deletions | additions       diff --git a/begin_abstract_We_probe_the__.tex b/begin_abstract_We_probe_the__.tex  index 58ff40b..ebed753 100644  --- a/begin_abstract_We_probe_the__.tex  +++ b/begin_abstract_We_probe_the__.tex 
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\begin{abstract}  We probe the systematic uncertainties from the \SNIAPSused~Type Ia supernovae (SN\,Ia) in the \PS~(PS1) sample along with \SNIAlowzused~SN\,Ia from a combination of low-redshift surveys. The companion paper by Rest et al. (2013) describes the photometric measurements and cosmological inferences from the PS1 sample. The largest systematic uncertainty stems from the photometric calibration of the PS1 and low-z samples. We increase the sample of observed Calspec standards from 7 to 10 used to define the PS1 calibration system. The PS1 and \SDSS~calibration systems are compared and discrepancies up to $\sim0.02$ mag are recovered. We find uncertainties in the proper way to treat intrinsic colors and reddening produce differences in the recovered value of $w$ up to $3\%$. We estimate masses of host galaxies of PS1 supernovae and detect an insignificant difference in distance residuals of the full sample of $0.037 \pm 0.031$ mag for host galaxies with high and low masses. Assuming flatness and including systematic uncertainties in our analysis of only SNe measurements, we find $w=$\wSNstasys. With additional constraints from BAO, CMB (Planck) and $H_0$ measurements, we find $w=\wCsys$~and~$\Omega_m=\fomCsys$ (statistical and systematic errors added in quadrature). Significance of the inconsistency with $w=-1$ depends on whether we use Planck or WMAP measurements of the CMB: $w_{\textrm{BAO+H0+SN+WMAP}}=-1.124^{+0.083}_{-0.065}$. measurements.  \end{abstract}