CO luminosity-Linewidth correlation of low and high redshift galaxies and its possible cosmological utilization. (arXiv:1902.02832v1 [astro-ph.CO])

CO luminosity-Linewidth correlation of low and high redshift galaxies and its possible cosmological utilization. (arXiv:1902.02832v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Wu_Y/0/1/0/all/0/1">Yi-han Wu</a> (Nthu), <a href="http://arxiv.org/find/astro-ph/1/au:+Goto_T/0/1/0/all/0/1">Tomotsugu Goto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eser_E/0/1/0/all/0/1">Ece Kilerci Eser</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hashimoto_T/0/1/0/all/0/1">Tetsuya Hashimoto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_S/0/1/0/all/0/1">Seong-jin Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chiang_C/0/1/0/all/0/1">Chia-ying Chiang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huang_T/0/1/0/all/0/1">Ting-chi Huang</a>

A linear correlation has been proposed between the CO luminosity
($rm{L}^{prime}_{rm{CO}}$) and full-width at half maximum (FWHM) for
high-redshift (z > 1) submillimeter galaxies. However, the controversy
concerning the $rm{L}^{prime}_{rm{CO}}$-FWHM correlation seems to have been
caused by the use of heterogeneous samples (e.g., different transition lines)
and/or data with large measurement uncertainties. In order to avoid the
uncertainty caused by using different rotational transitions, in this work we
make an extensive effort to select only CO($J = 1-0$) data from the literature.
We separate these wide-ranging redshift data into two samples : the
low-redshift (z < 1) and high-redshift (z > 1) samples. The samples are
corrected for lensing magnification factors if gravitational-lensing effects
appeared in the observations. The correlation analysis shows that there exists
significant $rm{L}^{prime}_{rm{CO}}$-FWHM correlations for both the
low-redshift and high-redshift samples. A comparison of the low- and
high-redshift $rm{L}^{prime}_{rm{CO}}$-FWHM correlations does not show
strong evolution with redshift. Assuming that there is no evolution, we can use
this relation to determine the model independent distances of high-redshift
galaxies. We then constrain cosmological models with the calibrated
high-redshift CO data and the sample of Type Ia supernovae in the Union 2.1
compilation. In the constraint for wCDM with our samples, the derived values
are w_{0} = -1.02 {pm} 0.17, {Omega}_{m0} = 0.30{pm}0.02, and H_{0} = 70.00
{pm}0.60 km,s^{-1},Mpc^{-1}.

A linear correlation has been proposed between the CO luminosity
($rm{L}^{prime}_{rm{CO}}$) and full-width at half maximum (FWHM) for
high-redshift (z > 1) submillimeter galaxies. However, the controversy
concerning the $rm{L}^{prime}_{rm{CO}}$-FWHM correlation seems to have been
caused by the use of heterogeneous samples (e.g., different transition lines)
and/or data with large measurement uncertainties. In order to avoid the
uncertainty caused by using different rotational transitions, in this work we
make an extensive effort to select only CO($J = 1-0$) data from the literature.
We separate these wide-ranging redshift data into two samples : the
low-redshift (z < 1) and high-redshift (z > 1) samples. The samples are
corrected for lensing magnification factors if gravitational-lensing effects
appeared in the observations. The correlation analysis shows that there exists
significant $rm{L}^{prime}_{rm{CO}}$-FWHM correlations for both the
low-redshift and high-redshift samples. A comparison of the low- and
high-redshift $rm{L}^{prime}_{rm{CO}}$-FWHM correlations does not show
strong evolution with redshift. Assuming that there is no evolution, we can use
this relation to determine the model independent distances of high-redshift
galaxies. We then constrain cosmological models with the calibrated
high-redshift CO data and the sample of Type Ia supernovae in the Union 2.1
compilation. In the constraint for wCDM with our samples, the derived values
are w_{0} = -1.02 {pm} 0.17, {Omega}_{m0} = 0.30{pm}0.02, and H_{0} = 70.00
{pm}0.60 km,s^{-1},Mpc^{-1}.

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