Constraints on $H_0$ from WMAP and baryon acoustic osillation measurements. (arXiv:1812.01877v1 [astro-ph.CO])

<a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_X/0/1/0/all/0/1">Xue Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huang_Q/0/1/0/all/0/1">Qing-Guo Huang</a>

We report the constraints of $H_0$ obtained from Wilkinson Microwave

Anisotropy Probe (WMAP) combined with the latest baryonic acoustic oscillations

(BAO) measurements. We use the BAO measurements from the 6dF Galaxy Survey

(6dFGS), the SDSS DR7 main galaxies sample (MGS), the BOSS DR12 galaxies and

the eBOSS DR14 quasars. Adding the recent BAO measurements to the cosmic

microwave background (CMB) data from WMAP, we constrain cosmological parameters

$Omega_m=0.298pm0.005$, $H_0=68.36^{+0.53}_{-0.52}$ km s$^{-1}$ Mpc$^{-1}$,

$sigma_8=0.8170^{+0.0159}_{-0.0175}$ in a spatially flat $Lambda$ cold dark

matter ($Lambda$CDM) model, and $Omega_m=0.302pm0.008$, $H_0=67.63pm1.30$

km s$^{-1}$ Mpc$^{-1}$, $sigma_8=0.7988^{+0.0345}_{-0.0338}$ in a spatially

flat $w$CDM model, respectively. The combined constraint on $w$ from CMB and

BAO in a spatially flat $w$CDM model is $w=-0.96pm0.07$. Our measured $H_0$

results prefer a value lower than 70 km s$^{-1}$ Mpc$^{-1}$, consistent with

the recent data on CMB constraints from Planck (2018), but in $3.1sim

3.5sigma$ tension with local measurements of Riess et al. (2018) in

$Lambda$CDM and $w$CDM framework, respectively. Compared with the WMAP alone

analysis, the WMPA+BAO analysis reduces the error bar by 75.4% in $Lambda$CDM

model and 95.3% in $w$CDM model.

We report the constraints of $H_0$ obtained from Wilkinson Microwave

Anisotropy Probe (WMAP) combined with the latest baryonic acoustic oscillations

(BAO) measurements. We use the BAO measurements from the 6dF Galaxy Survey

(6dFGS), the SDSS DR7 main galaxies sample (MGS), the BOSS DR12 galaxies and

the eBOSS DR14 quasars. Adding the recent BAO measurements to the cosmic

microwave background (CMB) data from WMAP, we constrain cosmological parameters

$Omega_m=0.298pm0.005$, $H_0=68.36^{+0.53}_{-0.52}$ km s$^{-1}$ Mpc$^{-1}$,

$sigma_8=0.8170^{+0.0159}_{-0.0175}$ in a spatially flat $Lambda$ cold dark

matter ($Lambda$CDM) model, and $Omega_m=0.302pm0.008$, $H_0=67.63pm1.30$

km s$^{-1}$ Mpc$^{-1}$, $sigma_8=0.7988^{+0.0345}_{-0.0338}$ in a spatially

flat $w$CDM model, respectively. The combined constraint on $w$ from CMB and

BAO in a spatially flat $w$CDM model is $w=-0.96pm0.07$. Our measured $H_0$

results prefer a value lower than 70 km s$^{-1}$ Mpc$^{-1}$, consistent with

the recent data on CMB constraints from Planck (2018), but in $3.1sim

3.5sigma$ tension with local measurements of Riess et al. (2018) in

$Lambda$CDM and $w$CDM framework, respectively. Compared with the WMAP alone

analysis, the WMPA+BAO analysis reduces the error bar by 75.4% in $Lambda$CDM

model and 95.3% in $w$CDM model.

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