis, T. M.; Vincenzi, M.; Armstrong, P.; Brout, D.; Camilleri, R.; Galbany, L.; Gill, M. S. S.; Huterer, D.; Jeffrey, N.; Lahav, O.; Lee, J.; Lidman, C.; Möller, A.; Sullivan, M.; Whiteway, L.; Wiseman, P.; Allam, S.; Aguena, M.; Annis, J.; Blazek, J.; Brooks, D.; Rosell, A. Carnero; Carretero, J.; Conselice, C.; da Costa, L. N.; Pereira, M. E. S.; Desai, S.; Diehl, H. T.; Doel, P.; Everett, S.; Ferrero, I.; Flaugher, B.; Frieman, J.; García-Bellido, J.; Gaztanaga, E.; Giannini, G.; Gruen, D.; Gruendl, R. A.; Gutierrez, G.; Hinton, S. R.; Hollowood, D. L.; Honscheid, K.; James, D. J.; Lee, S.; Marshall, J. L.; Mena-Fernández, J.; Miquel, R.; Palmese, A.; Pieres, A.; Malagón, A. A. Plazas; Porredon, A.; Samuroff, S.; Sanchez, E.; Sevilla-Noarbe, I.; Smith, M.; Suchyta, E.; Swanson, M. E. C.; Tarle, G.; Tucker, D. L.; Weaverdyck, N.
Published
2025
Language
EN

More by Shah, Paul; Davis, T. M.; Vincenzi, M.; Armstrong, P.; Brout, D.; Camilleri, R.; Galbany, L.; Gill, M. S. S.; Huterer, D.; Jeffrey, N.; Lahav, O.; Lee, J.; Lidman, C.; Möller, A.; Sullivan, M.; Whiteway, L.; Wiseman, P.; Allam, S.; Aguena, M.; Annis, J.; Blazek, J.; Brooks, D.; Rosell, A. Carnero; Carretero, J.; Conselice, C.; da Costa, L. N.; Pereira, M. E. S.; Desai, S.; Diehl, H. T.; Doel, P.; Everett, S.; Ferrero, I.; Flaugher, B.; Frieman, J.; García-Bellido, J.; Gaztanaga, E.; Giannini, G.; Gruen, D.; Gruendl, R. A.; Gutierrez, G.; Hinton, S. R.; Hollowood, D. L.; Honscheid, K.; James, D. J.; Lee, S.; Marshall, J. L.; Mena-Fernández, J.; Miquel, R.; Palmese, A.; Pieres, A.; Malagón, A. A. Plazas; Porredon, A.; Samuroff, S.; Sanchez, E.; Sevilla-Noarbe, I.; Smith, M.; Suchyta, E.; Swanson, M. E. C.; Tarle, G.; Tucker, D. L.; Weaverdyck, N.

Browse all works by Shah, Paul; Davis, T. M.; Vincenzi, M.; Armstrong, P.; Brout, D.; Camilleri, R.; Galbany, L.; Gill, M. S. S.; Huterer, D.; Jeffrey, N.; Lahav, O.; Lee, J.; Lidman, C.; Möller, A.; Sullivan, M.; Whiteway, L.; Wiseman, P.; Allam, S.; Aguena, M.; Annis, J.; Blazek, J.; Brooks, D.; Rosell, A. Carnero; Carretero, J.; Conselice, C.; da Costa, L. N.; Pereira, M. E. S.; Desai, S.; Diehl, H. T.; Doel, P.; Everett, S.; Ferrero, I.; Flaugher, B.; Frieman, J.; García-Bellido, J.; Gaztanaga, E.; Giannini, G.; Gruen, D.; Gruendl, R. A.; Gutierrez, G.; Hinton, S. R.; Hollowood, D. L.; Honscheid, K.; James, D. J.; Lee, S.; Marshall, J. L.; Mena-Fernández, J.; Miquel, R.; Palmese, A.; Pieres, A.; Malagón, A. A. Plazas; Porredon, A.; Samuroff, S.; Sanchez, E.; Sevilla-Noarbe, I.; Smith, M.; Suchyta, E.; Swanson, M. E. C.; Tarle, G.; Tucker, D. L.; Weaverdyck, N.