Calibrating effective Ia supernova magnitudes using the distance duality relation

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• 作者：Jarah Evslin ^{jarah@impcas.ac.cn" class="auth_mail" title="E-mail the corresponding author}
• 关键词：Baryon acoustic oscillations ; Supernova ; Distance/duality relation
• 刊名：Physics of the Dark Universe
• 出版年：2016
• 出版时间：December 2016
• 年：2016
• 卷：14
• 期：Complete
• 页码：57-64
• 全文大小：508 K

文摘

Using only Ia supernova (SN) observations, it is not possible to distinguish the evolution of the SN absolute magnitude M_B$M_B$ from an arbitrary evolution of the Hubble parameter H(z)$H\left(z\right)$. However, using Etherington’s distance-duality relation, which relates the angular and luminosity distances, together with the observed angular baryon acoustic oscillation (BAO) scale at any redshift z$z$, one may calibrate an effective M_B(z)$M_B\left(z\right)$. This calibration involves a scale which depends on the cosmological model, however the evolution of the effective M_B(z)$M_B\left(z\right)$ between two redshifts with BAO observations is independent of this scale. The line of sight BAO scale can be used to extend this calibration to redshifts near z$z$. As an application, using BOSS BAO at z=0.32$z=0.32$ and 2.34, JLA supernova at low z$z$ and Hubble Space Telescope SN at z>1.7$z>1.7$, we find a statistically insignificant downward shift M_B(2.34)−M_B(0.32)=−0.08±0.15$M_B\left(2.34\right)-M_B\left(0.32\right)=-0.08\pm 0.15$. Replacing BOSS data with the best fit Planck Λ$\Lambda$CDM BAO expectations, we find a shift of −0.24±0.13$-0.24\pm 0.13$. With the SN that will be observed by the James Webb Space Telescope, such a calibration at ae3e9" title="Click to view the MathML source">z=2.34$z=2.34$ will be more precise, and it will serve as an anchor for cosmological analyses with the SN that it will observe at yet higher z$z$.